- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:17:52 UT
NOTICE_TYPE: Swift-BAT GRB Position
TRIGGER_NUM: 509336, Seg_Num: 0
GRB_RA: 14.360d {+00h 57m 26s} (J2000),
14.495d {+00h 57m 59s} (current),
13.791d {+00h 55m 10s} (1950)
GRB_DEC: -46.788d {-46d 47' 17"} (J2000),
-46.724d {-46d 43' 25"} (current),
-47.058d {-47d 03' 29"} (1950)
GRB_ERROR: 3.00 [arcmin radius, statistical only]
GRB_INTEN: 0 [cnts] Image_Peak=1439 [image_cnts]
TRIGGER_DUR: 320.000 [sec] (=5.3 [min])
TRIGGER_INDEX: 20000 E_range: 15-50 keV
BKG_INTEN: 0 [cnts]
BKG_TIME: 0.00 SOD {00:00:00.00} UT
BKG_DUR: 0 [sec]
GRB_DATE: 15904 TJD; 343 DOY; 11/12/09
GRB_TIME: 25928.34 SOD {07:12:08.34} UT
GRB_PHI: -145.50 [deg]
GRB_THETA: 55.94 [deg]
SOLN_STATUS: 0x13
RATE_SIGNIF: 0.00 [sigma]
IMAGE_SIGNIF: 7.93 [sigma]
MERIT_PARAMS: +1 +0 +0 +6 +1 -2 +0 +0 +2 +0
SUN_POSTN: 255.72d {+17h 02m 52s} -22.79d {-22d 47' 15"}
SUN_DIST: 91.28 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 59.97d {+03h 59m 52s} +21.80d {+21d 48' 03"}
MOON_DIST: 79.87 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.88,-70.30 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 348.57,-47.41 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Coordinates.
COMMENTS: This is an image trigger. (The RATE_SIGNIF & BKG_{INTEN, TIME, DUR} are undefined.)
COMMENTS: A point_source was found.
COMMENTS: This does not match any source in the on-board catalog.
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is a GRB.
COMMENTS: This trigger occurred at longitude,latitude = 161.12,-19.41 [deg].
- red DSS finding chart
ps-file
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:19:49 UT
NOTICE_TYPE: Swift-XRT Position
TRIGGER_NUM: 509336, Seg_Num: 0
GRB_RA: 14.3462d {+00h 57m 23.08s} (J2000),
14.4815d {+00h 57m 55.57s} (current),
13.7781d {+00h 55m 06.73s} (1950)
GRB_DEC: -46.8005d {-46d 48' 01.7"} (J2000),
-46.7361d {-46d 44' 10.0"} (current),
-47.0706d {-47d 04' 14.0"} (1950)
GRB_ERROR: 4.7 [arcsec radius, statistical plus systematic, 90% containment]
GRB_INTEN: 1.20e-08 [erg/cm2/sec]
GRB_SIGNIF: 15.68 [sigma]
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26347.23 SOD {07:19:07.23} UT, 418.9 [sec] since BAT Trigger Time
TAM[0-3]: 327.66 237.24 261.50 243.66
AMPLIFIER: 2
WAVEFORM: 134
SUN_POSTN: 255.72d {+17h 02m 52s} -22.79d {-22d 47' 15"}
SUN_DIST: 91.26 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 59.98d {+03h 59m 56s} +21.80d {+21d 48' 10"}
MOON_DIST: 79.89 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.91,-70.29 [deg] galactic lon,lat of the burst
ECL_COORDS: 348.55,-47.42 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Coordinates.
COMMENTS: The XRT position is 0.92 arcmin from the BAT position.
COMMENTS: The object found at this position is either a very bright burst or a cosmic ray hit.
COMMENTS: Examine the XRT Image to differentiate (CRs are much more compact); see examples at:
COMMENTS: http://www.swift.psu.edu/xrt/XRT_Postage_Stamp_Image_Photo_Gallery.htm .
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:20:08 UT
NOTICE_TYPE: Swift-XRT Processed Image
TRIGGER_NUM: 509336, Seg_Num: 0
GRB_RA: 14.3462d {+00h 57m 23.0s} (J2000),
14.4815d {+00h 57m 55.5s} (current),
13.7781d {+00h 55m 06.7s} (1950)
GRB_DEC: -46.8005d {-46d 48' 01.7"} (J2000),
-46.7361d {-46d 44' 10.0"} (current),
-47.0706d {-47d 04' 14.0"} (1950)
GRB_ERROR: 4.7 [arcsec, radius, statistical plus systematic]
GRB_INTEN: 246 [cnts]
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26347.23 SOD {07:19:07.23} UT, 418.9 [sec] since BAT Trigger Time
CENTROID_X: 249.60, raw= 250 [pixels]
CENTROID_Y: 294.61, raw= 295 [pixels]
ROLL: 234.00 [deg]
GAIN: 4
MODE: 3, Long Image mode
WAVEFORM: 134
EXPO_TIME: 2.50 [sec]
GRB_POS_XRT_Y: -7.97
GRB_POS_XRT_Z: -127.50
IMAGE_URL: sw00509336000msxps_rw.img
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 15"}
SUN_DIST: 91.26 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 59.99d {+03h 59m 57s} +21.80d {+21d 48' 11"}
MOON_DIST: 79.89 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.91,-70.29 [deg] galactic lon,lat of the burst
ECL_COORDS: 348.55,-47.42 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Processed Image.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:20:02 UT
NOTICE_TYPE: Swift-XRT Image
TRIGGER_NUM: 509336, Seg_Num: 0
GRB_RA: 14.3462d {+00h 57m 23.0s} (J2000),
14.4815d {+00h 57m 55.5s} (current),
13.7781d {+00h 55m 06.7s} (1950)
GRB_DEC: -46.8005d {-46d 48' 01.7"} (J2000),
-46.7361d {-46d 44' 10.0"} (current),
-47.0706d {-47d 04' 14.0"} (1950)
GRB_ERROR: 4.7 [arcsec, radius, statistical plus systematic]
GRB_INTEN: 246 [cnts]
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26347.23 SOD {07:19:07.23} UT, 418.9 [sec] since BAT Trigger Time
CENTROID_X: 249.60, raw= 250 [pixels]
CENTROID_Y: 294.61, raw= 295 [pixels]
ROLL: 234.00 [deg]
GAIN: 4
MODE: 3, Long Image mode
WAVEFORM: 134
EXPO_TIME: 2.50 [sec]
GRB_POS_XRT_Y: -7.97
GRB_POS_XRT_Z: -127.50
IMAGE_URL: sw00509336000msxps_rw.img
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 15"}
SUN_DIST: 91.26 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 59.99d {+03h 59m 57s} +21.80d {+21d 48' 11"}
MOON_DIST: 79.89 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.91,-70.29 [deg] galactic lon,lat of the burst
ECL_COORDS: 348.55,-47.42 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Image.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:20:54 UT
NOTICE_TYPE: Swift-BAT GRB Lightcurve
TRIGGER_NUM: 509336, Seg_Num: 0
GRB_RA: 14.360d {+00h 57m 26s} (J2000),
14.495d {+00h 57m 59s} (current),
13.791d {+00h 55m 10s} (1950)
GRB_DEC: -46.788d {-46d 47' 17"} (J2000),
-46.724d {-46d 43' 25"} (current),
-47.058d {-47d 03' 29"} (1950)
GRB_DATE: 15904 TJD; 343 DOY; 11/12/09
GRB_TIME: 25928.34 SOD {07:12:08.34} UT
TRIGGER_INDEX: 20000
GRB_PHI: -145.50 [deg]
GRB_THETA: 55.94 [deg]
DELTA_TIME: 0.00 [sec]
TRIGGER_DUR: 320.000 [sec] (=5.3 [min])
SOLN_STATUS: 0x13
RATE_SIGNIF: 0.00 [sigma]
IMAGE_SIGNIF: 7.93 [sigma]
LC_URL: sw00509336000msb.lc
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 15"}
SUN_DIST: 91.27 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 59.99d {+03h 59m 59s} +21.80d {+21d 48' 13"}
MOON_DIST: 79.88 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.88,-70.30 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 348.57,-47.41 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Lightcurve.
