Requirements on array detectors from the

OWL Instrument Concept Studies

Sandro D’OdoricoEuropean Southern Observatory

SDW 2005TAORMINA

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OWL INSTRUMENT CONCEPT STUDIES

Framework, Scope, Status

8 Instrument Studies were launched in 2004 by ESO in the framework of the 100m OWL Concept Study,

The present set of instruments cover the spectral range from the blue to sub-mm with different scientific field of views and image quality requirements

The scope of the studies is:

• to support the OWL science cases

• to verify with actual instrument concepts interfaces and operation scheme of the telescope design

• to check feasibility of instrument concepts and identify needs and required R&D for the different subsystems

The Instrument Concept Study final Reports are due in September-October 2005. This

advanced overview of the detectors requirements is based on the work in

progress.

Thanks to the P.I.s!

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OWL Instrument Concept Studies (status June2005)

Instrument Wave range (m)

Capability Primary Science Goals (current guess)

Institutes External Responsible

Responsible at ESO

CODEX 0.4-0.7 High velocity accuracy, visual spectrograph

To measure the dynamics of the Universe

ESO, INAF-Ts, Geneve Obs, IoA

Cambridge

= L. Pasquini

T-OWL 2.5-20 Thermal, Mid Infrared Imager and possibly

Spectrograph

Search, study of planets, high redshift H galaxies

MPIfA, Heidelberg, Leiden Obs., ESO

R. Lenzen H.U. Kaeufl

QUANTEYE 0.4-1 Study will review /explore aspects of quantum

astrophysics with OWL

Astrophysical phenomena varying at sub-second time scale, others

tbd

Padova Univ., Lund University

C.Barbieri and D. Dravins

R. Fosbury

SCOWL 250-450-850 tbc

Imaging at sub-millimeter wavelengths

Surveys of dusty regions, of extr. fields for star-forming galaxies

ATC I. Egan R. Siebenmorgen

MOMFIS 0.8-2.5 Near IR spectroscopy with multi-object,multi field

units

Masses of high z galaxies, regions of star formation, GC stars

CRAL, LAM, OPM J.G. Cuby M. Casali

Large Field IR camera

0.8-2.5 NIR Imaging Camera on a field of 1x1 / 2x2 arcmin

Faint stellar and galaxy population INAF- ArcetriHeidelberg MPIfA

R. Ragazzoni E. Marchetti

EPICS 1-5 tbc

NIR Camera-Spectrograph at diffraction

limit(+coronograph)

Imaging and spectroscopy of earth-like planets

ESO + ext. experts = N.Hubin

Hyper-telescope Camera

1-2.5 Speckle interferometry with a partially filled

OWL aperture

Planetary disks, exo-planets LISE lab at OHP V. Borkowski G. Monnet

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Cosmic Dynamics EXperimentConcept Study carried out by ESO, Cambridge,

Geneve and INAF Oss. Trieste

Main GoalA direct measurement of the

cosmic acceleration

Obtained by comparing high resolution spectra of the Ly forest and metal systems in the direction of bright QSOs

over a large time interval (10 years or more)

Portion of the Ly forest at z=3

Simulation of the difference between 2 epochs

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Cosmic Dynamics EXperiment

Concept Study carried out by ESO, Cambridge, Geneve and INAF Trieste

RequirementsSpectral range: 400-650 nmResolution 100000-150000

Stability 1cm/s with long term absolute calibration

ConceptThe light is sent to 5 separate echelle

spectrographs a la HARPS (in vacuum, at very stable T)

Detector estateThe spectra are spread out over 60 2K x 4K CCD (15 pixel). Within a factor

of 2, depending on telescope size and resolution. r.o.n 1-2 e-,d.c. 1e/pix/h

Echelle mosaic 22 x 170 cm

Camera

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Earth-like Planet Imaging Camera Spectrograph

Concept study by ESO and a number of scientists and engineers from different institutes in F, I, D,NL and SUI

EPICS starting point are the current studies for the Planet Finder at the VLT

The instrument aims at the detection and characterization of earth-like planets

The AO system for this instrument is expected to be a combination of the standard system offered by the telescope + an EXAO internal to the instrument

The observing modes being presently considered are Differential Imaging, Polarimetry and Integral Field Spectroscopy in the visual and Y,J bands

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Earth-like Planet Imaging Camera Spectrograph

Concept study by ESO and a number of scientists and engineers from different institutes in F, I, D,NL and SUI

Mode Field (arcsec)

Pixel R Total Array Estate

Differential Imaging 4 x 4 0.5 mas 2( 8K x 8K) IR

Polarimetry 2 x 2 0.5 mas 8K x 4K , fast read-out

IFS red 1 x 1 0. 35 mas 10 8K x 8K CCD

J band 2 x 2 0.5 mas 10-50 8K x 8K NIR

Wawefront Sensor for EXAO

= 3K x 3K, ~1KHz (SH)

Preliminary detector requirements from EPICS

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QUANTEYE

Concept Study carried out by Dept.of Astronomy, Univ. Padova and Observatory, Univ. Lund (P.I.s C.

