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40inch Telescope

Overview

In the early 1960s, the Australian National University established a new astronomical site at Siding Spring in central New South Wales, partly in the expectation that it would provide somewhat clearer skies than those at Mount Stromlo, and partly to escape the increasing light pollution of the growing Canberra. The selection of Siding Spring followed an extensive site-testing programme organized by the then Director, Bart Bok. The new site was instrumented with three reflectors of modest size, all made by Boller & Chivens. The 40-inch is the largest of these, the other two being a 24-inch and a 16-inch. The 40-inch is heavily scheduled, and it has proved a useful instrument especially for photometric and imaging work.

Specifications

40inch (1.0m), f/5 primaryRitchey-Chritien opticsSecondaries for f/8 and f/18 Cassegrain imaging ( ~8100mm and ~18300mm focal length )German Equatorial mount

Telescope Control

ETS Manual (24,30 & 40in)Instrument Computer link to ETS

Instruments

Direct Imaging"Wide Field Imager (WFI)"

Andrew Jacob User Notes

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ANU - Research School of Astronomy and Astrophysics - RSAA http://www.mso.anu.edu.au/observing/ets_manual.php

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Page last updated: 07 January 2005Please direct all enquiries to: Webmaster



ETS_LINK http://www.mso.anu.edu.au/observing/ets_link.html

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J. van Harmelen, 17-NOV-1988, V3.1J. van Harmelen, 1993, V4.0 View Command addedJ. van Harmelen, 25 October 1996, V4.1 Configure Command added, general review.J. van Harmelen, 7 July 1999 V4.2 Other Telescope Commands added Autoguide Command added, Status Command addedJ. van Harmelen, 12 July 2000 V4.3 Added “Halt” command for small telescope control systems

SPECIFICATION OF A CONNECTION BETWEEN TELESCOPE AND INSTRUMENTCOMPUTERS

(ETS_LINK)

1. SCOPEThis document relates to the connection of stand alone instrument control computers to telescope control computers for the purposeof conveying telescope coordinate and time information. Other information and control commands have been added to the list ofcommands.

It does not concern instrument control by VAX computers, either by the telescope computer itself, or by other networked VAX’s,as user programs have access to telescope data and can control the telescope by the methods described in the 2.3m TelescopeObserver’s Manual (Chapter 12). The use of a dedicated serial line for this purpose should be regarded as a simple and convenient solution for the desired dataexchange. At a later time network connection will considered.

2. HARDWAREThe Telescope and Instrument computers are to be connected by R5232 ports, operating at 9600 bps, no parity, one stop bit. On a VAX this will be a general purpose terminal port, on a PDP11/24 port SLU2:, on other PDPll’s a comparable port with thesame address as SLU2:, on other computers a convenient serial port.

3. DATA EXCHANGE PROTOCOLAll data exchange will be in ASCII format. The Instrument computer is the master of the datalink: it requests information when needed, by sending a command to theTelescope computer, which will then reply with the requested data, or with an error message. The Telescope computer is available for exchange of information at any time while the telescope system is running. When thetelescope system is not running, there will be no reply from the telescope computer to any Instrument computer commands. Theinstrument computer software shall implement a time-out to cope with this condition.


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4. COMMAND AND DATA FORMATSThe command and reply repertoire described below is thought to cover the requirements of most existing instruments which arecontrolled by their own computer systems, but may need future extension. The CONFIGURE and VIEW commands are two suchextensions. The VAX Telescope computers use DCL parse routines and will generate the error message "UNRECOGNISED COMMAND" ifthe commands can not be recognised. Other types of telescope control computers shall mimic the behaviour of a VAX/VMSmachine as much as possible. All systems implement as a minimum the TELESCOPE, COORDINATES, TIME and VIEWcommands. Commands which control the telescope are only implemented on a needs basis. A command or qualifier can be abbreviated to the minimum number of characters necessary to uniquely identify it, but not to lessthan two characters, and has to be terminated with a carriage return <CR>. No more than four characters shall be required touniquely identify a command or qualifier. The command strings are not case sensitive. All replies are terminated with a <CR><LF> combination. All alphabetic information in the reply messages will be in capitals. The commands TELESCOPE, COORDINATES, TIME, VIEW and CONFIGURE are available together with qualifiers to indicatewhich coordinates or time are required, and whether the reply values will be in ’string’ or ’real’ format. 4.1 CONFIGURE

The command: CONFIGURE configuration_variable value shall be accepted by the telescope system as if it were issued on the command line at the telescope control terminal, or theequivalent information entered in the configuration dialog in menu driven systems. Refer to the Telescope Manuals for furtherdetails. A <CR><LF> reply indicates successful completion of the command, any error is signalled with the reply: UNRECOGNISED COMMAND. A special case is the control of the Dome_Control configuration variable, which on successful completion reports the previousvalue: DOME_CONTROL WAS MANUAL or DOME_CONTROL WAS AUTOMATIC This addition to the command repertoire introduced in version 4.1 has only been implemented on the 74” and 50” telescopesystems. Other systems will be revised as need for this command arises.

4.2 COORDINATES

If the telescope is tracking, this command causes the telescope computer to reply with the message: "object name" ra dec equinoxstring The object name is only included if available, and is always in capitals and enclosed in double quotation marks. The format of RA and DEC variables depends on the format qualifiers and is described in detail under the /REAL and /STRINGheaders. The equinox string contains seven or eight characters: the FK4/FK5 identifier "B" or "J", followed by the epoch as "yyyy.y"(seven characters), or the string "APPARENT" (eight characters) when apparent place is selected for the telescope display. If the telescope is not tracking, an error message is generated: TELESCOPE NOT TRACKING If the coordinate data are inaccessible or suspect, the reply is: DATA ACCESS ERROR

/BASEThe requested coordinates are Base Coordinates (refer to 2.3m Telescope Observer’s Manual for definition). (Not available ontelescopes which do not support the TRACK command)

/FILEThe requested coordinates are File Coordinates (refer to 2.3m Telescope Observer’s Manual for definition). (Not available ontelescopes which do not support the TRACK command)

/TRACK (default)The requested coordinates are the current telescope Tracking Coordinates (refer to 2.3m Telescope Observer’s Manual fordefinition).

/REAL


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RA and Dec are supplied in ASCII representation of their floating point values: 0 < RA < 2*PI, format: r.rrrrrr -PI/2 < Dec < PI/2, format: sd.dddddd (s=sign) The sign is only included if it is negative.

/STRING (default)RA and Dec are supplied in string format: RA: hh mm ss.d Dec: sdd mm ss (first s=sign) If the information is inaccessible or suspect, the reply is: DATA ACCESS ERROR

4.3 TIME

This command causes the telescope computer to reply with the message: mjd sidereal_time selected_time selected_date "mjd" is the Modified Julian Date (defined as JD - 2400000.5) in the format: ddddd.dddddd"sidereal_time" is Local Apparent Sidereal Time"selected_time" is either Universal Time or Civil Time as specified by the qualifiers /UT and /CT. The format of "sidereal_time" and "selected_time" variables depends on the format qualifiers and is described in detail underthe /REAL and /STRING headers. "selected_date" is either UT Date or Civil Date as specified by the qualifiers /UT and /CT.The "selected_date" is returned in string format: dd-mmm-yyyy If the time information is inaccessible or suspect, the reply is: DATA ACCESS ERROR

/CTThe "selected time" variable is returned as Civil Time: Australian Eastern Standard Time or Australian Eastern DaylightsavingTime as applicable (UT + 10, resp UT + 11 hours).

/UT (default)The "selected time" variable is returned as Universal Time.

/REAL

selected_time and sidereal time are supplied in ASCII representation of their floating point values: 0 < time < 2*PI format: t.tttttt

/STRING (default)selected time, which is UT or Civil Time depending on the /UT and /CT qualifiers, and sidereal time are returned in stringformat: hh:mm:ss.s in the range 0 to 24 hours.

4.4 TELESCOPE

This command causes the telescope computer to reply with an identification message: tel_id_string astr_latitude astr_east_longitude height_AMSL "tel_id_string" is the site and telescope identifier, a fixed length string of fifteen characters left justified, in the format: SSO 2.3METRE or MSO 74INCH etc. "astr_latitude" and " astr_east_longitude " are the astronomical latitude and east longitude in decimal degrees in the format: sdd.ddddd and ddd.ddddd (s=sign) "height_AMSL" is the integer value of the height above sea level of the telescope in metres: hhhhh

4.5 VIEWThe VIEW command permits an observer to see the value of any telescope display variable(even if it is not currently featured on one of the display screens). The command: VIEW variablename [,...]


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causes the names, values (and units where appropriate) of the specified display variable(s) to be returned. A list of displayvariable names for your telescope can be found in the chapter ’Telescope Display’ in your Telescope Observer ’s Manual. Thedetails of the format of the returned data vary with the type of data requested. Rather than trying to detail all possible cases here,it is recommended to obtain the data by typing in the VIEW command at the control terminal of the 2.3m, 74” or 50”telescopes.

Examples: command: reply: TELESCOPE SSO 2.3METRE -31.27336 149.06119 1149 TEL MSO 74INCH -35.32065 149.02433 768 COORDINATES "B CENT" 14 03 00.3 -60 19 05 51988.5 COORD/REAL "BCENT" 3.678281 -1.052749 J1988.5 COORD 12 34 56.7 +06 54 32 B1950.0 COORD TELESCOPE NOT TRACKING TIME 47465.711806 05:41:57.1 17:05:00.0 31-OCT-1988 TIME/CT 47465.711806 05:41:57.1 04:05:00.0 1-NOV-1988 TIME/REAL/CT 47465.711806 1.492038 1.060288 1-NOV-1988 4.6 OTHER TELESCOPE COMMANDS (2.3m, 74” and 50”)

Any telescope command can be given and will be executed. The reply for successful commands is just a <CR>, for unsuccessfulcommands the error message UNRECOGNISED COMMAND plus the body of the VMS error message generated by the controlsystem. On the 2.3m problems with the delivery of error messages have not yet been solved. It is not possible to discern acommand failure.

4.7 TRACK/COORDINATE, OFFSET[/BASE] and HALT COMMANDS (40”, 30” and 24”)For those small telescopes which operate under computer control (40”and 24” to be implemented in winter 2000), thefollowing telescope commands are supported: “TRACK/COORDINATE coordinates” (in standard MSSSO format),“OFFSET ra dec”, “OFFSET/BASE ra dec”, and HALT. The reply for successful commands is just a <CR>, forunsuccessful commands the error message UNRECOGNISED COMMAND plus the body of the VMS style error messagegenerated by the control system.

4.8 AUTOGUIDE COMMAND (2.3m only)The “AUTOGUIDE ew ns” command puts the sky offsets supplied into the autoguider offset fields of the control database. Thetelescope will react to this on the next control loop. 4.9 STATUS COMMANDThe telescope control system will reply to the “STATUS” command with one of the following strings indicating the currenttelescope status: “OFF”, “FAULT”, “HALTED”, “WAITING”, “SLEWING”, “TRACKING”. External systemscontrolling the telescope should use this command to determine when to continue with the next phase of their control program.


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5. IMPLEMENTATION ON THE TELESCOPE COMPUTERSThe implementation of the instrument connection on the VAX Telescope computers takes the form of a process as part of thetelescope system. The designated serial port is allocated to this process. The process reads from the port and waits till a commandarrives. DCL parse routines are used to decode the command, the reply string is assembled from information taken from thetelescope database, where necessary using the telescope library routines to do data conversions, and then written out to the port. On other telescope computer types the actions of the VAX computers shall be imitated as closely as possible. The communicationport used shall be polled frequently enough not to produce any noticeable delay in reply or be interrupt driven.

6. IMPLEMENTATION ON INSTRUMENT COMPUTERSThe implementation of the instrument connection on PDP11 Instrument computers uses an RT11 device handler to communicatewith the serial port. The instrument control program will contain a subroutine which writes the required commands to the port anddecodes from the received reply string theinformation it requires. On other types of instrument computers there is no prescribed method of implementation. The use of reply parsing routines whichare character position dependent is to be discouraged. Small differences in replies between types of telescope computers arepossible and should be coped with. Examples of these differences are the number of significant digits in scientific notation ofvariable values returned by the VIEW command and the number of spaces separating fields.

40inch Direct Imaging http://www.mso.anu.edu.au/observing/40in/DirectIm/#overview

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40inch Direct Imager

This manual describes the operation and specifications of the direct imager on the 40inch telescope at SSO.

The imager is suitable for optical imaging at pixel scales of 0.4-0.6"/pixel, depending on the CCD. The MSODetector Lab has a list of currently available CCDs. The automated 6-position filter wheel is normally usedwith standard UBVRI filters, but can be loaded with observer-provided 50??mm filters if required.

A f/18 secondary is also available, however the focal scale (0.2-0.3"/pixel) and typical SSO seeing mean thatit seldom used.

Instrument Capabilities OverviewFiltersSensitivity

ObservingGetting Going Quickly The AutoGuiderObserving ProceduresFault reportsObserving Report

Software CommandsInstrument ControlDetector ControlTelescope Control

Data ReductionImaging

ResourcesPhotometric StandardsTerrestrial Atmospheric Transmission

Imager HardwareOptical DesignDetectorElectronic Control SystemMechanical Design

Intrument CapabilitiesOverviewThe imager is suitable for optical imaging at pixel scales of 0.4-0.6"/pixel, depending on the CCD. The MSODetector Lab has a list of currently available CCDs. A f/18 secondary is also available, however the focalscale (0.2-0.3"/pixel) and typical SSO seeing mean that it seldom used.

FiltersThe filter wheel can hold six 50??mm filters and is normally used with standard UBVRI(+clear) filters. It canbe loaded with observer-provided filters if required. The filter wheel is fully controllable from the observingsoftware, Cicada.A f/18 secondary is also available, however the focal scale (0.2-0.3"/pixel) and typical SSO seeing mean thatit seldom used.

SensitivitySensitivity data is sparse. Measurements made in late 1993 indicate about 20 and 15 electrons/sec for a 20thmagnitude star, in V and I respectively. Figures for newer CCDs are unknown.

ANU - Research School of Astronomy and Astrophysics - RSAA http://www.mso.anu.edu.au/observing/detectors/current_info.php

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Dewar numbers Dn indicate re-furbished heads.

Detector

Dewar

Type Frame Format

Pixel Size

Read Noise(e) Details

SiTE 2k D10 Tek 2048x2048 24um 12 thinned, on 40" f/8

E2V CCD4210 D11 E2V

Imaging: 2048x512

Frame: 2148x562

13.5um(Full Well

~120ke)

3.5(G=2)4.65(G=3)

thinned, R/O time 7s, on 2.3m

telescopeNew DBS-B

(Old Tek 1kx1k)

E2V CCD4240 D6 E2V

Imaging: 2048x2048

Frame: 2148x2148

13.5um(Full Well

~120ke)

4.4(G=2)3.6(G=1)


telescope New Imager

(Old EEV 2kx1k)

E2V CCD4210 D7 E2V

Imaging: 2048x512

Frame: 2148x562

13.5um(Full Well

~120ke)

3.5(G=2)4.65(G=3)


telescopeScience

Detector will be installed on

May 9thCommissioning:

Delayed till early June

New DBS-R(Old Tek

1752x532)

DBS-R D9 SiTE 1752x532 15um 5

grade 1, DBS only.

This head to be retired

E2V Imager Timing Files and Gain SettingsFor the Imager, fast = medm = slow, the detector is read-out at the same speed i.e. about 15 seconds. There is now NO slow or medium speed with the new Imager.So the DEFAULT, 2.4e/adu lod file is - fast.lod

ANU - Research School of Astronomy and Astrophysics - RSAA http://www.mso.anu.edu.au/observing/detectors/current_info.php

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The GAIN setting of the Imager may now be changed using the GAIN option on the Cicada Menu, rather than re-loading a timimg file

The gain settings and noise are as follows

GAIN CDS Gain System Gain(e/adu) Noise(e) Bias Comment

0 9.5 0.53 4 -- Very Hi Gain

1 4.75 1.1 3.6 1343 Hi Gain

2 2 2.4 4.4 1190 Default

3 1 5.6 6.8 -- Low Gain

DBSB Timing Files and Gain SettingsFor the DBSB, fast = medm = slow, the detector is read-out at the same speed i.e. about 7 seconds. There is now NO slow and medium speed with the new DBSB (or DBSR) So the DEFAULT, 1.04e/adu lod file is - fast.lod

However, the GAIN setting of the system may be changed according to the table below -

The gain settings and noise are as follows

GAIN CDS Gain System Gain(e/adu) Noise(e) Bias Comment

1 4.75 0.45 9 -- Hi Gain

2 2 1.04 3.5 1230 Default

3 1 2.35 4.65 1241 Low Gain

Enquiries about Current Detector [email protected]


Page last updated: 06 May 2005Please direct all enquiries to: Webmaster



A short user’s guide to the http://www.mso.anu.edu.au/observing/40in/DirectIm/40in/

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A short user’s guide to the 40-inch and its CCD-camera system

April 1999

This document describes the basics of the use of the 40-inch for CCD imaging. It is recommended that it beread in its entirety before the observing run commences.

1 Before you start

Some things which should be done early in the afternoon before you start your run:

Check that the CCD/Dewar you want is on the telescope and is cold.1.Check that the LN2 dewar is in the dome and full enough to do a couple of fills. If it is Friday it will

need to last over the weekend. Hold times for the large dewars is 18-22 hours, the smaller ones hold forup to 12 hours.

2.

Check that the filters that you need have been installed in the filter wheel in their correct positions.3.Check that you can run CICADA (see Section 3) and can write files to the data disk.4.Make sure you have tapes and can write to them with the tape drive.5.Check that the CCD sees light. Verify that the gain and readout speed is what you want and that thebias levels and RON are reasonable (bias is typically 600-1200 ADU).

6.

Check that the telescope computer and TCS is running and reading the coordinates.7.Check that you can move the telescope. (see Section 2). Check that when the telescope is tracking and you do an exposure that the FILTER and RA and DEC are written to the fits headers of your files.

8.

In all cases, if you have problems - contact the technicians as early as possible.

2 Starting up and using the telescope

3 Starting up and using Cicada

4 Shutting things down

Once your flats and biases are taken:

replace the telescope lid, and close the dome slit.1.TURN OFF THE TRACKING so the telescope doesn’t run into the floor.2.fill the CCD dewar so you don’t have to get up just to fill it before the vacuum is degraded.3.write in the weather log book, and dim the lights.4.submit any faults to the so the technicians can work on it during the morning.5.watch the sunrise, go to the lodge, and go to sleep.6.

5 General Tips about observing with the 40’’

6 Troubleshooting

Loud alarm goes off while slewing

You’ve slewed past the RA axis limit.

A short user’s guide to the http://www.mso.anu.edu.au/observing/40in/DirectIm/40in/

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Hit alarm off button (the sound yet won’t stop yet)1.Hold down the top of the horizontal limit button while2.slewing in the direction opposite to what got you in trouble in the first place. Once the telescopeis back within the limits, the alarm will stop.

3.

Dome won’t rotate

Dome being domes, get stuck sometimes.

Try rotating the dome back in the opposite direction until it gets unstuck, then try again.1.If the dome is completely stuck, the circuit-breakers might have tripped. To check, try theflourescent switch under the dome shutter - if the lights don’t go on then you have to reset thecircuit breakers. Go to the ground floor and check all the breakers in the loading dock area.

2.

If that didnt work, fuses might be blown or worse, and the technicians will have to fix it.3.

You can’t find any of your objects, well-known bright stars, globular clusters nor even the Moon.

The telescope pointing calibration is bad.

If you used the 1996 Astronomical Almanac Bright Stars section to calibrate your pointing, goback and do it again using a *different* year’s edition of the Astronomical Almanac. The 1996Almanac Bright Star coordinates are incorrect.

1.

see section on Pointing2.

7 Acknowledgements

This document is an (updated) compendium of various user guides written over the years. Thanks go to thefollowing people for their earlier guides, upon which much of this document is based.

Mike Bessell, Jayanne English, Albert Bosma, Garry Kitley and Helmut Jerjen.

Version InformationV1.1: 990404, Kim Sebo: Updated and rearranged for inclusion on the WWW,including notes from Helmut Jerjen, and autoguider info fromMike Bessell.V1.0: 970922, Mike Bessell: original version based on the combined notesof Jayanne English, Albert Bosma, Garry Kitley and others.

File translated from TEX by TTH, version 2.25.

On 25 May 1999, 21:54.

RSAA - Computing - Cicada http://www.mso.anu.edu.au/computing/cicada/

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CICADA PROJECT DOCUMENTATION

Requirements Specification

Functional Specification

CICADA Design

CICADA V3.1 User’s Manual (postcript)

CICADA V3.1 Writing Plug-Ins (postscript)

CICADA V3.1 Configuration Manual (postscript)

Graphing and Imaging Tool V3.0 User’s Manual (postscript)

CICADA ADASS ’96 Paper

CICADA ADASS ’98 Paper (postscipt)

CICADA System Documentation (in prep)

Cicada binaries

GSFind Manual V2.0 (postscript)

AAO 6dF V1.0 (postscript)

Pipeline Manual V1.0 (postscript)

Pipeline ADASS 1998 Paper (postscript)

Developer Notes

Configuration Manager

Testing

Versions





ccdrs http://www.mso.anu.edu.au/computing/cicada/ccdrs/ccdrs/ccdrs.html

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MOUNT STROMLO & SIDING SPRING OBSERVATORIES CCD/2.2 Computer Section 2.2

17 June, 1994

CCD User Interface Software -- Requirements Specification

PurposeThe CCD User Interface System (CUIS) will provide access to, control of, and retrieval of data from, theCCD detectors attached to instruments mounted on observatory telescopes. User access will be in the contextof a scheme whereby users will access software at the telescope through a workstation similar to those usedfor data reduction at MSO. [This scheme will be specified in a separate paper.]

RationaleThe existing situation with the CCD systems is that they are controlled through i386 or i486 systems runningInteractive Unix. The observer enters commands into these systems via keyboard and tablet, views output ontwo monitors (image and data). This system has a number of shortcomings relating to the specific hardware(tablet, and monitors) that are required. There is also a proliferation of keyboards and monitors in theobserving rooms. The user interface is quite specific to the Astromed controller, and would need to bereplaced when a controller from another source was introduced.

CUIS will allow the observer to operate the CCD from a standard workstation through a window-basedinterface, using a keyboard and mouse for input. The same workstation will be used for other tasks, such asdata reduction, telescope control, and more mundane tasks such as email.

The observer will be dealing with a computer system much like that in his office, and will have fewer(ideally, one) workstations to access.

CapabilitiesThe CUIS will:

Be the point from which the observer will enter commands to be transmitted to the CCD controller.1.Provide the observer with a means of monitoring the CCD.2.Collect data from the CCD, storing it on both disk and removable media.3.Provide technical staff with a means of testing the CCD.4.Provide the above capabilities for multiple CCD systems on a given telescope.5.Be designed to adapt to future CCD controllers, while presenting the same interfact to users.6.

[ The CUIS will not provide data analysis capabilities. These will be provided by standard analysis packages ,such as IRAF or Figaro.]


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Technical Constraints

Throughput

Data throughput will be comparable to or better than that of the Astromed system in use in October 1993,with regard to

read out1.display2.file archiving3.

External Standards

Data files written to tape, or to disk for access by other software systems, will be in FITS format.1.Windowing will be based on X. OpenWindows may be used initially; Motif at a later stage.2.

Configuration

Hardware

The present CCD controller is an EISA card in a i386 or i486 system, which is connected to theworkstation is via ethernet. Future controllers may operate through an S-bus card on the ethernet, orother similar configuration.

1.

The CUIS will run on a Sun (or similar Unix-based) workstation. Currently Sun IPC’s are used.2.

Operating System

The workstation will run Unix. Currently SunOS 4.1.3 is used. The system will operate under Solaris2.3 as well. The design will anticipate the possibility of Unix from other vendors.

1.

The ix86 systems run Unix.2.The windowing software will be based on X11.3.

Third-Party Software

The present CCD controller on the ix86 uses software provided by Astromed. Future controllers willprobably be supplied by the manufacturer with low-level software.

1.

IRAF - compatible image display software (e.g. SAOimage or Ximtool.)2.

UsersThe CUIS will be used by observers -- both MSO staff and visitors. All users can be assumed to be frequentcomputer users, and have familiarity with some windowing systems, but they will vary widely in the depth oftheir knowledge of Unix and X11. Furthermore there will be a wide range in knowledge of the functioning ofthe CCDs themselves.

The CUIS will be used by people who have been up all night and may not be too wide awake. Appropriatefail-safe features will be included.

Tasks


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The CUIS will provide the tools for the user to perform a number of tasks, including initialising the CCD,setting exposure parameters, initiating exposures, monitoring the system, and archiving data. The completelist of tasks is given in the Functional Specification (CCD/1).

DocumentationDocumentation will include

On-line manual pages in the standard Unix format.1.Tutorial documentation available in hard copy at the telescopes, aimed especially at casual users.2.On-line help available from window system menus. These will incorporate hypertext cross-referencingwhere appropriate.

3.

Technical Risks[This section itemises those areas where problems may arise which would make it difficult to meet therequirements.]

Technical difficulties

The Unix implementation on the ix86 (Interactive Unix v 2.x) is not robust.

External Dependencies

The system depends on the Astromed software and controller.

Certainty of requirements

The CUIS will be used by observers with a range of requirements. Some of these requirements may not beidentified or articulated until the system is put into use.

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The command line arguments were: latex2html -init_file /opt/local/html/latex2html/cicada.init ccdrs.tex

The translation was initiated by Super-User on 2001-10-12

ccdfs http://www.mso.anu.edu.au/computing/cicada/ccdfs/ccdfs/ccdfs.html

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MOUNT STROMLO & SIDING SPRING OBSERVATORIES CCD 1.2 Computer Section

2 August 1994

CCD User Interface System - Functional Specification

Contents

ContentsIntroductionRequired features of the MSSSO CCD User Interface System

General RequirementsSet up and Data AcquisitionData OutputSystem Status Information

About this document ...

IntroductionThis document describes the required functionality of the CCD User Interface System (CUIS)which is to be developed by the MSSSO Computing Section. The operation of eachcomponent of the system is described in general terms -- the details of how each operation isto be implemented are beyond the scope of this document. However, it is envisaged that thesoftware will be written in C++ and/or C with code written for CCD controllers as required.The eventual aim is that the system will run under Solaris 2 on a Sun workstation with thegraphical part of the interface built using the Motif widget set.

Required features of the MSSSO CCD User Interface SystemThis section lists, in no particular order, those features of any CCD user interface whichwould be required before such a system could be considered useful to observers usingMSSSO CCDs.