COMMENTS:
COMMENTS: The next comments were copied from the BAT_POS Notice:
COMMENTS: This is an image trigger.
COMMENTS: A point_source was found.
COMMENTS: This does not match any source in the on-board catalog.
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is a GRB.
COMMENTS: This trigger occurred at longitude,latitude = 161.12,-19.41 [deg].
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:22:08 UT
NOTICE_TYPE: Swift-UVOT Source List
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.389d {+00h 57m 33s} (J2000)
POINT_DEC: -46.782d {-46d 46' 55"} (J2000)
POINT_ROLL: 234.002d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26355.68 SOD {07:19:15.68} UT, 3.3 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 1.768
N_STARS: 30
X_OFFSET: 640 [pixels]
Y_OFFSET: 504 [pixels]
X_MAX: 1599 [pixels]
Y_MAX: 1463 [pixels]
DET_THRESH: 11
PHOTO_THRESH: 5
SL_URL: sw00509336000msufc0003.fits
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 16"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.00d {+04h 00m 01s} +21.80d {+21d 48' 18"}
MOON_DIST: 79.87 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Source List.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:21:22 UT
NOTICE_TYPE: Swift-BAT Transient Position
TRIGGER_NUM: 509337, Seg_Num: 0
GRB_RA: 14.363d {+00h 57m 27s} (J2000),
14.498d {+00h 57m 59s} (current),
13.794d {+00h 55m 11s} (1950)
GRB_DEC: -46.802d {-46d 48' 05"} (J2000),
-46.737d {-46d 44' 13"} (current),
-47.072d {-47d 04' 17"} (1950)
GRB_ERROR: 3.00 [arcmin radius, statistical only]
GRB_INTEN: 0 [cnts] Image_Peak=7679 [image_cnts]
TRIGGER_DUR: 64.000 [sec]
TRIGGER_INDEX: 20000 E_range: 15-50 keV
BKG_INTEN: 0 [cnts]
BKG_TIME: 0.00 SOD {00:00:00.00} UT
BKG_DUR: 0 [sec]
GRB_DATE: 15904 TJD; 343 DOY; 11/12/09
GRB_TIME: 26352.34 SOD {07:19:12.34} UT
GRB_PHI: -122.73 [deg]
GRB_THETA: 0.03 [deg]
SOLN_STATUS: 0x1000001D
RATE_SIGNIF: 0.00 [sigma]
IMAGE_SIGNIF: 22.54 [sigma]
MERIT_PARAMS: +0 +0 +100 +6 +1 +8 +0 +0 +2 +0
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 15"}
SUN_DIST: 91.27 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.00d {+04h 00m 00s} +21.80d {+21d 48' 15"}
MOON_DIST: 79.89 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.88,-70.29 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 348.56,-47.42 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT Transient Coordinates.
COMMENTS: This is an image trigger. (The RATE_SIGNIF & BKG_{INTEN, TIME, DUR} are undefined.)
COMMENTS: A point_source was found.
COMMENTS: This matches a source in the on-board catalog: Num=29336=(null) (probably an AT_Slot).
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is not a GRB -- it is a hard x-ray transient.
COMMENTS: This trigger occurred at longitude,latitude = 171.04,-20.33 [deg].
COMMENTS:
COMMENTS: NOTE: This BAT event is spatially(0.00<0.1deg) coincident with the SWIFT_BAT event (trignum=509336).
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:21:17 UT
NOTICE_TYPE: Swift-BAT GRB Position
TRIGGER_NUM: 509337, Seg_Num: 0
GRB_RA: 14.363d {+00h 57m 27s} (J2000),
14.498d {+00h 57m 59s} (current),
13.794d {+00h 55m 11s} (1950)
GRB_DEC: -46.802d {-46d 48' 05"} (J2000),
-46.737d {-46d 44' 13"} (current),
-47.072d {-47d 04' 17"} (1950)
GRB_ERROR: 3.00 [arcmin radius, statistical only]
GRB_INTEN: 0 [cnts] Image_Peak=7679 [image_cnts]
TRIGGER_DUR: 64.000 [sec]
TRIGGER_INDEX: 20000 E_range: 15-50 keV
BKG_INTEN: 0 [cnts]
BKG_TIME: 0.00 SOD {00:00:00.00} UT
BKG_DUR: 0 [sec]
GRB_DATE: 15904 TJD; 343 DOY; 11/12/09
GRB_TIME: 26352.34 SOD {07:19:12.34} UT
GRB_PHI: -122.73 [deg]
GRB_THETA: 0.03 [deg]
SOLN_STATUS: 0x1000001D
RATE_SIGNIF: 0.00 [sigma]
IMAGE_SIGNIF: 22.54 [sigma]
MERIT_PARAMS: +0 +0 +100 +6 +1 +8 +0 +0 +2 +0
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 15"}
SUN_DIST: 91.27 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.00d {+03h 59m 59s} +21.80d {+21d 48' 15"}
MOON_DIST: 79.89 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.88,-70.29 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 348.56,-47.42 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Coordinates.
COMMENTS: This is an image trigger. (The RATE_SIGNIF & BKG_{INTEN, TIME, DUR} are undefined.)
COMMENTS: A point_source was found.
COMMENTS: This matches a source in the on-board catalog: Num=29336=(null) (probably an AT_Slot).
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is not a GRB.
COMMENTS: This trigger occurred at longitude,latitude = 171.04,-20.33 [deg].
COMMENTS:
COMMENTS: NOTE: This BAT event is spatially(0.00<0.1deg) coincident with the SWIFT_BAT event (trignum=509336).
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:22:37 UT
NOTICE_TYPE: Swift-UVOT Processed Source List
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.389d {+00h 57m 33s} (J2000)
POINT_DEC: -46.782d {-46d 46' 55"} (J2000)
POINT_ROLL: 234.002d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26355.68 SOD {07:19:15.68} UT, 3.3 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 1.768
N_STARS: 30
X_OFFSET: 640 [pixels]
Y_OFFSET: 504 [pixels]
X_MAX: 1599 [pixels]
Y_MAX: 1463 [pixels]
DET_THRESH: 11
PHOTO_THRESH: 5
SL_URL: sw00509336000msufc0003.fits
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 16"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.01d {+04h 00m 02s} +21.81d {+21d 48' 19"}
MOON_DIST: 79.87 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Source List.
COMMENTS: If you have elected to receive attachments:
COMMENTS: The uvot_catalog_srclist.fits.gz file does not exist; skipping the attachment.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:23:31 UT
NOTICE_TYPE: Swift-UVOT Image
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.389d {+00h 57m 33s} (J2000)
POINT_DEC: -46.782d {-46d 46' 55"} (J2000)
ROLL: 234.002d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26355.68 SOD {07:19:15.68} UT, 3.3 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 345107963
X_OFFSET: 1035 [pixels]
Y_OFFSET: 749 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1195
Y_GRB_POS: 909
BINNING_INDEX: 1
IM_URL: sw00509336000msuni0011.fits
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 16"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.02d {+04h 00m 04s} +21.81d {+21d 48' 22"}
MOON_DIST: 79.88 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Image.
COMMENTS: The GRB Position came from the XRT Position Command.
COMMENTS: The image has 2x2 binning (compression).
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:23:47 UT
NOTICE_TYPE: Swift-UVOT Processed Image
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.389d {+00h 57m 33s} (J2000)
POINT_DEC: -46.782d {-46d 46' 55"} (J2000)
ROLL: 234.002d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26355.68 SOD {07:19:15.68} UT, 3.3 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 345107963
X_OFFSET: 1035 [pixels]
Y_OFFSET: 749 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1195
Y_GRB_POS: 909
BINNING_INDEX: 1
IM_URL: sw00509336000msuni0011.fits
SUN_POSTN: 255.72d {+17h 02m 53s} -22.79d {-22d 47' 16"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.02d {+04h 00m 05s} +21.81d {+21d 48' 23"}
MOON_DIST: 79.88 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Image.
COMMENTS: The GRB Position came from the XRT Position Command.
COMMENTS: The image has 2x2 binning (compression).