Barbieri and D.Dravins)

Ultra-fast photometer for Quantum Astronomy

Main mode: to study the single photon arrival time statistics at the largely unexplored 10-3 -10 -9 second resolution. Large advantage from telescope size when studying photon correlation.

Wavelength range 400-700 nm, target on axis + reference in the 3 arcmin field, 2D resolution not required,

Single photon counting detectors with required ns resolution , high efficiency, low dark current

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QUANTEYE

Concept Study carried out by Univ. Padova and Univ. Lund (P.I.s C. Barbieri and D.Dravins)

1 arcsec in OWL focalplane ~ 3mm. Present concept: to sample collimated beam in 100 subpupils

Possible Detectors: 2 disperse arrays of 10 x 10 Si Single Photon Avalanche Diode (SPAD-A)

Antireflection Coating on SPADs

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

400 450 500 550 600 650 700 750 800

Wavelength [nm]

Det

ectio

n E

ffic

ienc

y

Multilayer 78 nm SiO2 50 nm Si3N4

120 nm SiO2

No coating

AR coatings on SPAD-courtesy of S.Cova

OWL focus f/6f/1

f/1

… …

f/1 SPAD

M = 1/6 M = 1/10

SPADA Test Chip-PoliMi

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Large-Field NIR Camera

Concept Study carried out by INAF-Arcetri and MPIfA Heidelberg (P.I. R. Ragazzoni)

•J,H,K; central field (30-60 arcsec diameter sampled at ~diffraction limit); outer field 3-6 arcmin. Choice dictated by AO performance, science case, cost and complexity.

•MCAO using 2-3 DM for the central part, GLAO for the outer part

Detector Requirements

Central field of 30” sampled at 1mas (Nyquist at K) 15 x15 (2K x 2K)Hg Cd Te arrays (or 8 x 8 (4K x 4K), 12m pixels)

Outer field (e.g. 3’ x 3’) with a 10mas sampling 9 x 9 (2K x 2K)Hg Cd Te arrays

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Multi–Object Multi–Field Imager Spectrograph

Concept Study carried out by LAS Marseille, GEPI, Obs. Meudon, Obs. Lyon (P.I. J.G. Cuby)

Multi-IFU (30) system to pick up targets over the 3’ (6’) scientific field

“local” AO using mini DM in the light path of each IFU

Spectroscopy J or H or K in one shot at R= 4000

Spatial sampling 50 mas, N pixels per IFU 30 x30

18 Hg Cd Te (2K x 2K) arrays / band

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T – OWL (Thermal IR Camera - Spectrograph for OWL)

Concept Study carried out by MPIfA Heidelberg and Leiden Observatory (P.I. R. Lenzen)

Wavelength Range: 3- 27 m

Imaging Pixel Scale: 3.5 mas@ 3-5 m,

7.0 mas @ 7-14 and 16-25 m

FOV 15x15 arcsec

4 (2k x 2k) InSb (0.9 – 5.4 m)

4 (1k x1k) Si-As (2-28 m)*

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SCOWL (SCUBA at OWL)

Concept Study carried out by ATC (P.I. I. Egan)

Imager in the 350 and 450 m bands (850 m desiderable)

FOV 2 x 2 arcmin, Surveyer for ALMA targets Resolution <2 arcsec

4 SCUBA 2 TES Detectors (20480 pix)

Transition Edge Sensors hybridized to a Superconducting Quantum Interference Design (SQUID) time-division multiplexer

Ceramic PCB 40x32 sub-array

NiobiumFlex Cable

Woven Cables to Room Temperature

SQUIDSeriesArray

Amplifiers

Ceramic PCB 40x32 sub-array

NiobiumFlex Cable

Woven Cables to Room Temperature

SQUIDSeriesArray

Amplifiers

subarray

Readout PCBs

subarray

Readout PCBs