General Requirements


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The following requirements are taken from the CUIS Requirements Specification.

provide a common interface to all CCD systems regardless of CCD-vendor supplied hardware orsoftwaredeliver the images to the image tool, disk and/or tape in similar amount of time to the current Astromed3200 system.a Graphical User Interface (GUI) which adheres to de-facto standards for the ‘‘look and feel’’ of suchan interface. The idea being that observers are presented with an interface which operates in a wayfamiliar to users of Openwindows.provide on-line ‘‘help’’provide LARGE exposure counters, audible end-of-exposure alarmsuse colour coded windows and widgets adhering to Australian Standards for layout and colour ofcontrol panels. This will ensure that the CCD interface and the telescope control system will be usingthe same colour codings for warnings, errors, OK status, etc.

Set up and Data Acquisition

provide facilities for technical staff to test CCDs and fine tune the hardware setup of CCD controllersprovide a focussing ‘‘mode’’. (e.g. the system takes a series of exposures at different focus settingsallowing the observer to see the results of each exposure. During the focus exposures the telescopefocus is altered manually or automatically depending on the observers preference and/or thesophistication of the CCD system/Telescope Control system interface.) Software must be providedwhich will calculate Point Spread Functions and assist the observer to obtain the best focus.ability to define and read out regions of the CCD. Interaction (using the mouse) with the Image DisplayTool will allow for rectangular regions to be specified on a previously taken image. The number ofregions which can be specified will be limited by the capabilities of the CCD controller.ability to alter the row and column binning of CCD pixels. This will permit different binning indifferent regions where the CCD controller allows thisinitialise the CCD hardware.provide a facility to perform drift-scan exposures. This will mean being able to read out one row of theCCD upon receipt of a signal from the telescope control system.provide facilities for performing time-resolved imaging and spectroscopyallow for control of multiple CCD systems (e.g. as in operation at the DBS). This will requiresynchronising the start of exposures on multiple CCD controllers. Status information from the multiplecontrollers will be required. Multiple fits files will be written. (For the DBS, allowance will be madefor use of only one side of the DBS and for different exposure times to be specified for each CCDcontroller.)allow for exposures to be interrupted and restarted or aborted and allow for exposure times to bechanged when an exposure has been ‘‘paused’’allow for exposures to be automatically repeated. The number of such exposures will be set by theobserver.provide the observer with the facility to vary the number of flushes performed before each exposureAllow for the use of table-driven sequences of instructions (e.g. a series of exposures, changing filtersbetween exposures). The system will provide a standard set of such tables and allow the observer tospecify new sequences.provide filter wheel control where this is available on the CCD controller.provide basic graphical image analysis tools to help with checking data quality, calculation of requiredexposure times, etc. Such tools will include summing a number of rows or columns and producing aplot of the data.provide facility to save and reload an individual observer’s set-up files. Data such as default imagedirectories, optional fits header keywords, the observer’s own sets of instruction sequences, observerdefined CCD regions will be held in such a file

Data Output

write fits files with header information obtained from the telescope and the observer. This will includeobject name (from the telescope system) where possible


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allow for all hardware set-up information to be included in fits headers.allow observer to select from all available possible fits header keywords. There will be a minimum setof ‘ ‘mandatory’ ’ keywords (e.g. RA, Dec, dates) and many specialised keywords (e.g. CCD hardwareinfo) from which the observer can choose. The set of required keywords will be stored in the usersset-up file.place fits files in a user specified directory. This will allow the observer to place images in the /homearea or on one of MSSSO’s data or book disksallow the observer to specify a fits filename to which <run number>.fits will be appended.display details of available disk space

System Status Information

provide feedback on system status. This includes such things as voltages and temperatures as well asthe ‘ ‘dead or alive’ ’ status of any software sub-processesprovide feedback on progress of exposures, readouts, initialisation (even when window is ‘ ‘ iconified’ ’ )provide a restart facility should any part of the system fail. This will include advice to the observer thatan error has occurred and that part or all of the system should be restarted. Of course, whereverpossible, any error recovery will be carried out without requiring any action on the part of the observer.



The command line arguments were: latex2html -init_file /opt/local/html/latex2html/cicada.init ccdfs.tex


cicada_design2 http://www.mso.anu.edu.au/computing/cicada/cicada_design/cicada_des...

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MOUNT STROMLO & SIDING SPRING OBSERVATORIES Computer Section

October 12, 2001

Computerised Instrument Control and Data Acquistion System (CICADA) Programmers Guide

Contents

ContentsIntroductionDescription

Component descriptionError Handling


IntroductionThis guide describes the MSSSO CICADA software system design from a programmer’s point of view. Otherdocumentation describes the rationale for developing the system, this instead will concentrate on describingthe techniques adopted to develop the software.

DescriptionThe aim of CICADA is to build on the techniques developed during the CCD system prototype [#!ref1!#]That is, to extend the CCD prototype to be a general MSSSO telescope instrument interface using the XWindow system from an observers Unix workstation.

As shown in Fig 1, CICADA consists of a process group running on the observers workstation and potentiallymore than one process group running on perhaps more than one instrument computer (which may also be theobservers workstation).


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Figure 1: CICADA Block Diagram

Note that the block diagram is drawn in a way that illustrates the hierarchy in the process chain. A processbox which encloses other process boxes is a parent to those enclosed and has responsibility for organizing


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their execution (starting, stopping and ensuring they are still alive when required).

Inter process communication (IPC) between processes on the same machine is achieved by using standardUnix SysV IPC routines (see [#!ref2!#] ), while communication between the two machines is by RemoteProcedure Call (RPC) routines (see [#!ref3!#]) across an ethernet link.

The basic functioning of the system requires that an observer sitting at the Sun workstation be able to issue acommand to the instrument and receive feedback (image data or status information) at the workstationwithout having to know anything about the instrument computer at all. The image data needs to be displayedand then archived as FITS files in real time (limited by the speed of the ethernet link). Full functionality isdescribed in the Functional Specification (see [#!ref4!#]).

This basic functionality is extended to allow the observer to monitor more than one instrument at, possibly,more than one intrument computer simultaneously. Obviously this model is constrained be hardware at theCPU, display and communication levels, but should not be constrained by software.

Component description

The observer computer runs the process Instrument Control which spawns processes Database Manager, Graphical Tool and RPC Server. When the observer selects an instrument Instrument Control will spawn a Controller process which in turn makes contact with the instrument computer and starts up a remote RPC Server and remote Controller process. This group of processes form the link between observer and instrumentand are the essential components of the system. The following pseudocode algorithms describe the specificfunctionality of each of these components:

Instrument Control

Start ‘‘Database Manager’’, ‘‘Graphical Tool’’ and ‘‘RPC Server’’. Establish mailbox. Loop Wait on observer requests and mailbox messages. If new instrument requested start instrument ‘‘Controller’’. otherwise post requests to instrument ‘‘Controller’’ mailbox. Endloop

Database Manager

Establish mailbox. Loop Wait on requests for data from mailbox. Collect data from telescope or cache, update cache if necessary. Post data to requesting process’s mailbox. Endloop

Graphical Tool

Establish mailbox. Loop Wait on requests from observer for graphical analysis of image data. Connect to image in virtual memory, do computation and display results. Endloop

RPC Server

Establish mailbox. Loop Listen for RPC image data requests on network, and watch for mailbox messages fron ‘‘Instrument Control’’. Interpret request and post to appropriate ‘‘Controller’’ process which will be a ‘‘Displayer’’ sub-process. Endloop

Remote RPC Server

Loop Listen for RPC instrument requests on network. Interpret request and post to appropriate ‘‘Remote Controller’’ process depending on instrument. That is, if Instrument Computer hosts more than one instrument, the ‘‘Remote RPC Server’’ needs to pass requests to the correct ‘‘Remote Controller’’ process. Start and restart ‘‘Remote Controller’’ processes as appropriate, ie, monitor that they are still alive. Endloop

Controller

Establish mailbox.


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Start sub-processes ‘‘Archiver’’, ‘‘Displayer’’ and ‘‘Remote’’. Start remote ‘‘RPC Server’’ and ‘‘Remote Controller’’. Establish a shared memory segment for status. Loop Check for user requests from mailbox. If any requests current, monitor progress and sub-process status. Restart any sub-processes or remote processes if failed. If new request pass on to sub-processes. ‘‘Remote’’ handles requests to instrument, ‘‘Displayer’’ handles requests to get data from the image display and ‘‘Archiver’’ takes requests to create new FITS files (memory mapped). Display progress and status information. Endloop

Remote Controller

Establish mailbox. Start sub-processes ‘‘Slave’’, and ‘‘Data’’. Establish shared memory segments for status and image data. Loop Check for user requests from mailbox. If any requests current, monitor progress and sub-process status. Restart any sub-processes if failed. If new request pass on to process ‘‘Slave’’. Post status and progress requests back to ‘‘RPC Server’’ on the Observer Computer. Endloop

Archiver

Establish mailbox. Establish interrupt handler (can be interrupted by ‘‘Controller’’). Connect to the status shared memory segment. Loop Check for requests in mailbox from ‘‘Controller’’. Requests will be either to create a new FITS file, gather telescope information (post request to ‘‘Database Manager’’ to construct the FITS header and close the FITS file. Post a ‘‘ready’’ message to the ‘‘Displayer’’ process when FITS file ready for data. (Or use semaphore to control access) Place regular heatbeat signal onto status memory. Endloop

Displayer

Establish mailbox. Establish interrupt handler (can be interrupted by ‘‘Controller’’). Connect to the status shared memory segment. Loop Check for requests in mailbox from ‘‘RPC Server’’ to display and store image data from the instrument. Requests will be either to start a new image, build on an already started image or to close it off. If the request is to start a new image then wait for a ‘‘ready’’ message from the ‘‘Archiver’’ process (or wait on semaphore) before copying data to virtual memory FITS file. Place regular heatbeat signal onto status memory. Endloop

Remote

Establish mailbox. Establish interrupt handler (can be interrupted by ‘‘Controller’’). Connect to the status shared memory segment. Loop Check for requests in mailbox from ‘‘Controller’’ to formulate RPC requests to the instrument computer (or, if the instrument is local, post mailbox messages to the ‘‘Remote Controller’’). Post results of status requests onto the status memory. Place regular heatbeat signal onto status memory. Endloop

Slave

Establish mailbox. Establish interrupt handler (can be interrupted by ‘‘Remote Controller’’). Connect to the status shared memory segment. Connect to the image shared memory segment. Loop Check for requests in mailbox from ‘‘Remote Controller’’ for instrument action requests. Instrument requests will involve loading the controller with appropriate commands, starting, pausing, resuming, aborting the controller and retrieving data from the controller. Post regular progress information onto status memory during an instrument request, otherwise post heartbeat information. Image data retrieved from the controller is placed into the image shared memory when ready (Either wait for ‘‘ready’’ message in mailbox from ‘‘Data’’ or wait on semaphore). Signal ‘‘Data’’ that new data is ready. Endloop

Data


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Establish mailbox. Establish interrupt handler (can be interrupted by ‘‘Remote Controller’’). Connect to the status shared memory segment. Connect to the image shared memory segment. Loop Wait for requests in mailbox from ‘‘Slave’’ for new image data (or wait on semaphore). Formulate RPC request to Observer Computer with the image data. (or if on same computer post mailbox message to ‘‘Displayer’’). Post regular heartbeat information to status memory. Endloop

Error Handling

In a distributed processing environment like CICADA it is easy for the error locality and the notificationinterface to become detached thus making reporting difficult. In CICADA it is proposed that the LocalController process for each instrument be responsible for reporting all error conditions. Therefore any errorsgenerated by child processes (local and remote) should be propagated back, through the IPC interface, to theLocal Controller for reporting.

Within a process, the C++ exception handling facilities [#!ref5!#] will be used to concentrate error processingat one location in the code thus eliminating the need for explicit error handling right through. Size andcomplexity of the code is, hence, also reduced.

For example the pseudocode version for the slave process, rewritten with exception handling, becomes:

try { Establish mailbox. Establish interrupt handler (can be interrupted by ‘‘Remote Controller’’). Connect to the status shared memory segment. Connect to the image shared memory segment. Loop try { Check for requests in mailbox from ‘‘Remote Controller’’ for instrument action requests. Instrument requests will involve loading the controller with appropriate commands, starting, pausing, resuming, aborting the controller and retrieving data from the controller. Post regular progress information onto status memory during an instrument request, otherwise post heartbeat information. Image data retrieved from the controller is placed into the image shared memory when ready (Either wait for ‘‘ready’’ message in mailbox from ‘‘Data’’ or wait on semaphore). Signal ‘‘Data’’ that new data is ready. } catch(CICADA_error E) { Post error condition to status memory, or rethrow to outer error handlers. } Endloop } catch(CICADA_error E) { Post error condition to status memory }



The command line arguments were: latex2html -init_file /opt/local/html/latex2html/cicada.init cicada_design2.tex


CICADA V3.1 User’s Manual http://www.mso.anu.edu.au/computing/cicada/cicada/cicada.html

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CICADA V3.1 User’s Manual

Computer Section Mount Stromlo and Siding Spring Observatories Research School of Astronomy and Astrophysics

Australian National University

December 13, 2000

Contents

ContentsList of FiguresIntroduction

CICADA featuresGetting Started

Quick Start GuideRequirementsTake CareConfiguring fonts and colours

CICADA Main Menu BarStart Observing

Data ArchivingToolsOptions

PreferencesHelp

Send CommentsWhat’s NewAbout Cicada

The CICADA Observing WindowMenu Options

Actions menuTools


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Options menuController menuInstrument Controls menu

ToolbarImage naming and displaying options

Exposure TypeSave and Display options

Exposure optionsNo pre-flush and No Readout toggles

Status indicatorsButtonsThe Regions WindowThe FITS Keyword WindowAutomated Focusing

The SDSU controllerInitialisation of the SDSUThe SDSU menu

SDSU Controller CommandsThe Astromed 3200 controller

Initialisation of the AM3200The AM3200 menu

CICADA FITS filesCICADA FITS DictionarySite Specific FITS headers

Interface to the Telescope Control SystemOptional Interface to the Exposure ControllerOptional Site Instrument FITS additionsOptional FITS TableOptional FITS Plug-InKeyword Translation Table

CICADA ScriptingExample scripts

CICADA Debug LevelsKnown BugsTroubleshootingAbout this document ...

List of Figures

CICADA startup window1.CICADA startup window2.General Preferences3.Image Display and Scaling Preferences4.CICADA observing window5.A Filter Control GUI6.A Telescope Control GUI7.GUI Toolbar Buttons8.CICADA Regions window9.CICADA FITS keyword window10.CICADA Automated Focusing Parameters11.CICADA Focus Image12.CICADA Focus Fit13.SDSU readout mode display14.Temperature Display and Control Window15.Temperature Plots16.SDSU Configuration Engineering Interface17.SDSU Sbus DSP Commands18.


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SDSU Timing DSP Commands19.SDSU Utility DSP Commands20.

IntroductionThis manual describes the operation of the CICADA system (Configurable Instrument Control and DataAcquisition). This version of the manual accompanies release 3.1 of CICADA. To find out what changeshave been made since earlier releases, select What’s New from the CICADA main window Help menu.

Version 3 of CICADA supports the Astromed 3200 controller and the SDSU Generation 1 and Generation 2controllers.

CICADA featuresThe aim of the CICADA system is to provide a common interface to many different CCDs and severaldifferent types of CCD controllers. It has been designed and built to be as flexible as possible so that newCCDs can easily be incorporated into the system and the support of new controller types can be provided in arelatively straightforward manner. Version 3 furthers gains made with version 2 - the code has, again, beenextensively re-worked to provide a more general software solution for multi-part instruments and CCDmosaics. It also supports the simple control of instrumentation associated with a CCD camera.

The system is comprised of several unix processes each of which handles one aspect of the data acquisitionand control process. These processes are divided into two groups - observer control and instrument control,and may run on one or more computers. For example, in the observer control group there is a process whichdisplays images, another which writes FITS files, and a graphical user interface (GUI) with which theobserver monitors and controls the system. In the instrument group, there is a slave process whichcommunicates with the CCD controller, a data process which moves image data and a director process formanaging operations. More than one instrument group is possible allowing for the control of multiple-partinstruments. The use of several processes allows a certain amount of ‘‘parallelism’’ in the process of takingan exposure (e.g. a section of an image is displayed while the next section is being read out) resulting in somesystem performance gains. Further parallelism is achieved through the use of multi-threading in the internalsof these sub-processes where appropriate.

For a complete description of the CICADA design, refer to CICADA technical documentation athttp://www.mso.anu.edu.au/computing/cicada/

Getting Started

Quick Start GuideCICADA is predominantly GUI-based observing software with a familiar ‘‘look-and-feel’’ and an intuitiveinterface. If you want to start up CICADA and get going quickly without first reading the rest of this manual,do the following (presuming CICADA hardware configuration has already been performed):

type cicada and press <Return>once the CICADA menu-bar appears, select Start Ximtool from the Tools pull-down menuselect the Telescope/Instrument you are observing at from the Start Observing pull-down menuoptionally select Start GIT from the Tools pull-down menuset your desired exposure options and start observing.

You will now be taking data and FITS files will be written to a default location (probably your home area).You may wish to alter your output directory via Preferences from the Options pull-down menu.


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Use the Start Teldisk option of the Tools pull-down menu to clear the previous observer’s data from any‘‘observer’s’’ disk and create a directory for your data. This will depend on the disk configuration at yoursite.

RequirementsTo run CICADA, you will need an account and sufficient disk space to store captured images. Start CICADAby using the command cicada, you will then be presented with a menu bar from which an instrument andconfiguration can be selected. CICADA runs in conjunction with the Graphing and Imaging Tool (GIT) and amodified version of Ximtool - these must be started from within CICADA so that correct environments andinterconnections are set up. Use the Start Ximtool option of the Tools pull-down menu (if you forget to do this, CICADA will automatically start Ximtool the first time you start an exposure).

CICADA can also run in conjunction with its own (IRAF based) data reduction pipeline. Use the Start Pipeline option to get this going - refer to the Pipeline User’s Manual for more information.

Take CareNOTE: CICADA and GIT can be very memory hungry! How much memory the system requires depends onthe size of images you are taking. Both programs indicate when memory is getting low, so please take note ofthese warnings as performance can be affected. In particular,

Limit running of non-CICADA processes. Other utilities and packages such as Netscape and IRAF can compete with CICADA for system resources - try to run these on other hosts on the network.Stop and restart CICADA if in trouble. If system resources have been drained - it is fast and simple tostop and restart the observing window. This will recover system resources to the starting point,provided no other memory hungry processes are running.

Configuring fonts and coloursSetting up fonts and colours for X windows applications can be a complicated process. X applications use‘‘resources’’ to determine the fonts and colours they should use when displayed on the screen. If you wish tochange the default colours and fonts for CICADA, you will need to add the following lines to your.Xdefaults file:

cicada*fontList: -*-lucida sans-medium-r-*-*-*-100-*-*-*-*-*-*=TAG1,\ -*-lucida sans-bold-r-*-*-*-110-*-*-*-*-*-*=TAG2cicada*background: wheatcicada*foreground: blackcicada*selectColor: yellow

To select a font you like, use the program xfontsel which allows you to preview various fonts and then cutand paste your chosen font descriptor into your .Xdefaults file. Note that there are two fonts listed in thefontlist resource. CICADA uses the first font for most of the labels in all windows. The second font is usedto highlight various buttons and text fields such as the status indicators. You do not need to specify a secondfont as CICADA will use the first font you specify for all labels and text if no second font is in the fontlist.Note the syntax of the fontlist resource as the =TAG1 and =TAG2 are very important.

The cicada*background resource sets the colour of all window, button, etc. backgrounds. Text on buttons andlabels will be in the colour specified by the cicada*foreground resource. cicada*selectColor sets the colourused by toggle buttons when they are turned ‘‘on’’.

Similar selections may be made for other CICADA tools, that is, GIT, Pipeline. GSFind and Teldisk.

CICADA Main Menu Bar


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Figure 3.1 shows the CICADA Main Menu Bar. This is the first window the observer will see upon startingCICADA.

Figure 3.1: CICADA startup window

Start ObservingThis pull-down menu contains a list of possible telescope/instrument configurations. The observer selects theparticular telescope/instrument for which they have been scheduled. CICADA has an internal table which isconfigured by technical staff that indicates to the system such things as the CCD in use on the selectedinstrument, the controlling computer, the controller type, etc. After selecting the appropriate item, anobserving window will appear.

Data Archiving

As part of supporting the archiving of RSAA’s Wide Field Imager data, version 3 of CICADA can optionallyrequest the observer to provide name and proposal ID details for inclusion in FITS headers. These details canbe used for retrieving data from an archive at a later date. The proposal ID will be matched with a passwordand used as part of a system to restrict access to data in the archive. Figure 3.2 shows the Proposal ID confirmation window. This window will appear if the instrument has been configured to support archiving ofdata. If for some reason the details are incorrect, this window provides the observer with an opportunity tocorrect the error. It is also possible for the observer to select not to archive any FITS data.

Figure 3.2: CICADA startup window

ToolsThis menu has items for starting the Graphing and Imaging Tool (GIT), Ximtool, Pipeline, Teldisk andGSFind.


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GIT provides ‘‘quick look’’ plotting and data reduction tools - see the GIT User’s Manual for full details.

Ximtool is used for displaying the image as it is read out. You may either start Ximtool manually via thismenu option or it will be started automatically if display mode is set when taking an exposure. CICADA uses a modified version of Ximtool and it MUST be started from within CICADA

Pipeline is a data reduction pipeline that can run stand-alone or closely integrated with CICADA. It uses theIRAF ccdred and mscred packages for performing the actual work. The idea behind Pipeline is that itprovides an automated way of performing simple recipe reduction on a collection of images.

GSFind is a Guide Star Finder that uses the Guide Star Catalogue and a description of theinstrument/telescope to assist with locating guide stars. It is loosely coupled with CICADA and can also runin standalone mode.

The other option available under Tools is Start Teldisk. Teldisk allows the current observer to clear the previous observer’s data from the ‘‘Observer Data disk’’ and create a new directory for storing FITS files.The configuration of disks is site dependent, so talk to the local Systems Managers about disk space forobservers.

Options

Preferences

Preferences are user configurable parameters which affect the operation of CICADA. CICADA Preferencesare stored in the observer’s home area in a file called .cicadarc-hostname. The file is read once at CICADAstartup time. This file is host name differentiated because of the possibility that a user might run more thatone session of CICADA at a site with multiple instruments and CICADA observer hosts. It is important thatthese files are not mixed.

General Preferences

Figure 3.3 shows the Preferences window with the General Preferences displayed.


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Figure 3.3: General Preferences

Use these preferences to specify the default filename prefix, suffix and location (output directory) for FITSfiles. There are also options here to:

use the large counter in a separate window as well as using an exposure counter in the progress displayof the observing window. Turn the toggle ‘‘on’’ to use the large counter in a separate window.show messages window at startup will cause the CICADA messages window to be displayed andpositioned below the observing window when the first status messages are received from a CICADAsub-process (i.e. there may be a delay after the observing window has appeared before the messageswindow is seen).reset the Number of exposures field to 1 after running a sequence of exposures. e.g. (with this toggle‘‘on’’) the observer enters ‘‘5’’ in Number of exposures and selects Expose. The five exposures are runand at the end of the last one, Number of exposures is automatically reset to 1.toggle binning when switching between Save and No-Save modes. e.g. the observer bins 4x4 whilepositioning the science object on the CCD and using Display Only mode. However, the observer uses1x1 binning during data acquisition with Save and Display mode. With this toggle ‘‘on’’, CICADAwill remember the two different binning factors and toggle the binning whenever the observer switchesbetween Save and Display and Display Only modes.The number of CCD flushes to perform when doing an exposure.X window screen numbers to display each CICADA tool - only applicable for multi-screenworkstations. By setting the screen number here, each of the tools will be started on the preferredscreen.Automated focusing parameters. See section 4.9 on automated focusing for a description of how thisworks. Set the following parameters for running the sequence.

Focusing steps - the number of focus steps to perform in the sequence.Value of the first focus position in the sequence.The focus position step size. This can be used for systems that have a computer controlledfocusing mechanism. The focus position is adjusted by this amount each successive step in thesequence.The radius (in pixels) from the star centroid to use for fitting a gaussian.

Image Display & Scaling Preferences

Figure 3.4 shows the Preferences window with the Image Display and Scaling Preferences displayed.


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Figure 3.4: Image Display and Scaling Preferences

These property items affect the way in which images are displayed as they are read out:

Clear display before next image will cause the image display to be cleared before the next image isdisplayed. When not selected, a following image will gradually overwrite the currently displayedimage. This may be useful in focussing or positioning the science object on the CCD.Highlight saturated pixels will cause any pixels with a value greater than that specified in the‘‘saturation value’’ field to be highlighted in red on the image display.Display distinct image regions in separate frames,... This option affects the way images are displayedfrom CCD mosaics, multi-amplifier CCDs and multi-region readouts. If ‘‘on’’, each separate region isdisplayed in a separate frame of the image tool. If ‘‘off’’ all regions are displayed in one image toolframe in ‘‘detector’’ coordinates.Use approximate integer maths for scaling... Uses shift division for placing each pixel into its displaybin (for Ximtool this is a maximum of 200 levels). This, if used in conjunction with the Ultra SparcVIS instruction set (see General options), can speed up image display by nearly 4x for most images.Wait for image display during readout... sets the maximum amount of time CICADA will wait for theimage display to show a chunk of data before sending the next one. Small values will result in ‘‘gaps’’in the image display, but does NOT mean data has been lost. The default value will result in goodperformance and zero or minimal gaps in the display.Adaptive scaling will calculate appropriate minimum and maximum image display values as each‘‘chunk’’ of image is read out. Depending on the settings of ‘‘% of image to readout before rescaling’’and ‘‘Num SDs tolerance before rescaling’’ the range is re-calculated after each chunk and the entireimage redisplayed. Minimum and maximum values are calculated as a weighted deviation from themedian or mode after sampling a proportion of the pixels. Better performance, but perhaps poorerscaling will result from decreasing the number of pixels to sample. The min/max range can be modifiedby altering the contrast adjustment value between 0 and 1.Fixed scaling allows the observer to specify the range of image display values to be used by the imagedisplay. This may be necessary in certain situations where adaptive scaling is not giving the desiredresults.

Sounds Preferences

These preferences control the number of beeps issued by Cicada at certain key points during an exposure.The observer can set the number of beeps to be heard when the shutter opens, the shutter closes and whenreadout finishes.