COMMENTS: If you have elected to receive attachments:
COMMENTS: The uvot_catalog_image.fits.gz file does not exist; skipping the attachment.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:30:47 UT
NOTICE_TYPE: Swift-UVOT Source List
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.391d {+00h 57m 34s} (J2000)
POINT_DEC: -46.779d {-46d 46' 44"} (J2000)
POINT_ROLL: 234.001d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26784.10 SOD {07:26:24.10} UT, 431.8 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 1.684
N_STARS: 158
X_OFFSET: 475 [pixels]
Y_OFFSET: 189 [pixels]
X_MAX: 1914 [pixels]
Y_MAX: 1628 [pixels]
DET_THRESH: 11
PHOTO_THRESH: 5
SL_URL: sw00509336000msufc0431.fits
SUN_POSTN: 255.73d {+17h 02m 54s} -22.79d {-22d 47' 18"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.08d {+04h 00m 20s} +21.81d {+21d 48' 47"}
MOON_DIST: 79.91 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Source List.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:31:05 UT
NOTICE_TYPE: Swift-UVOT Processed Source List
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.391d {+00h 57m 34s} (J2000)
POINT_DEC: -46.779d {-46d 46' 44"} (J2000)
POINT_ROLL: 234.001d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26784.10 SOD {07:26:24.10} UT, 431.8 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 1.684
N_STARS: 158
X_OFFSET: 475 [pixels]
Y_OFFSET: 189 [pixels]
X_MAX: 1914 [pixels]
Y_MAX: 1628 [pixels]
DET_THRESH: 11
PHOTO_THRESH: 5
SL_URL: sw00509336000msufc0431.fits
SUN_POSTN: 255.73d {+17h 02m 55s} -22.79d {-22d 47' 18"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.09d {+04h 00m 21s} +21.81d {+21d 48' 48"}
MOON_DIST: 79.91 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Source List.
COMMENTS: If you have elected to receive attachments:
COMMENTS: The uvot_catalog_srclist.fits.gz file does not exist; skipping the attachment.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:32:18 UT
NOTICE_TYPE: Swift-UVOT Image
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.391d {+00h 57m 34s} (J2000)
POINT_DEC: -46.779d {-46d 46' 44"} (J2000)
ROLL: 234.001d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26784.10 SOD {07:26:24.10} UT, 431.8 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 345108391
X_OFFSET: 1034 [pixels]
Y_OFFSET: 748 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1194
Y_GRB_POS: 908
BINNING_INDEX: 1
IM_URL: sw00509336000msuni0439.fits
SUN_POSTN: 255.73d {+17h 02m 55s} -22.79d {-22d 47' 18"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.10d {+04h 00m 23s} +21.81d {+21d 48' 52"}
MOON_DIST: 79.92 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Image.
COMMENTS: The GRB Position came from the Window Position in the Mode Command.
COMMENTS: The image has 2x2 binning (compression).
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 09 Dec 11 07:32:35 UT
NOTICE_TYPE: Swift-UVOT Processed Image
TRIGGER_NUM: 509336, Seg_Num: 0
POINT_RA: 14.391d {+00h 57m 34s} (J2000)
POINT_DEC: -46.779d {-46d 46' 44"} (J2000)
ROLL: 234.001d
IMG_START_DATE: 15904 TJD; 343 DOY; 11/12/09
IMG_START_TIME: 26784.10 SOD {07:26:24.10} UT, 431.8 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 345108391
X_OFFSET: 1034 [pixels]
Y_OFFSET: 748 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1194
Y_GRB_POS: 908
BINNING_INDEX: 1
IM_URL: sw00509336000msuni0439.fits
SUN_POSTN: 255.73d {+17h 02m 55s} -22.79d {-22d 47' 18"}
SUN_DIST: 91.29 [deg] Sun_angle= -7.9 [hr] (East of Sun)
MOON_POSTN: 60.10d {+04h 00m 24s} +21.81d {+21d 48' 53"}
MOON_DIST: 79.92 [deg]
MOON_ILLUM: 98 [%]
GAL_COORDS: 299.82,-70.31 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 348.60,-47.42 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Image.
COMMENTS: The GRB Position came from the Window Position in the Mode Command.
COMMENTS: The image has 2x2 binning (compression).
COMMENTS: If you have elected to receive attachments:
COMMENTS: The uvot_catalog_image.fits.gz file does not exist; skipping the attachment.
- GCN Circular #12632
E. A. Hoversten (PSU), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), A. Y. Lien (NASA/GSFC/ORAU),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
M. C. Stroh (PSU), G. Tagliaferri (INAF-OAB) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:
At 07:12:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111209A (trigger=509336). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 14.360, -46.788 which is
RA(J2000) = 00h 57m 26s
Dec(J2000) = -46d 47' 17"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). After the original 320 second long image
trigger, the source caused a second trigger (#509337) over the
64 second time interval starting at T+424s, at much higher intensity.
The XRT began observing the field at 07:19:07.2 UT, 418.9 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 14.3462, -46.8005 which is equivalent to:
RA(J2000) = 00h 57m 23.08s
Dec(J2000) = -46d 48' 01.7"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 56 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
The initial flux in the 2.5 s image was 1.20e-08 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White
filter starting 427 seconds after the BAT trigger. There is a
candidate afterglow in the rapidly available 2.7'x2.7' sub-image at
approximately the same position as the XRT source with a magnitude of
18.1. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.02.
Burst Advocate for this burst is E. A. Hoversten (hoversten AT astro.psu.edu).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
- GCN Circular #12633
Klotz A. (CESR-OMP), Gendre B. (ASDC),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:
We imaged the field of GRB 111209A detected by SWIFT
(trigger 509336) with the TAROT robotic
telescope (D=25cm) located at the European Southern
Observatory, La Silla observatory, Chile.
The observations started 358s after the GRB trigger.
The elevation of the field decreased from
13 degrees above horizon and weather conditions
were good.
We detected the candidate couterpart mentioned
by Hoversten et al. (GCNC 12632)
at the following position (+/- 1 arcsec):
RA(J2000.0) = 00h 57m 22.7s
DEC(J2000.0) -46d 48' 05"
OT peaked at R~16.2 about 680s after GRB.
Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.
This message may be cited.
- GCN Circular #12634
D. Fugazza, S. Covino (INAF/OAB), E. Palazzi (INAF/IASF-Bo), on behalf of a larger collaboration, report:
The robotic 60-cm REM telescope located at La Silla (Chile) observed automatically the field of GRB 111209A (Hoversten et al. GCN 12632) with the ROSS optical and REMIR near-infrared cameras in imaging mode.
Observations started about 30 s after the Swift alert (about 5 min after the reported burst time) when the field was only 13 deg on the local horizon.
Summing H band images from 7 to 13 min after the burst a weak counterpart is visible at coordinates RA=00:57:22.78 DEC=-46:48:04.2 (error approximately 0.5 arcsec on both axes) and with magnitude H = 14.7 +- 0.2, calibrated against the 2MASS catalogue. The source is coincident with the optical counterpart reported by Klotz et al. (GCN 12633).
Further observations are in progress.
- GCN Circular #12635
C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB),
S. Kobayashi, C.G. Mundell (LJMU), A. Gomboc (U. Ljubljana)
report on behalf of the LJMU GRB group:
The 2-m Faulkes Telescope North robotically followed
up Swift GRB 111209A (Hoversten et al. GCN Circ. 12632)
from 07:20:00 UT, corresponding to 7.9 minutes after the
BAT trigger time.
Within the XRT error circle we clearly detect the optical
afterglow in the i' filter reported by Klotz et al. (GCN 12633)
and Fugazza et al. (GCN 12634) with the following magnitude:
Mid time from Total Exp Filter Magnitude
trigger (s) (s)
-------------------------------------------------
697 30 i' 18.3 +- 0.2
-------------------------------------------------
Magnitude has been calibrated from I nominal
values of nearby USNOB1.0 stars.
- GCN Circular #12637
Klotz A. (IRAP-OMP), Gendre B. (ASDC),
Boer M. (OHP-OAMP), Atteia J.L. (IRAP-OMP) report:
We obtained an optical follow-up until 4500 seconds
after the trigger of GRB 111209A detected by SWIFT
(trigger 509336-7) using the TAROT robotic telescope
(D=25cm) located at the European Southern Observatory,
La Silla observatory, Chile.
