john nousek (penn state university) neil gehrels (goddard space flight center)
DESCRIPTION
Five Years of Science: GRBs and More!. John Nousek (Penn State University) Neil Gehrels (Goddard Space Flight Center). International Workshop on Astronomical X-ray Optics - Prague, Czech Rep. – 6-9 Dec. 2009. Swift launch: 20 Nov 2004 !!. - PowerPoint PPT PresentationTRANSCRIPT
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John Nousek (Penn State University)Neil Gehrels (Goddard Space Flight Center)
Five Years of Science:GRBs and More!
International Workshop on Astronomical X-ray Optics - Prague, Czech Rep. – 6-9 Dec. 2009
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Swift launch:
20 Nov 2004 !!
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5th Anniversary of Swift Conference
• Celebration of Swift held at Penn State, 18-20 Nov. 2009
• Attracted more than 150 participants – 1/3 Penn State, 1/3 US & 1/3 from ten other countries
• Discussed impact of Swift on areas of astrophysics, and planned for future developments and science direction of the Swift Observatory
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Swift has redefined the field of GRB science.
GRB backgroud
Swift comparisonsDuration
Host galaxiesDistance distributions
EnergeticsBeaming
Swift GRB Science
ARAA Annual Reviews 2009 Gehrels, Ramirez-Ruiz and Fox
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GRB PropertiesTwo types:
Short GRBs (t < 2s) Long GRBs (t > 2s)
Redshift range: 0.2 - ~2 SGRBs 0.009 - 8.2 LGRBs
Energy release in -rays: 1049-1050 ergs SGRBs 1050-1051 ergs LGRBs
Jet opening angle: ~15 deg SGRBs ~5 deg LGRBs
Both types have delayed& extended high-E emission
ARAA article
GRB 990123HST image
Fruchter et al.
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GRB Spectraprompt
afterglow withsynchrotron fit
GRB 051111
Butler et al. 2006
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VELA GRB discovery
1973
Compton / BATSE isotropy &
inhomogeneity 2 duration classes
1991
Compton / EGRET GeV extended emission
1994shortlong
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BeppoSAX afterglow & distance
1997
Fireball Model 1997
Mészáros & Rees 1997
HETE-II GRB030329 / SN2003dh
XRFs ~ 2003
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BAT
XRTUVOT
3 instruments, each with:
- lightcurves - images - spectra
Rapid slewing spacecraft
Rapid telemetry to ground
.
Swift Mission
BAT Position - 2 arcmin
T<10 sec
XRT Position - 5 arcsec
T<90 sec
UVOT Position - < 1 arcsec
T<2 min
XRT
BAT
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Short GRB
Short GRB
Swift Statistics475 GRB as of 1 Nov 2009
85% with X-ray detections ~60% with optical detection
155 with redshift (41 prior to Swift) 46 short GRBs localized (0 prior to Swift)
Fast Rise Exponential Decay
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Swift GRB Data
UVOT image
BAT lightcurve
XRT lightcurve
GRB 091029
GRB
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Swift GRB Data
BAT lightcurve
XRT lightcurve
GRB 091029flare
steep-flat-medium shape
UVOT image
GRB
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Shortvs
Long
short long
Time (s)
Number Gamma Rays
Time (s)
Numåber Gamma Rays
Soft
Hard
Hardness
Ratio
Duration (s)
shortlong
Kouveliotou et al. 2003
•
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GRB Spectroscopy
z Time GRB Optical Brightness
(109 years)
8.3 13.0 090423 K = 20 @ 20 min
6.7 12.8 080813 K = 19 @ 10 min 6.29 12.8 050904 J = 18 @ 3 hrs
5.6 12.6 060927 I = 16 @ 2 min
5.3 12.6 050814 K = 18 @ 23 hrs
5.11 12.5 060522 R = 21 @ 1.5 hrs
Prochaska et al. 2008
Savaglio 2006
GRB 080607
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Blast from the past!GRB 090423
