- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:44:06 UT
NOTICE_TYPE: Swift-BAT GRB Position
TRIGGER_NUM: 214805, Seg_Num: 0
GRB_RA: 320.862d {+21h 23m 27s} (J2000),
320.975d {+21h 23m 54s} (current),
319.985d {+21h 19m 56s} (1950)
GRB_DEC: -53.034d {-53d 02' 02"} (J2000),
-53.006d {-53d 00' 21"} (current),
-53.249d {-53d 14' 54"} (1950)
GRB_ERROR: 3.00 [arcmin radius, statistical only]
GRB_INTEN: 7444 [cnts] Image_Peak=563 [image_cnts]
TRIGGER_DUR: 1.024 [sec]
TRIGGER_INDEX: 151 E_range: 25-100 keV
BKG_INTEN: 28654 [cnts]
BKG_TIME: 45814.74 SOD {12:43:34.74} UT
BKG_DUR: 8 [sec]
GRB_DATE: 13900 TJD; 165 DOY; 06/06/14
GRB_TIME: 45828.50 SOD {12:43:48.50} UT
GRB_PHI: 34.17 [deg]
GRB_THETA: 44.14 [deg]
SOLN_STATUS: 0x3
RATE_SIGNIF: 68.38 [sigma]
IMAGE_SIGNIF: 18.45 [sigma]
MERIT_PARAMS: +1 +0 +0 +0 +2 +19 +0 +0 +60 +1
SUN_POSTN: 82.74d {+05h 30m 57s} +23.27d {+23d 16' 12"}
SUN_DIST: 127.34 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.70d {+20h 10m 47s} -24.59d {-24d 35' 20"}
MOON_DIST: 31.58 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.08,-43.94 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 305.00,-35.60 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Coordinates.
COMMENTS: This is a rate 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 = 264.99,2.43 [deg].
- red DSS finding chart
ps-file
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:46:02 UT
NOTICE_TYPE: Swift-XRT Image
TRIGGER_NUM: 214805, Seg_Num: 0
GRB_RA: 320.8848d {+21h 23m 32.3s} (J2000),
320.9975d {+21h 23m 59.3s} (current),
320.0079d {+21h 20m 01.8s} (1950)
GRB_DEC: -53.0256d {-53d 01' 32.1"} (J2000),
-52.9977d {-52d 59' 51.7"} (current),
-53.2403d {-53d 14' 24.9"} (1950)
GRB_ERROR: 5.0 [arcsec, radius, statistical plus systematic]
GRB_INTEN: 79 [cnts]
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45919.90 SOD {12:45:19.90} UT, 91.4 [sec] since BAT Trigger Time
CENTROID_X: 247.39, raw= 247 [pixels]
CENTROID_Y: 339.31, raw= 339 [pixels]
ROLL: 100.93 [deg]
GAIN: 1
MODE: 2, Short Image mode
WAVEFORM: 134
EXPO_TIME: 0.10 [sec]
GRB_POS_XRT_Y: 95.49
GRB_POS_XRT_Z: -127.08
IMAGE_URL: sw00214805000msxps_rw.img
SUN_POSTN: 82.74d {+05h 30m 57s} +23.27d {+23d 16' 12"}
SUN_DIST: 127.33 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.72d {+20h 10m 52s} -24.58d {-24d 35' 03"}
MOON_DIST: 31.58 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.09,-43.95 [deg] galactic lon,lat of the burst
ECL_COORDS: 305.02,-35.59 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Image.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:46:00 UT
NOTICE_TYPE: Swift-XRT Position
TRIGGER_NUM: 214805, Seg_Num: 0
GRB_RA: 320.8848d {+21h 23m 32.3s} (J2000),
320.9975d {+21h 23m 59.3s} (current),
320.0079d {+21h 20m 01.8s} (1950)
GRB_DEC: -53.0256d {-53d 01' 32.1"} (J2000),
-52.9977d {-52d 59' 51.7"} (current),
-53.2403d {-53d 14' 24.9"} (1950)
GRB_ERROR: 5.0 [arcsec radius, statistical plus systematic, 90% containment]
GRB_INTEN: 6.00e-08 [erg/cm2/sec]
GRB_SIGNIF: 8.88 [sigma]
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45919.90 SOD {12:45:19.90} UT, 91.4 [sec] since BAT Trigger Time
TAM[0-3]: 327.62 237.17 261.17 243.30
AMPLIFIER: 2
WAVEFORM: 134
SUN_POSTN: 82.74d {+05h 30m 57s} +23.27d {+23d 16' 12"}
SUN_DIST: 127.33 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.72d {+20h 10m 52s} -24.58d {-24d 35' 03"}
MOON_DIST: 31.58 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.09,-43.95 [deg] galactic lon,lat of the burst
ECL_COORDS: 305.02,-35.59 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Coordinates.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:46:19 UT