In this GCN circular we describe the behaviour of the
optical transcient discovered by Hoversten et al.
(GCNC 12632).
From 470s to 2000s, we observe a fluctuating
optical emission at a mean level R~17.5 that reaches
sometimes R=16.6.
From 2100s to 2550s we recorded an optical flash
that reached R=15.4. This peak is followed by
a plateau R=16.3 between 2700s to 3700s.
After 3700s the flux seems begin to decrease but
the low elevation 5 degrees above horizon does
not allow to conclude definitively about the
phase decay.
All the magnitudes are based on the assumption
that the color index of the GRB in optical
wavelengths is the same as the reference star
NOMAD1 0431-0011481 (V-R=0.34).
This message may be cited.
- GCN Circular #12638
B. Gendre (ASDC/INAF-OAR), J.L. Atteia (IRAP-OMP), M. Bo=EBr (OHP-OAMP),
A. Klotz (IRAP-OMP), L. Piro (INAF-IASF-Roma), G. Stratta
(ASDC/INAF-OAR), on behaf of a larger collaboration, report :
Following the trigger of the exceptionally long and bright GRB 111209A,
we have activated a 50 ks (net) TOO on XMM-Newton starting on
2011-12-09:22:12:58 UT. We encourage any simultaneous follow-up of this
event at any wavelength.
This message can be quoted.
- GCN Circular #12639
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2386 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 111209A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 14.34424, -46.80112 which is equivalent
to:
RA (J2000): 00h 57m 22.62s
Dec (J2000): -46d 48' 04.0"
with an uncertainty of 1.4 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
- GCN Circular #12640
D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
Using the data set from the recent telemetry downlink, we report further
analysis of BAT GRB 111209A (trigger #509336 and #509337)
(Hoversten, et al., GCN Circ. 12632). The BAT ground-calculated position
using the event data of trigger #509337 (on-axis observation)
is RA, Dec = 14.350, -46.799 deg which is
RA(J2000) = 00h 57m 24.1s
Dec(J2000) = -46d 47' 57.1"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
The mask-weighted light curve shows an excess rate already around T-150 s
when the spacecraft settled to the pre-planned target (T is the BAT trigger
time of #509336, which is 07:12:08.3 UT). A gradual increase in the rate
continues up to T+850s. And then, the rate started to decay. The positive
rate is still seen at T+1400 s where the end of the event data. Further
analysis using the BAT survey data is on-going to address the duration of
this event detected by BAT.
The time-averaged spectrum from 358 to 1337 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.48 +- 0.03. The fluence in the 15-150 keV band measured during this
time interval is 3.6 +- 0.1 x 10^-05 erg/cm2. The 1-sec peak photon flux
measured from T+824 sec in the 15-150 keV band is 0.5 +- 0.1 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/509336/BA/
http://gcn.gsfc.nasa.gov/notices_s/509337/BA/
- GCN Circular #12641
E. A. Hoversten (PSU), D.N. Burrows (PSU), S. Campana (INAF-OAB), P.
A. Evans (U Leicester), N. Gehrels (GSFC), D. Grupe (PSU), M. H.
Siegel (PSU), report on behalf of the Swift team:
We report an update on Swift observations of the unusual event GRB
111209A. BAT triggered twice and is saw extended duration emission
from this event. It peaked at 900s and decreased in flux after 1100s,
but continued well beyond that to >10ks.
We have analyzed 11.9 ks of XRT data for GRB 111209A (Hoversten et
al. GCN Circ. 12632), from 425 s to 25.16 ks after the BAT trigger.
The data contain 9.4 ks in Windowed Timing (WT) mode data and the
remainder in photon counting (pc) mode.
The light curve is highly complicated showing multiple flares. The
afterglow is very bright and XRT remained in WT mode through 4 orbits
(20ks after the trigger). The light curve after the fourth orbit
suggests a sharp drop in the count rate from about 14 counts s^-1 at
the end of the forth orbit to 5 counts s^-1 at the beginning of
the fifth orbit. The data of the 5th orbit were entirely taken in
photon counting (pc) mode and the decay slope steepens significantly.
The Swift/UVOT began settled observations of the field of GRB 111209A
427 s after the BAT trigger. The afterglow is clearly detected in all
seven UVOT filters. We find a refined UVOT position of
RA (J2000) 00:57:22.63 = 14.34429 (deg)
Dec (J2000) -46:48:03.8 = -46.80106 (deg)
with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence,
statistical + systematic). This position is 0.25 arcseconds from the
UVOT-enhanced XRT position, which is within the errors.
The white, v, and b filter show a fading source over the first orbit,
however at the end of the first orbit the white magnitude increases
abruptly by 0.6 magnitudes corresponding with a significant flare in
the X-rays. The v, b, u, uvw1, and uvm2 magnitudes show a
rebrightening between 5.4 and 7 ks after the burst of 0.3 to 1.1
magnitudes.
The data from all three instrument is similar is several ways to GRB
060218, the long event associated with SN2006aj, and to GRB 101225A,
the Christmas burst. The detection in all UVOT filters implies a low
redshift of z < 1.6. We note that at 18 ks after the burst the source
is still at 18th magnitude in the white filter which is extremely
unusual. Given the rare behavior exhibited by GRB 111209A we advocate
for additional observations at all wavelengths.
- GCN Circular #12642
E. A. Hoversten (PSU) and M. H. Siegel (PSU), report on behalf of the
UVOT team:
The Swift/UVOT began settled observations of the field of GRB 111209A
427 s after the BAT trigger (Hoversten et al., GCN Circ. 12632). The
afterglow is clearly detected in all seven UVOT filters. We find a
refined UVOT position of
RA (J2000) 00:57:22.63 = 14.34429 (deg)
Dec (J2000) -46:48:03.8 = -46.80106 (deg)
with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence,
statistical + systematic). This position is 0.25 arcseconds from the
UVOT-enhanced XRT position (Evans et al., GCN Circ. 12639), which is
within the errors.
The white, v, and b filters show a fading source over the first orbit,
however at the end of the first orbit the white magnitude increases
abruptly by 0.6 magnitudes corresponding with a significant flare in
the X-rays. The v, b, u, uvw1, and uvm2 magnitudes show a
rebrightening between 5.4 and 7 ks after the burst of 0.3 to 1.1
magnitudes. Preliminary magnitudes using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag Err
white_FC 427 577 147 17.94 0.04
white 855 1005 147 17.73 0.04
white 1856 1876 19 18.01 0.11
white 2030 2050 19 17.40 0.08
v 584 603 19 17.25 0.24
b 1134 1154 19 18.16 0.21
u 6064 6264 196 18.11 0.09
w1 633 653 19 17.16 0.24
m2 5653 5853 196 18.23 0.17
w2 5244 5443 196 17.96 0.12
The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.02 in the direction of
the burst (Schlegel et al. 1998).
The data from all three instrument is similar is several ways to GRB
060218, the long event associated with SN2006aj, and to GRB 101225A,
the Christmas burst. The detection in all UVOT filters implies a low
redshift of z < 1.6. We note that at 18 ks after the burst the source
is still at 18th magnitude in the white filter which is extremely
unusual. Given the rare behavior exhibited by GRB 111209A we advocate
for additional observations at all wavelengths.
- GCN Circular #12643
D. Grupe (PSU) and E. A. Hoversten (PSU) reports on behalf of the
Swift-XRT team:
We have analyzed 11 ks of XRT data for GRB 111209A (Hoversten et al.
GCN Circ. 12632), from 425 s to 25.2 ks after the BAT trigger. The
data comprise 9.4 ks in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 12639).
The light curve can be modeled with a series of power-law decays. The
light curve initially rises, with an index alpha=-0.21 (+/-0.04). At
T+864 s it breaks to an alpha of 7.3 (+0.7, -2.6). The light curve
breaks again at T+899 s to a decay with alpha=0.679 (+0.012, -0.087),
and again at T+5807 s s to alpha=1.179 (+/-0.016), before a final
break at T+19.4 ks s after which the decay index is 6.3 (+1.2, -0.4).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.333 (+/-0.012). The
best-fitting absorption column is 1.38 (+/-0.04) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.83 (+0.17, -0.16)
and a best-fitting absorption column of 1.3 (+0.5, -0.4) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.1 x 10^-11 (5.2 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.3 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: 4.4 sigma
Photon index: 1.83 (+0.17, -0.16)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00509336.