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Expert

These preferences control the following:

Whether or not the observer is warned at startup if CICADA cannot allocate a colour. CICADA uses asmall number of colours on the GUI for highlighting buttons and warning of error conditions. If theobserver is running a colour-hungry application such as Netscape, it is possible that CICADA may notbe able to use one or more colours and so the software will try to find an alternative. If an alternative isneeded or no colour can be found, a warning will be displayed at startup if this preference is ‘‘on’’.Write an observations log. When ‘‘on’’ CICADA will write a log of each image taken showing RA,Dec, run number, exposure time, sidereal time, object.Show timestamps in messages window. Whether or not to show a timestamp with every line in theCICADA Messages Window.Show Balloon Help. Turns on and off the ‘‘balloon help’’ on toolbar itemsShow toolbar items as text, not picturesUse the Ultra Sparc VIS instruction set. For improved performance in some operations. (eg byteswapping or image display).Write a temperature log. Selecting this option will allow a CCD temperature log be kept for the run.

Help

Send Comments

This will pop-up a window allowing the observer to enter a message which will be sent to the local CICADAadministrators. Use this to report problems, ask questions or request changes/new features. CICADA isconfigured to have an email address of the local CICADA administrator. At RSAA this is staff of theComputer Section who will endeavour to respond promptly to your submission with a resolution or anestimation of when a resolution can be made.

What’s New

This will popup a window showing a revision history of CICADA which outlines the major changes betweenversions.

About Cicada

Well, everyone else has one of these...

The CICADA Observing WindowFigure 4.1 shows the CICADA observing window. It is from this window that the observer initiates andcontrols data acquisition. The appearance of this window is largely the same irrespective of the particularcontroller used to drive the CCD (e.g. AM3200, SDSU Generation 1). Of course, each controller has certainunique features and these are accessed via a pull-down menu on the observing window. e.g. when using theAM3200 controller, the pull-down menu will be called AM3200 and will have items such as ‘‘Edit Gain Values’’ and ‘‘Continuous Flush & Read Temps’’.


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Figure 4.1: CICADA observing window

Menu Options

Actions menu

Initialise CCD Hardware

Selecting this action will cause hardware initialisation of the CCD controller to be performed. Duringinitialisation status messages will be displayed in the Cicada Messages Window and progress will be shown in the status indicators of the Observing Window (see below).

Run CICADA Script...

This action will pop-up a file selection box allowing the observer to select a file containing a TCL script to beexecuted. The script must be a valid TCL script with CICADA commands. See Chapter 8 for further details.

Repeat Last Script

This item will become active once a script has been run and when selected will re-run the most recentlyexecuted script.

Do Focus Sequence...

A focus sequence consists of a series of exposures run with different telescope focus settings followed byanalysis of the resultant image to determine the optimal setting. Focus settings are either set manually by theobserver when prompted or, if the capability exists, automatically through the telescope control interface. A


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plot of the calculated optimal setting (a quadratic fit through the set of points) is produced at the end of thesequence. The user is required to select a small region around a single star before performing the focussequence.

Quit Observing Window

Close the Observing Window and shutdown all sub-processes. The observer should use this action whenfinished observing or if a restart of the CICADA sub-processes is required.

Tools

This pull-down menu is a copy of the Tools menu of the CICADA Main window and has items for startingGIT, Ximtool, Teldisk, Pipeline and GSFind.

Options menu

Preferences

Select this to pop-up the User Preferences window

Exposure Time Unit

Use this pull-right menu to change the time unit used when specifying exposures.

Show Regions Window

Selecting this will pop-up the Regions window allowing the observer to specify regions of interest on theCCD

Show Messages Window

This option will pop-up a messages window. Certain parts of the CICADA software send messages to thiswindow and it may be useful to the observer to see these messages - for example, during a hardwareinitialisation.

Show Counter

The observer can use this option to re-display the counter window if it has been dismissed during an exposurecountdown.

Show FITS Keyword Window

This will display a window where the user can enter any extra keyword/value pairs they would like to add totheir FITS files. See section 4.8 at the end of this Chapter for more information on the FITS keywordwindow.

Hide Toolbar

Selecting this option will remove the toolbar from the observing window. The Toolbar can be redisplayed byselecting Show Toolbar from the Options menu (the Hide button changes to Show and vice versa asappropriate).

Controller menu


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This menu will appear on the menu bar with a name such as AM3200 or SDSU and holds all hardware specific actions and options for a particular controller type. See the relevant chapter in this manual forinformation about this menu item for specific controller types.

Instrument Controls menu

Note: This menu item will only appear if the CICADA instrument description includes site instrumentcontrol or filter control specifications.

Simple instrument controls are optionally configured for an instrument. This facility is provided as part ofCICADA’s ‘‘plug-in’’ capability. Each of the items under this menu is built as a simple instrument GUIplug-in - see the CICADA plug-in reference manual for further information.

An example simple control plug-in is one for a filter wheel (See Figure 4.2).

Figure 4.2: A Filter Control GUI

This popup window displays the current filter wheel position by highlighting the current position in green.The filter wheel is moved to another position by selecting the item corresponding to the desired filter. Theselected position will flash orange while the filter wheel moves and will be highlighted in green once thewheel is locked into position.

Another example is one for telescope control (See Figure 4.3).


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Figure 4.3: A Telescope Control GUI

ToolbarThe Toolbar is intended to give one-button-click access to some of the more commonly used items from thepull-down menus. ‘‘Balloon Help’’ will pop-up under the Toolbar item if the cursor is positioned in theToolbar. (To turn off the balloon help see the Expert section of the Preferences window)

There are buttons in the Toolbar for Hardware Initialisation, Run CICADA Script, Repeat last script, showPreferences, show FITS keyword window, show Temperatures window, show Regions window and ReadRegions from Image Display (See Figure 4.4).


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Figure 4.4: GUI Toolbar Buttons

Image naming and displaying optionsThis section of the window displays the destination directory the observer has selected along with a filenameprefix, suffix and run number which will be used to create a filename for the FITS file. There are also fieldsfor entering a comment and object name to be added to the FITS header. CICADA stores up to 20 objectnames and comments. Use the down arrow next to the object name or comment field to select frompreviously used names and comments . New items can be added to these lists by simply entering a new valuein the text field and hitting <Enter> or by entering a new value and taking an exposure. To delete an item,blank it out and hit <Enter>. These lists of names will be remembered by CICADA between runs (they arekept in the .cicadarc-hostname file in your home area Note that the list of objects and comments may growlonger than 20 during one invocation of CICADA - but only 20 will be stored when the observer quits.

If a filter is in use, the filter name will be displayed next to the object name.

Before the exposure is carried out, the system checks to see if a file already exists with the same name as theone about to be generated. If such a file is found, the observer is prompted with a pop-up window asking ifthis existing image should be overwritten. If the observer responds that the image should be overwritten,THE EXISTING FILE IS IMMEDIATELY REMOVED. Note also that NO EXPOSURE is happeningwhile the prompt is displayed.

Exposure Type

The setting of these toggles affects the value of the IMAGETYP FITS keyword. In addition, when BIAS isselected, CICADA sets the exposure time to zero. The previous exposure time is restored when an optionother than BIAS is subsequently selected.

The Expose button will change to the orange warning colour and the Exposure Type label will flash orange when anything other than Object is selected.

Save and Display options

Images read out from the CCD can optionally be displayed and optionally written to disk. Appropriatewarnings are displayed on the GUI if the observer chooses NOT to save images. There is also a button in thissection of the window which will allow the observer to save the last image taken when taking images in ‘‘no


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save’’ mode. This might be useful if the observer was taking a series of frames of the science object whilefocusing the telescope. Images are discarded until a good frame is taken, when pressing the Save Imagebutton will write the last image to disk.

Exposure optionsThis section of the window is where the observer specifies exposure time and the number of exposures to betaken once the Expose button is selected.

No pre-flush and No Readout toggles

Normally, an exposure consists of a flush, followed by integration and readout. The observer can alter thissequence with these two toggles by choosing to omit the pre-flush and/or the readout. The Expose button willchange to the orange warning colour when this toggle is selected and the selected toggle(s) will flash orange.If No readout is selected, No pre-flush is also automatically selected.

Status indicatorsThese indicators give the observer some feedback as to the state the system is in at any particular moment.The upper left-hand indicator will read one of Idle, Running or Paused and indicates the state of the processresponsible for communicating with the CCD controller. The upper right-hand indicator gives more detail ofthe particular function currently being carried out. This indicator will display such messages as Initialising, Shutter Open, Shutter Closed, Reading Out. In addition to these messages, this indicator will show a greenbackground when the shutter is closed and an orange background when the shutter is open (NOTE: thisindicator is not controlled by any hardware and reflects only a status of the software. Therefore, if the shuttermechanism were to jam open or closed, this indicator WILL BE INCORRECT). This indicator is also where an exposure counter will be shown if the observer has de-selected the CICADApreference Display exposure counter. During CCD readout, this indicator will show progress as a number ofrows read out against the total to be read.

Also in this section of the window are three indicators displaying free disk space on the observer’s chosenoutput disk, free memory available in the workstation and the current CCD temperature.

The free disk space indicator will flash orange when there is not enough space for two full readouts ofthe CCD. When there is a warning about low disk space, either free some space on the disk byremoving files or select another output directory via Preferences from the CICADA Options pull-down menu.

The free memory display will flash orange when there is less than 16 Mb of free memory in theworkstation. When there is a warning about low memory, quit some applications running on the samehost as CICADA. In this situation, it might also be a good idea to quit and restart CICADA and GIT ifyou are using it.The CCD temperature indicator will display HWinit needed if the temperature has not been read or ifthe controller hardware needs re-initialising. The behaviour of this indicator is controller dependent.Additionally, the temperature indicator will change to an orange background if any focalplanetemperature sensors measure a temperature which is out of range (the name of the sensor will appear inthis indicator should this happen). Choose Show Temperatures from the controller-specific menu in theobserving window (e.g. the menu labelled AM3200 or SDSU) to see all temperature sensors for thecurrent instrument (or click on the thermometer button in the toolbar).

ButtonsHere is a brief description of the function of each button:


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Expose: Start an exposure using the various fields in the GUI for exposure parameters, file name,destination directory. This button will be orange if the observer has selected an option in the GUIwhich may result in no data being written to disk or if some other non-standard exposure option hasbeen chosen (e.g. dark frame, no readout, no pre-flush). CICADA will check to see if there is alreadyan image with the same name as the one about to be created and prompt the observer to ask if theexisting file should be overwritten. CICADA will also check to make sure there is sufficient disk spacefor the new image and sufficient free memory in the workstation for the readout to be completed.Readout: Read out the CCD, display the image and save the FITS file (if save to disk has beenselected).Pause: Pause the exposure by closing the shutter and stopping the counter. The observer may thencontinue the exposure by selecting the Resume button. It is also possible to change the exposure timeand number of exposures while paused and these new values will be used when the exposure isresumed. Note that even though the shutter is closed, dark current and cosmic rays are still beingaccumulated on the CCD.Resume: Continue the paused exposureFlush: Flush the CCDAbort: Stop whatever is happening (eg. exposure, readout). Note that aborting an action may take from a few seconds to several 10’s of seconds. This is because, depending on the controller, someactions cannot be immediately interrupted and must finish before the abort request can becarried out and the GUI reset to allow further action.

The Regions Window

Figure 4.5: CICADA Regions window


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The Regions Window is where the observer can specify the region(s) of the CCD or CCD mosaic to be readout and saved to disk. There are also fields in this window for changing the row and column binning factorsand for specifying row and column overscan.

The window has five main sections:

The Region Diagram This diagram shows the layout of the CCD(s) on the focal plane and will displaya shaded area indicating the currently selected region(s) of interest. The diagram will be updated aschanges to the region of interest are made in other section of the window.

User Defined regions This section can be used to manually key in a region of interest. However, asimpler way to set the values in these fields is to have CICADA do it via the Read Regions from Image Tool feature. To use this, first do a full readout of the CCD or mosaic, then mark the region of interestby drawing a box on the image display (click mouse-button 1 and drag in the Ximtool window), thenselect Read regions from imtool from the Actions menu in the Regions window. There is also a buttonon the observing window toolbar to perform this function. It is possible to mark either one or tworegions in this way.

Also in this section of the window are settings which allow the observer to specify which of the tworegions is to be read out (both regions can be selected simultaneously). Attempting to turn ‘‘off’’ theonly ‘‘on’’ toggle will automatically turn ‘‘on’’ the other toggle and display that region.

Pre-defined regions This section allows the observer to select from the following regions of interest:Entire detectorA region in the centre of the detector. The size is selected using the option button. The sizesavailable are determined dynamically by CICADA based on the size of the entire detectorA region in the centre of each CCD. The size is selected using the option button. The sizesavailable are determined dynamically by CICADA based on the size of each CCD.selected CCDs. The numbers in this section correspond to the numbers shown in the RegionsDiagram. This ‘‘masking’’ can be used in conjunction with selecting a region in the centre ofeach CCD

Binning and Overscan This section contains input fields where the observer can specify row andcolumn binning and also the amount of row and column overscan. Note that when overscan isspecified, it will NOT be shown in the image display for CCD mosaics if the display is showing theentire mosaic (overscan will be seen if each CCD is shown in a separate frame of the image display).The overscan IS written to the FITS file, regardless of what the display is showing.

Actions pull-down menu The Actions menu at the top of the window has buttons which allow theobserver to:

Read the region(s) marked on the image displayreset the region values to their initial state (full CCD for region 1 and nothing for region 2)Save the currently defined regions to a fileLoad regions from an existing regions file (e.g. to use the regions from a previous observing run)

The FITS Keyword Window


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Figure 4.6: CICADA FITS keyword window

The FITS Keyword Window (Figure 4.6) allows the observer to enter keyword/value pairs to be added to theheader of each FITS file written by CICADA. These keywords are in addition to any standard keywordsprovided by CICADA (e.g. EXPTIME) or by any telescope system (e.g. AIRMASS). The intention of thiswindow is to allow CICADA users to enter keywords that the system does not supply (e.g. where there is notelescope computer or only a manual filter wheel).

Keywords and values can simply be typed into the text fields. CICADA will remember up to six items foreach keyword and value field. Use the down-arrow to the right of the field to see a list of previously entereditems and click on an item to select it. The list may grow longer than six items during one invocation ofCICADA, but upon exit, CICADA will only store the six most recently used items.

NOTE: Changes made in these text fields will not propagate into FITS files unless the Apply button is pressed. Visual confirmation that your changes have been communicated to the CICADA sub-processes willbe in the form of a command string in the CICADA Messages Window. Provided the Apply button is pressed before a readout starts, it is possible to modify these values during an exposure and have these modifiedvalues appear in the FITS file about to be produced.

Each keyword/value pair has a toggle next to them labelled ‘‘Include in next FITS header’’. This toggle canbe used to stop a keyword/value pair from being added to a FITS header. Turning all these toggles off willdisable all user-specified FITS keywords. Remember to press the Apply button if you change these toggles.

CICADA stores any keywords and values that the observer enters in the .cicadarc-hostname file in the observer’s home area so that they remain available after a restart of the CICADA software. When anobserving window starts up, CICADA will check to see if there are any ‘‘active’’ user-specified FITSkeyword/value pairs left-over from a previous CICADA run. If any are found, CICADA will prompt theobserver to either view these keywords (and then press Apply if they are to be used) or decide not to use themat all.

FITS keywords are edited by CICADA to make sure they have no leading or embedded blanks and that theyare uppercase. Embedded blanks will be replaced by a hyphen (‘‘-’’).

If the keyword ‘‘FILTER’’ is specified, the value associated with this keyword is displayed next to the objectname in the observing window.

A full description of CICADA FITS file construction is contained in chapter 7.

Automated FocusingAn automated focus sequence consists of a series of exposures taken of a star with incremental focus shifts


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made between each exposure. These exposures are stacked together to form a composite image to which afocus fitting routine is applied. The FWHM of each star is measured and then a quadratic is fitted todetermine the optimal focus position. This fitted curve is then plotted and an indication of the minimum isdisplayed.

When Do Focus Sequence... is chosen from the Actions menu the window shown in figure 4.7 is shown.

Figure 4.7: CICADA Automated FocusingParameters

Select the number of focus steps to make and the initial focus position. CICADA will then expose theselected region (this should be a small region around a star) for the required exposure time. After theexposure, depending on whether the telescope has computer controlled focus setting or not, CICADA willprompt for the next focus position. The observer should set the focus position and enter the value in thedialog box before proceeding with the next exposure in the sequence. The composite image will then looklike figure 4.8.

Figure 4.8: CICADA FocusImage


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CICADA will then calculate the star centroid and fit a gaussian using the user preferences. The result will bea quadratic fit of FWHM and focus position which is then displayed. See figure 4.9.

Figure 4.9: CICADA Focus Fit

The SDSU controller

Initialisation of the SDSUCICADA will not initialise the SDSU controller when the observing window starts up. This is becausere-initialising will mean resetting the controller electronics and possibly destabilising the CCDs. However,the observer can re-initialise the controller at any time using the Initialise CCD Hardware option from the Actions menu of the Observing Window. This should only be performed as a last resort when all otherremedies for restoring normal operation have failed. Progress of an initialisation will be shown in the Cicada Messages Window.

The SDSU menuThese are the SDSU specific menu items appearing under the SDSU menu button in the Observing Window:

Readout modes

The SDSU controller has been set up to allow the selection of different readout modes. These are selectedfrom the SDSU menu on the observing window. There is a menu item Readout mode which is a ‘‘pull-right’’menu from which it is possible to select Fast, Medium or Slow. Once a selection is made, the mode will beshown in the exposure options section of the observing window. See

Figure 5.1


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Figure 5.1: SDSU readout mode display

Show Temperatures

Selecting this item will popup a window showing the last read values for all active temperature sensors. Pressthe Read Temperatures button to begin reading temperatures at an interval specified in the Read Temperatures every ... field. When idle, CICADA will read temperatures at this interval automatically. WhileCICADA is busy taking data it may not always be possible for the temperatures to be read. In this case, thesoftware waits until the system is idle before updating the temperatures window and the temperature displayon the observing window. Figure 5.2 shows available options.

Figure 5.2: Temperature Display and ControlWindow

CICADA can perform a controlled rate warmup of a CCD - parameters for controlling this operation are setdynamically from this window and are loaded, by default, from the Cicada focalplane configuration. This isan engineering mode only operation.

Progressive plots showing temperatures for those sensors configured can also be viewed. These plots willonly show values read back since the plot window has been popped up. A log of temperatures for the wholeCICADA run is stored in /opt/cicada/logs in a date stamped file. More extensive analysis of temperatureperformance can be made using these data.


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Figure 5.3: Temperature Plots

Note that changing the temperature read interval to a small value will impact on the performance ofCICADA.

Shutdown Controller

This option should be used before disconnecting the power to the controller. A shutdown sends a POFcommand to the SDSU controller making it safe for the SDSU controllers to be powered down.

Get Hardware Status

This option simply sends a GET_STATE command to the SDSU camera slave process. Normally these are runautomatically when the system is IDLE - at a regular interval (determined by the temperature readback intervalin the Temperatures window). This option allows for the retrieval of system status whenever required.

SDSU Configuration

Engineering Mode Operation

Controlling the setup of the SDSU controllers is via the loading of SDSU setup parameters. This is normally done from the preconfigured file /opt/cicada/config/sdsu/controller_name/sdsu.setup. A user in thecicada group will be able to setup this file by using the Configure Controller... option under the SDSU menu. Choosing this option will popup the window displayed in Figure 5.4.


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Figure 5.4: SDSU Configuration Engineering Interface

Here, the ability to selectively enable different initialisation options is available. Once a stable configurationis arrived at, it can be saved in the default configuration file for default loading by the observer.

SDSU Controller Commands

CICADA also provided the engineer with the ability to send individual commands to the SDSU controller viathe DSP Commands window found under the SDSU menu. This window allows the engineer to directcommands to each of the SBUS, Timing or Utility circuit boards of the SDSU controller.

To increase the diagnostic output from these commands, the CICADA debug level needs to be modified. This debug level operates as a mask and the values in Table5.2.1 are pertinent for SDSU operations.

Table 5.1: Debug levels for SDSU operation

Level Output Description

0 Show nothing

256 Show only errors from submitted commands

512 Show commands sent to the SDSU controller

1024 Show replies from the SDSU controller

2048 Run in dummy mode - neither sending or receiving data

Figure 5.5 shows the commands available for sending to the SBUS board. These allow the readback of theCommand Status Register (CSR), the Address register (ADR) and the Byte Count Register (BCR) of the


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SDSU astro device driver. The ability to reset the device driver is also available.

Figure 5.5: SDSU Sbus DSPCommands

Figure 5.6 shows the commands available for sending to the Timing board. Here basic (boot) commands toread a memory location (RDM), write a memory location (WRM), reset the timing board (RST) and test the data link (TDL) (fibre-optic link between SBUS interface card and timing card) are available. In addition,basic controller operations can be performed including: clear (flush) the CCD (CLR), go into idle mode (IDL), set gain to high (HGN), and low (LGN), start a CCD read (RDC) (though CICADA will not be ready to capture read back bytes - they will just spill) and stop any current operation (STP).

Memory operations can be directed to each of P, X, Y or R memory locations and need an address setting.Some operations also require a data value to use, for example the TDL command will echo the supplied datavalue - if the controller communications are functioning correctly.

Figure 5.6: SDSU Timing DSPCommands

Figure 5.7 shows the commands available for sending to the Utility board. Here basic (boot) commands toread a memory location (RDM), write a memory location (WRM), reset the timing board (RST) and test the data link (TDL) are available. In addition, basic utility operations can be performed including: abort anexposure countdown (AEX), open the shutter (OSH), turn on the power (PON), and turn off the power (POF), start an exposure countdown (SEX), close the shutter (CSH), pause an exposure countdown (PEX), resume anexposure countdown (REX) and perform a full system reset (SYR).


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Figure 5.7: SDSU Utility DSPCommands

Refer to the SDSU documentation for a full description of each of the DSP commands available.

The Astromed 3200 controller

Initialisation of the AM3200The observer may start a hardware initialisation of the AM3200 controller at any time by selecting theInitialise CCD Hardware option from the Actions menu of the Observing Window. Progress will be shown inthe Cicada Messages Window and voltages and temperatures will be shown as the hardware initialisationproceeds. When the initialisation is complete a window showing the final settings for all voltages will bedisplayed. (This window can be redisplayed at any time by selecting Hardware Status from the Optionsmenu. Be aware that the figures shown are as read at the end of the last hardware initialisation). Occasionallyduring Astromed 3200 hardware initialisation, the black level is not set correctly (very high values). This bugalso exists with the current Imager software - we are tracking it down. Just repeat the hardware initialisationto clear.

NOTE: The CCD temperature display on the Observing Window will not display a value until after aHardware Initialisation has been run. This is a limitation of the interaction between CICADA and theAM3200 hardware - basically, the software is unaware of the hardware state until after a hardwareinitialisation has been run.

The AM3200 menuThese are the AM3200 specific menu items appearing under the AM3200 menu button in the Observing Window:

Continuous Flush & Read Temps

Selecting this button will place the system in a loop where it flushes the CCD and then reads the temperaturesand updates the temperature meters display. The temperature of the CCD is CCDTMP1 and the figure isunder the Actual heading in Kelvin.

Edit Gain Values


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This item will pop-up a window allowing the observer to change the default values for PGain, CCDI and TC.

PGain is a scaling factor which affects the number of electrons per ADU. It’s value and what this valuemeans by way of a final e/ADU is CCD dependent and the observer should consult with Electronicsstaff to find out appropriate values for their particular CCD. A sensible default for each chip is alwaysset and shown in the pop-up window.CCDI is the integration time per pixel and adjusting this affects CCD readout time and noise levels.Once again, consult with Electronics staff before modifying this.TC is the integrating Time Constant and is used in conjunction with CCDI to set gain. If CCDI ischanged, it is likely that there must be a corresponding change to TC. Electronics staff have the detailsabout this relationship.

A Hardware Initialisation can be started using the Initialise button in this pop-up window. Use the Defaultsbutton to reset PGain, CCDI and TC to the defaults for the current CCD.

If the observer wishes to alter the gain of the CCD and modifies these values, the new values are stored in the.cicadarc-hostname file in the observer’s home area. These values will be restored the next time CICADA isrun and a warning will be given the next time a hardware initialisation is requested so that the observer hasthe opportunity to revert to the default values.

Show Temperatures

This is as for the SDSU controller - see section 5.2.

Show Voltage Meters

This option will display a window where the observer can choose to monitor Bias voltages, Clock voltages orTemperatures. Note that it is not possible to do this concurrently with taking exposures as the reading out ofvoltages requires separate software to be loaded into the Astromed controller.

Show Hardware Status

This will display a window showing the voltages set in the Astromed controller at the most recent hardwareinitialisation. Some of these voltages change with time and so the values shown in this window may beincorrect depending on how much time has elapsed since the last hardware initialisation.

Shutdown Controller

This option should be used before disconnecting the power to the controller. A shutdown sets all controllervoltages to zero.

CICADA FITS filesCICADA writes the new multi-extension FITS format. This format is understood in IRAF V2.11 but requiresspecial processing. For a full description see NOAO’s mosaic image definition.

For single region readouts from single CCDs, normal single image format is written (i.e. no special datareduction software is required in this case).

FITS files are sized according to the current instrument configuration. Because data and headers are writtenby separate Unix processes, enough space has to be set aside in the FITS file to accommodate all headers atthe beginning of an exposure. This space is predetermined by the local site CICADA system administratorusing the camera configuration table. See the CICADA Configuraionanualhttp://www.mso.anu.edu.au/computing/cicada/cicada_config/cicada_config.html for detailed information on


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CICADA hardware configuration.

FITS file header composition is made up of a standard set of keywords and additional site-specific keywords.