NOTICE_TYPE: Swift-XRT Processed Image
TRIGGER_NUM: 214805, Seg_Num: 0
GRB_RA: 320.8848d {+21h 23m 32.3s} (J2000),
320.9975d {+21h 23m 59.3s} (current),
320.0079d {+21h 20m 01.8s} (1950)
GRB_DEC: -53.0256d {-53d 01' 32.1"} (J2000),
-52.9977d {-52d 59' 51.7"} (current),
-53.2403d {-53d 14' 24.9"} (1950)
GRB_ERROR: 5.0 [arcsec, radius, statistical plus systematic]
GRB_INTEN: 79 [cnts]
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45919.90 SOD {12:45:19.90} UT, 91.4 [sec] since BAT Trigger Time
CENTROID_X: 247.39, raw= 247 [pixels]
CENTROID_Y: 339.31, raw= 339 [pixels]
ROLL: 100.93 [deg]
GAIN: 1
MODE: 2, Short Image mode
WAVEFORM: 134
EXPO_TIME: 0.10 [sec]
GRB_POS_XRT_Y: 95.49
GRB_POS_XRT_Z: -127.08
IMAGE_URL: sw00214805000msxps_rw.img
SUN_POSTN: 82.74d {+05h 30m 57s} +23.27d {+23d 16' 12"}
SUN_DIST: 127.33 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.72d {+20h 10m 52s} -24.58d {-24d 35' 00"}
MOON_DIST: 31.58 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.09,-43.95 [deg] galactic lon,lat of the burst
ECL_COORDS: 305.02,-35.59 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Processed Image.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:49:17 UT
NOTICE_TYPE: Swift-UVOT Image
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.818d {+21h 23m 16s} (J2000)
POINT_DEC: -53.047d {-53d 02' 48"} (J2000)
ROLL: 100.930d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45929.61 SOD {12:45:29.61} UT, 101.1 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 171981930
X_OFFSET: 928 [pixels]
Y_OFFSET: 585 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1088
Y_GRB_POS: 745
BINNING_INDEX: 1
IM_URL: sw00214805000msuni0101.fits
SUN_POSTN: 82.74d {+05h 30m 57s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.36 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.75d {+20h 10m 60s} -24.58d {-24d 34' 34"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [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: Wed 14 Jun 06 12:51:25 UT
NOTICE_TYPE: Swift-UVOT Source List
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.819d {+21h 23m 17s} (J2000)
POINT_DEC: -53.045d {-53d 02' 41"} (J2000)
POINT_ROLL: 100.929d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 46034.84 SOD {12:47:14.84} UT, 206.3 [sec] since BAT Trigger Time
FILTER: 3, V
BKG_MEAN: 1.089
N_STARS: 61
X_OFFSET: 608 [pixels]
Y_OFFSET: 265 [pixels]
X_MAX: 1567 [pixels]
Y_MAX: 1224 [pixels]
DET_THRESH: 9
PHOTO_THRESH: 4
SL_URL: sw00214805000msufc0206.fits
SUN_POSTN: 82.74d {+05h 30m 58s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.36 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.77d {+20h 11m 05s} -24.57d {-24d 34' 14"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Source List.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:52:46 UT
NOTICE_TYPE: Swift-UVOT Processed Source List
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.819d {+21h 23m 17s} (J2000)
POINT_DEC: -53.045d {-53d 02' 41"} (J2000)
POINT_ROLL: 100.929d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 46034.84 SOD {12:47:14.84} UT, 206.3 [sec] since BAT Trigger Time
FILTER: 3, V
BKG_MEAN: 1.089
N_STARS: 61
X_OFFSET: 608 [pixels]
Y_OFFSET: 265 [pixels]
X_MAX: 1567 [pixels]
Y_MAX: 1224 [pixels]
DET_THRESH: 9
PHOTO_THRESH: 4
SL_URL: sw00214805000msufc0206.fits
SUN_POSTN: 82.74d {+05h 30m 58s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.36 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.79d {+20h 11m 09s} -24.57d {-24d 34' 02"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Source List.