This circular is an official product of the Swift-XRT team.
- GCN Circular #12645
M. Nysewander, J. Haislip, A. LaCluyze, K. Ivarsen, D. Reichart, J. Moore, A. Trotter, R. Egger, A. Foster, A. Oza, T. Cromartie, E. Speckhard, and J. A. Crain report:
Skynet observed the field of GRB 111209A with the PROMPT telescopes located at CTIO in Chile. Observations began in VRI at 378 sec (34 sec after the alert) and lasted for 13.2 min before the source set below PROMPT's elevation constraints.
We detect the fading afterglow discovered by Hoversten et al. (GCN 12632). Preliminary calibration to USNO B1.0 catalog stars yields the follow initial detections:
Start Time t - t0 Exp Telescope Filter Mag Err
07:18:28 380s 40s Prompt5 I 18.0 0.20
07:18:31 383s 40s Prompt4 R 18.3 0.30
- GCN Circular #12646
M.Sokolowski,A.Majcher,T.Batsch,A.Majczyna,K.Nawrocki,G.Wrochna (NCNR,Swierk),
M.Cwiok,W.Dominik,L.W.Piotrowski,A.F.Zarnecki (University of Warsaw),
K.Malek,L.Mankiewicz,R.Opiela,M.Siudek,V.Repei (CFT PAN),
G.Kasprowicz,M.Zaremba (Warsaw University of Technology),
from the "Pi of the Sky" collaboration (http://grb.fuw.edu.pl).
The wide field "Pi of the Sky South" apparatus, installed in the private
observatory of Alain Maury in San Pedro de Atacama
(http://grb.fuw.edu.pl/pi/index.html#spda_site.htm) observed the position
of GRB 111209A ( SWIFT trigger #590336 ).
Three 10s images of this field have been taken at 01:59:03 - 01:59:51 UT
( 5 hours 13 min 5 sec before the first BAT alert ). No new object can be
seen within the error box and the limit on 3 coadded images is 12.7 mag.
After receiving the trigger from SWIFT, the field was observed 480 seconds
after the GRB. The field has been observed in time period from 7:20:09 to
7:44:25 UT, no new object brighter than 10.2 mag was observed on 10s
images. The limit on 20 coadded images is 10.7 mag.
Limits are based on the reference star magnitudo in V filter.
We acknowladge great support received from Alain Maury at SPdA Observatory.
- GCN Circular #12647
D.A. Kann, S. Klose (TLS Tautenburg), T. Kruehler (DARK/NBI) and J.
Greiner, (MPE Garching) report on behalf of the GROND team:
We observed the field of the "Swift Burst of Interest" GRB 111209A (Swift
trigger 509336 and 509337; Hoversten et al., GCN #12612) simultaneously in
g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP, 120, 405) mounted at
the 2.2 m ESO/MPG telescope at La Silla Observatory (Chile). Observations
started on December 10, 2011, at 00:56 UT, 0.74 days after the GRB
trigger, during twilight. They were performed at an average seeing of 0".9
and at an airmass of 1.
At the position of the optical afterglow (Klotz et al., GCN #12633;
Fugazza et al., GCN #12634; Guidorzi et al., GCN #12635; Hoversten &
Siegel, GCN #12642; Nysewander et al., GCN #12645), we clearly detect a
source in single 35 second integrations in g'r'i'z'.
Based on co-added images of 142 s integration time in g'r'i'z' and 240 s
in JHK, centered 0.74144 days after the trigger, the following magnitudes
(AB magnitude system) have been derived:
g' = 20.3 +/- 0.1
r' = 20.1 +/- 0.1
i' = 19.9 +/- 0.1
z' = 19.8 +/- 0.1
J = 19.3 +/ 0.2
H = 19.0 +/- 0.2
K = 18.6 +/- 0.4
The spectral slope is found to be beta ~0.8, which is typical for a GRB
afterglow, and dissimilar to thermally dominated emission.
Magnitudes were calibrated against an SDSS standard field in g'r'i'z' and
2MASS field stars in JHK.
Observations have continued at high cadence under excellent conditions. We
note these observations are contemporaneous to the planned XMM-Newton
observation (Gendre et al., GCN #12638).
- GCN Circular #12648
Paul Vreeswijk (U. Iceland), Johan Fynbo (DARK), Andrea Melandri
(INAF-OAB) report on behalf of the X-shooter GTO GRB afterglow
collaboration:
The afterglow of Swift GRB 111209A (Hoversten et al., GCN 12632, Klotz
et al., GCN 12633, Fugazza et al., GCN 12634) was observed with the
X-shooter spectrograph mounted at the Kueyen unit of the VLT on Cerro
Paranal, Chile. Starting around 1 UT on 10 December 2011 (0.75 days
after the burst), a series of four spectra of 1200s each were secured,
covering the approximate wavelength range 0.3-2.5 micron. The slit
width was set to 1", resulting in a resolving power range of
4500-7500.
Preliminary reduction of the ultraviolet and visual parts of the
spectra shows a smooth continuum with several absorption features that
we can identify with resonance absorption lines of FeII, MgII, MgI,
CaII H and K at a redshift of z=0.677; this is the likely redshift of
GRB 111209A.
We are grateful for the excellent support from the Paranal Observatory
staff, in particular Willem-Jan de Wit and Dimitri Gadotti.
- GCN Circular #12649
Myungshin Im, Hyunsung Jun, and Dohyeong Kim (CEOU/Seoul National Univ)
We observed GRB 111209A (Hoversten et al., GCN 12632) using SpeX
on IRTF. The observation started at 12-09-07:42:13 UT, or about 0.5 hrs
after the BAT alert. H-band images were taken using a guider camera
revealing a bright NIR counterpart with its flux at H~12 mag.
Note that calibration is done by an observation of a standard star
next night and needs a further refinement.
NIR spectra were taken at 0.8-2.5 micron with R=750 for
about 24 min, starting at ~35 min after the BAT alert,
showing good S/N but no obvious features in raw spectra.
Analysis of the spectral/imaging data is onging.
- GCN Circular #12656
D. A. Kann (TLS Tautenburg), and J. Greiner, (MPE Garching)
report on behalf of the GROND team:
We have analyzed the J-band observations (Kann et al., GCN #12647)
obtained with GROND over a total of five hours (0.74 to 0.93 days after
the trigger) of GRB 111209A (Hoversten et al., GCN #12632). Astrometry and
calibration were obtained against the 2MASS catalog.
We find the afterglow experiences a strong rise during our observations,
rising from J ~ 19.3 to J ~ 18.8 (AB Magnitudes). The slope of the rise is
alpha < -2 (assuming F(t) propto t^-alpha). This behavior may be due to a
strong energy injection.
Highly variable behavior in the first hours has already been reported by
Klotz et al. (GCN #12637) and Hoversten & Siegel (GCN #12642).
Dense photometric follow-up is strongly encouraged.
- GCN Circular #12663
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind
team report:
The exceptionally long GRB 111209A (Swift-BAT trigger #509336: Hoversten=20
et al., GCN 12632; Palmer et al., GCN 12640) was detected by=20
Konus-Wind in the waiting mode.
The burst light curve shows the main multipeaked episode of emission=20
started at ~T0(BAT)-1900 s and lasted until ~T0(BAT)+4400 s (the=20
duration is ~6300 s; T0(BAT)=3D25928 s UT (07:12:08)). There is also a=20
weaker broad pulse of emission seen before the main pulse from=20
~T0(BAT)-5400 s to ~T0(BAT)-2600 s and a hint of an additional episode=20
of emission after the main pulse from ~T0(BAT)+5000 s to ~T0(BAT)+10000=20
s. Both these episodes might be related to GRB 111209A (they were=20
detected by the same KW detector, and the KW ecliptic latitude responses=20
for them are consistent with the common origin with the main episode).=20
The most intense peak in the Konus-Wind light curve, (which started at=20
~T0+1740 s, peaked at ~T0+2040 s, and ended at ~T0+2300 s), corresponds=20
to a significant raise in the XRT lc=20
(http://www.swift.ac.uk/xrt_curves/00509336/ - Grupe & Hoversten GCN=20
12643) and a bright optical flash (Klotz et al., GCN 12637).
