swift x-ray telescope operations– monitor blast wave evolution (time resolution: 0.14 ms or 2.2...
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![Page 1: Swift X-ray Telescope Operations– Monitor blast wave evolution (time resolution: 0.14 ms or 2.2 ms) XRT Science Goals 6 7 September 2004, Swift Workshop @ HEAD 2004 XRT Instrument](https://reader030.vdocument.in/reader030/viewer/2022041104/5f0475ec7e708231d40e1478/html5/thumbnails/1.jpg)
117 September 2004, Swift Workshop @ HEAD 2004
Swift X-ray Telescope Operations
David BurrowsXRT Lead
University Partners:PSU UL OAB
Calibration Partners:PSU / UL / OAB / MPE
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227 September 2004, Swift Workshop @ HEAD 2004
Swift Artist’s View
Burst Alert Telescope(BAT)
Spacecraft
Optical Bench
UV/Optical Telescope(UVOT)
X-Ray Telescope(XRT)
XRT Radiator
Sunshade
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337 September 2004, Swift Workshop @ HEAD 2004
The Swift Observatory
XRTTelescope
Tube
XRTElectronics
UVOT
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447 September 2004, Swift Workshop @ HEAD 2004
The Swift Observatory
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557 September 2004, Swift Workshop @ HEAD 2004
1) Rapid determination of GRB position(accuracy < 5’’, transmit to ground < 100 s after burst)
2) X-ray spectroscopy– Determine Redshift from Emission Lines or Absorption Features in
X-ray Spectrum– Determine physical conditions of ISM in vicinity of burst
(energy resolution < 140 eV @ 6 keV at launch)
3) Burst/Afterglow Lightcurve– Monitor blast wave evolution
(time resolution: 0.14 ms or 2.2 ms)
XRT Science Goals
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667 September 2004, Swift Workshop @ HEAD 2004
XRT Instrument Characteristics
Telescope 3.5m Wolter I
Telescope PSF 18 arcsec HPD @ 1.5 keV22 arcsec HPD @ 8.1 keV
Detector e2v CCD-22
Detector Format 600 x 602 pixels
Detector Readout Modes
Photon-counting, Imaging, & Timing
Field of View 23.6 x 23.6 arcmin
Pixel Scale 2.36 arcsec / pixel
Energy Range 0.2 - 10 keV
Effective Area 135 cm 2 @ 1.5 keV
Sensitivity 2 x 10 -14 ergs/cm2/s in 10 4 s
Position Accuracy 2.5 arcseconds
Operation Autonomous
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777 September 2004, Swift Workshop @ HEAD 2004
Observing Scenario
BAT Burst Image
T<10 secd_ ~ 4’
1. Burst Alert Telescope triggers on GRB, calculates position on sky to < 4
arcmin
2. Spacecraft autonomously slews to GRB position in 20-75 s
3. X-ray Telescope determines position to ~3 arcseconds
4. UV/Optical Telescope images field, transmits finding chart to ground
BAT Error Circle
XRT Image
T<300 sec
UVOT Image
T < 100 sec dθ ~ 3 arcseconds
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887 September 2004, Swift Workshop @ HEAD 2004
XRT Readout Modes
<0.0001
.00005- .15
.05 –60
.025 -37
Flux(Crabs)
Bias mapsubtraction
Bias rowsubtraction
Bias levelsubtraction
No biassubtraction
Bias DataTimingSpectroscopy
Imaging
Mode
3x3 neighborhoodsabove threshold
2.5 sFull2-DPhoton-Counting
Events above threshold2.2 msFull1-DWindowedTiming
Events above threshold0.14 msFullNonePhotodiodeTiming
Centroid, Postage-stamp, thresholdedimage
0.1 / 2.5s
None2-D
Low GainImaging(centroid)
XRT must autonomously select readout modes suited toobservations of GRBs and afterglows:
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997 September 2004, Swift Workshop @ HEAD 2004
XRT AutonomousObserving Sequence
Δ t < 5 s
1 mCrabs < F < 600 mCrabs
F < 1 milliCrabs
Start Slew Take Bias Images
On Target?