COMMENTS: All 4 attachments are included.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:52:55 UT
NOTICE_TYPE: Swift-UVOT Image
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.819d {+21h 23m 17s} (J2000)
POINT_DEC: -53.045d {-53d 02' 41"} (J2000)
ROLL: 100.929d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 46034.84 SOD {12:47:14.84} UT, 206.3 [sec] since BAT Trigger Time
FILTER: 3, V
EXPOSURE_ID: 171982036
X_OFFSET: 928 [pixels]
Y_OFFSET: 585 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1088
Y_GRB_POS: 745
BINNING_INDEX: 1
IM_URL: sw00214805000msuni0206.fits
SUN_POSTN: 82.74d {+05h 30m 58s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.36 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.79d {+20h 11m 09s} -24.57d {-24d 34' 01"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [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: Wed 14 Jun 06 12:54:25 UT
NOTICE_TYPE: Swift-UVOT Processed Image
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.819d {+21h 23m 17s} (J2000)
POINT_DEC: -53.045d {-53d 02' 41"} (J2000)
ROLL: 100.929d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 46034.84 SOD {12:47:14.84} UT, 206.3 [sec] since BAT Trigger Time
FILTER: 3, V
EXPOSURE_ID: 171982036
X_OFFSET: 928 [pixels]
Y_OFFSET: 585 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1088
Y_GRB_POS: 745
BINNING_INDEX: 1
IM_URL: sw00214805000msuni0206.fits
SUN_POSTN: 82.74d {+05h 30m 58s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.37 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.80d {+20h 11m 13s} -24.56d {-24d 33' 47"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [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: All 4 attachments are included.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:48:32 UT
NOTICE_TYPE: Swift-UVOT Source List
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.818d {+21h 23m 16s} (J2000)
POINT_DEC: -53.047d {-53d 02' 48"} (J2000)
POINT_ROLL: 100.930d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45929.61 SOD {12:45:29.61} UT, 101.1 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 2.045
N_STARS: 53
X_OFFSET: 576 [pixels]
Y_OFFSET: 368 [pixels]
X_MAX: 1535 [pixels]
Y_MAX: 1327 [pixels]
DET_THRESH: 12
PHOTO_THRESH: 6
SL_URL: sw00214805000msufc0101.fits
SUN_POSTN: 82.74d {+05h 30m 57s} +23.27d {+23d 16' 12"}
SUN_DIST: 127.36 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.74d {+20h 10m 58s} -24.58d {-24d 34' 40"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Source List.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:57:21 UT
NOTICE_TYPE: Swift-UVOT Position
TRIGGER_NUM: 214805, Seg_Num: 0
GRB_RA: 320.8838d {+21h 23m 32.1s} (J2000),
320.9965d {+21h 23m 59.1s} (current),
320.0069d {+21h 20m 01.6s} (1950)
GRB_DEC: -53.0266d {-53d 01' 35.7"} (J2000),
-52.9987d {-52d 59' 55.3"} (current),
-53.2413d {-53d 14' 28.5"} (1950)
GRB_ERROR: 0.4 [arcsec radius, statistical only]
GRB_MAG: 18.39 +/- 0.50 [mag]
FILTER: 10, White
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45930.00 SOD {12:45:30.00} UT, 101.5 [sec] since BAT Trigger Time
SUN_POSTN: 82.75d {+05h 30m 59s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.33 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.83d {+20h 11m 20s} -24.56d {-24d 33' 21"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.09,-43.95 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 305.02,-35.60 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT UVOT Position Notice.