CICADA FITS DictionaryCICADA will write a standard set of FITS keywords from the CICADA FITS dictionary - table 7.1:

Table 7.1: CICADA FITS Keyword Dictionary Version 1.1

Keyword Type Note Example Value Description

SIMPLE Bool P T Fits standard

BITPIX Int P E 16 Bits per pixel

NAXIS Int P E 0 Number of axes

BSCALE Float P E 1.000000E0 REAL = TAPE*BSCALE + BZERO

BZERO Float P E 3.276800E4

EXTEND Bool P T FITS extensions are part of this file

NEXTEND Int P 8 Number of extensions

OBSERVER String P ’Gary Da Costa’ Observer name

PROPID String P ’P12345’ Site specific observing proposal identifier

FILENAME String P ’/datagdc/ccd0037.fits’ Original host filename

OBSID String P ’T_40.20000904.184013’ Observation ID

RUN Int P 37 Run number

OBJECT String P ’47 Tuc 120s R’ Observation title

IMAGETYP String P ’object’ Observation type

EXPTIME Float P 1.200000e+02 Exposure time (sec)

EXPREQ Float P 1.200000e+02 Requested exposure time (sec)

DARKTIME Float P 1.206810e+02 Dark time (sec)

INSTRUME String P ’WFI’ Instrument name

CAMERA String P ’WFI1’ Camera name

FILTYP String P ’’ Type of filter

FILTER String P ’R’ Filter name

FILPOS Int P 4 Filter position

DEWAR String P ’DWFI’ Dewar name

READMODE String P ’FAST’ CCD readout mode

WINDOW String P ’USER_DEFINED’ Readout window name

DETECTOR String P ’WFI1’ Detector Name

DETSIZE String P ’[1:8422,1:8282]’ Detector size

NCCDS Int P 8 Number of CCDs


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NAMPS Int P 8 Number of amplifiers

CCDTEMP Float P 1.582721e+02 CCD temperature (K)

FITSKW1 String P ’’ Optional user keyword 1




RA String P T ’00:24:05.4’ Initial RA 1.051125e-01

DEC String P T ’-72:09:08’ Initial Dec -1.259294e+00

EQUINOX String P T ’J2000.0’

LST-OBS String P T ’ 3:32:-968092763.0’ LST at start (hh:mm:ss.s) -7.0401e+04 rad

LSTEND String P ’ 3:32:-968092763.0’ LST at end (hh:mm:ss.s) : -7.0401e+04 rad

MJD-OBS Float P T 4.058700000000e+04 MJD of observation (days)

OBSERVAT String P T ’SSO’ Observatory

TELESCOP String P T ’40INCH’ Telescope

OBJNAME String P T ’’ Telescope object name

LAT-OBS Float P T 3.127336e+01 Degrees

LONG-OBS Float P T 1.490610e+02 Degrees east of Greenwich

ALT-OBS Float P T 1.149000e+03 Metres above mean sea level

AIRMASS Float P T 1.483511e+00 Airmass

HA String P T ’11:30:23.3’ Hour angle at MJD (hh:mm:ss.s): rr.r (radians)

HAEND String P ’11:40:11.6’ Hour angle at end (hh:mm:ss.s): rr.r rad

ZD Float P T Zenith distance at start of exposure

ZDEND Float P Zenith distance at end of exposure

TIMESYS String P ’UTC’ Default time system

UTC-OBS String P T ’18:40:13’ UTC of observation start

UTCEND String P ’18:50:23’ UTC of observation end

DATE-OBS String P T ’2000-09-04T18:40:13’ Y2K date of observation start

TELPAN Float P T dd.d Telescope position angle (degrees)

PIERSIDE String P T ’East’ Side of pier

TELFOCUS Float P T 0.000000e+00 Focus position

FOCNEXPO Int P F 5 Number of focus steps

FOCSHIFT Int P F 40 Number of rows read each focus step

FOCPOSn Float P F 32.3 Focus position n

FOCSOLN Float P F 32.8 Optimal focus position

IMAGESWV String P ’CICADA Release 3.1’ Image creation software version

KWDICT String P ’CICADA FITS V 1.1’ Keyword dictionary version


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XTENSION String E ’IMAGE ’ Image extension

EXTNAME String E ’im1 ’ Extension name

EXTVER Int E 1 Extension version

INHERIT Bool E T Inherit global keywords

IMAGEID Int E 1 Image identification

CONTROLR String E ’WFI_Bottom’ Controller Name

CONSWV String E ’V0.1493’ Controller software version

CONHWV String E ’’ Controller hardware version

READTIME Int E 52416 Controller readout time (ms)

CCDNAME String E ’WFI0_CCD20’ CCD identification

CCDSIZE String E ’[1:2098,1:4136]’ CCD size

CCDNAMPS Int E 1 Number of amplifiers used to readout CCD

AMPNAME String E ’A’ Amplifier identification

GAIN Float E 0.000000e+00 Amplifier Gain (e-/ADU)

RDNOISE Float E 0.000000e+00 Read noise for amp (e-)

SATURATE Float E 0 Maximum good data value - ADU

LINCOEF Float E 0.000000e+00 Linearity coefficient No=Nt(1+Nt**lincoef)

SUMSAT Int E 65000 Saturation level of summing wells

AMPSIZE String E ’[1:2098,1:4136]’ Amplifier size

CCDSEC String E ’[1:2098,1:4136]’ Region of CCD read

CCDSUM String E ’1 1’ CCD pixel summing

BIAS0001 String E ’[1:10,1:4136]’ Bias section - prescan cols

BIAS0002 String E ’[2059:2098,1:4136]’ Bias section - postscan cols

AMPSEC String E ’[1:2098,1:4136]’ Amplifier section

DATASEC String E ’[1:2098,1:4136]’ Data section

DETSEC String E ’[6325:8422,1:4136]’ Detector section

P. Primary header unit

E. Extension header unit

T. Delivered from site-specific telescope control system plugin

F. Only in CICADA generated focus sequence images

Site Specific FITS headersIn addition to the CICADA standard keywords (table 7.1) other keywords can be added to cater forsite-specific requirements. There are a number of ways CICADA can be customised so that these extrakeywords can be included.

Telescope Control System (TCS) interface. Local plug-in interface to the TCS can incorporate extrakeywords.

1.


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Optional Interface to the Exposure Controller. Local plug-in to the exposure controller to account forlocal exposure timing information.

2.

Optional Site Instrument FITS additions. Site instrument plug-ins can, optionally, have an associatedset of FITS keywords.

3.

Optional FITS Table. A table of keywords copied into the FITS file without interpretation.4.Optional FITS Plug-In. A plug-in called after the FITS file is closed to allow it to be rewritten withupdated information.

5.

Keyword name translation. In addition to adding extra keywords, keywords from the standard set maybe renamed by using an IRAF like keyword translation table.

6.

These techniques are described fully in the following sections.

Interface to the Telescope Control System

CICADA expects that an interface to the site telescope control system (TCS) be provided through asite-specific plug-in. By default, CICADA will use a dummy TCS that will provide fake telescopeinformation for the FITS headers. This dummy TCS will use the system time and date to generate UTC dateand time headers.

For each exposure a single call is made to the TCS plug-in for supply of the FITS keywords flagged with a Tin the 7.1 table. If some of these keywords are not available then they should be set to be invalid by theplug-in - CICADA will then indicate so by placing a COMMENT keyword in its place in the FITS file. The call tothe TCS is made near the start of an exposure but because CICADA is a multi-process system, this is notnecessarily at the same time that the shutter opens. To account for this corrections are applied to the returnedTCS time information so that they are correctly aligned with when the shutter actually opened.

In addition to the standard telescope keywords, the site TCS plug-in can deliver an arbitrary number of extrakeywords that are of local interest. These are placed in the primary header unit of the FITS file withoutinterpretation.

Optional Interface to the Exposure Controller

Some sites will have exposure controllers (shutter, filter wheel controller), that can provide more accuratelocal information about each exposure. For example, shutter opening/closing behaviour that cannot beaccounted for by the simple shutter delay setting in CICADA’s configuration. CICADA supports theseinstruments by providing a call to the exposure controller plug-in at the end of each exposure. The extraexposure information is added to the FITS headers along with standard exposure information.

Note that CICADA supports accurate timing of exposures that have been paused/resumed. Using exposurecontroller timing information provided by a plug-in might not be able to cope in these situations - check withthe local site to see if this is the case.

Optional Site Instrument FITS additions

For each configured site instrument CICADA allows for the addition of an arbitrary number of keywordswhich have been setup for the site instrument. These are configured as a table of keywords in a file set up(and probably rewritten for each exposure) by the plug-in. This file is re-opened and read at the end of everyexposure and the data is copied without interpretation - it is imperative that the formatting comply with tostandard FITS keyword formatting rules.

This feature allows for the support of site instrument specific keywords that CICADA needs to know nothingof.

Optional FITS Table

A simple copy of any data in the file /opt/cicada/config/fits_table is made (to the FITS file) if the file exists.


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This data is copied without interpretation, so it is important that it be formatted with standard eighty characterFITS keyword entries. CICADA provides no way of linking the contents of this file with the current exposureother that through other optional plug-ins. The file is re-opened and read after each exposure finishes and alsoafter the optional exposure-controller plug-in has been called. This gives the site the opportunity, forexample, to rewrite the file during the exposure controller plug-in - if necessary.

Optional FITS Plug-In

At the end of CICADA’s FITS file construction one last opportunity is given to the local site to modify thefinal FITS file. CICADA closes the FITS file and then, optionally, calls a FITS plug-in routine to update thefile with any extra information that cannot be provided by using any of the other methods described above.For example, the AAO 6dF instrument has FITS BINTABLE extensions that describe the configuration ofthe instrument for each exposure. This information can only be added through this FITS plug-in mechanism.

The disadvantage of using the FITS plug-in is the extra time required to read and rewrite a new FITS file.This cannot be avoided when other methods do not provide the required functionality.

Keyword Translation Table

The keyword translation table enables CICADA standard keywords from the dictionary in Table 7.1 to be rewritten so that they comply with site requirements. This table lives in the file/opt/cicada/config/keyword_translation_table. An example file is as follows and consists of simplekeyword name pairs, with the CICADA (IRAF) standard keyword name on the left.

Table 7.2: An example keyword translation table for CICADA.

The same table can also be used during IRAF data reduction to translate site keywords back to the standardnames expected by IRAF. See the IRAF help system for more information about keyword translation.

CICADA ScriptingIt is possible to write scripts in the Tcl language for use with CICADA. These scripts must be run fromwithin the CICADA observing window using the Run Cicada Script item from the Actions pulldown menu.CICADA starts a Tcl interpreter and passes the script to the interpreter for execution. CICADA commandsembedded in the script are read by the Tcl interpreter and passed back to CICADA for processing.

A CICADA command consists of the keyword cicada followed by a verb, optionally an instrument partname, and then optional parameter/value pairs. For example: cicada readout xo1=100 width1=100. The


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following table lists available verbs with associated parameters.

A CICADA command has the following structure:

[cicada] command [instrument_part_name] [parameter=value [parameter=value ...]]

For example:

expose dbs_red duration=100 do_save=1 do_display=1 run_number=100

will run an expose request on the dbs_red camera for 100 seconds saving and displaying the image.

The full CICADA command dictionary is detailed in the following table. The table is formatted into groupsof commands belonging to a particular context, each command is then given in bold followed by a set ofparameters.

The parameters are described with data type and default value enclosed in square brackets. For example, theparameter ‘‘comment [string , undefined]’’ is a string parameter with an undefined initial value. String valuescan be enclosed in double quotes. Boolean parameters take either 0 for false or 1 for true. List parametershave values separated by commas, for example ‘‘r_x=0,100,200’’. All parameter/value pairs are separated bywhite space.

CICADA also sets values of a set of global TCL variables that can be used inside a script. The table liststhese variables, if avaiable, next to each parameter’s default value, for example ‘‘object [string , undefined,CICADA_OBJECT]’’. They are always upper-case. As an example, one could make use of the variableCICADA_RUN_NUMBER as follows:

expose dbs_red duration=100 do_save=1 do_display=1 run_number=$CICADA_RUN_NUMBER

These global TCL variables are set at the start of a script and not updated during a script execution.

General Commands status Fetch current status of the instrument.

state [ boolean , false] If true, get only status structures without status messages.

abort Abort the current operation. Usually tries to do this in a clean way so sometimes could see smalldelay. Takes no parameters.set Set the value of a parameter for any other command. The set value remains current untilmodified by another set or specific command. The following list of parameters can only bechanged with set.

comment [string , undefined] Set an optional COMMENT FITS keyword.object [string , undefined, CICADA_OBJECT] Set an optional OBJECT FITS keyword.observer [string , undefined] Current observer name.prop_id [string , undefined] Current proposal id.read_mode [fast|medium|slow , undefined] Readout mode.auto_archive [boolean , undefined] True if FITS files to be archived to configured archive disk.imagetyp [string , undefined] Type of current observation.fitskw1 [string , undefined] Set first user-defined FITS keyword.fitsv1 [string , undefined]


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Set value of first user-defined FITS keyword.fitskw2 [string , undefined] Set second user-defined FITS keyword.fitsv2 [string , undefined] Set value of first user-defined FITS keyword.fitskw3 [string , undefined] Set third user-defined FITS keyword.fitsv3 [string , undefined] Set value of first user-defined FITS keyword.fitskw4 [string , undefined] Set fourth user-defined FITS keyword.fitsv4 [string , undefined] Set value of first user-defined FITS keyword.

script Execute a TCL script. Cicada runs a TCL interpretor to execute the script that has embeddedCicada commands.

cmds [filename , undefined] Identifies the name of a TCL script file - use a full pathname of a file on the observer’scomputer.

Camera Commands. These commands are specific to Cicada cameras.

get_state Get state of active components of an instrument - this command forces a reread of instrumentmeters rather than collecting state from current shared memory, as the status command does.

get_temps [boolean , true] Make a reading of the camera’s temperature sensors.get_volts [boolean , false] Make a reading of the camera controller’s voltages.get_filter [boolean , false] Get camera’s current filter position.

pause Pause the exposure. The shutter is closed and the system is ready for a change of exposure timeor repeat count - see command resume.resume Resume the exposure with optionally updated parameters.

duration [seconds , undefined] Resume with new exposure duration - this is expressed as a total exposure time, so anyexposure before the pause will be subtracted from this value.repeat [count , undefined] Readjust the exposure sequence counter.do_readout [boolean , false] Do a readout after resume.

init Run a camera initialisation sequence

config [boolean , true] If true then use configuration data from database, else use data from parameters in memoryand those set on this command line.do_warmup [boolean , true] Do a controlled warmup of the camera using specified warmup rates.warmup_step [degrees K , 5] Warmup at this step for each warmup interval.warmup_tol [degrees K , 3] Continue warmup until temperature is within this proximity to target temperature.warmup_interval [seconds , 600] The interval at which to apply the warmup step.setpoint [degrees , undefined] Temperature setpoint degrees K.


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flush Flush the CCDs of charge.

count [integer , 1] The number of times to perform the flush operation.

shutter Open the shutter for the specified duration.

unit [mseconds , 1000] The number of millisecond units.duration [integer , 1] The shutter unit counter. For example, if set to 1 with the unit set to 1000, then the shutterwill open for 1000*1 milliseconds.dark [boolean , false] If true, then the shutter is not opened - ie a dark frame.open [boolean , false] Direct open shutter flag. Interpreted when shutter command used alone.

readout Readout the CCD array. Use the parameters set to configure the readout.

do_save [boolean , true] save the exposure do_display [boolean , true] display the image clear_display [boolean , true] clear display frame_mode [boolean , false] separate frame display approx_scaling [boolean , true] true for faster integer scaling vis_instructions [boolean , true] faster ultra VIS instructions wanted camera_coords [boolean , true] camera coordinates, otherwise CCDwait_display [integer , 100] display timeout msecs display_levels [integer , 200] number display levels ccdmask [integer , 65535] which ccds on a mosaic to read out window [string , undefined] readout window name nregions [integer , 1] number of regions xo [integer list , 0] x offset of region yo [integer list , 0] y offset of region width [integer list , 0] width of regions height [integer list , 0] height of regions overscan_cols [integer , 0] number overscan columns overscan_rows [integer , 0] number overscan rows rcf [integer , 1] row compression factor ccf [integer , 1] column compression factor


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adaptive_scaling [boolean , true] auto adapt scaling contrast [double , 0.5] contrast adjustment (0-1) rescale_tol [double , 0.1] sigmas diff before rescaling rescale_rate [double , 0.1] rescale rate - fraction of image sample_pix [integer , 1000] number of pixels to sample display_min [double , 0.0] fixed min scaling display_max [double , 65535.0] fixed max scaling display_xmag [integer , 1] display row zoom display_ymag [integer , 1] display column zoom hotpix_val [double , 65535.0] hot pixel value do_hotpix [boolean , false] mark hot pixels in red scaling_type[mode|median,mod] adaptive scaling type run_number [integer , undefined, CICADA_RUN_NUMBER] run number for FITS header bitpix [integer , 16] number of bits per pixel bscale [double , 1.0] FITS scaling factor bzero [double , 0.] FITS Offset factor out_dir [directory , undefined, CICADA_OUT_DIR] output directory out_prefix [string , undefined, CICADA_OUT_PREFIX] output filename prefix out_suffix [string , undefined, CICADA_OUT_SUFFIX] output filename suffix

expose Run an exposure sequence. This command would normally run a flush, shutter and readout in sequence to complete, so all parameters for these commands can be set here as well. Thecommand also has a few specific parameters.

do_readout [boolean ,true] optionally do the readout do_flush [boolean , true] optionally do the flush repeat [count , 1 ] exposure repeat count

focus Run an focus sequence. This command would normally run a flush, shutter and readout in sequence to complete, so all parameters for these commands can be set here as well. Thecommand also has a few specific parameters.

focus_steps [count , 5] number of focus steps do_flush [boolean , true] optionally do the flush

drawrect This command draws a set or rectangles of a specified colour on the image display.

n_rects [integer , 0]


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number rectangles to draw.r_colour [colour number , BLUE] rectangle colourr_x [integer list , 0] x position of rectanglesr_y [integer list , 0] y position of rectanglesr_width [integer list , 0] width of rectanglesr_height [integer list , 0] height of rectangles

set_filter Set a new filter position.

filter_pos [integer , 0] The numerical position of the required filter.

Sdsu Commands. These commands are for the SDSU I and II CCD controllers.init Extra initialisation parameters can be set for the SDSU in addition to the standard cameraparameters.

do_long_test [boolean , false]

do_short_test [boolean , false]

do_reset [boolean , false]

do_power_on [boolean , false]

pon_timeout [integer , false] Timeout for performing a power-on - secs.clr_timeout [integer , false] Timeout for performing a flush - secs.do_tim_board [boolean , false]

do_tim_download [boolean , false]

do_util_board [boolean , false]

do_util_download [boolean , false]

do_target_temp [boolean , false]

do_heater_adu [boolean , false]

do_gain [boolean , false]

do_tc [boolean , false]

do_ab [boolean , false]

do_idle [boolean , false]

do_test_pattern [boolean , false]

test_pattern_constant [boolean , false]

test_pattern_constant_val [integer , 0]


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test_pattern_seed_val [integer , 0]

gain_setting [integer , 0]

tc_setting [integer , 1]

ab_setting [integer , 0]

idle_set [boolean , false]

auto_rdc [boolean , false]

tim_set [boolean , false]

util_set [boolean , false]

tim_filename [string , undefined]

util_filename [string , undefined] dsp_cmd This command sends a specific DSP command directly to the hardware. To be used for low leveltesting of specific actions.

board [integer , undefined] cmd [sdsu_cmd , undefined] memory_space [P|X|Y , undefined] address [integer , undefined] data [integer , undefined]

set_clock clk,hl,bd [string , undefined] Change a clock parameter, where clk is name of clock, hl is either hi or lo and bd is board number.set_bias bias,bd [string , undefined] Change bias parameter.set_board_param par,bd [string , undefined] Change board parameter.set_param par [string , undefined] Change parameter.set_board_define def,bd [string , undefined] Change board define.set_define def [string , undefined] Change define.build_dsp Rebuild DSP code with new parameters

Astromed 3200 Commands These commands are specific to the Astromed 3200 controller.

init Specific Astromed 3200 initialisation parameters in addition to standard set.tc [integer , undefined] time constant pgain [integer , undefined] programmable gain ccdi [integer , undefined] integration time ccds [integer , undefined] serial transfers ccdp [integer , undefined] parallel transfers

volts This command runs the Astromed volts sequence, where voltages are read back and reported in acontinuous loop.


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mode [integer , undefined] Mode of volts monitoring, either 1=BIAS, 2=CLOCK or 3=TEMPS.iterations [integer , undefined] Number of iterations to run the cycle.

set_volts Set a particular voltage value.

vod [volt , undefined] controller voltages.vog [volt , undefined] vrbg [volt , undefined] vrd [volt , undefined] vabg [volt , undefined] vabd [volt , undefined] vssl [volt , undefined] vssh [volt , undefined] ids [volt , undefined] vrol [volt , undefined] vroh [volt , undefined] vrspl [volt , undefined] vrsph [volt , undefined] viml [volt , undefined] vimh [volt , undefined] vstoh [volt , undefined] vtherm [volt , undefined] userp [volt , undefined]

TipTilt Commands Commands specific to the Tiptilt camera are:

change_state

Dummy Camera Commands. These commands are for the simulation CCD controllers. This allows fortesting of the CICADA data flows when no hardware is attached. A standard FITS image is used forinput data. Alternatively by specifying GENERATE_DATA as the input image, test data is generated.

readout Extra readout parameters need to be set for the dummy controller.

in_image [string , undefined] name of input FITS file.pixel_time [double , 3.4] time delay to clock a pixel (usecs).

Telescope Plugin Commands Cicada supports a simple interface to the local telescope control system, through the use of a plugin.

telescope_get_data Get all standard CICADA FITS header keywords from the TCS.timeout [integer , undefined] Command timeout

telescope_get_param Get the value of a particular parameter from the TCS.timeout [integer , undefined] Command timeout.param [string , undefined] Name of parameter to get.

telescope_set_param Set the value of a particular TCS parameter.timeout [integer , undefined] Command timeout.param [string , undefined] Name of parameter to set.value [string , undefined] Value to set parameter.

telescope_command Run an arbitrary telescope command.timeout [integer , undefined]


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Command timeout.command [string , undefined] Name (and parameter list) of command to run.

Filter (Exposure Controller) Plugin Commands Cicada supports a simple interface to the local filter wheel controller (sometimes named exposurecontroller), through the use of a plugin. The following filter controller commands are supported.

get_filter Gets the current filter position.timeout [integer , undefined] Command timeout.

get_filter_exposure_info Get exposure information from the filter controller if available.Returns exposure start time, exposure duration, filter name and filter position.

timeout [integer , undefined] Command timeout.param [string , undefined] Name of parameter to get.

set_filter Sets the filter position.timeout [integer , undefined] Command timeout.filter_pos [integer , undefined] Filter position to set.

Site Instrument Control Plugin Commands Cicada does not interpret commands for site instruments, so support for a simple interface is providedwith an arbitray string command. The site instrument plugin can interpret the string as required.:

site_command Only command supported for site instruments - takes two parameters:command [string , undefined] Site instrument command string.timeout [integer , undefined] Command timeout.

Example scriptsFollowing are some simple script examples showing, for instance, the use of global CICADA Tcl variables,Tcl looping, Tcl local variables, Tcl error handling, quoted strings etc.

Exposures with different filters.

# Sample Cicada TCL script for reading out a CCD with different filter# settings. In this instance, the filter wheel is controlled through the # camera interface.#set filter 1# Set exposure parameterscicada set width=416 height=578 XO1=0 YO1=0 cicada set DO_SAVE=1 DO_DISPLAY=1 DARK=0 DO_READOUT=1cicada set UNIT=1000 DURATION=5 REPEAT=1 cicada set out_dir=${CICADA_OUT_DIR} out_prefix=${CICADA_OUT_PREFIX}cicada SET object=\"${CICADA_OBJECT}\"cicada set comment=\"This is a comment\"

# Loop to read 3 images, automatically incrementing run_numberfor {set i 0} {${i} < 3} {incr i 1} {# remove the temporary image if already there, catch any failures catch {exec /bin/rm -f /tmp/IM${i}.fits}# execute an expose request - abort script if an error occurs set filter [expr ${filter} + ${i}] cicada set_filter filter_pos=${filter} set run [expr ${CICADA_RUN_NUMBER} + ${i}] cicada EXPOSE RUN_NUMBER=${run} comment=\"Exposure ${i} of script\"}

1.

Following script shows how to command a telescope instrument control module and take some data.2.


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# Sample Cicada TCL script for slewing the telescope and taking some # exposures#

cicada set width1=100 height1=100 XO1=0 YO1=0 cicada set DO_SAVE=1 DO_DISPLAY=0 DARK=0 DO_READOUT=1cicada set UNIT=1000 DURATION=5 REPEAT=1 cicada set out_dir=${CICADA_OUT_DIR} out_prefix=${CICADA_OUT_PREFIX}cicada SET object=\"${CICADA_OBJECT}\"for {set i 0} {$i < 1} {incr i 1} {# remove the temporary image if already there, catch any failures catch {exec /bin/rm -f /tmp/IM${i}.fits}# execute an expose request - abort script if an error occurs set run [expr ${CICADA_RUN_NUMBER} + ${i}] cicada telescope_command T_APT command=\"coord 12 13 14.5 -23 12 13 slew\" cicada telescope_get_data T_APT cicada EXPOSE RUN_NUMBER=${run}}cicada telescope_command T_APT command=\"coord 20 13 14.5 -15 12 13 slew\"cicada telescope_get_data T_APT

CICADA Debug LevelsTo increase the diagnostic output from CICADA, the debug level needs to be modified. This debug leveloperates as a mask and the values in Table9 are used for assistance during troubleshooting diagnosis. Thelevel can be set as a command line switch when starting CICADA or from the Cicada Configuration dialogwhen running in Engineering Mode.

Table 9.1: Debug levels for CICADA

Level Name Output Description

0 Show nothing

1 DEBUG_ESSENTIAL Essential debugging info

2 DEBUG_ENTRYPOINTS Entry point messages

4 DEBUG_INDICATORS Tracewrites to indicate location

8 DEBUG_CALCS Progressive calculations

16 DEBUG_STATUS All status handling

32 DEBUG_SPECIAL Special case temporary debugging

Known BugsThe free disk space shown in the Mb free field does not give the correct amount of free space availableto the observer on quota controlled disks (e.g. /home, /book disks). The figure displayed will be thetotal free space on the disk and not the space remaining in the user’s quota.When using the SDSU controller for the WFI, during readout an occasional buffer overflow occurs.This results in missing data in the top four CCDs. At present the observed rate of these failures is lessthan 1/100. The top half of the mosaic image from WFI should be discarded.

TroubleshootingThings don’t work: Most problems with CICADA are resolved by quitting and restarting the software.So, the first thing to try if there are problems is quitting CICADA and starting up again. WhenCICADA starts up it looks for and kills any old CICADA processes as well as initialising operatingsystem resources that are needed by the software. Note that for the Astromed 3200 controller this does


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not mean you need to do another hardware initialisation. Unlike the Astromed Imager software,CICADA does not require you to go through the HWINIT procedure upon restart. If problems stillpersist, and you suspect the software, contact the Computer Section for help.Things still don’t work: make sure your home area is not full. Run the command quota -v and make sure you have not hit your hard disk limit. CICADA writes preferences and log files in your home areaand insufficient free space can cause problems.Noise levels rising: Check the temperature of the CCD and/or try re-initialising the controller.Low memory - performance affected: CICADA and GIT can be very memory hungry, depending onthe size of images being taken. Keep a close watch on the memory warning indicators both programshave. In the case of GIT, a list of images is maintained - only one of which is loaded into memory atany one time. These could be floating point images, thus requiring four bytes or memory per pixel. Sometimes the system fails to free space occupied by previously loaded images - the space has becomefragmented - it is probably a good idea to stop and restart GIT. In general stopping and restarting bothCICADA and GIT is fast and easy, these problems are then managed.