As observed by Konus-Wind, the burst (the main episode) had a fluence of=20
(4.86 =B1 0.61)x10^-4 erg/cm2 (in the 20 - 1400 keV energy range).
Modeling the KW 3-channel time-integrated spectrum (from T0-1890 s to
T0+4400 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha =3D -1.31 =B1 0.09, and Ep =3D 310 =B1 53 keV.
Assuming z =3D 0.677 (Vreeswijk, Fynbo, & Melandri GCN 12648) and a=20
standard cosmology model with H_0 =3D 71 km/s/Mpc, Omega_M =3D 0.27,
Omega_Lambda =3D 0.73, the isotropic energy release, E_iso, is (5.82 =B1=20
0.73)x10^53 erg, and Ep_rest is 520 =B1 89 keV.
Thus, the prompt gamma-ray emission properties of this GRB: fluence, Ep,=20
and E_iso are similar to those observed in other long energetic GRBs.=20
The only exceptional feature of the prompt gamma-ray emission is the=20
huge duration.
All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.
The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB111209A/
- GCN Circular #12664
Paul J. Hancock, Tara Murphy, Bryan Gaensler (U of Sydney), Ashley
Zauderer (Harvard)
On the 11th December 04:44-05:50UT (T=+1.9days) we observed GRB 111209A
(GCN12632) with the Australia Telescope Compact Array (ATCA) at 34GHz.
We do not detect any radio emission consistent with the GRB optical
position (GCN12642). We place a 3sigma upper limit of 132uJy on the flux
of the afterglow. Further observations are planned.
We thank the staff of the ATCA for their help in organising these
observations.
- GCN Circular #12684
J. Wren, W. T. Vestrand, P. Wozniak, and H. Davis
of Los Alamos National Laboratory report:
The RAPTOR wide-field optical monitors were observing the location of
GRB 111209A (Hoversten et al., GCN 12632) during the gamma-ray emitting
interval as seen by the Swift BAT (Palmer et al., GCN 12640). Our
system acquired 10 s exposures at 20 s intervals during the entire
emission period. We have analyzed the the 77 images taken between
T-150 and T+1400 and we do not detect the counterpart to a typical
3-sigma limiting magnitude of 10.3. Our unfiltered images were
calibrated to the Tycho-2 V-band.
- GCN Circular #12804
Paul J. Hancock, Tara Murphy, Bryan Gaensler (U of Sydney), Ashley
Zauderer (Harvard)
Following our 34GHz non-detection (GCN12664) we observed GRB 111209A
(GCN12632) with the Australia Telescope Compact Array (ATCA) at 5.5,
9, and 18GHz on the 14th of December (T=+5.1days). The mean observing
time was 11:12UT at 5.5 and 9GHz, and 11:47UT at 18GHz. We easily detect
the GRB at each frequency as listed below:
Freq Flux
5.5GHz 0.85+/-0.04mJy
9GHz 0.97+/-0.06mJy
18GHz 3.23+/-0.05mJy
We thank the staff of the ATCA for their help in organising these observations.
- 1212.2392 from 12 Dec 12
B. Gendre et al.: The ultra-long Gamma-Ray Burst 111209A: the collapse of a blue supergiant?
We present optical, X-ray and gamma-ray observations of GRB 111209A, at a redshift of z = 0.677. We show that this event was active in its
prompt phase for about 25000 seconds, making it the longest burst ever observed. This rare event could have been detected up to z ~ 1.4.
Compared to other long GRBs, GRB 111209A is a clear outlier in the energy-fluence and duration plane. The high-energy prompt emission shows no
sign of a strong black body component, as expected if the event was caused by a tidal disruption event or a supernova shock breakout. Given the
extreme longevity of this event, and a lack of a supernova signature, we propose that GRB 111209A is a relatively rare stellar collapse of a
low metallicity blue super giant star. Only this progenitor can supply mass to the central engine over a duration of thousands of seconds.
Hence, GRB 111209A could have more in common with population III stellar explosions, rather than normal long gamma ray bursts.
- 1212.6431 from 1 Jan 13
Kazumi Kashiyama et al.: Luminous supernova-like UV/optical/infrared transients associated with ultra-long gamma-ray bursts from metal-poor blue supergiants
Metal-poor massive stars may typically end up their lives as blue supergiants (BSGs). Gamma-ray bursts (GRBs) from such progenitors could have
ultra-long duration of relativistic jets. For example Population III (Pop III) GRBs at z ~ 10-20 might be observable as X-ray rich events with
a typical duration of T_90 ~ 10^4(1+z) sec. Recent GRB111209A at z = 0.677 has an ultra long duration of T_90 ~ 2.5*10^4 sec so that it have
been suggested that the progenitor might be a metal-poor BSGs in the local universe. Here, we suggest luminous UV/optical/infrared emissions
associated with such a new class of GRB from metal poor BSGs. Before the jet head breaks out the progenitor envelope, the energy injected by
the jet is stored in a hot-plasma cocoon, which finally emerges and expands as a baryon-loaded fireball. We show that the photospheric
emissions from the cocoon fireball could be intrinsically very bright (L_peak ~ 10^(42-44) erg/sec) in UV/optical bands (E_peak ~ 10 eV) with a
typical duration of ~ 100 days in the rest frame. Such cocoon emissions from Pop III GRB might be detectable in infrared bands at ~ years after
Pop III GRBs at up to z ~ 15 by up-coming facilities like JWST. We also suggest that GRB111209A might have been rebrightening in UV/optical
bands up to an AB magnitude of < 26. The cocoon emissions from local metal-poor BSGs might have been already observed as luminous supernovae
without GRB since they can be seen from the off-axis direction of the jet.
- 1302.2352 from 12 Feb 13
A.J. Levan et al.: A new population of ultra-long duration gamma-ray bursts
We present comprehensive multiwavelength observations of three gamma-ray bursts (GRBs) with durations of several thousand seconds. We
demonstrate that these events are extragalactic transients; in particular we resolve the long-standing conundrum of the distance of GRB 101225A
(the "Christmas-day burst"), finding it to have a redshift z=0.847, and showing that two apparently similar events (GRB 111209A and GRB
121027A) lie at z=0.677 and z=1.773 respectively. The systems show extremely unusual X-ray and optical lightcurves, very different from
classical GRBs, with long lasting highly variable X-ray emission and optical light curves that exhibit little correlation with the behaviour
seen in the X-ray. Their host galaxies are faint, compact, and highly star forming dwarf galaxies, typical of "blue compact galaxies". We
propose that these bursts are the prototypes of a hitherto largely unrecognized population of ultra-long GRBs, that while observationally
difficult to detect may be astrophysically relatively common. The long durations may naturally be explained by the engine driven explosions of
stars of much larger radii than normally considered for GRB progenitors which are thought to have compact Wolf-Rayet progenitor stars. However,
we cannot unambiguously identify supernova signatures within their light curves or spectra. We also consider the alternative possibility that
they arise from the tidal disruption of stars by supermassive black holes.
- 1305.3194 from 15 May 13
B. Gendre et al.: Models and possible progenitors of gamma-ray bursts at the test field of the observations
During the last 15 years, a standard paradigm has emerged to explain both the progenitor nature and the observed radiations of gamma-ray
bursts. In this work we show three GRBs for which the standard paradigm could be tested with high statistics due to their exceptional spectral
and temporal coverage. While GRB 1110205 represents a very good example of the standard scenario, GRB 090102 and GRB 111209A do not fit into
the standard paradigm.