Image mode Position to TDRSS
Photodiode (no position)
Windowed Timing (1-D position)
Photon-Counting
-
0.6 Crabs < F < 60 Crabs x
x
x
N
Y
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10107 September 2004, Swift Workshop @ HEAD 2004
Swift GRB Monitoring
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11117 September 2004, Swift Workshop @ HEAD 2004
Day in the Life of Swift XRT
PPT1PPT2PPT3PPT4AT (GRB)
Snapshot 1/15
Snapshot 2/31
Snapshot 3/42
Snapshot 4/22
Snapshot 1/16
Snapshot 2/32
Snapshot 3/43
Snapshot 4/23
Snapshot 1/17
2/33
Snapshot 3/44
Snapshot 4/24
# 5/1
Snapshot 1/18
Snapshot 5/2
#2/35
2/34
Snapshot 3/45
Snapshot 4/25
Snapshot 5/1Bias | PD | Image | --- PD --- | --------- WT ---------
SLEW Snapshot 3/45Bias | PD |------ WT ----- | ------------------ PC -----------------------
SLEW
Orbit 1 Orbit 2 Orbit 3 Orbit 4 Orbit 5 Orbit 6 Orbit 7 Orbit 8 Orbit 9
Centroid Position Message
Postage-Stamp Image Message
Raw Spectrum Message
TDRSS messages:
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12127 September 2004, Swift Workshop @ HEAD 2004
Typical XRTObservation Sequence
Slew
Bias row, Bias map,
(Raw frame),Photodiode
Bias map600 x 602,
(Raw Frame635 x 602)
Settle
Photodiodemode
Photodiodeevents, 1 pixel
24’ x 24’
Centroid
Imagemode
Flux (mCrabs) 5000 5000 3000 800 100
Time (s) 0 43 50 55 400 1000
Mode
ScienceDataProducts
Activity
Imagepixels,
600 x 602 24’ x 24’
TDRSSDataProducts
Automated Observation
Photodiode mode,8s per ‘frame’
Photodiodeevents, 1 pixel
24’ x 24’
Windowed Timing mode,0.8 s per ‘frame’
Windowed Timingevents,
200 columns8’ x 24’
Centroid Position
Postage-Stamp Image,
51 x 51 pixels,2’ x 2’
Raw Spectrum,1024 channels,
0-10 keV
ConstraintViolation
Slew
GCN
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13137 September 2004, Swift Workshop @ HEAD 2004
XRT Calibration – Munich,September/October 2002
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14147 September 2004, Swift Workshop @ HEAD 2004
XRT Angular Resolution
PSF is uniform over FOVHPD = 18 arcsec @ 1.5 keV = 22 arcsec @ 8.1 keV
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15157 September 2004, Swift Workshop @ HEAD 2004
XRT Position DeterminationAccuracy
Panter test results: Centroid Accuracy vs Flux
1.0 10.0 100.00.10.01
Flux (Crabs)
Switches from 2.5 s to 0.1 s exposure
Cen
troi
d A
ccur
acy
(arc
seco
nds)
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16167 September 2004, Swift Workshop @ HEAD 2004
XRT Position DeterminationTiming
1.0 10.0 100.00.10.01
Flux (Crabs)
Total time (exposure + readout + calculation) < 5.2 s
Switches from 2.5 s to 0.1 s
Flux (Crabs)
1.0 10.0 100.00.10.01
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17177 September 2004, Swift Workshop @ HEAD 2004
XRT Spectroscopy
55Fe spectrum (Mn Kα and Kβ lines at 5.89 and 6.40keV) measured during XRT thermal balance tests.
XRT monitors these lines in the corners of the CCDimage continuously.
138 eVWindowedTiming
133 eVPhoton-Counting
140 eVPhotodiode
N/AImaging
EnergyResolution
Readout Mode
Preliminary Energy Resolution (5.9 keV, Panter)(requirement is < 150 eV at launch)
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18187 September 2004, Swift Workshop @ HEAD 2004
XRT Spectroscopy
• X-ray spectroscopy of GRBs and afterglows– Redshift determination, ISM measurements
Simulated 1 hr observation of aGRB afterglow, 1.5 hours after theburst. Based on Beppo-SAXobservation of GRB000214.
XMM observation of 5 ks from theafterglow of GRB011211,beginning 11 hours after the burst.
Energy resolution < 140 eV @ 5.9 keV
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19197 September 2004, Swift Workshop @ HEAD 2004
XRT Calibration Spectrum
55Fe Calibration spectrumE=5.9 keV / 6.4 keVNoise = 5.0 e- (rms)Resolution = 130 eV (FWHM)
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20207 September 2004, Swift Workshop @ HEAD 2004
XRT Data Products
• Prompt GRB data transmitted through TDRSS anddistributed via GCN
• Full data sets transmitted through Malindi ground-station– Converted to standard OGIP FITS formats by Swift Data
Center at NASA/GSFC
– Data products available on SDC Quick-Look site within 2hours of ground pass
– XRT Data Analysis Software (ASDC) performs high-levelprocessing and analysis (see talk by Tagliaferri)
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21217 September 2004, Swift Workshop @ HEAD 2004
Summary
• XRT is a powerful, flexible instrument that will providerapid, arcsecond GRB positions and spectroscopy
• Ground calibrations will be validated on-orbit usingstandard X-ray calibration sources
• GRB prompt data products converted to standardFITS formats and distributed in minutes via GCN
• Data products converted to standard FITS binarytable formats and publicly available to communitywithin hours