About this document ...CICADA V3.1 User’s Manual

This document was generated using the LaTeX2HTML translator Version 99.2beta8 (1.43)


The command line arguments were: latex2html -init_file /opt/local/html/latex2html/cicada.init cicada.tex

The translation was initiated by Hoa Nguyen on 2000-12-13

[email protected]

CICADA V3.1 Writing Plug-Ins http://www.mso.anu.edu.au/computing/cicada/cicada_plugins/cicada_pl...

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CICADA V3.1 Writing Plug-Ins



December 13, 2000

User Plug-In Extensions to CICADAV3.0 of CICADA supports the concept of a user plug-in. This feature extends the capabilities of CICADA sothat local site conditions are handled. Specifically, plugins can be written for:

An interface to a local telescope control system (TCS)1.An interface to the local filter (exposure) controller.2.Interfaces to other site instrument controllers.3.A FITS plug-in for modifying the contents of each FITS file at the end of each exposure.4.Site-specific GUI plug-ins to interface to the low level control plug-ins.5.

Figure 1.1 shows how these plug-ins fit into the CICADA design. The shaded boxes represent the plug-incode written to support local requirements.

Figure 1.1: CICADA Plug-In Architecture


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ImplementationPlug-ins are implemented though the use of shared libraries. The user writes a plug-in that conforms with theCICADA C++ API and then builds the shared library using the supplied makefile. The built shared libraryreplaces the default supplied shared library for the particular facility.

The API is defined with the remote procedure call language (RPCL) and is compiled using the "rpcgen"command to generate a "C" header file, which is then referenced in the user plug-in. RPC is used so thatplug-in code can run on a machine remote from the user’s workstation. This functionality is transparent to theuser.

Template and include files are supplied in the directory structure under /opt/cicada/user_libs where shared libraries can be rebuilt after modification/addition of site specific plug-ins. Once built the shared libraryshould be moved to /opt/cicada, replacing the shared library that was already installed. Care should be takento make a copy of the original shared library in case problems occur.

The plug-in facility requires the use of a recent version of the Sun C++ compiler. GNU compilers (or anyother C++ compiler) will not work since C++ object files from different compilers cannot be linked.

For the GUI plug-ins the user is required to write a C++ Motif class that inherits basic attributes from a SunWorkshop Visual generated C++ GUI definition. Though not necessary to use Visual to generate the plug-in,it is recommended for simplicity - and in that way the CICADA simple_control GUI can be included as a base definition.

Telescope Control System InterfaceCICADA’s interface to the telescope control system is through the shared library libtelescope.so. The interface requires that the following functions be written by the user, where the User_Telescope class isderived from the base Cicada_Telescope class:

Cicada_Telescope* create_telescope_object(Cicada_Telescope_Desc tel, int do_connect, FILE* report,int debug)

Takes as input a Cicada_Telescope_desc which describes the characteristic of a particular telescopeincluding its name. Based on this name a new User_Telescope instance is created.

int User_Telescope::get_data(int timeout)

Retrieves all available telescope data as described in the Cicada_Telescope_Data structure which is defined using the RPCL definition. This might consist of a series of individual get_param calls to make up the full data structure.

int User_Telescope::get_param(char* parameter, char* value, int timeout)

Gets the value of an arbitrary (locally defined) telescope parameter. Sets Cicada_Tele_Config with retrieved value.

user_telescope::set_param(char* parameter, char* value, int timeout)

Sets the value of an arbitrary telescope parameter.

int User_Telescope::command(char* command, char* value, int timeout)

Runs an arbitrary command which might have an associated parameter value. Sets Cicada_Tele_Configwith retrieved result of command.


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Supplied with CICADA is an example implementation of a plug-in: mssso_telescope.cc. This example provides support for the current MSSSO telescopes and is, perhaps, a little more complex than needed formost cases. However, the user should easily be able to follow this example to construct a new plug-in andthen modify the supplied Makefile to build it.

The definition Cicada_Telescope_Desc for a user telescope is maintained through the standard CICADAconfiguration GUI. This GUI allows the user to create a new named telescope with specified interfaceinformation such as controlling host, available data etc. Currently, both serial line and unix socket support areavailable for communicating with a telescope computer.

Filter Control System InterfaceCICADA’s interface to a filter controller is through the shared library libfilter.so. As for the telescope interface, a user filter class, derived from Cicada_Filter needs to be written. The following functions need tobe supplied:

Cicada_Filter* create_filter_object(Cicada_Filter_Desc filter_desc, int do_connect, FILE* report, intdebug)

Takes as input a Cicada_Filter_Desc which describes the characteristics of a particular filter includingits name. Based on this name a new filter instance is created.

int User_Filter::get(int timeout)

Returns as much of the information a filter can deliver for the CICADA filter data structure. This is setin the filter objects filter_status member variable.

int User_Filter::set(char* value, int timeout)

Sets the filter to value requested.

int User_Filter::get_exposure_info(int timeout)

Returns as much of the information a filter can deliver for the Cicada_Exposure_Ctl_Info data structure. This is set in the filter objects filter_status member variable.

Again, the example mssso_filter.cc is provided to show how a user filter plug-in can be built.

Site Instrument Control System InterfaceCICADA’s interface to an arbitrary site instrument controller is through the shared library libsiteinst.so. As for the telescope and filter interfaces, a site instrument class, derived from Cicada_Site_Instrument, needs to be written. The following functions need to be supplied:

Cicada_Site_Instrument* create_siteinst_object(Cicada_Site_Instrument_Desc siteinst_desc, intdo_connect, FILE* report, int debug)

Takes as input a Cicada_Site_Instrument_Desc which describes a particular site instrument includingits name. Based on this name a new site instrument instance is created.

int User_Siteinst::command(char* command, int timeout)

Runs an arbitrary command which might have embedded parameter value information. CICADA doesnot interpret command in any way.

Again, the example mssso_siteinst.cc is provided to show how a user site instrument plug-in can be built.


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FITS Plug-inThe shared library libfits_plugin.so contains the users FITS plug-in code. This is called to update a FITSfile at the end of an exposure. The plug-in must supply a function to create an instance of aCicada_Fits_Plugin, which must be the base class of a user defined object.

Cicada_Fits_Plugin* create_fits_plugin_object(Nametype fits_plugin_name, FILE* report, intdebug_on)

Simply takes the name of the the FITS plugin object to create.

int User_Fits_Plugin::update(char* fits_name)

Takes the name of a fits file to update.

The example mssso_fits_plugin.cc is provided to show how a user fits plug-in can be built.

GUI Plug-insGUI plug-in derived class must include as part of its ‘‘public’’ definition the declarations provided insimple_control_public.h. simple_control_public.h has the following public methods which must beimplemented by the plug-in:

void Simple_Control_c::initialise_control()

Called immediately after the creation of the telescope GUI by CICADA, allows the plug-in to performarbitrary initialisation steps.

void Simple_Control_c::start_status_check()

CICADA calls this routine when it wants the GUI to start a telescope interface status check. This isusually in response to a CICADA initiated query to the telescope interface which would then requirethe plug-in to perform a display update of status.

void Simple_Control_c::handle_status(void *this_status, int idle)

This function must be provided so that CICADA can pass a pointer to a Cicada_Telescope_Statusstructure. CICADA calls this routine after the the telescope interface returns status in response to theplug-in calling the send_command callback. The GUI can then update its window based on the statusinformation.

Telescope GUI Plug-in

CICADA’s interface to the telescope GUI is through the shared library libsimplegui.so. The GUI requires that public methods be written by the user, where the User_Telescope_GUI class is derived from the baseSimple_Control_c class. The plug-in must provide a GUI creation function create_telescope_control that returns a pointer to the Simple_Control_c object. This definition is provided in the headercicada_simplegui.h.

Simple_Control_c* create_telescope_control(Widget parent, Cicada_Telescope_Desc *tel)

This routine must be provided by the plug-in. CICADA calls it in response to a trigger to popup thetelescope GUI. CICADA passes as input a Cicada_Telescope_Desc which describes the characteristicsof a particular telescope including its name. Also provided as input is the name of a parent X11 widgetfor the telescope GUI. Two callbacks are provided, one for handling telescope commands which the


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plug-in uses and the other for requesting command status. These callbacks must be used by the plug-infor accessing the telescope interface from within CICADA. Based on this information a newUser_Telescope_GUI instance is created and returned by the plug-in.

Filter GUI Plug-in

CICADA’s interface to the filter GUI is also through the shared library libsimplegui.so. Again, the User_Filter_GUI class is derived from the base Simple_Control_c class and the plug-in must provide a GUIcreation function create_filter_control that returns a pointer to the Simple_Control_c object. Thisdefinition is provided in the header cicada_simplegui.h.

Simple_Control_c* create_filter_control(Widget parent, Cicada_Filter_Desc * filter)

This routine must be provided by the plug-in. CICADA calls it in response to a trigger to popup thefilter GUI. CICADA passes as input a Cicada_Filter_Desc which describes the characteristics of aparticular filter including its name. Also provided as input is the name of a parent X11 widget for thefilter GUI. Two callbacks are provided, one for handling filter commands which the plug-in uses andthe other for requesting command status. These callbacks must be used by the plug-in for accessing thefilter interface from within CICADA. Based on this information a new User_Filter_GUI instance iscreated and returned by the plug-in.

Site Instrument GUI Plug-in

As for the telescope and filter GUI plug-ins a number of site instrument interfaces can be supported throughthe GUI plug-in mechanism. Any interfaces built must also be included in the shared librarylibsimplegui.so. And a GUI creation create_siteinst_control must be provided.

Simple_Control_c* create_siteinst_control(Widget parent, Cicada_Site_Instrument_Desc *siteinst)

Its definition is similar to those for telescope and filter plug-ins.

Error HandlingAll plug-in functions are designed to handle a returned integer which indicates error status. If an error occurs,the plug-in should set this return status to a non-zero value and fill the telescope or filter integer valid and string error variables with appropriate values.

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CICADA V3.1 Configuration Manual http://www.mso.anu.edu.au/computing/cicada/cicada_config/cicada_conf...

1 of 11 16/05/05 11:41 AM

CICADA V3.1 Configuration Manual



December 13, 2000

Contents

ContentsIntroduction

Design of the TablesThe Table Hierarchy

IntroductionViewing the tablesThe Tables

The Instrument Table - the top levelCamerasCCD ControllersCCDsDewarsfocalplanesFilter WheelsTelescopesInstrument ControllersTemperature Sensor TypesTemperature SensorsCICADA Table

Modifying the tablesIntroductionAdding Entries

In General


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GuidelinesModifying EntriesDeleting EntriesWhen is it necessary to restart CICADA after changing Tables?Instrument Changeovers


IntroductionThis document describes the use of the CICADA configuration tables.

Design of the TablesEarly releases of CICADA had many built-in site-specific sections of code which meant that it was verydifficult to ‘‘export’’ to other observatories. One of the aims of CICADA v2 was to replace these sections ofthe code with ‘‘self-configuring’’ code based around simple ASCII tables.

Another aim of releases 2 and later of CICADA was to provide support for multi-controller, multi-CCDinstruments. This requirement also impacted on the design of the Configuration Tables.

The Table Hierarchy

IntroductionAn instrument is specified using relational type text tables arranged in a hierarchy. The following diagram 2.1depicts an instrument consisting of a camera with a dual CCD focalplane and a single ‘‘simple instrument’’controller.

Figure 2.1: Example instrument component hierarchy

The dashed lines in the diagram indicate that multiple components can be configured. Each node in thediagram is described by an entry in one of the component tables and is referenced by a component name.Each entry occupies a single named item in the text table with fields indicated by namevalue pairs. A typicalentry from the camera table looks like this:


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[DUMMY_WFI] comment=Dummy camera with 2 controllers; config1=; config2=; cont_master=1,0; cont_shutter=1,0; cont_temp=1,0; cont_xgap=0,0; cont_xo=0,0; cont_ygap=0,0; cont_yo=0,4096; controller1=DUMMY1; controller2=DUMMY2; dewar=DUMMY; host=mistress; ihu=2; n_controllers=2; phu1=3; phu2=3; shutter_closed_when_idle=1; shutter_delay=0; synchronise_readout=1;

This entry describes the camera called DUMMY_WFI which is hosted on mistress. It has two CCD controllers named DUMMY1 and DUMMY2 and is mounted onto dewar named DUMMY and does not have a filter wheel.Controller positioning information is given by vectors cont_xo and cont_yo. Flags are set indicating whichcontroller controls the shutter and temperature sensors and which is the master. The size of generated FITSheader units is given by phu and ihu. Parameters for shutter_delay and synchronisation during readout are also available.

Once an instrument is described by the configuration tables, it can be selected from the user interface and thenecessary processes are started on the configured computers. Configuration tables are maintained either by atext editor or through the CICADA table GUI interface (accessed via the Hardware Configuration option ofthe Options menu).

Viewing the tablesWhen viewing/editing the configuration tables using the CICADA GUI, the window in figure 2.2 is displayed. Simply edit the fields as indicated and click the Apply button to rewrite the table.

Figure 2.2: CICADA Hardware Configuration GUI

As indicated in figure 2.2 use the Category popup menu to select a table for editing. The GUI will thendisplay the available fields for that table - be careful to select the desired item for editing from the scroll-ablelist. Use the Add and Delete buttons to change the number of items in the list for each table. Moreinformation on modifying the CICADA configuration tables is contained in chapter 3.


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The Tables

The Instrument Table - the top level

CICADA is used to control data acquisition instruments and associated simple components controllers.These instruments are made up of one or more cameras, zero or more instrument controllers and (optionally) a connection to a telescope system.

To make the instrument available from CICADA’s Start Observing menu click on the Available at this sitetoggle. To enable CICADA to write an observing proposal id into the FITS file headers, select Require Proposal ID for FITS. This is a site-dependent option, it requires that a relational database be available withobserving proposal information. Currently CICADA uses the free MySQL package for implementing arelational database.

Finally, site archiving of data is supported by CICADA. If an archiving directory is entered in the Archive Directory field a second copy of the FITS file is made and placed in the specified directory with anobservation identification style filename.

Cameras

Cameras are made up of several components - the dewar, focalplane, temperature sensors, CCD controllers,possibly filter wheels and CCDs. As explained above, these are configured using the instrument tables in arelational fashion. The format of each of these tables is described below. Figure 2.3 shows the GUI forediting the camera table.

Figure 2.3: CICADA Camera Table

CCD Controllers

The entries in this table tell the CICADA software the type of controller in use, the names of the CCDsconnected to that controller and their geometry specified in ‘‘controller coordinates’’ (i.e. if using a mosaic of8k x 8k pixels, this table holds the information that allows the software to determine where an individualCCD sits inside the 8k x 8k coordinate space). Figure 2.4 shows the GUI for editing the controller table.


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Figure 2.4: CICADA Controller Table

CCDs

Each entry in this table describes the size and amplifier geometry of a CCD. The values entered in this tableare used in conjunction with the controller geometry to assemble the FITS file and image display generatedby CICADA. Figure 2.5 shows the GUI for editing the CCD table.


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Figure 2.5: CICADA CCD Table

Dewars

At present, for the purposes of CICADA, dewars contain nothing but a focalplane.

focalplanes

Each entry in the focalplane table describes the parameters to do with CCD temperature control. There aresettings here for controlling the rate at which a CCD will be warmed up as well as temperature setpoint andparameters for heater control and temperature sensor min/max values. Figure 2.6 shows the GUI for editingthe focalplane table.


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Figure 2.6: CICADA focalplane Table

The function of some of these fields are controller dependent. At the time of writing, CICADA supports theAstromed 3200 controller (AM3200) and the Leach SDSU Generation 1 and 2 controllers. The heaterparameters are not used when the controller is an AM3200. Additionally, because many features which areconfigurable with the Leach controllers are ‘‘hard-wired’’ in the AM3200, the specification of temperaturesensors for the AM3200 MUST be as follows:

CCDTEMP1, hardware number 0CCDTEMP2, hardware number 1LN2, hardware number 2PCBTEMP, hardware number 3

In addition, CCDTEMP1 must have the Is Setpoint Temp turned on.

Filter Wheels

This table provides the mapping between filter wheel position and filter name (the name added to FITS fileheaders). Note that filter wheels may be controlled directly from a Unix host or from a CCD controller. If viaUnix then either through a serial line or across the network via a socket. Enter the relevant host and portdetail required. Figure 2.7 shows the GUI for editing the filter table.


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Figure 2.7: CICADA Filter Table

Telescopes

This table holds configuration items relating to CICADA’s communication with Telescope Control Systems(TCS). As for filter wheels access to a TCS is via a Unix host serial line or socket interface. Figure 2.9shows the GUI for editing the telescope table.

Figure 2.8: CICADA Telescope Table

The CICADA TCS interface is through a site-specific plug-in. Standard data items are delivered by theplug-in for insertion in each FITS file - items that are available for each site telescope are indicated bychecking the toggle buttons on this window. Take particular note of the Focus toggle - if this is checked, CICADA will try to use the FOCUS command to set the telescope focus for automated focus sequences.

Instrument Controllers

CICADA supports control of instrument hardware in addition to CCD controller hardware. The Instrument Controller table is used to store instrument controller configuration items. Instrument control consists ofpassing instrument specific commands and setting/getting parameters.

Specific support is available for interfacing to the local telescope control system and the instruments filter


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(exposure) controller.

More generic support is available for site-specific instruments. Here CICADA will allow the specification ofsimple instrument controls and provide no interpretation of any I/O to and from the controller.

Figure 2.9 shows the GUI for editing the telescope table.

Figure 2.9: CICADA Telescope Table

Temperature Sensor Types

This table allows for the specification of temperature sensor types to be controlled by and connected to aLeach SDSU controller. The entries in this table contain coefficients for converting ADUs output by thesensor to temperature. As temperature sensors are usually acquired in batches and the individual sensors ofeach type will have nearly identical characteristics, each entry in this table can be re-used many times as thetemperature sensor type in the focalplane table. If individual sensors require minor changes to a standardtype, they should be specified in the Temperature Sensor Table.

Temperature Sensors

The entries in this table inherit characteristics from one of the ‘‘standard’’ temperature sensor types definedin the Temperature Sensor Types Table. Changes can be made to the polynomial coefficients where theyvary from the standard values.

CICADA Table

This table holds a few software settings such as CICADA administrators e-mail address and group name aswell as a location for CICADA logs.

Modifying the tables

IntroductionThe GUI which allows modification of the tables is accessed by selecting Hardware Configuration from the


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Options menu, either from the CICADA main window or the Observing Window. This menu item is notavailable to users who are not members of the CICADA administrators group.

Once the window is visible, you will see the Instrument Table with the entry names of the table displayed inthe scrolling list on the left and the details of the first Instrument in the table displayed on the right.

At the top of the window is a popup menu which gives access to the other tables. When another table isselected, the scrolling list will change to show the entry names of that table and the details section of thewindow will show the first entry in the table (or the entry most recently selected from the scrolling list thelast time that table was selected for viewing).

Depending on the speed of the workstation you are viewing the tables from, you may see the GUIconstructing itself as you move from table to table or entry to entry. This is because the GUI is builtdynamically based on the contents of the table entries.

Adding Entries

In General

The easiest way to add a new entry to a table is to select an entry from the scrolling list which is similar to theone you wish to add and then click the Add button below the scrolling window. This will make a copy of theselected entry and blank out the name ready for you to key in a new name and modify any fields as necessary.

If you are building the tables from scratch, just click the Add button and then enter the values in the fields asrequired.

Note that not all fields have bounds checking or checks for correctness, so make sure you key details incarefully.

Note also that the new entry is not really in the table until you click on the Apply button or the Ok button (the Ok button performs an Apply and dismisses the window).

If you change your mind about adding the new entry, you can click on the Delete button to remove it.

Guidelines

If you are constructing a new instrument, the easiest way to set up the tables is to work from the bottom up.i.e. define the entries in the tables lower in the table hierarchy before the new entries in upper tables of thehierarchy. e.g. in the example shown in 2.1, you would define the tempsensors, then the focalplane, then thedewar, followed by the CCDS, the controller, the filter, then the simple instrument control and telescope andfinally the instrument itself.

Modifying EntriesModifying an entry is simply a matter of selecting it from the scrolling list, making the required changes andselecting the Apply button or the Ok button.

Deleting EntriesTo delete a table entry, select it from the scrolling list and click on the Delete button beneath the scrollinglist. CICADA will check to see if the table entry you are trying to delete is in use by any other tables higherup in the hierarchy and will display an error if this is the case and not allow the delete to proceed.


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Once you have succeeded in deleting the entry from the table click on the Apply button or the Ok button to write the changes to disk.

When is it necessary to restart CICADA after changing Tables?Most changes do not require a full CICADA restart. However, if you modify the configuration while anobserving window is open, you will need to quit and restart the observing window for your changes to takeeffect. (This is because the tables are read once when an observing window is opened and used to configurethe sub-processes which are started. Changes made to tables are not communicated to already runningsub-processes.)

If you modify the Cicada Table, you must quit and restart CICADA for changes to take effect.

Instrument ChangeoversLet us suppose that your site has a telescope with cassegrain and coudé focii and that there are several CCDsin common use at either of these focus positions. There are two approaches to setting up the CICADA tablesto cope with changeovers in this case. One is to define all the CCDs and controllers and just have twotop-level Instruments (one for cass and one for coudé). Then, each time there is a changeover someone willneed to go through the hierarchy of tables and make sure that all settings are correct.

Depending on the complexity of the situation at your site, a better approach might be to have multipleinstruments set up for all common configurations, so that you might have instruments named ‘ ‘Cass CCD1SDSU1’ ’ , ‘ ‘Cass CCD2 SDSU1’ ’ , ‘ ‘Coudé CCD1 AM3200’ ’ , etc. This way, the tables need only be set uponce and rarely modified. All that the changeover staff need to do is make one instrument ‘ ‘available’ ’ andthe other unused setups ‘‘unavailable’’ using the Available at this site toggle in the Instrument Table entry.

About this document ...CICADA V3.1 Configuration Manual



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Graphing and Imaging Tool V3.0 User’s Manual http://www.mso.anu.edu.au/computing/cicada/git/git.html

1 of 25 16/05/05 11:41 AM

Graphing and Imaging Tool V3.0 User’s Manual



May 29, 2001

Contents

ContentsList of FiguresIntroduction

Starting GITFrom CICADAStandalone

The User InterfaceMenu Bar

The File MenuThe Image MenuThe Vector MenuThe Options MenuThe Help MenuKeyboard Accelerators

Toolbar Button AreaImage ListInformational TextGraphics Help TextPreferences

Preferences FileFITS Files

PreferencesReading an ImageUnloading an ImageWriting an ImageFITS Headers

WARNING : FITS Header InformationImage Operations

2-Dimensional ImagesImage DisplaySub-ImagesHardcopy

1-Dimensional ImagesImage DisplaySub-image ExtractionHardcopy


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ManipulationStoring an Image in MemoryHardcopyImage Statistics

2-Dimensional Images1-Dimensional ImagesPreferences

Image ArithmeticResultsError Checking

Image Object ProfilesPreferencesUse

Full Width Half-Maximum2-Dimensional FWHM1-Dimensional FWHM

Focus FittingMiscellaneous

CICADA ModeImage DisplayPreferences

QuittingGetting HelpLimitations

Sample $HOME/.gitrc Preferences FileBibliographyIndexAbout this document ...

List of Figures

GUI upon initial startup1.GUI toolbar buttons2.Popup window for image display Preferences3.X-Y slice from pixel (36,204) to (374,220) of the image ccd0698.fits not summing any additional rows, with no sky subtraction, and not zoomed.

4.

Popup window for the Vector display Preferences5.Popup window for the image Statistics Preferences6.Arithmetic popup window7.Popup window for the Star Profile Preferences8.Popup window for the Focus Fitting parameters9.Popup window for the General Preferences10.

IntroductionAs a part of the CICADA system MSSSO astronomers identified the need for a quick look window-basedtool that would allow some basic interactive manipulation and display of raw CCD data. To this end theGraphing and Image Tool (GIT) was devised..

The GIT is not designed to be an image reduction facility but simply to provide basic functionality(e.g. display, statistics, basic arithmetic, and I/O). It operates on FITS [1] files, and as such can be used intandem with versions of IRAF (Image Reduction Analysis Facility, KPNO).

This manual describes version 3.0 of the GIT.


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Starting GIT

From CICADA

When running the CICADA software the GIT and image display can be started up via the Tools menu. Formore details see Chapter and the ‘‘CICADA User Manual’’ [2].

Standalone

The GIT can also be operated independently of CICADA in standalone mode. To start up the GIT simplytype /opt/cicada/git [optional parameters] (see Section for optional parameter details). This will fireup the GIT graphical user interface (GUI) and the image display.

Optional Parameters

The GIT accepts the standard X11 optional parameters (e.g. geometry, colour, etc) as well as:

-imagedir directoryDefault directory to read and write images and FITS files from and to. If not specified the directoryfrom which the GIT was started is used.

-cicada nThe GIT will be started in CICADA mode. See Chapter for details.

-debugSwitches on debug mode.

The User Interface

The GIT user interface (Figure ) was designed and constructed using a GUI builder. It is an X-windowbased GUI built from Motif widgets, with a few extra specialist widgets.

Figure: GUI upon initial startup


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The GUI is comprised of six distinct and separate areas :

Menu Bar (Section )Toolbar Button area (Section )(scrollable) Image List (Section )(scrollable) Messages area (Section )Help text (Section )Graphics Help text (Section )

Menu BarThe menu bar contains pull-down menus (File, Image, Vector, Options and Help). These menus can beactivated with either left or right mouse button. Single clicking will pop the menu up. Holding the mousebutton down will only keep menu items visible while the button is depressed over the menu title.

Some menu items will appear greyed out from time to time. When an item is greyed out the specific option isnot currently meaningful. For example, when the GIT is started up the menu item for displaying an imagewill be inactive, and will stay that way until the user loads an image.

Some menu items have keyboard accelerators (Section ) associated with them.