Lyman break redshifted from UV to IR
z = 8.29 look back time = 13.0 billion light years
GROND Greiner et al
•
Tanvir et al. 2009; Salvaterra et al. 2009
McMahon & Tanvir
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Evolution of Swift Operations – GRBs & More!• Original prime mission: 2004-2006 – Swift the GRB Explorer
• Up to Nov. 2004 – Pre-launch:– Swift primarily a GRB detection and afterglow followup mission
– Ground-breaking operations design allows immediate response to GRBs
– Automated follow-up allows introduction of new GRB without new schedule
– Targets of Opportunity limited to new non-Swift GRBs or rare events
• Expected schedule re-plans only once / month; ToO once / week
– Planning using TAKO software / five times a week• Prime mission – 2005-2006:
– Execution closely follows plans, except:• XRT TEC power supply fails, forcing operations to passively maintain XRT
below -50 C• Automated target process is great success allowing highly flexible and rapid
ToO response
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Swift Operations Currently• 1st mission extension: 2006-2008 – High-z GRBs and the GI Program
– Swift reduces time on late afterglow followup and increases effort on finding high redshift GRBs
• Swift introduces GI targets, followed by pressure for increased ToO and monitoring campaigns
– TAKO planning software modified to incorporate XRT temperature control; other ancillary software improves ACS reliability
– Improved ToO automation allows multiple ToOs in short period without new schedule (including nights and week-ends)
– Targets of Opportunity and Monitoring Campaigns occur every day
• Typical load of 4-12 ToO or Monitoring observations every day
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Supernova Studies with Swift
XRT and UVOT observations
of SNe
-66 observed to date of all types (26 Ia, 18 Ibc, 22 II)
-UV, optical & X-ray densely-sampled light curves
-Largest sample of SN light curves in the UV
-Unique UV characterizations of SN Ia's (incl UV spectra)
SN 2006bp (Type IIP)
Immler et al. 2007 Brown et al. 2008
XRT UVOT opt UVOT UV
SupernovaLightcurves
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X-Ray SN Studies
Immler et al.
- XRT observations probe SNe
environments & mass-loss rates
- Signature of SN shock traveling
through dense shell
- Shells are outer H/He-rich layers
from Luminous Blue Variable phase
SN 2006jc
SN 2008bo
SN 2006bp
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SN 2008D Shock Breakout
- XRT monitoring of NGC 2770 (27 Mpc)
revealed extremely luminous X-ray outburst
- EX ~ 2x1046 ergs
- No BAT, no radio late >> probably no jets
- UVOT detection of SN rising 90 min later
- SN Ib/c
- Shock breakout. May occur for all SN
Soderberg et al. 2008
9 Jan 2008
SN 2007uy
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- 25 novae observed
- Rise and fall of few keV
emission from shocked ejecta
- Super-Soft emission in
some from WD surface (kTBB ~ 30 eV)
- Extensive observations of
RS Oph 2006 (~400 ksec) revealed
unexpected luminous SSS state and 35
sec QPO
- Earth mass ejected at ~4000 km/s into wind of companion
Red Giant
RS Oph
Nova Studies with SwiftThermonuclear detonation of
accumulated accretion on white dwarf
1.6 kpc
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• BAT triggered on a stellar flare from nearby (d=5 pc) EV Lac (dM3e, Prot ~4 days)
• XRT spectra show Fe K 6.4 keV emission
first for an active dMe star
• UVOT enhancement large but unknown: instrument safed at >200,000 counts/s
• Brightest stellar flare observed
• Erad ~ 1038 erg
• EV Lac is young magnetically active
isolated star.