- 1306.1699 from 10 Jun 13
G. Stratta et al.: The ultra-long GRB 111209A - II. Prompt to afterglow and afterglow properties
The "ultra-long" Gamma Ray Burst GRB 111209A at redshift z=0.677, is so far the longest GRB ever observed, with rest frame prompt emission
duration of ~4 hours. In order to explain the bursts exceptional longevity, a low metallicity blue supergiant progenitor has been invoked. In
this work, we further investigate this peculiar burst by performing a multi-band temporal and spectral analysis of both the prompt and the
afterglow emission. We use proprietary and publicly available data from Swift, Konus Wind, XMM-Newton, TAROT as well as from other ground based
optical and radio telescopes. We find some peculiar properties that are possibly connected to the exceptional nature of this burst, namely: i)
an unprecedented large optical delay of 410+/-50 s is measured between the peak epochs of a marked flare observed also in gamma-rays after
about 2 ks from the first Swift/BAT trigger; ii) if the optical and X-ray/gamma-ray photons during the prompt emission share a common origin,
as suggested by their similar temporal behavior, a certain amount of dust in the circumburst environment should be introduced, with rest frame
visual dust extinction of AV=0.3-1.5 mag; iii) at the end of the X-ray "steep decay phase" and before the start of the X-ray afterglow, we
detect the presence of a hard spectral extra power law component never revealed so far. On the contrary, the optical afterglow since the end of
the prompt emission shows more common properties, with a flux power law decay with index alpha=1.6+/-0.1 and a late re-brightening feature at
1.1 day. We discuss our findings in the context of several possible interpretations given so far to the complex multi-band GRB phenomenology.
We also attempt to exploit our results to further constrain the progenitor nature properties of this exceptionally long GRB, suggesting a
binary channel formation for the proposed blue supergiant progenitor.
- 1307.5061 from 19 Jul 13
Daisuke Nakauchi et al.: Blue Supergiant Model for Ultra-Long Gamma-Ray Burst with Superluminous-Supernova-Like Bump
Long GRBs (LGRBs) have typical duration of $\sim 30\ {\rm s}$ and some of them are associated with hypernovae, like Type Ic SN 1998bw.
Wolf-Rayet stars are the most plausible LGRB progenitors, since the free-fall time of the envelope is consistent with the duration, and the
natural outcome of the progenitor is a Type Ic SN. While a new population of ultra-long GRBs (ULGRBs), GRB 111209A, GRB 101225A, and GRB
121027A, has a duration of $\sim 10^4$ s, two of them are accompanied by superluminous-supernova (SLSN) like bumps, which are $\lesssim 10$
times brighter than typical hypernovae. Wolf-Rayet progenitors cannot explain ULGRBs because of too long duration and too bright SN-like bump.
A blue supergiant (BSG) progenitor model, however, can explain the duration of ULGRBs. Moreover, SLSN-like bump can be attributed to the
so-called cocoon-fireball photospheric emissions (CFPEs). Since a large cocoon is inevitably produced during the relativistic jet piercing
though the BSG envelope, this component can be a smoking-gun evidence of BSG model for ULGRBs. In this paper, we examine u, g, r, i, and J-band
light curves of three ULGRBs and demonstrate that they can be fitted quite well by our BSG model with the appropriate choices of the jet
opening angle and the number density of the ambient gas. In addition, we predict that for 121027A, SLSN-like bump could have been observed for
$\sim 20 \mbox{-} 80$ days after the burst. We also propose that some SLSNe might be CFPEs of off-axis ULGRBs without visible prompt emission.
- 1308.1001 from 6 Aug 13
B. Gendre et al.: The diversity of progenitors and emission mechanisms for ultra-long bursts
GRB 111209A is the longest ever recorded burst. This burst was detected by Swift and Konus-Wind, and we obtained TOO time from XMM-Newton as
well as prompt data from TAROT. We made a common reduction using data from these instruments together with other ones. This allows for the
first time a precise study at high signal-to-noise ratio of the prompt to afterglow transition. We show that several mechanisms are responsible
of this phase. In its prompt phase, we show that its duration is longer than 20 000 seconds. This, combined with the fact that the burst
fluence is among the top 5% of what is observed for other events, makes this event extremely energetic. We discuss the possible progenitors
that could explain the extreme duration properties of this burst as well as its spectral properties. We present evidences that this burst
belong to a new, previously unidentified, class of GRBs. The most probable progenitor of this new class is a low metalicity blue super-giant
star. We show that selection effects could prevent the detection of other bursts at larger redshift and conclude that this kind of event is
intrinsically rare in the local Universe. The afterglow presents similar features to other normal long GRBs and a late rebrightening in the
optical wavelengths, as observed in other long GRBs. A broad band SED from radio to X-rays at late times does not show significant deviations
from the expected standard fireball afterglow synchrotron emission.
- 1310.4944 from 21 Oct 13
Michel Boer et al.: Are Ultra-long Gamma-Ray Bursts different?
The discovery of a number of gamma-ray bursts with duration exceeding 1,000 seconds, in particular the exceptional case of GRB 111209A with a
duration of about 25,000 seconds, has opened the question on whether these bursts form a new class of sources, the so called {\em ultra-long}
GRBs, or if they are rather the tail of the distribution of the standard long GRB duration. In this Letter, using the long GRB sample detected
by {\em Swift}, we investigate on the statistical properties of ultra-long GRBs and compare them with the overall long burst population. We
discuss also on the differences observed in their spectral properties. We find that ultra-long GRBs are statistically different from the
standard long GRBs with typical burst duration less than 100-500 seconds, for which a Wolf Rayet star progenitor is usually invoked. We
interpret this result as an indication that an alternative scenario has to be found in order to explain the ultra-long GRB extreme energetics,
as well as the mass reservoir and its size that can feed the central engine for such a long time.
- 1312.0794 from 4 Dec 13
Y.B. Yu et al.: Fall back accretion and energy injections in the ultra-long GRB 111209A
The ultra-long Gamma Ray Burst 111209A, which occurred at a redshift of $z = 0.677$, is the longest duration burst ever observed due to a rest
frame prompt emission duration of order of $10^{4}$ s. The very early X-ray afterglow of Gamma Ray Burst 111209A showed unusual behavior, with
a significant bump observed at about 2000 s after the BAT trigger. One possible explanation is that the bump resulted from mass fall back. In
this paper, we present a detailed numerical study of the fall back process to interpret the very early X-ray afterglow light curve of Gamma Ray
Burst 111209A. For the afterglow at late times, we apply external shock by adding an energy injection. In our model, we assume two periods of
energy injection, each with a constant injection power. One injection starts at $8.0\times10^{3}$ s and lasts for about 8000 s, with an
injection power of $9.0\times10^{47}$ ${\rm erg}$ ${\rm s^{-1}}$; this energy injection accounts for the plateau at X-ray wavelength in the
early stage. The other injection starts at $6.5\times10^{4}$ s and lasts for about 16 ks with an injection power of $6.0\times10^{46}$ ${\rm
erg}$ ${\rm s^{-1}}$. This second energy injection can help to explain the other plateau at X-ray wavelengths and the rebrightening in the
optical band at about $10^{5}$ s. We argue that the two periods of energy injection can be produced by the infall of clumpy mass onto the
central compact object of the burster, which leads to an enhancement of the accretion rate and results in a strong temporary outflow.
- A very luminous magnetar-powered supernova associated with an ultra-long gamma-ray burst
Nature 523, 189 (2015) or
preprint Version
- 1509.03279 from 11 Sep 15
Jochen Greiner et al.: A very luminous magnetar-powered supernova associated with an ultra-long gamma-ray burst
A new class of ultra-long duration (>10,000 s) gamma-ray bursts has recently been suggested. They may originate in the explosion of stars with
much larger radii than normal long gamma-ray bursts or in the tidal disruptions of a star. No clear supernova had yet been associated with an
ultra-long gamma-ray burst. Here we report that a supernova (2011kl) was associated with the ultra-long duration burst 111209A, at z=0.677.
This supernova is more than 3 times more luminous than type Ic supernovae associated with long gamma-ray bursts, and its spectrum is distinctly
different. The continuum slope resembles those of super-luminous supernovae, but extends farther down into the rest-frame ultra-violet implying
a low metal content. The light curve evolves much more rapidly than super-luminous supernovae. The combination of high luminosity and low
metal-line opacity cannot be reconciled with typical type Ic supernovae, but can be reproduced by a model where extra energy is injected by a
strongly magnetized neutron star (a magnetar), which has also been proposed as the explanation for super-luminous supernovae.