The File Menu

The file menu has three main uses :

Reading and writing FITS files into and out of the GIT (Chapter ).Displaying FITS header keywords (Section )Exiting the GIT

The Image Menu

The image menu is designed mainly to operate on 2-dimensional images and allows the user to :

Display an image (Section )Perform arithmetic on images (Chapter )Examine stellar profiles (Chapter )Calculate full width half-maximum (Section )Perform a focus fit of a focus image (Section )Calculate statistics (Chapter )Extract a sub-image (Section )Get a hardcopy of an image (Section and Chapter )Store an image in the GIT internal memory (Chapter )

The entries for Statistics, Subimage and Print are described in detail in Chapter , and Sections , and .

The Vector Menu

The vector menu is designed to operate on 1-dimensional images and allows the user to :


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Plot a vector (Section )Show/hide the vector plot windowStore a vector in the GIT internal memory (Chapter )

The Options Menu

The Options menu has items that permit the user to start up a private image display when in CICADA mode,or to reconnect to the CICADA display. The user can also access the GIT preferences (Chapter ) under this menu.

The Help Menu

The help menu currently has options What’s New and About GIT. For more information see Chapter .

Keyboard Accelerators

A number of menu items have keyboard accelerators associated with them. All are of the formcontrol+<key>. This means the appropriate control sequence at any time will select that command withoutuse of the menu. Table lists all accelerators.

Table: Keyboard Accelerators

Ctrl+<Key> Operation

A Image Arithmetic

D Display Image

Q Quit

H FITS Header

I Sub-Image (via display)

M Interactive Vector Modification

P Star Profile

F Full Width Half Maximum

L Load Image

S Image Statistics (whole Image)

U Unload Image

V Vector Plot mode

W Write Image

Toolbar Button Area


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This area contains a number of icon buttons for commonly used operations, some of which do not havekeyboard accelerators associated with them. The buttons are one-off operations as opposed to putting the GITinto a mode. The buttons and the commands they carry out are described in Figure . When the cursor is moved over one of these icons, a line of help text is displayed in the line help area of the GUI.

Figure: GUI toolbar buttons

Image ListThe image list is a scrollable window containing the names of all images currently loaded into the GIT. Thesenames are full pathnames of FITS files on disk. If the user tries to load or create an image with the samename as one already in memory they will be asked whether they wish to overwrite. Only one image can becurrently in use, and the name of that image is shown in inverse video.

Single clicking with the mouse will select an image as the current one, and an informational message indicating that it has been loaded is displayed. The selected image is also displayed on the appropriate displaydepending on whether it is 1- or 2-dimensional.

Informational TextInformational text is located in a scrollable window in the right portion of the GUI. Messages appear whenimages are loaded, unloaded, displayed; when statistics are calculated; sub-images taken, etc. As well,warnings and error messages are written to this area. There

There are also progress and informational messages displayed in the text area of the GUI window while GITis processing or when the cursor is moved over the toolbar.


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Graphics Help TextWhen the user selects a mode that requires graphics input, either from the image display or the vector display, legal keystrokes and their operation are displayed in this help text area. Legal keystrokes for eachmode are listed in the appropriate sections of this manual.

PreferencesThere are a number of preferences available for the user to customise the behaviour of GIT.Choosepreferences under the Options menu to see a pop up a window with available parameters (see Figure

for an example). Separate preference screens for Image Display (Section ), Vector Display (Section ), Statistics (Chapter ), Star Profile (Section ) and General (Sections and ) are available.

Appropriate sections of this manual describe each of the preferences, with valid ranges and values. To selecta screen click either the LH and RH mouse button over the Select Category menu button, and select therequired preference set to display.

After setting one or more preferences the user may click Apply which will ensure that the new values arepicked up by the GIT but leave the window open. Selecting Ok will save the preferences and close the popup window. Cancel will remove the window without updating preferences (although any prior Apply’s will have already been carried out).

Preferences File

Preferences are written to disk in the file $HOME/.gitrc, where $HOME is a pre-defined system environment variable pointing to a user’s home area (see Appendix for an example $HOME/.gitrc file). When the GIT is started up the $HOME/.gitrc file is read, if it exists, and is re-read whenever the preferences window is poppedup.

Users can edit the .gitrc file by hand but must ensure that they do not corrupt the format. If the file is editedwhile the GIT is running, changes will take effect when the preferences option is selected.

Lines beginning with a # are comment lines, they are followed by the parameter name and value separated bya colon. For example,

# Image display scaling type (HOPT/MINMAX)image_display_mode : HOPT

FITS FilesThe GIT uses its own internal data format which has many similarities to the FITS format.

Images are read into, and written out from, the GIT’s internal memory via disk FITS format files. These maybe 1- or 2-dimensional FITS images. Irrespective of the FITS data type (integer, real or double precision) theGIT stores the data internally in 4 byte floating format (i.e. single precision). This means a double precisionFITS file may cause over or under-flows. At this stage there is no plan to enable the use of double precisionnumbers due to memory and speed restrictions. If a double precision FITS file is read into the GIT the userwill receive a warning message.


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PreferencesThere is no separate preferences page for FITS files, but one user-definable preference is found under theGeneral category - FITS output.

There are two standard FITS header keywords : BSCALE and BZERO. Their default values are 1 and 0,respectively. Data values in a FITS file are scaled such that

= × +

This permits data with a large dynamic range, or a large scale value, to be represented by a more compactdata type than would be otherwise possible. There is a drawback in a possible loss of precision.

A user has the ability to set the preference such that either precision is preserved or the output data type is thesame as the input data type. If precision is preserved then the output data type is set to real (BITPIX = -32) so that BSCALE is left as 1. Otherwise, BSCALE and BZERO are calculated, written to the FITS header record, and data values scaled accordingly with a possible loss of accuracy.

Reading an ImageTo read an image into the GIT select the Load Image item in the File menu (accelerator: Ctrl+L). A standardfile-selection popup window is then displayed allowing directory browsing for the required file.

As a FITS file is being read a message of the form: FITS READ: directory/filename will appear in the information window. Upon successful loading a further message will be issued: IMAGE LOAD: filename (x × y) where (x × y) are the dimensions of the image.

Images that are successfully loaded are visible in the scrollable image list portion of the main GIT window.Their name is the full pathname of the original FITS filename on disk.

When an image is loaded it becomes the current image and is displayed. The current image is indicated in theimage list by being shown in reverse video.

Unloading an ImageAny image read into the GIT takes up an amount of computer memory approximately equal to 4×x×y bytes(i.e. 4Mb for a 1024×1024 image). - when it is the current image. All other images in the list are not loadedinto memory until they are selected. The GIT provides an unload mechanism to remove unwanted images. Touse this, select the image to be unloaded, and then Unload Current Image (Ctrl+U) from the File menu. Whenin CICADA mode images are unloaded automatically as soon as more than the maximum number ofCICADA images is exceeded (see Chapter ).

The GIT provides a mechanism to ensure that a user does not accidentally run out of memory when readingimages in, or operating on them. Before each memory intensive operation a check is made of the availablememory to determine if it will still leave a GIT-defined amount free after the operation. If not, the user willbe notified and will not be able to load the image until some memory is freed up.

There are several possible sources of memory usage. Examples to look for are:


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Too many memory intensive applications running (for example, Web browsers, News readers). If thisis a likely cause kill off some to free memory./tmp may have been filled up with junk files. Check and remove if necessary.

Writing an ImageAny image in the GIT memory may be written out to disk in FITS format. To do this, select the image to bewritten, and then Write Image from the File menu (accelerator: Ctrl+W). A file selection box will popupwhose areas and operation is the same as when reading a FITS file into the GIT (see Section ). The defaultselection is made up of the current directory and a filename comprising the image name stub with .fitsappended. The user can then change the output directory, filename and/or the file extension and write theimage out by hitting the OK button, or <return>.

It is not possible to overwrite a FITS file that already exists. If this is attempted a message will be printed tothe informational window : File (filename) already exists

Any images created within the GIT will be written out as real format FITS files (i.e. BITPIX = -32). If an input image was a FITS file the output type will be the same as the input type (e.g. short integer input will bewritten out as short integers). However, in this case it is necessary to determine whether the desired outputtype is compatible with the image range and scaling. If not, if the user has asked for precision to bemaintained (Section ) the output bitpix is set to real, otherwise the output type is kept the same and BSCALEand BZERO are calculated and used.

FITS HeadersIf an image is read in from a FITS file the user is able to look at all the FITS header keywords/values presentin the original file. This is done by selecting FITS Header from the File menu (accelerator: Ctrl+H). If theoperation is done on an image that is not a FITS file a warning is printed to the informational window: FITS HDR: Not a FITS file.

WARNING : FITS Header Information

An image stored in the GIT internal memory that was read from a FITS file retains only a few of the originalFITS header keywords that are directly required in creation of the image :

BITPIXThe number of bits/pixel (i.e. the datatype)

NAXISThe number of axes (i.e. 1- or 2-dimensional)

NAXIS1, NAXIS2The dimensions of the image axes

BSCALE, BZERO(if they exist) Specifying scaling of the data values from the FITS file to actual values

All other keywords are ignored. Hence, if the user reads a FITS file in, and then writes a copy of it back out(whether or not it has been modified) any other original FITS keywords will be lost.


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Image Operations

2-Dimensional Images

Image Display

The GIT uses the MSSSO modified version of the IRAF ximtool for displaying 2-dimensional images. Whenthe GIT is started it automatically fires up a custom version of ximtool using private input and output pipes.The full functionality of ximtool is available to a user using the GIT. To make the best use of ximtool usersshould be familiar with its capabilities. When the GIT is exited the image display will be closed down.

To display an image, select it from the image list. To redisplay the currently selected image, select Displayunder the Image menu (accelerator: Ctrl+D), or use the Display button.

Preferences

Figure: Popup window for image display Preferences

Image ScalingThe image scaling preference defines how the minimum and maximum displayed pixel intensities aredetermined. Pixels below the minimum value (lower cutoff) are shown in ‘‘black’’ while those greaterthan the maximum (upper cutoff) appear ‘‘white’’. The three possible values are: HistOpt - Median,HistOpt - Mode and Min/Max. The Min/Max option allows the user to specify the cutoff values, whilewith HistOpt values are calculated automatically. [Valid values : HOPT_MEDIAN, HOPT_MODE, MINMAX]

Sample %Used with Hist Opt scaling. It represents the percentage of total number of pixels in an image to samplewhen determining the lower and upper intensity cutoffs. The sampling is done linearly. The larger thevalue the slower the calculation of cutoff values. For most images a value of 5 - 15% is adequate. [Valid range 1...100]

Num SDs below for cutoffUsed with Hist Opt scaling to calculate lower intensity cutoffs to be a number of standard deviationsbelow the median or mode. Values of 1 - 1.5% are usually adequate in obtaining images displayed witha good dynamic range. [Valid range 0.01...10]

Num SDs above for cutoffUsed with Hist Opt scaling to calculate upper intensity cutoffs to be a number of standard deviationsabove the median or mode. Values of 1 - 1.5% are usually adequate in obtaining images displayed witha good dynamic range. [Valid range 0.01...10]


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X BinBinning factor for display compression in the x-direction. [Valid range 1...20]

Y BinBinning factor for display compression in the y-direction. [Valid range 1...20]

RotationAngle to rotate the image by before display. [Valid range 0...359]

Display FrameXimtool frame in which to display the image. Ximtool has the ability to dynamically create frames when requested. [Valid range 1...4]

Hot PixelsIf checked, will enable pixel intensities greater than the selected value to be displayed in red.

Hot Pixel ValueA numerical value which is the limit, above which, hot pixels will be shown if that preference isselected. [Valid values: any real number]

Saturated Pixels

The ability for a user to be able to easily see saturated pixels on a CCD image has driven this functionality.The user can specify whether pixels greater than a given threshold limit are shown in red by checking the HotPixels toggle button to enable it.

Note that if a user modifies the image display colour look-up table to one that has reddish tones these‘‘saturated’’ pixels may not be visible.

Sub-Images

Sub-images (either 1 or 2-dimensional) can be created from a displayed image (Section ) using the image display, or the limits can be specified manually (Section ). In both cases the sub-image is sent to theappropriate image display, and the user can then elect to store it in the GIT’s internal memory if required(Chapter ).

When a 1-dimensional image is extracted, sky subtraction will be performed if the user has selected thatpreference (Section ) and the extraction was done via the image display. See Section for details of 1-dimensional image extraction.

Sub-image via Image Display

A sub-image can be selected from a displayed image via the image display using the Subimage via Displayoption under the Image menu (accelerator: Ctrl+I). This puts the GIT into subimage mode and warps thecursor into the image display. Valid keystrokes (case independent) which can be used in the image displaywindow are listed in the Graphics Help Text section of the main GIT window (Table ). This mode must beexited before control is returned to the main GIT window.


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Table: Valid Sub-image mode keystrokes (caseindependent) for the image display.

Keystroke Operation Dimension

C Column extraction 1

Q Quit subimage mode

R Row extraction 1

X X-Y slice extraction 1

<space> Use twice specifying diagonally

opposite corners 2

Sub-image via Popup Window

A sub-image of a displayed image can be selected via a popup window by the Subimage via Popup option under the Image menu. Lower and upper limits in X and Y are specified. If a value is entered outside theimage limits it is automatically reset to the lowest or highest legitimate value. Selecting Apply will extract thesub-image, leaving the popup visible. Selecting Ok will extract the sub-image, and close the popup.

To extract a 1-dimensional sub-image give either the X or Y low and high values the same, as required. It isnot possible to extract a 1-dimensional X-Y slice via this method, use the image display method instead.(Section ).

Hardcopy

A hardcopy of the currently displayed image can be made by selecting Print under the Image menu. For moredetails on printing see Chapter .


Image Display

The GIT uses MIT plotter widget for displaying 1-dimensional images (vectors) (see Figure for an example).

To display a vector choose it from the image list and then select Display under the Image menu (accelerator: Ctrl+D), or use the Display button. Double clicking on a vector in the image list will also load and thendisplay it.


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Figure: X-Y slice from pixel (36,204) to (374,220)of the image ccd0698.fits not summing any

additional rows, with no sky subtraction, and notzoomed.

The plot window may be resized at any time and the current plot will be resized and redrawn.

Preferences

Figure: Popup window for the Vector displayPreferences

Scaling FunctionDefine a function (none, natural logarithm, log base 10, mode, square, square root, or inverse) to be applied to the data before plotting the vector. With the mode calculation the lower and upper cutoff values are taken from those given as the statistics preferences (Section ). [Valid values: NONE, LN,LOG10, MODE, SQR, SQRT, or INVERT]

Scale FactorA multiplicative factor applied to the data before plotting if a scaling function of either none or mode isused. [Valid values: any real number]

nsumNumber of image ‘‘lines’’ to add together before plotting. ‘‘Lines’’ can be either rows, columns, orX-Y slices depending on the type of extraction used (see Section ). [Valid range: 1...100]

nsum skyNumber of image sky ‘‘lines’’ to add together. These rows are normalised to match the image nsum. [Valid range: 1...100]

Start pixelLowest pixel to use in a vector plot. [Valid range: 1...4196]

End pixel


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Highest pixel to use in a vector plot. [Valid range: 1...4196]Subtract sky

If checked, then sky subtraction is performed before plotting.Maintain zoom factor

If checked, causes the vector plot zoom factor to be remembered and used with subsequent plots.Auto plot on image load

If checked, then the last plotted ‘‘line’’ is re-plotted when a new image is loaded in the GIT memorywhen running in CICADA mode.

Sub-image Extraction

To extract a 1-dimensional image from a displayed 2-dimensional image select Line Plot from the Vectormenu (accelerator: Ctrl+V). This will put the GIT into line plot mode and warp the cursor to the imagedisplay. Valid keystrokes are those listed in Table . Note that the mode needs to be exited before controlis returned to the main GIT window.

Table: Valid line plot modekeystrokes (case independent) for

the image display

Keystroke Operation

C Column extraction

Q Quit subimage mode

R Row extraction

X X-Y slice extraction

If the user wishes to do a single line plot, then the Line Plot icon button may be used instead of entering lineplot mode. The same keystrokes are available.

The Repeat Line Plot icon button will repeat the last line plot again (same type of plot, same coordinates,same zoom factor). This is of use when displaying a number of images and wanting to do a vector plot of thesame section.

When a 1-dimensional sub-image (vector) is extracted from a 2-dimensional image there are a number ofparameters that affect how the vector is formed. These are described above (Section ).

Firstly, the parameter nsum is used to determine how many ‘‘lines’’ to sum together. The ‘‘line’’ that the userspecifies is the central ‘‘line’’. If sky subtraction is required the user will have specified a sky ‘‘line’’ as well.The parameter nsum sky is then used to create a summed sky ‘‘line’’. The sky is normalised to the imagebefore being subtracted off the vector. Finally, if a scaling function and/or scale factor was specified they areapplied to the vector, and the result plotted.

If the user has selected sky subtraction then after specifying either the row or column to plot they will beprompted for a sky row or column. Note: in the current version there is no sky subtraction for X-Y slices,nor for vector extraction through the sub-image popup window.

If the maintain zoom factor option is set then new vector plots will be done with the current zoom factor.

Vector plots are titled with: image name, row/column/x-y values, nsum, an indication if sky subtracted, andzoom factor (if zoomed).


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Hardcopy

To get a hardcopy of the currently plotted vector select Print under the Vector menu. For more details onprinting see Chapter .

Manipulation

It is possible to manipulate a 1-dimensional vector plot somewhat via modify plot mode. This is entered by selecting the Modify item under the Vector menu (accelerator: Ctrl+M). Table shows the valid keystrokesavailable from within the plot window while in this mode. Note that this mode must be exited before controlis returned to the main GIT window, and that the GIT window will not be refreshed while you are in themode. It is anticipated that this limitation will be addressed in a future release.

Table: Modify Vector Plot Mode Keystrokes

Key Operation

A Expand and Auto-scale

C Redraw Original

F Full Width Half-Maximum

M Statistics

Q Quit

R Reverse/Flip

S Smooth

U Zoom out

Z Zoom in

> or . Display line plot section to the Right

< or , Display line plot section to the Left

<space> Print (x,y) coordinates

Expand and Auto-scaleHit this key twice, specifying the x-position of both ends of the expanded plot. The y-scale of the newplot will be determined based on the data in the expanded section.

Redraw OriginalThe original plot is redrawn, with no smoothing or zooming.

Full Width Half-MaximumThis key must be hit twice to determine the FWHM of a profile, once on either side of the line. They-position is important because it is used to calculate a base-line. The result is output to the vector plotwindow. See Chapter for general details on FWHM calculations. This does not work for absorptionlines.

StatisticsThis key must be hit twice, to specify the x-position of both ends of the vector segment for whichstatistics are calculated. The minimum, maximum, and mean values, together with standard deviation,


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are output to the vector plot window.Quit

Use this to exit modify vector plot mode.Smooth

The user will be prompted to enter a smoothing value (odd number) in the vector plot window. Arunning box of the requested size is used for smoothing.

Zoom In/UnzoomThe plot is zoomed in (or out) by a factor of 2 in the x-direction around the x-position of the cursor.The y-scale is auto-scaled.

Left/Right SectionsUsing the less-than and greater-than keys (or comma and period) allows a user to move along anexpanded plot in the x-direction.

(x,y) CoordinatesHitting the <space> bar causes the x-value of the cursor position to be output to the vector plot window,together with a linearly interpolated y-value.

Storing an Image in MemoryAny image (either 1- or 2-dimensional) that is displayed can be stored in the GIT’s internal memory. SelectStore in Memory under the Vector or Image menu as appropriate. A file selection popup window will appearallowing the user to specify the new FITS file name.

HardcopyThe hardcopy device is that which the user has defined in their Unix environment at the time the GIT isstarted up. This is controlled by the PRINTER Unix environment variable. If not set, hardcopies will be sent tothe default system-defined printer.

The engine driving the output for 2-dimensional images is ilaser -- the same as that available from FIGARO.There are no user-configurable options with the GIT version.

Vector (1-dimensional) plots are carried out using the MIT plotter widget (see, for example, Figure ).

Image StatisticsWhen statistics are calculated the results are written to the informational text section of the main GITwindow. Information comprises the image name, and dimensions; the minimum and maximum values; themean, mode and standard deviation. For example,

IMAGE STATS: /tmp/130.fits (416x578) min=0.00, max=65535.00, mean=1622.30, std dev=754.61, mode=1607.00


2-dimensional image statistics can be calculated for the whole image, or specified in either a popup windowor via cursor input on the image display.


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For the whole image select All Image from the Statistics menu under the Image menu (accelerator: Ctrl+S).Alternatively, use the Statistics icon button on the main GIT window.

To specify part, or all, of an image via a popup window select via Popup from the Statistics menu. A window will pop up with default values in X and Y of the image dimensions. The operation of this window isidentical to when specifying sub-image extraction (see Section ).

To specify part of an image via the image display select via Display from the Statistics menu. The GIT will enter statistics mode which is identical in operation to sub-image extraction via the image display (Section ). Either a 1- or 2-dimensional section will be used for statistics depending on the keystroke(s) (Table ).


Statistics can be calculated for part, or all, of a 1-dimensional image while in modify vector mode (Section ).

If a 1-dimensional image is the current image in memory, either via selection from the image list or by beingthe last image displayed, the Statistics button (accelerator: Ctrl+S) will operate on that image.

Preferences

There are a number of configurable statistics preferences which are accessed via the Statistics category from the Preferences option under the Options menu (Figure ).

Show Statistics PlotIf checked, a line plot window will show a histogram of values in the statistics.

Ignore Values < =Values less than this will be ignored when calculating statistics. [Valid values: any real number]

Ignore Values > =Values greater than this will be ignored when calculating statistics. [Valid values: any real number]

Figure: Popup window for the image StatisticsPreferences

Image ArithmeticThe GIT is able to carry out a range of basic arithmetic functions on images. These are operations:


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with images as both operandswith an image and a scalarto apply a function to an image

To enable calculations to be carried out select Arithmetic from the Image menu (accelerator: Ctrl+A). Thiswill pop up the arithmetic window (Figure ).

Figure: Arithmetic popup window

To select the type (that is, Image, Scalar, or Function) for the left and right operands use the appropriatepull-down menus in the Arithmetic popup window. When an image is used the list of currently loaded imagesis displayed. When a scalar operand is required a numeric box will show up. For functions a list of availableoptions will appear as check boxes.

Function types available are:

Natural Logarithm (ln)Square (sqr)InverseSquare Root (Sqrt)Base-10 Logarithm (Log10)

Results

Clicking the Result button will carry out the calculation, and if an image is involved pop up a windowallowing the user to save and the resulting image. The result is then displayed and set to be the current image.Memory checking is done, as with loading any image, to ensure that sufficient resources exist on thecomputer.

Irrespective of whether an image is involved information on the calculation will be written to theinformational section of the main GIT window.

The input type of images, and the types of any function or scalar used are checked so that the FITS file iscreated with appropriate precision. Some examples are:

two short integer input images would create a short integer output FITS filetwo integer input images would create an integer output FITS fileany division creates a float output FITS fileany function creates a float output FITS fileapplication of an integer scalar to an integer image will create an integer FITS fileapplication of a float scalar to an integer image will create a float FITS file

Error Checking

When arithmetic is done on two images they are first checked to ensure they have the same X and Y


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dimensions. If not, the user is informed and no calculation done.

It is possible to get divide by zero and other non-meaningful numbers in calculations, and these are handledgracefully. For example:

ARITH: 1.000000 / 0.000000 = InfARITH: Sqrt(-1.000000) = NaN

These results are part of the IEEE floating point standards, and values such as infinity and not a number(NaN) are representable in the IEEE floating point format.

Image Object ProfilesThe image display can be used to plot radial profiles of objects. The option Star Profile under the Imagemenu (accelerator: Ctrl+P) will put the user into profile mode. The keystrokes listed in Table are the only ones available.

Table: Profile ModeKeystrokes

Key Operation

Q Quit

<space> Select object

Preferences

The Star Profile page (Figure ) of Preferences under the Options menu has the following:

Display profileIf checked, the profile is plotted to the line plot window.

Aperture SizeThe radius of the aperture (pixels) to be used when determining the centroid, and for setting plottinglimits. [Valid range: 1...50]


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Figure: Popup window for the Star ProfilePreferences

Use

The user selects an object using the image display cursor, and the GIT determines a centroid based on anaperture size. If the centroiding fails a message is printed out to the informational text area on the main GITwindow. If the display profile preference is selected the radial profile is plotted.

Irrespective of whether the profile is plotted the (x,y) values of the centroid and full width half-maximum(Chapter ) are written to the informational text area. For example,

Centroid: (203.78,341.86) Aperture Size=12FWHM = 4.52

Full Width Half-MaximumThe GIT may be used to determine the full width half-maximum (FWHM) from a 2-dimensional image viathe display, or from a 1-dimensional image via the line plot window.

The FWHM is calculated by fitting a Gaussian to the data values using the Levenburg-Marquardt method.

2-Dimensional FWHM

This is invoked by the FWHM button on the Image menu and will put the user into FWHM mode with the keystrokes listed in Table available. The GIT stays in the mode until explicitly exited, at which stagecontrol is returned to the main window.

Table: FWHM Mode Keystrokes

Key Operation

Q Quit

X at each end to select object


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The user must specify each end of the X-Y slice that is used to determine a FWHM. This 1-dimensionalvector is plotted to the line plot window. The value of the FWHM is written to the GIT informational textwindow.

1-Dimensional FWHM

A 1-dimensional image which is plotted can have a FWHM calculated from within modify line plot mode --see Section for details of use.

Focus FittingThis is invoked by the Focus Fit button on the Image menu and will start an automated focus fittingprocedure of the selected image - if it is a focus image. GIT will check the image FITS headers to see if theFOCNEXPO and FOCSHIFT keywords are present, if not then GIT prompts the user for values to use (see figure).

Figure: Popup windowfor the Focus Fitting

parameters

Using these parameters GIT attempts to locate a sequence of stars in the image to which FWHM arecalculated and then a quadratic is fitted to the FWHM and focus position data. This is then plotted with theoptimal focus position indicated.

Miscellaneous

CICADA ModeWhen the GIT is started up with the optional parameter -cicada n it will automatically load images into its memory directly as they are read out from a CCD with CICADA. Informational messages will appearnormally, and the images will show up in the image list together with any images the user reads in or creates.

Display of the CCD images is done automatically by the CICADA software [2].

The parameter n indicates the maximum number of CICADA images to be retained. This value can bemodified from within the GIT as a preference. NB. Normally the GIT is started from CICADA itself wherethis value defaults to 10.


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Image Display

By default, when in CICADA mode the GIT uses the CICADA ximtool image display. If GIT attempts todisplay an image while CICADA is displaying, a message indicating that the ‘‘display is already in use’’ iswritten to the message window.