– Previous super-flare was from binary
RS CVn system, II Peg
Swift Trigger on Large Stellar Flare
Osten et al 2007, 2008
EV Lac25 Apr 2008
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Newly discovered source (Atel #1456) Known pulsar in outburst (Atel #1426)
536 sources monitored
65 detectable on a
daily basis
~60 with > 30 mcrab
outbursts
~15 mCrab sensitivity
in 1 day
http://swift.gsfc.nasa.gov/docs/swift/results/transients/
BAT Sky Monitoring
SWIFT J1816.7-1613 4U 0115+634
Krimm et al
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TOOs for Transients & GRBs
- Swift can perform rapid X-ray and optical
observations of transients
- TOO rapidly uploaded as RA & DEC. Response time
is <1 hour to 1 day
- Web page for TOO requests http://www.swift.psu.edu/too.html
- Duty scientists always on call for urgent TOOs
- New "command from home" mode for after-hour TOOs
- Expert international teams provide rapid advice* GRB follow-up (48 members)* Supernova (22 members)* CVs & novae (24 members)
* Hard X-ray survey(18 members)* AGN (4 members)
* GeV and TeV -rays(4 members)
- Daily planning telecon to decide schedules
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Swift Operations Ahead
• 2nd mission extension: 2009-2011 – Swift: the ToO Observatory– Swift executes ~70-75 separate pointings per day
• Each pointing is planned, although significant labor by human science planner to have each pointing a different target
– Under an initiative approved by 2008 Senior Review, MOC has conducted an Automation Initiative to streamline science planning
– Elements include:
• Target management database – MySQL database to automatically ingest target information from ToO requests, target lists from GI approved proposals and GRB information from GCN circulars
• More highly automated TAKO software – will allow higher automation to XRT temperature control and ACS slew behavior
– Goal is to allow faster, easier science planning, with capability to increase GI monitoring campaigns and rapid ToO response to large numbers of targets
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Conclusions
• Swift has delivered a remarkably successful science mission to date, powered by an innovative operations concept that has continued to evolve as driven by scientific interest
• The latest changes will enable an even more responsive observatory, giving more GI monitoring and ToO responsiveness
• For Senior Review 2010, How do you suggest ways to use Swift, and how is that important for astrophysics?
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Cosmic Timeline & Early Universe Probes
z=12 z=5 z=0
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Hint That These Probes Work
z=6.29
GRB 050904 SDSS Quasar
z=6.28
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• Swift & SDSS only probed the very near edge of reionization
• We need a statistically significant sample that probes well into the epoch of reionization– We need to find 30-50 GRBs from 5<z<12
• ~10x what Swift found (5<z<7)
– We need to find 200-400 quasars from 6<z<10• ~10x all z>6 quasars found (6<z<6.5)
We Need Higher Redshift Observations
z=12 z=5
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• Current capabilities from Swift & SDSS needed to observe high redshift objects are:– Rapid localization and observations of GRBs– Rapid notifications to enable observations by other facilities– A very large field of view for finding GRBs & quasars
• BREADTH versus Depth for rare objects (Critical)
• To probe high redshift objects we need:– Greater sensitivity to high redshift bursts
• Redshifted gamma-ray photons into the X-ray
– Prompt, uniform follow-up of afterglows in the IR (Critical)– Rapid redshift determination (in minutes)– Observations above the atmosphere are essential to
eliminate terrestrial lines that confuse surveys
Current Capabilities & Needs
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The Solution: JANUS
1960 1980 2000
Testing
Support
BCD DEF
GHIJKL RST VWX XYZ TUV
Space Network
ABC
1960 1970 20201980 1990 2000 2010
Increasing Capabilities
X-Ray Flash Monitor (XRFM): Detects &
localizes high-z GRBs 1-20 keV, 4 sr field-of-
view
Near-IR Telescope (NIRT):
High-z GRB & quasar spectroscopy
0.7-1.7 μm, 1″ pos, redshifts,
0.36 degree2 field-of-view,
Spacecraft: Rapid
communication w/ ground, rapid
slewing (50°/100 sec),
stable platform
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JANUS Mission Concept – Sky Survey Mode
~400 quasars
20,000 square degreeSurvey
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JANUS Mission Concept – GRB Mode
~50 GRBs
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JANUS Objectives
• Determine star formation history• by using ~50 GRBs
• Explore the coevolution of galaxies & black holes • by using ~400 quasars
• Determine if dominant source of reionization