- 1603.00388 from 2 Mar 16
P. A. Mazzali et al.: Spectrum formation in Superluminous Supernovae (Type I)
The near-maximum spectra of most superluminous supernovae that are not dominated by interaction with a H-rich CSM (SLSN-I) are characterised by
a blue spectral peak and a series of absorption lines which have been identified as OII. SN2011kl, associated with the ultra-long gamma-ray
burst GRB111209A, also had a blue peak but a featureless optical/UV spectrum. Radiation transport methods are used to show that the spectra
(not including SN2007bi, which has a redder spectrum at peak, like ordinary SNe Ic) can be explained by a rather steep density distribution of
the ejecta, whose composition appears to be typical of carbon-oxygen cores of massive stars which can have low metal content. If the
photospheric velocity is ~10000-15000 km/s, several lines form in the UV. OII lines, however, arise from very highly excited lower levels,
which require significant departures from Local Thermodynamic Equilibrium to be populated. These SLSNe are not thought to be powered primarily
by 56Ni decay. An appealing scenario is that they are energised by X-rays from the shock driven by a magnetar wind into the SN ejecta. The
apparent lack of evolution of line velocity with time that characterises SLSNe up to about maximum is another argument in favour of the
magnetar scenario. The smooth UV continuum of SN2011kl requires higher ejecta velocities (~20000 km/s): line blanketing leads to an almost
featureless spectrum. Helium is observed in some SLSNe after maximum. The high ionization near maximum implies that both He and H may be
present but not observed at early times. The spectroscopic classification of SLSNe should probably reflect that of SNe Ib/c. Extensive time
coverage is required for an accurate classification.
- 1605.04660 from 17 May 16
He Gao et al.: Black hole central engine for ultra-long gamma-ray burst 111209A and its associated supernova 2011kl
Recently, the first association between an ultra-long gamma-ray burst (GRB) and a supernova is reported, i.e., GRB 111209A/SN 2011kl, which
enables us to investigate the physics of central engines or even progenitors for ultra-long GRBs. In this paper, we inspect the broad-band data
of GRB 111209A/SN 2011kl. The late-time X-ray lightcurve exhibits a GRB 121027A-like fall-back bump, suggesting a black hole central engine. We
thus propose a collapsar model with fall-back accretion for GRB 111209A/SN 2011kl. The required model parameters, such as the total mass and
radius of the progenitor star, suggest that the progenitor of GRB 111209A is more likely a Wolf-Rayet star instead of blue supergiant, and the
central engine of this ultra-long burst is a black hole. The implications of our results is discussed.
- 1606.06791 from 21 Jun 16
Kann et al.: Highly Luminous Supernovae associated with Gamma-Ray Bursts I.: GRB 111209A/SN 2011kl in the Context of Stripped-Envelope and Superluminous Supernovae
GRB 111209A, the longest Gamma-Ray Burst (GRB) ever observed, is linked to SN 2011kl, the most luminous GRB-Supernova (SN) detected so far, which shows evidence for being powered by a magnetar central engine. We place SN 2011kl into the context of large samples of SNe, addressing in more detail the question of whether it could be radioactively powered, and whether it represents an extreme version of a GRB-SN or an underluminous Superluminous SN (SLSN). We model SN 2011kl using SN 1998bw as a template and derive a bolometric light curve including near-infrared data. We compare the properties of SN 2011kl to literature results on stripped-envelope and superluminous supernovae. Comparison in the k,s context, i.e., comparing it to SN 1998bw templates in terms of luminosity and light-curve stretch, clearly shows SN 2011kl is the most luminous GRB-SN to date, and it is spectrally very dissimilar to other events, being significantly bluer/hotter. Although SN 2011kl does not reach the luminosities of true SLSNe and evolves faster than any of them, it resembles SLSNe more than the classical GRB-associated broad-lined Type Ic SNe in several aspects. GRB 111209A was a very energetic event, both at early (prompt emission) and at very late (SN) times. We have shown in a further publication that with the exception of the extreme duration, the GRB and afterglow parameters are in agreement with the known distributions for these parameters. SN 2011kl, on the other hand, is exceptional both in luminosity and spectral characteristics, indicating that GRB 111209A was likely not powered by a standard-model collapsar central engine, further supporting our earlier conclusions. Instead, it reveals the possibility of a direct link between GRBs and SLSNe.
- 1608.02938 from 11 Aug 16
Kunihito Ioka et al.: Are Ultra-long Gamma-Ray Bursts Caused by Blue Supergiant Collapsars, Newborn Magnetars, or White Dwarf Tidal Disruption Events?
Ultra-long gamma-ray bursts (ulGRBs) are a new population of GRBs with an extreme duration $\sim 10^{4}$ s. Leading candidates for their origin
are blue supergiant Collapsars, magnetars, and white dwarf tidal disruption events (WD-TDEs) by massive black holes (BHs). Recent observations
of supernova-like (SN-like) bumps associated with ulGRBs challenged both the WD-TDE and the blue supergiant models because of the detection of
SNe and the absence of hydrogen lines, respectively. We propose that WD-TDEs can accommodate the observed SN-like bumps if the fallback WD
matter releases energy into the unbound WD ejecta. The observed ejecta energy, luminosity, and velocity are explained by the gravitational
energy, Eddington luminosity, and escape velocity of the formed accretion disk, respectively. We also show that the observed X-rays can ionize
the ejecta, eliminating lines. The SN-like light curves (SN 2011kl) for the ulGRB 111209A are consistent with all three models, although a
magnetar model is unnatural in which the required spin-down time is hundred times longer than the GRB. Our results imply that TDEs are a
possible energy source of SN-like events.
- 1702.05507 from 17 Feb 17
Gompertz et al.: Magnetars in Ultra-Long Gamma-Ray Bursts
Supernova 2011kl, associated with the ultra-long gamma-ray burst (ULGRB) 111209A, exhibited a higher-than-normal peak luminosity, placing it in the parameter space between regular supernovae and super-luminous supernovae. Its light curve can only be matched by an abnormally high fraction of 56Ni that appears inconsistent with the observed spectrum, and as a result it has been suggested that the supernova, and by extension the gamma-ray burst, are powered by the spin-down of a highly magnetised millisecond pulsar, known as a magnetar. We investigate the broadband observations of ULGRB 111209A, and find two independent measures that suggest a high density circumburst environment. However, the light curve of the GRB afterglow shows no evidence of a jet break (the steep decline that would be expected as the jet slows due to the resistance of the external medium) out to three weeks after trigger, implying a wide jet. Combined with the high isotropic energy of the burst, this implies that only a magnetar with a spin period of ~ 1 ms or faster can provide enough energy to power both ULGRB 111209A and Supernova 2011kl.
- 1706.00601 from 02 Jun 17
Kann et al.: The Optical/NIR afterglow of GRB 111209A: Complex yet not Unprecedented
Afterglows of Gamma-Ray Bursts (GRBs) are simple in the most basic model, but can show many complex features. The ultra-long duration GRB 111209A, the longest GRB ever detected, also has the best-monitored afterglow in this rare class of GRBs. We want to address the question whether GRB 111209A was a special event beyond its extreme duration alone, and whether it is a classical GRB or another kind of high-energy transient. The afterglow may yield significant clues. We present afterglow photometry obtained in seven bands with the GROND imager as well as in further seven bands with the UVOT telescope on-board Swift. The light curve is analysed by multi-band modelling and joint fitting with power-laws and broken power-laws, and we use the contemporaneous GROND data to study the evolution of the spectral energy distribution. We compare the optical afterglow to a large ensemble we have analysed in earlier works, and especially to that of another ultra-long event, GRB 130925A. We furthermore undertake a photometric study of the host galaxy. We find a strong, chromatic rebrightening event at \u22480.8 days after the GRB, during which the spectral slope becomes redder. After this, the light curve decays achromatically, with evidence for a break at about 9 days after the trigger. The afterglow luminosity is found to not be exceptional. We find that a double-jet model is able to explain the chromatic rebrightening. The afterglow features have been detected in other events and are not unique. The GRB and and afterglow parameters of GRB 111209A are in agreement with the known distributions for these parameters. While the central engine of this event may differ from classical GRBs, there are multiple lines of evidence pointing to GRB 111209A to result from the core-collapse of a massive star with a stripped envelope.
Previous IAU Circulars 