Alternatively, the user can start up a ‘‘private’’ image display when in CICADA mode, thus avoiding anycontention. This is just the normal standalone display that is started when not running CICADA. There is apreference that can be set to allow this as default (Section ). When this is used the CICADA imagescontinue to be displayed automatically to one display, while the user is free to use the other for display and/ormanipulation.

A user can start this separate image display using Start Private Ximtool under the Options menu. It can becancelled and the GIT reconnected to the CICADA display at any time via cancel Private Ximtool under the Options menu.

Preferences

CICADA preferences are found under the General preferences screen (see Figure ).

Figure: Popup window for the General Preferences

Cicada modeIf checked, indicates to use CICADA mode upon startup. If the GIT is started by CICADA then thisbox will not need to be checked by the user for correct operation.

Maximum Cicada imagesThe user can modify the maximum number of images to be held in the GIT’s image list while it isrunning. [Valid range: 1...10]

Private Ximtool in Cicada modeChecking this box allows the GIT, upon startup, to use its own ‘‘private’’ image display when inCICADA mode (see Section for details).

QuittingTo quit the GIT select Quit from the File menu (accelerator: Ctrl+Q). Any images which have been stored inmemory but not written to disk can be saved at this time. If there are any such images a window will pop upasking the user if they wish to save the image(s). The user has the following options:


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Saving none and exiting immediately (No to all).Saving all automatically (Yes to all).Prompting whether to save one by one (Yes or No).

If Yes to All is selected the popup window will appear for each unsaved image (see Section ).

Getting HelpThis user manual is the first step in getting help. If something is not described clearly or fully in here, orsomething simply does not work as described please report it.

If you have a problem that is reproducible, or one that is intermittent but not reproducible at will, pleasereport it in as much detail as possible.

If you have a ‘‘glitch’’ -- something that occurs only once and you don’t see again it may not be useful toreport that.

The GIT maintains a time-stamped log file to which much information is written. This is not stored in theuser’s area. The contents of this file can be used with any bug report to help track down problems.

All reports should be sent via email to cicada (don’t forget to add @mso.anu.edu.au if outside RSAA) to the RSAA Computer Section. Or, if you prefer, in person.

LimitationsThese limitations are known and will be fixed in future releases:

There is no sky subtraction for X-Y slices.There is no sky subtraction for vector extraction through the sub-image popup window.Sub-image and statistics via display modes, modify vector mode and profile mode must be exitedbefore control is returned to the main GIT window.Colour Table Problems - the current version of GIT uses the IRAF application ximtool modified by MSSSO as the image display. If you already have a number of applications running which use a fairnumber of colours then ximtool will load its own private colourmap and colour flashing will occurwhen moving in and out of that window. This will definitely happen if you are running a colourintensive application such as Netscape Navigator irrespective of whether you have told it to start upwith a private colour map or not. We have not found it possible to have Netscape running at all whileximtool is in use and not encounter colour problems.

There will be other things that some users will consider limitations. It should be remembered that the GITwas designed for limited quick-look purposes and in no way should it be thought of as being a general imageanalysis or reduction tool. However, the authors are always open to suggestions on how its functionality, easeof use, etc could be improved.

Sample $HOME/.gitrc Preferences File#=========================================================================# Configuration Table: .gitrc# This table has been automatically generated and consists of a series of# named items , eg [name], followed by a set of parameter and value# pairs, which could be multiple per line. # Default valued items might not appear. Take care if editing by hand.


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#=========================================================================

cicada.max_loaded_images:8cicada.mode:0image_display.angle:0image_display.binx:1image_display.biny:1image_display.display_frame:1image_display.display_max:1761.220318image_display.display_min:1456.779682image_display.hopt_contrast:0.500000image_display.hopt_sampling:1000image_display.hot_pix:0image_display.hot_pix_value:65535.000000image_display.mode:HOPT_MEDIANimage_display.vis_scaling:0image_display.ximtool_height:564image_display.ximtool_screen:1image_display.ximtool_width:512image_display.ximtool_x:564image_display.ximtool_y:310misc.auto_line_plot:0misc.image_load_dir:/priv/mistress/pjy/data/cicada/pjy/misc.image_save_dir:/priv/mistress/pjy/cicada/misc.mef_extension_list:1-8misc.mosaic_mef:0misc.private_ximtool:0plot.plot_height:417plot.plot_width:614star.aperture:18statistics.display_profile:1statistics.plot:1statistics.sample_full:0statistics.sample_size:1000statistics.scale_function:LINEARvector.end:4196vector.maintain_zoom:0vector.nsum_sky:1vector.scale_factor:1.000000vector.scale_function:LINEARvector.smooth_box:3vector.start:1vector.subtract_sky:0vector.use_bscale:0vector.vector_nsum:1

Bibliography

1NASA/Science Office of Standards and Technology. Definition of the Flexible Image Transport System (FITS) (September 29, 1995).

2MSSSO Computing Section. CICADA User Manual (1998).

Index

About this document ...Graphing and Imaging Tool V3.0 User’s Manual



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The command line arguments were: latex2html -init_file /opt/local/html/latex2html/cicada.init git.tex

The translation was initiated by Bill Roberts on 2001-05-29

[email protected]

No Title http://www.mso.anu.edu.au/computing/cicada/cicada_adass96/cicada_ad...

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Next: Introduction

CICADA

CCD and Instrument Control Software

CICADA - Computerised Instrument Control and Data Acquisition is a software system for control oftelescope instruments in a distributed computing environment. It is designed using object-oriented techniquesand built with standard computing tools such as RPC, SysV IPC, Posix threads, Tcl and GUI builders. Thesystem is readily extensible to new instruments and currently supports the Astromed 3200 CCD controllerand MSSSO’s new tip-tilt system. Work is currently underway to provide support for the SDSU CCDcontroller and MSSSO’s Double Beam Spectrograph. A core set of processes handle commoncommunication and control tasks, while specific instruments are ‘‘bolted’’ on using C++ inheritancetechniques. CICADA offers consistent user interface, image display, data archiving and quick-look analysisfor a variety of instruments.

P.J. Young, M. Brooks, S.J. Meatheringham, W.H. RobertsMount Stromlo and Siding Spring [email protected] September, 1996

IntroductionInstrument Control Model

Action RequestsData Delivery - Data StructuresStatus and Message Passing

Implementation and Techniques UsedCurrent Applications

Astromed 3200 CCD ControllerMSSSO’s New Tip-tilt SecondarySan Diego CCD Controller

Adding New Instrument SupportCreating a C++ Hardware Interface ClassCreating a GUI or CLI for the New Instrument

Graphical Image ToolFuture Plans and Work In Progress

MSSSO’s Double Beam SpectrographMosaic CCD Camera Support - Using Multi-threading

ReferencesAbout this document ...

Peter Young Tue Oct 29 11:48:29 EST 1996

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Use camera named 6dF

Select an instrument controller forthe TCS plug-in and the instrumentconfiguration

Select the UK-SCHMIDTtelescope plug-in

Click the "available" toggle

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Select the 6dF dewar from this popup

Select the 6dF controller from this popup

Allow space for 4 FITS header blocks because we have more than 108 keywords

6dF requires the rotater value at the end of the exposureinstruct CICADA to make a TCS call at the end

This name is fixed as it is used to key to thespecifically written FITS plugin for the 6dF

Select the Solaris host holding the SBUSinterface card to the SDSU controller

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The SBUS device name that holds theSDSU controller which is a generation2 device

Only one CCD and it is named CCD_102

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Include WCS information when calibrationdetail is known and enterred here

Readout amplifier configured as shown

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The 6dF camera has two temperature sensors, they are configured as shown below.FOCALPL is the setpoint sensor. Alarms are shown if temps go out of range.

Temperatur sensor type chosen from these popupsThese are the SDSU controller address values

Temperature setpoint is entered here - the SDSU controller will control tothis value

Control warmupo parameters entered here

CICADA will request temperature values from thecontroller at this rate. NB temperature readouts arenot done during exposures.

These servo parameters are sentto the SDSU controller for thetemperature control model

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Enter socket number for communicationwith Wincenter TCS server

via network socketIndicate that TCS interface is

Timeout for getting a responsefrom TCS

These data items can be delivered (as a minimum) by TCS

This Solaris host willrun the TCS slaveprocess

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Select the SITE instrument controltype

Select the AAO 6dF instrumentname

This is the host that will run theinstrument control slave process.Not required for the 6dF

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This is the file that stores the currentlyselected configuration

FITS headers are written tothis file when the observerclicks the "Record" button

This SITE instrument has no slavecontrol process - no need to enteranything here

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Object

Object

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Object

ZeroZero

ZeroZero

ZeroZero

Zero

Dark

Dark

Dark

Dark

Dark

Dark

Dark Dark

Dark

Flat

Flat

Flat

Flat

Flat Flat

Flat Flat

Flat FlatObject

Flat

Object

Object

Object

1 Subtract overscan

2 Trim

3 Zero combine

4 Subtract zero

5 Dark combine

6 Subtract dark

7 Flat combine

9 Fix bad pixels

10 Other corrections

8 Divide by flat

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Cicada Development - Developer Notes http://www.mso.anu.edu.au/computing/cicada/developer.shtml

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Developer Notes

Developing and maintaining a system such as cicada is not easy. A stable maintainable version is required forproduction use. Developers need the freedom to work on new features. These two requirements are notcompatible. To help make this problem easier to deal with please read the following guidelines and try tofollow them. Additional background information can be found in the rationale.

Tagging

Every release of cicada that is installed at a telescope will be tagged.Tags look like this: Rel-4-2-1, where the first digit indicates the major release number of cicada, thesecond digit indicates the minor release number, and the third digit indicates the bugfix release number.Minor release numbers that are even indicate that this release is considered stable. Minor releasenumbers that are odd indicate that this release is considered unstable.Unstable versions of cicada should never be installed at a telescope except for testing purposes.Unstable versions of cicada will periodically be tagged when they reach a point that is consideredmeaningful in some way. Examples of this include the addition of major new functionality, or therearchitecture of some part of the system.

Bug fixing

Before working on a bugfix you should consult the versions web page to determine which tagged stablerelease your fix will apply to. The web page will show which version of cicada is installed for whichinstruments on which telescopes.Check out the tagged version appropriate to the bugfix you need to make.Anything that is not a bugfix does not belong on a stable branch. You will most likely know whetherwhat you have done counts as a bug fix or whether it is something more complicated. If in doubt, checkwith the configuration manager.Before any fixes you have made can be committed you must thoroughly test cicada, using the testing checklist.Bugfixes to a stable version of cicada can only be checked in on a branch. Branch tags look like this:Rel-4-2-1-branch. If the stable version you are working on does not already have a branch then see theconfiguration manager.You must include a meaningful log message when you commit your changes.The configuration manager is responsible for building a new cicada package, installing it at theappropriate telescope, and merging your bugfixes back into the main trunk (if appropriate). See their web page if you want to know what they will do, or if they’re not around and you need to do ityourself.

Feature addition

Feature additions do not belong on a stable branch.Feature additions only belong on the main trunk.I think you get the idea.

Code portability

The code you write should be as portable as possible. Keep in mind that not only will the code be runon Solaris machines, but potentially also on VxWorks, QNX, and Linux machines in the future. #ifdefswill be (and are) used where appropriate. Before changing any code that is inside an #ifdef block, besure you know what you are doing and how it will affect each of the platforms involved.If there are good reasons to include OS specific code in a module then by all means use it (but delimitit by #ifdefs). For example we gain performance improvements on the UltraSPARC architecture byusing the VIS instruction set, and we use the mmap system call on Solaris because it’s incrediblyhandy.Your code may run on both big and little endian machines.

Cicada Development - Configuration Manager http://www.mso.anu.edu.au/computing/cicada/configuration_manager.shtml

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Configuration Manager

The configuration manager is responsible for looking after the cicada source tree, and making sure that it isalways possible to build a stable working version of cicada for each of the instruments and telescopes itsupports. Their tasks are as follows.

Tagging, Branching, and Merging

Every stable release of cicada must be tagged with a unique tag of the form: Rel-4.2.1.If a bugfix must be applied to a stable release then the source tree branches at that point with a branchtag of the form: Rel-4.2.1-branch.Subsequent stable releases do not need to be branches.Bugfixes must be merged back into the main trunk whenever this is possible.Unstable versions of cicada should be tagged when a major new feature is added, when a rearchitectureof any part of the system takes place, before a new port is undertaken, and probably at some otherpoints when it feels right to do so.The source tree should never branch at an unstable release.

Installing cicada at a telescope

Before cicada can be installed at a telescope there are a number of things to be done:

The version of cicada to be installed must be stable. The only exception to this is if it will only be usedfor testing purposes, in which case the previous stable version must be reinstalled before the nextobserver is due to use the telescope (probably that night).A version of cicada is only considered stable if it passes all the automated tests and all the tests on the testing checklist.The version number in cicada_version.h must match the tag, and these must be unique so that there canbe no doubt about which bugs and bugfixes are in the currently installed version.The cicada_knownbugs and cicada_whatsnew files must be updated to indicate what has changed sincethe last release.The OPTFLAGS variable in all the appropriate makefiles must include optimisation flags and notdebugging flags.The package built must include a working cicada_ximtool for that platform (only sparc and ultra at thisstage).The versions page must be kept up to date.

Cicada Development - Testing Checklist http://www.mso.anu.edu.au/computing/cicada/testing.shtml

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Testing Checklist

The following is a checklist of those things that must be tested before a release of cicada can be given a stableversion number. After any changes to a stable version it must pass these tests again before being installed at atelescope. Most of these tests have been incorporated into a Tcl script. This belongs in the cicada tree but ithasn’t been put there yet.

start cicada without errorsinitialise the controllerclose the shutteropen the shutterperform a flushperform a readoutread temperaturesdo 20 consecutive exposures of the whole detectorfor each controller:

do 20 consecutive exposures of a single CCDdo 20 consecutive exposures of a region within a single CCDdo 20 consecutive exposures of a region that spans multiple CCDsdo 20 exposures that alternative between regions on different CCDs

do 20 exposures that alternative between regions on different controllersdo 20 exposures of a region that spans CCDs on multiple controllerswith a region that has dimensions that are odd in both x and y:

do 20 exposures using binning that is not 1x1do 20 exposures using x overscan that is not 0do 20 exposures using y overscan that is not 0do 20 exposures using x and y overscan that are not both 0do 20 exposures using x and y overscan that are not both 0, with binning that is not 1x1

pause and resume an exposurepause and resume multiple times during a single exposurepause and resume multiple times during a single exposure, changing the exposure timepause then readout an exposurepause then abort an exposureabort an exposureabort an exposure then successfully take a new exposureverify that FITS headers are correctverify that FITS files can be read into IRAFget the filter position using the appropriate filter pluginset the filter position using the appropriate filter pluginget telescope information using the appropriate telescope pluginsend telescope commands using the appropriate telescope plugintest any site control pluginscheck that no cicada processes have memory leaks

The tests should be performed with a configuration as close to the actual production configuration aspossible. In particular consider:

Testing with a dummy controller is not the same as testing with real hardwareRemember that cicada usually runs in a multi-machine configuration at the telescopes. Testing on asingle machine does not exercise the RPC services fully.

Cicada Development - Versions http://www.mso.anu.edu.au/computing/cicada/versions.shtml

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Versions

Telescope Instrument Version Dateinstalled

Bugsreported Comments

40" WFI 4.0.10 April 2004 WFI bugs None

2.3m

DBS Blue 5.1.10 May 2005 2.3m bugs None

DBS Red 2.0.10 Unknown 2.3m bugs None

Imager 5.1.10 May 2005 2.3m bugs None

UK-Schmidt 6dF 4.0.12 June 2004 6dF bugs None

AAT WFI 4.0.12 June 2004 WFI bugs None

UTas UTascamera 4.0.13 July 2004 None

A new filter plugin wasdeveloped for the UTas filter controller. No reports have yetbeen received as to how well it works.

WFI http://www.mso.anu.edu.au/observing/40in/wfi/

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Introduction | Specs and status | Development (password protected)

WFI - Wide Field Imager http://www.mso.anu.edu.au/observing/40in/wfi/intro.shtml

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WFI - Wide Field ImagerThe Wide Field Imager will provide a focal plane CCD detector system with a size of123 by 123 mm, 8192 by 8192 pixels, made up of a 4 x 2 array of 2048 x 4096 pixelthinned, back-illuminated CCDs, to be used on both the Anglo Australian and ANU40inch Telescopes. The output of the system is pixel data in the form ofmulti-extension FITS files written on an archiving medium which is part of the system,and/or transported to a device of the user’s choice over a Local Area Network, or fedinto an automated archiving and reduction pipeline where available.

Top and side-on views of the WFI dewar showing the eight CCDs in place

At the centre of the system is a 123 x 123 mm focal plane mosaic of eight three sidebuttable 2048 x 4096 15 micron pixel CCDs which AAO and MSSSO are procuringas a result of a being partners in a consortium of astronomical institutions fundingdevelopment of such devices at Lincoln Labs in the USA.

The focal plane will be housed in an evacuated vessel (the "dewar") and will becooled to about 170 K by the use of liquid nitrogen refrigeration.

The dewar fits onto exposure controllers located on the AAT Prime Focus and the40" Cassegrain Focus, each comprising a filterwheel with at least four positions,shutter and their control electronics frames. The AAT exposure controller will alsoaccommodate their existing acquisition and guide cameras.

Autoguiding at the 40" will be accomplished by the use of one of eight small guideCCDs located on the focal plane next to the scientific detectors. They are connectedto (preferably) a commercial CCD controller (SBIG ST4 or similar/better) and a PCwhich interfaces to the Telescope Control System. Alternatively, the guiding facilitywhich will have to be incorporated in the exposure controller for the tiptilt system canbe used. This can probe inside the camera field, shadowing it. If such a system iscompatible with the existing AAT autoguider, it may be used there as well.

Two San Diego State University second generation CCD controllers will be mountedon the dewar to read out the CCDs and transfer the data over fibre optic links to the

WFI - Wide Field Imager http://www.mso.anu.edu.au/observing/40in/wfi/intro.shtml

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data acquisition computer system.

The control and data acquisition computer system will consist of two Sunworkstations with enough capacity to efficiently handle the data stream from the CCDcontroller for display, storage and archiving, plus data reduction. The use of twocomputers will allow the time-critical control of CCD readout to be separated from theuser interface and data reduction computer. It will also allow user interface and datareduction computers to be set up permanently at both telescopes, optimallyconfigured for each organisation’s data pipelining procedures. The control and datahandling software will be the MSSSO CICADA package, suitably adapted to dealwith reading out CCD mosaics through the SDSU controller.

Partners

The following organisations are involved in the WFI project:MSSSO: MSSSO will provide the overall project management, CCD expertise, four 2048 x 4096 CCD chips and the MSSSO’s workshop infrastructure.AAO: the Anglo Australian Observatory will provide 4 of the 8 CCDs. University of Melbourne: The astrophysics group will develop the scientific requirements for the Project.Auspace Ltd: Auspace will provide project management, quality assurance and mechanical design to the project.

Contractors

The following are the major contractors that will help in the WFI project:GL Scientific: Building the focal plane, assembly of instrument and testing.

http://www.mso.anu.edu.au/observing/40in/wfi/specs.shtml

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WFI, the Wide Field Imager for the ANU 1m and the AAT.

The Wide Field Imager (WFI) is CCD mosiac camera being fabricated by the Research School of Astronomy& Astrophysics, ANU, for use on both the ANU 1m telescope and on the AAT prime focus at Siding SpringObservatory.

Construction

WFI will use 8 4k x 2k 3-side buttable CCDs arranged in a 2 x 4 mosaic to give a total format of 8k x8k pixels. The CCDs in WFI will come from the MIT-LL consortium lot runs in which the RSAA andthe AAO are joint participants. Each institution will contribute 4 CCDs to WFI.The AAO is engaged in upgrading the prime focus to accommodate WFI while the RSAA has designed(in collaboration with Auspace and the University of Melbourne) and manufactured the WFI dewar.The RSAA is also providing the CCD Controllers (dual 4 channel SDSU V2 controllers), controller software, user interface and data pipeline processing software, as well as commissioning theinstrument.The focal plane mosaic is being assembled by Dr. Gerry Luppino in Hawaii.The goal is to be able to read out the full WFI array in under 60 sec; recent tests at the RSAAdemonstrated that this goal is likely to be met - a full 4k x 2k readout through a single channel tookunder 50 sec with 5 electron read noise. WFI will have one channel per CCD.

WFI on the ANU 1m telescope at Siding Spring Observatory

The CCDs have 15 micron pixels which will give a scale of 0.38"/pix at the 1m telescope Cass focuswith a field-of-view of 52 arcmin on a side (diagonal ~1.2 deg). Available filters will be standardUBVRI plus a far-red z filter. Any 5 can be held in the wheel at the same time.Gary Da Costa ([email protected]), is the RSAA astronomer who acts as WFI Project Scientist.

WFI at the AAT

WFI will be a stand-alone instrument at the AAT.The scale at the AAT prime focus will be 0.23"/pix with a field-of-view of 31 arcmin on a side(diagonal ~0.75 deg). Filters available will be standard UBVRI.Chris Tinney ([email protected]), is the AAO astronomer responsible for WFI on the AAT andthe AAT prime focus upgrade.For more information see the WFI/PFU WWW Page.

Current Status

The WFI dewar and the controllers are in Hawaii awaiting sufficient CCDs to complete the focal planemosaic, after which the first part of the integrate and test phase will be carried out. The complete instrumentwill then be shipped back to Australia and commissioning on the ANU 1m telescope will follow.Commissioning on the AAT will occur once the prime focus upgrade is complete and WFI is successfully operating on the ANU 1m.

Gary Da Costa, WFI Project Scientist, RSAA ([email protected]) Last Update 9 July 1999

WFI/40inch Help Notes http://www.mso.anu.edu.au/observing/40in/WFI_40inch.html

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WFI on MSSSO 40" Notes ==================== June 2001

As a first-time observer at the 40 inch I found there was virtually no usefuldocumentation, ie troubleshooting notes. However, with just a few simplefixes, and some minor changes to the way I used CICADA, I could have savedabout three lost nights. I hope this saves you similar trouble.Although I did have first-night training and excellent help from technicalsupport that doesn’t cover a problem that crops up after midnight laterin the run!

These should be properly html’ised but I don’t have time.At present they are athttp://www.physics.usyd.edu.au/~ande/astronomy/WFI_40inch.html

These notes have grown out of notes written by Terry Bridges(his file was /data/murky3/tjb/transit/WFI_notes but I can’t find it now asmurky3 has gone) and the collective experience of myself, Bob & JohnShobbrook, John Goodyear, Winston Campbell, Gary Da Costa, Malcolm Harrisand others.

Things change: new problems appear, old ones get fixed, new fixes are discovered. So feel free to copy, edit, improve, correct, add to, embelish,simplify or whatever these notes.

Clear Skies!Andrew Jacob

*****************************************************************************

CONTENTS========1/ BEFORE YOUR RUN...2/ SOURCES OF INFORMATION A The "40-Inch & WFI DIY Manual" B "40 Inch Telescope Observer’s Technical Guide" C http://www.mso.anu.edu.au/observing/40in/DirectIm/40in/ D http://msowww.anu.edu.au/computing/cicada/cicada/ E And the WFI web pages F Other Hardcopy Manuals in the Control Room G http://msowww.anu.edu.au/observing/tc_manual/ H Additional Notes for Shobbrooks manual3/ GENERAL INFORMATION BASIC DATA CICADA, GIT & Ximtool General GIT (Graphic & Imaging Tool) Ximtool Screen Preferences for GIT and Ximtool Other COMPUTERS FOCUSING OTHER CCD GUIDER SYSTEM GSFIND Procedure Restarting Guider PC TELESCOPE & DOME Telescope SDSU Cooling CAMERA SHUTTER Priming the shutter Shutter Priming Delay IRAF3/ TROUBLESHOOTING In the control Room In the Dome

***************************************************************************

1/ BEFORE YOUR RUN...Before your run I recommend you read:- a) The "40-Inch & WFI DIY Manual". [hardcopy only: email [email protected]] b) http://www.mso.anu.edu.au/observing/40in/DirectIm/40in/ c) http://msowww.anu.edu.au/computing/cicada/cicada/ d) These notes


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***************************************************************************

2/ SOURCES OF INFORMATIONThere are many sources of information, some more useful than others (froman observers point-of-view). Not all of it is on the web.

A) The "40-Inch & WFI DIY Manual"Contents self-explanatory. Essential reading for first-time observersusing WFI at the 40inch.Get your hands on a copy of this. Written by John & Bob Shobbrook.This manual is not on the web. Would someone please put it there?Email John at [email protected] for a copy.

This manual has sections: Running CICADA Telescope Setup Filling the Dewars Bias Frames Flat Fields Dark Frames Pointing The Telescope - Calibrating the Pointing Focusing the Telescope Autoguiding Data taking Data Archiving Shutdown Accessingthe MSSSO Online Comment File Autoguider Settings Initialising CCD Hardware Shutter Priming WFI - General

B) "40 Inch Telescope Observer’s Technical Guide"A new (June 2001) compendium of useful information and fixes.More essential reading. You are encouraged to add to this guide to asssistfuture observers.Located on the control room bookshelf.

C) http://www.mso.anu.edu.au/observing/40in/DirectIm/40in/This contains some basic 40" observing info. In particular, a list of whatto check when you arrive at the telescope.

D) http://msowww.anu.edu.au/computing/cicada/cicada/The online Cicada User’s Manual

E) And the WFI web pages:MSSSO: http://msowww.anu.edu.au/observing/wfi/index.shtmlAAO : http://www.aao.gov.au/local/www/cgt/wfi/wfi_pfu.html The AAO page contains QE curves or the CCDs.

F) Other Hardcopy Manuals in the Control Room"CICADA User’s Manual" - white folder on 40" control-room bookshelf Probably the same as the Cicada web pages, but best to use D above."40 inch Telescope ETS - A Short Users Manual" - located as above. A useful guide to operating the ETS. Only exists in hardcopy."A Short User’s Guide to the 40-Inch and its CCD Camera System" An old manual. Not entirely relevant to WFI but still useful in parts. Now contained in the "40 Inch Telescope Observer’s Technical Guide" folder

G) http://msowww.anu.edu.au/observing/tc_manual/ An online "Telescope Command Reference Manual". More technical than the average user needs. Use the "40 inch Telescope ETS - A Short Users Manual" instead (see F).

H) Additional Notes for Shobbrooks manualSome additional or alternative notes to add to the Shobbrook manual.Running CICADA: -See additioinal notes belowFilling the dewars: -Press the big red STOP button on the dome console to prevent errant telescope movement. -Remove (or replace) the lens-cap BEFORE filling the dewar to avoid (minor) LN2 spillage from the camera dewar. -Need a step by step procedure for pressurising the small LN2 tank?? -Need a step by step procedure for refilling small LN2 tank from large LN2 tank??Flat fields: Dome flats


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-Do these BEFORE filling the dewar to prevent major LN2 spillage. -Dome at azimuth=~70deg. Telescope at ZD~=-70deg gets flat screen in place. -Use dome lights (tungstens only!) or preferably sunlight by slightly opening the upper shutter. -Dome flats are not good. Use twilight and dark sky flats. [Terry Bridges]Focusing the Telescope -See additional notes belowAutoguiding -If the autoguider PC has to be restarted: -When asked for a password, just click "cancel". -After windows starts open "vncviewer for WFI guider" icon. The "VNC server" is m40slave:0 . Password is in the back of the 40" CCD Temp Log Book. You will need to scroll down the "Maxim Dl" window to access the "Guide CCDs - WFI" chooser.Data archiving -the DDS3 DAT drive is now on monsoon (since Nov 2000). -mt rewoffl rewinds and ejects the tape -How to skip over a tape file if you want to read or extract the second, etc file??Shutdown -Press the big red STOP button when not using the telescope to prevent errant telescope movement.Initialising CCD Hardware -this should be done as a last resort, though there is some disagreement on this!Shutter priming -See additional notes below

****************************************************************************

3/ GENERAL INFORMATION

Some useful information, most of which doesn’t seem to appear anywhere else.

BASIC DATA==========WFI chips:Eight 2k x 4k (2048x4096) CCDs in a 2x4 mosaic.Each sees 13’x26’ (arcmin) making a 52’x52’ field.Pixels are 15micron giving 0.375"/pix (on the 40in at f/8)Gaps between CCDs are ~20-30arcsec.Gains are ~1.5-2.1 electron/ADURONs are ~3.5-5.5 electrons (To get Gain & RON follow procedure in "40 Inch Telescope Observer’s Technical Guide")The awesome SDSU controllers read out the entire array in 55 seconds!!

A full array image is 140Mb in size.One CCD is 17.5MbThe /data/monsoon1 disc on Monsoon holds almost 100Gb - About 4-8 days data.A DDS3 125m tape holds fractionally over 18Gb compressed (ie using allocate mt1)Writing to tape takes ~11.5min/Gb (~3.5hrs per full tape). So don’t getcaught out on your last night, save early!

See also the AAO and MSSSO WFI pages.

CICADA, GIT & Ximtool=====================General-------Strategies to deal with CICADA.

Cicada has a tendency to hang, usually during readout, and sometimesfor no obvious reason (even if you are doing none of the bad things listedbelow).

The only remedy is to restart it. To do this: - In the Observers Window menu select actions|quit_observing_window - In the CICADA menu select Start_Observing|Exit_CICADA - From the command line do: - psef |grep cicada - Look for cicada processes. Ignore *_svc. Kill others with cicada_cleanup -p 0 cicada_cleanup -p 1 cicada_cleanup -p 2 cicada_cleanup -p 3 - Restart using "cicada &"


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In general restarting solves Cicada problems, but it’s a pain so...

Follow these next practices for relatively trouble-free operation:-

Pause - DON’T use ’pause’. This crashes cicada so badly you need to logout to restart! (apparently, but I never dared try it) NumLock - Keep NumLock untoggled. It interferes with ximtool (and GIT?) operation. In particular, it prevents you using right-mouse scrolling to change brightness/contrast, and inactivates the ximtool menus. Initialise Hardware - advice is to use this as a last resort. (Doesn’t appear to cause any trouble tho, despite comments to the contrary)

Avoid: -Using ABORT. You’ll often then need to exit cicada and restart. -doing too much (processor or memory intensive stuff) on monsoon during readout. In particular avoid: -Beginning or ending a tar command during readout (during exposing is OK) -Doing much in Netscape (on-line banking is bad!) -Copying images (and other operations) in iraf Could do these things from murky but its way slower. (For 6 CCDs (104Mb image) the limit might be ~400Mb (as shown on the Observers window at "Memory:???MB")) -leaving the little "graphics keystrokes" window open during readout -changing regions (in regions window) during readout [This may not be true?]

During readout you CAN do these: -change filter, change exposures, change duration

GIT (Graphic & Imaging Tool)----------------------------GIT (presently) has a problem with displaying mosaiced images. It displaysthem OK on readout but it cannot set sensible scaling parameters to allowyou to calculate star profiles, get single line plots, etc. The ximtoolwindow just goes all black or white and displays a single value.

To overcome this limitation do the following:-untoggle NumLock-select options|start_private_ximtool-select options|preferences : -select category "General" -untoggle "Mosaic MEF files in Cicada mode" -enter the "MEF extension list", ie a list of which CCDs you want available for loading into the private ximtool. Note that if you are only using CCD numbers 1,2,7,8 (say) their MEF image extension numbers will be 1,2,3,4. ie CCD number and extension number are different things. -set "Maximum Cicada images" if necessary-The list of extensions you have requested will appear in the "image list" window. Click one and it loads into the private ximtool.

Now you can get star profiles, cross sections, stats, etc. But when the nextimage is read out it will automatically be loaded into the private ximtool.

But avoid leaving the little "graphics keystrokes" window open during readoutor GIT will crash out.

Ximtool-------North is right, East down.1 pixel = 0.375arcsec

To move a star N dec offset on ETS is -veTo " S dec " +veTo " W RA " +veTo " E RA " -ve (This is better seen with a diagram)

Astigmatism leads to elliptical star images when defocused (see Focusingbelow)

Screen Preferences for GIT and Ximtool--------------------------------------Select the monitor for these in options|preferences|generalCommon practice puts GIT and Ximtool on screen 1.

Other-----BinningIf you change the binning, it may not change back again when you reset


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it to 1 x 1, even though the regions window shows it as 1 x 1.Watch the file sizes: should be 271440 blocks (full 8xCCDs?)

BleedingIf readout shows bleeding on brighter stars on some CCDs and bias changes,restart cicada.

Wrong Frame SizeIf there is an error message about ximtool having the wrong frame size,check that there is not an old cicada ximtool process running:ps -ef | grep cicada will show it

Many Red Error WindowsIf lots of red error windows appear from cicada, and restarting impossibleor doesn’t work, try logging out (and back in). That can fix it. If theerror messages involve SDSU, then probably need hardware init (from actionmenu): if such error message reported when cicada is restarted, may needtwo hwinits. Do the hwinit right after restarting cicada.

COMPUTERS========= mosaic (in rack) runs controllers monsoon (on desk) does rest - cicada murky (in office) is a bit slow.

Data is stored on monsoon in /data/monsoon1/cicada/username

FOCUSING========This is difficult to maintain. There is backlash in the mechanism. And it’spretty temperamental. But then just wait till you’re 38 years old!

I found the best method was:

1/ At the beginning of a run (or if focus is lost completely) Use Cicada’s semi-automatic routine under actions|do_focus_sequence... Follow the prompts and/or read the Cicada manual. Move the focus by 0.03-0.05 units between each image, starting at about 31.70. When do_focus_sequence is done set the focus position with the bottons on the round control paddle

2/ From now on use the telescope’s astigmatism. Star images are elongated: NW-SE => focus too high: Press out [display decreases] NE-SW => " too low : " in [ " increases]

3/ Check star profiles too as you go. Out of focus => lots of scatter in the profile, of course.

...but then I was only taking short exposures (1-3 mins). Maybe you coulduse the autoguider image to maintain focus with long exposures? See also theShobbrook manual.

It takes a couple of nights to get the hang of focusing.Approach a focus position from the same direction to remove backlash. Otherwiseget double and/or smeared images.

Typical focus values range from 31.65 - 31.88

OTHER=====Readout speed Use fast readout for broadband imaging when there is a choice.

CCD temperature This appears on the Cicada observers window (from 158-165K for TB). Was ~183.0 for my run.

Filter control Select instrument_control|Filter:F_40 to open the filter control window. To initialise, hit "get filter position"

Dewar vacuum Watch the vacuum gauge - rises about 1E-07 per day. Probably OK up to about 1E-04. LN2 hold time is about 12 hours. If much less, dewar needs pumping (can be done cold in daytime).[TB]


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CCD GUIDER SYSTEM=================I had no trouble with autoguiding, just used all the settings that were there.The following are Terry’s notes. [AJ]

To disable completely, turn off the switch near the mains plug boardson the north side of guider box, low (on telescope)

GSFIND------This shows outline of the main and guiding CCDs relative to GSCstars. Can start from cicada|tools menu or directly from command line.Then drag to enlarge the window.

Choose monitor from cicada|options|preferences|general. Display onmonitor 0 to see a green outline against a black background. Onmonitor 1 the outline and the sky are black [OK for me on monitor 1, AJ].

Put in the field coordinates and magnitude limits for stars (< 12 for 5 sec exposures).

Set position angle = 90.

Move CCD outline with the LMB - gives (RA, dec) coordinates of the detectorcenter.

Put cursor on star and hit spacebar to see the star highlighted in table.Also gives (x,y) position of selected star in the focal plane.

Procedure---------[needs editing? go ahead...]-Select a guide star and the guide CCD.-Set telescope, *open shutter*.-Now go to the autoguider console. VNCviewer is the guider program to choose from desktop. Maxim is the autoguider program itself, similar to the one on the DBS.-Choose "Guide CCDs - WFI" from the menu bar at the bottom of the window. Choose which guide CCD you are using: same orientation as in GSFIND.-In the "Maxim CCD" indow click the guide tab, enter the exposure time and declination.-Take an exposure with guide CCD: Click "expose" then "start".-Wait for exposure to read out in big window.-Move the star where you want it in the guide CCD field: Use telescope offsets on round "box" to offset telescope; North pulls the star *down* on guide window, East pulls the star *right*.-When star is centered (or where you want it), left-click on it, then click on Track, then click Start.-After it reads out it will create a little box in the upper left-hand corner where you should see the star centered (roughly).-Wait a bit to make sure telescope is tracking OK (no huge jumps in star in guide window).-When telescope tracking ok, close shutter and start the real exposure.

**If you don’t see any star in guide window, make sure shutter open!!**

Restarting Guider PC--------------------The Autoguider PC will ask for a password, just click "cancel". -After windows starts open "vncviewer for WFI guider" icon. The "VNC server" is m40slave:0 . Password is in the back of the 40" CCD Temp Log Book. You will need to scroll down the "m40slave" window to access the "Guide CCDs - WFI" chooser.

Hit VNCviewer - this downloads display from m40slave (= m40spare).Should see icons for WFI GS selector and Maxim. Run Maxim. Get the maingui up by hitting the CCD control toggle button on the uppermenu bar. Go to setup/restart (don’t worry about the "controlleroff" message). Need to scroll window up and down to access thebars at the top and bottom. Don’t forget to put in the dec in themain gui.

Settings for guider: make sure x,y axes enabled. Aggressiveness 4is OK. X speed 10, Y speed 4.83, x axis cal time 1, y axis cal time 3.

On the guider display: all RA, dec buttons push the image.


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TELESCOPE & DOME================**Red Emergency STOP buttons** One is on dome console One is on electronics rack in control room

Typically, you will run the telescope from the control room while observingand from the dome when starting-up/closing-down, setting up for dome-flats,filling dewar, showing-off to visitors, etc.

To transfer control TO dome: 1/ On ETS PC select Configuration|configure. Toggle Dome Control to manual. 2/ Go to dome. 3/ On dome console: switch to slew/set 4/ Move telescope, dome and floor as necessary 5/ Hit big red STOP button if filling dewar or stopping observing.

To transfer control TO control-room: 1/ Hit "emergency-stop reset" button (illuminated beside STOP button) 2/ Ensure floor is fully down 3/ Switch to auto 4/ Go to control room 5/ On ETS PC select Configuration|configure. Toggle Dome Control to automatic.

Telescope---------Telescope RA tracking sometimes drops out. Just redo the tracking commandto restart.

SDSU Cooling------------The SDSU controllers are cooled by the NESLAB cooler (downstairs in corridorthrough library on the left)

If controllers get hot, probably means NESLAB has failed.Check temperature of controller heat sinks occasionally - touch them.

CAMERA SHUTTER==============The shutter is badly designed. At large easterly hour-angles (>~4hrs) itfails to reset. Recognise this by the star trails on an image (trails on CCDs 1-4 trail up, on CCDs 5-8 trail down). There will bea ramp in the signal across the CCDs too. [need an example image here]

To fix, you will need to prime the shutter manually.

You can listen to the shutter operation (loud CL-LICK on open and close)with control room door open. A failed shutter sounds different, a woosy,fainter click. You’ll just have to listen! [need an example sound file here]

Priming the shutter-------------------Transfer control to the dome.Move telescope to ~-45deg dec, HA=2.5hrs East. Move floor up to the levelof step 5 on the concrete stairs. This gives access to the big electronicsrack on the side of the telescope tube.

Follow the procedure in the "Observers Technical Guide" and/or Shobbrooksprocedure.

But then test the shutter is working again: -return prime switch to NOR -toggle mode switch to manual -toggle display switch on -toggle shutter switch open and closed to test. (Don’t forget to wait 8 seconds for the shutter to reset after closing) -Return all four switches UP before resuming observing.

Shutter Priming Delay---------------------The shutter takes a few seconds to prime, so need to **wait** 8-10 secondsafter closing the shutter (eg after acquiring guide star) before exposing.

IRAF====WFI produces mosaiced images. In iraf need to specify the extension number in


8 of 9 16/05/05 11:48 AM

the filename, as below.

Hopefully you’ve used IRAF before!If not see http://msowww.anu.edu.au/computing/lun/lun35/lun35.html Set the terminal type as xgterm (at the prompt after mkiraf) and edit login.cl (or loginuser.cl) to set set stdimage = imt4096 set imtype = "fits"

Then: ximtool & :brings up an ximtool to display images in. cl :starts iraf

And: display filename[#CCD] 1

imcopy filename[#CCD][xmin:xmax,ymin:ymax] outfile.fits

imexamine filename[#CCD][xmin:xmax,ymin:ymax] image operations: v does plot from two cursor input positions r gives radial profile of star, fwhm etc a gives mag and fwhm etc for star, no plot

Even for a single CCD readout or a small region readout, needthe extension filename[1]

Use the mscred package in iraf to reduce mosaiced images.

ds9, saotng are nice alternative display tools. ds9 can handlemosaics.

3/ TROUBLESHOOTING==================If stuff goes wrong...Here are some possible causes. Solutions are in these notes or somewherein the sources listed above. Sorry, I didn’t have time to finish this quitethe way I would have liked. But I’m sure you’ll manage :)

First, follow the suggestions above to keep Cicada as stable as possible.

In control Room---------------My object doesn’t appear on Ximtool after readout? -Cloud -Dome is blocking view -Dome shutter blocking view -Camera shutter failure

I see streaks on my image? -Camera shutter failure -Initialise hardware (a last resort)

I can’t analyse images (star profiles, stats, etc) in ximtool.The image just goes to a single value! -start a private ximtool in GIT.

Cicada has hung? -Exit Cicada, cleanup, restart Cicada. -Stop processor/memory intensive processes -Avoid using abort -Don’t use pause

Lots of Red Error Windows, Can’t Stop Them! -Kill Cicada from the command line, cleanup and restart

I can’t point the telescope more accurately than 20arcsec? -Tough! The telescope only points to within about 20arcsec -But, use buttons on round focus/guide/set paddle. Use set or guide speeds. With practice this becomes fairly accurate (to within a few pixels).

Ximtool menus are inactive -untoggle NumLock

I can’t change brightness/contrast using left mouse scrolling? -untoggle NumLock

New images keep loading into my private Ximtool? -turn off automatic loading of images by toggling the "cicada mode" button under the GIT options|preferences|general menu.


9 of 9 16/05/05 11:48 AM

(This is suposed to work, but doesn’t)

My star images are elliptical -focus telescope

Focussing is difficult -too bad! -try focusing from same direction to take up backlash

There is bleeding on stars & bias has changed -restart cicada.

I can’t see my guide star (while setting up guiding) -Open the shutter!

I can’t find the "Guide CCDs - WFI" chooser window -scroll down in the m40slave window

Autoguiding doesn’t seem to be working accurately -set the declination correctly on the "guide" tab in the Maxim CCD window

In Dome-------Dome doesn’t follow telescope? -Check dome position encoder (high on the western wall) is flashing its green LEDs at you. If not restart ETS (select file|shutdown, then startup at the prompt). -Put dome in auto mode on ETS (select configuration|configure)

Telescope pointing is bad -Calibrate the pointing -Reset the time (Phone 1-1194)

Telescope doesn’t move -ensure floor is fully down -Fault in ETS (Call technical support?)

Telescope moves unexpectedly by itself -Press big red STOP button on dome console, or on electronics rack in control room

Shutters don’t move -press shutter|stop button and try again (Listen for the relays clicking downstairs) -If upper shutter doesn’t close it needs to be driven fully open (onto its springs) first.

LN2 leaking from filling tube? -Tighten the various nuts on the tube

LN2 leaking from camera dewar at high ZD angles? -Remove lens-cap before filling camera dewar -do dome-flats before filling camera dewar

LN2 small tank pressure low? -small tank needs filling from large tank (call technical support?) -pressurise small tank with N2(or air?) line (How?)

SDSU controllers feel hot -Water cooler has failed. Check it and restart it, if necessary.

Dewar vacuum rising or focal plane temperature not holding -pump dewar (call technical support?)

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How to get to Siding Spring ObservatoryFrom SydneyCoonabarabran is about 500 kilometres north west of Sydney and Siding SpringObservatory is about 40km from Coonabarabran. Most people travel to Coonabarabraneither by air or car, though other modes of travel (train, bus) are possible for theadventurous or those with time to spare.

Travel optionsFor detailed information on travel between SSO and Sydney, please refer to theAAO’s Travel and Accommodation page.

Travelling by road - some adviceIt is worth reminding people who travel to or from Coonabarabran by road of themain risks, which are:

The standard of even the main highways in NSW varies from excellent topotentially dangerous and the journey from Sydney to Coonabarabraninvolves mainly secondary roads. There are several places where roadconditions change rather suddenly and can catch drivers unaware, especiallyif they are travelling fast.Some stretches of road pass through countryside frequented by kangarooswhich constitute a serious traffic hazard, especially in twilight and at night. Tryto ensure that you start your journey early enough to avoid them whenapproaching Coonabarabran.The road journey between Sydney and Coonabarabran is quite long (around7 hours). Drivers should be well rested before they embark on it, and shouldalso stop for short rest breaks along the way.

From Mount Stromlo Observatory

By AirThere are no air services between Canberra and Coonabarabran but check theAAO’s Travel and Accommodation page for air (and other) services between Coonaand Sydney.

By CarStromlo staff and students travel by car from MSO to SSO. It should be possible foryou to share a car with someone else going to SSO for an observing run. The triptakes about seven hours, so be prepared to share the driving and read the abovewarnings about driving on N.S.W. country roads.

If you have your own hire car, ask anyone at Stromlo for advice on directions toSSO.





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AAO Travel and AccommodationWant to book your travel for your next observing run? Use our Travel Booking Form.

Travel between Sydney and Coonabarabran

Coonabarabranis about 500 kilometres north west of Sydney. Most people travel to Coonabarabran either by air or car, though other modes oftravel (train,bus) are possible for the adventurous or those with time to spare. For some helpful advice on places along the route to Coonabarabranand Siding Spring, please go to our Librarian’s information on the Road to Coona

By air: Either via Dubbo Airport, which is the closest main airport in the area, or Coonabarabran Airport**NOTE: BIG SKY EXPRESS has suspended it flights to Coonabarabran until further notice. A review is planned for April 2005, and anydevelopments will be posted here.

If you require further assistance please contact the Travel Officer.

Dubbo:The next closest airport is Dubbo, which is currently only serviced by Qantas (code sharing with Eastern Airlines.) Details of services andcharges can be found on their web site (you can also book on-line): www.qantas.com.au

Getting to Siding Spring from Dubbo Airport: If you want a taxi booked, please let us know on the travel form and we will arrange it. The taxi fare is now $AUD 350 each way and takesabout two hours.

You can also arrange a hire car. It would be wise to do so in advance. (See the warnings below relating to car travel.) Thrifty Car Rentaloperates out of Dubbo airport. Further details on their web page:

By car: Road travel notes are available here.It is worth reminding people who travel to or from Coonabarabran by road of the main risks, which are:

The standard of even the main highways in NSW varies from excellent to potentially dangerous and the journey from Sydney toCoonabarabran involves mainly secondary roads. There are several places where road conditions change rather suddenly and cancatch drivers unaware, especially if they are travelling fast.Some stretches of road pass through countryside frequented by kangaroos which constitute a serious traffic hazard, especially intwilight and at night. Try to ensure that you start your journey early enough to avoid them when approaching Coonabarabran.The road journey between Sydney and Coonabarabran is quite long (around 7 hours). Drivers should be well rested before theyembark on it, and should also stop for a short rest breaks along the way.

It is possible to hire a car in Sydney to do your round trip to site. The prices for the main hire car companies vary slightly but for under 5days $60.00 to $70.00 is about average per day, plus, in some cases, an additional kilometre charge.The AAO usually books hire cars through Red Spot Car Rentals, or Avis Car Rentals. Both companies deliver to where observers arestaying in Sydeny, and pick up the returned vehicle, for no additional cost (within a 10Km radius of the nearest rental office). Their rates arealso fairly competative, with Red Spot averaging at $42 per day. Alternatively, Bayswater Car Rentals is even cheaper, however clients must pick up the vehicle in person at the Kings Cross office, andthey are not open on Saturday afternoons or Sunday all day. The Travel Officer can book the car if instructed to do so on the Travel Form

By train:

The CountryLink division of State Rail offer a linked train/bus service to Coonabarabran, this has the longest journey time but thetrain leg through the Blue Mountains is very picturesque. The service departs from Sydney Central Railway Station, arriving inLithgow 2hrs and 20 mins later. In Lithgow meet the coach to Coonabarabran, which takes between 5hrs to 5hrs and 25mins. Thetotal cost is $AUD119.00 return. A combination train/coach ticket can be purchased as one ticket from the CountryLink office.The website for CountryLink is www.countrylink.nsw.gov.au(Note: Currently, the website does not include a complete schedule for the train/coach between Sydney and Coonabarabran.)For international visitors, you will find information on international agents for CountryLink on their website. These are listed in the‘Bookings’ section under ‘International’. You are able to book the ticket through an agent closest to you.For Australian observers, the bookings phone number within Australia is 13 22 32The current schedule is as follows:TO COONABARABRAN:MONDAYS:Sydney to Lithgow; 7.10 - 9.30Lithgow to Coonabarabran; 10.00am - 3.25pmTUESDAYS, WEDNESDAYS, THURSDAYS:Sydney to Lithgow; 7.10am - 9.30amLithgow to Coonabarabran; 10.00am -2.50pmFRIDAYS:Sydney to Lithgow; 7.10am - 9.30amLithgow to Coonabarabran; 10.00am -2.50pmSATURDAYS:No ServiceSUNDAYS:Sydney to Lithgow; 4.00pm - 6.45pm

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Lithgow to Coonabarabran; 7.05pm - 12.15amTO SYDNEY:MONDAYSCoonabarabran to Lithgow; 12.35pm - 6.05pmLithgow to Sydney; 6.25pm -8.50pmTUESDAYS, WEDNESDAYS, THURSDAYSCoonabarabran to Lithgow; 1.00pm - 6.05pmLithgow to Sydney; 6.25pm - 8.50pmFRIDAYCoonabarabran to Lithgow; 9.50-2.50pmLithgow to Sydney; 3.05pm-5.45pmSATURDAYNo service.SUNDAYCoonabarabran to Lithgow; 1.00pm - 6.05pmLithgow to Sydney; 6.25pm - 8.50pm

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26 October 2004

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Accommodation Facilities at Siding SpringAccommodation on Siding Spring Mountain is at The Lodge, which is run by theAustralian National University. Bookings must be made well in advance of yourobserving run.

The current Lodge tariff is $113.30 (including GST) per day, including meals,and can be paid with a Credit Card (VISA/MASTERCARD/BANKCARD), inAustralian dollar traveller’s cheques or Australian currency. Personal chequesdrawn on an Australian Bank are accepted.

Partners can stay at The Lodge (1 or 2 larger rooms are available) for anadditional charge (this covers the extra meals and linen required). There is alsoa self-contained cottage on the mountain for families; enquiries about itsavailability should be made directly to The Lodge staff (Tel +61 2 6842 6246, Fax +61 2 6842 6252).

Lodge staff are usually able to cater for special dietary needs or preferences,but prior arrangement should be made. Alcoholic beverages may be consumedat The Lodge, but strictly on a BYO (Bring Your Own, there is a bottle shop inCoona) basis. Two meals are prepared each day - a breakfast/lunch (youchoose depending on your body clock - just let the kitchen staff know the nightbefore) and dinner served before twilight each day. There is also a small kitchenavailable 24 hours a day where Lodge guests can make their own tea, coffee orbreakfast if they choose. A "midnight lunch" is normally provided for observersto have with them at the telescopes.

The Lodge reading room has a range of recreational reading matter, includingthe latest newspapers. There is a small library of videos for those cloudy nightsas well as a pool table and dart board in the recreation room. A washingmachine, dryer and ironing board are also available.

SSO Accommodation Booking Form

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NB: This service is for observers external to RSAA only.RSAA staff should follow the internal admin procedure.

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If you are flying into Coonabarabran please give your flight details:

Do you need a taxi to pick you up from the airport? Yes No

If you are flying out of Coonabarabran please give your flight details:

Do you need a taxi to take you to the airport? Yes No

Do you need to book accommodation for more than yourself (e.g. partner, children)? Yes No

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Page last updated: 08 March 2005Please direct all enquiries to: Webmaster



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After hours support - Siding Spring Observatory

The telescopes operated by the ANU (RSAA) at Siding Spring (2.3m, 40", 24", 16") are covered after hours by the following arrangements:

A member of ANU SSO Technical Staff is present at the Observatory until 18:00. This person can be contacted in the 16" dome or on the mobilephone number posted in each dome.A member of ANU SSO Technical Staff is on-call from 18:00-22:00 each working day. This person’s name and contact details are posted in eachdome.A member of ANU SSO Technical Staff is on-call from 11:00-23:00 at weekends and public holdays EXCEPT that there is no support during the Christmas and Easter holidays

Computer problems at the SSO telescopes are covered by an informalarrangement as follows:

If possible, first consult with the on-site SSO Technical Staff memberThe following staff have agreed to offer advice by phone, but no later than 10:30 pm. On occasions and at their discretion, they may offer furtherassistance. If problems arise before 10:30 pm, call the staff listed in theorder on the following list.Jon NielsenGreg WilsonBill RobertsPeter Young





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