COMMENTS: This Notice was ground-generated -- not flight-generated.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:48:09 UT
NOTICE_TYPE: Swift-BAT GRB Lightcurve
TRIGGER_NUM: 214805, Seg_Num: 0
GRB_RA: 320.862d {+21h 23m 27s} (J2000),
320.975d {+21h 23m 54s} (current),
319.985d {+21h 19m 56s} (1950)
GRB_DEC: -53.034d {-53d 02' 02"} (J2000),
-53.006d {-53d 00' 21"} (current),
-53.249d {-53d 14' 54"} (1950)
GRB_DATE: 13900 TJD; 165 DOY; 06/06/14
GRB_TIME: 45828.50 SOD {12:43:48.50} UT
TRIGGER_INDEX: 151
GRB_PHI: 34.17 [deg]
GRB_THETA: 44.14 [deg]
DELTA_TIME: 64.00 [sec]
TRIGGER_DUR: 1.024 [sec]
SOLN_STATUS: 0x3
RATE_SIGNIF: 68.38 [sigma]
IMAGE_SIGNIF: 18.45 [sigma]
LC_URL: sw00214805000msb.lc
SUN_POSTN: 82.74d {+05h 30m 57s} +23.27d {+23d 16' 12"}
SUN_DIST: 127.34 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.74d {+20h 10m 57s} -24.58d {-24d 34' 44"}
MOON_DIST: 31.58 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.08,-43.94 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 305.00,-35.60 [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 a rate 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 = 264.99,2.43 [deg].
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Wed 14 Jun 06 12:50:39 UT
NOTICE_TYPE: Swift-UVOT Processed Image
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.818d {+21h 23m 16s} (J2000)
POINT_DEC: -53.047d {-53d 02' 48"} (J2000)
ROLL: 100.930d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45929.61 SOD {12:45:29.61} UT, 101.1 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 171981930
X_OFFSET: 928 [pixels]
Y_OFFSET: 585 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1088
Y_GRB_POS: 745
BINNING_INDEX: 1
IM_URL: sw00214805000msuni0101.fits
SUN_POSTN: 82.74d {+05h 30m 58s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.36 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.76d {+20h 11m 03s} -24.57d {-24d 34' 21"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [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: Wed 14 Jun 06 12:50:24 UT
NOTICE_TYPE: Swift-UVOT Processed Source List
TRIGGER_NUM: 214805, Seg_Num: 0
POINT_RA: 320.818d {+21h 23m 16s} (J2000)
POINT_DEC: -53.047d {-53d 02' 48"} (J2000)
POINT_ROLL: 100.930d
IMG_START_DATE: 13900 TJD; 165 DOY; 06/06/14
IMG_START_TIME: 45929.61 SOD {12:45:29.61} UT, 101.1 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 2.045
N_STARS: 53
X_OFFSET: 576 [pixels]
Y_OFFSET: 368 [pixels]
X_MAX: 1535 [pixels]
Y_MAX: 1327 [pixels]
DET_THRESH: 12
PHOTO_THRESH: 6
SL_URL: sw00214805000msufc0101.fits
SUN_POSTN: 82.74d {+05h 30m 58s} +23.27d {+23d 16' 13"}
SUN_DIST: 127.36 [deg] Sun_angle= 8.1 [hr] (West of Sun)
MOON_POSTN: 302.76d {+20h 11m 03s} -24.57d {-24d 34' 24"}
MOON_DIST: 31.57 [deg]
MOON_ILLUM: 90 [%]
GAL_COORDS: 344.07,-43.91 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 304.97,-35.60 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Source List.
COMMENTS: All 4 attachments are included.
- GCN Circular #5252
A. M. Parsons (GSFC), J. R. Cummings (NASA/ORAU),
N. Gehrels (NASA/GSFC), M. R. Goad (U Leicester), C. Gronwall (PSU),
S. T. Holland (GSFC/USRA), J. A. Kennea (PSU),
V. La Parola (INAF-IASFPA), V. Mangano (INAF-IASFPA),
F. E. Marshall (NASA/GSFC), K. M. McLean (LANL/UTD), C. Pagani (PSU),
D. M. Palmer (LANL), P. Romano (INAF-OAB) and
M. Stamatikos (NASA/ORAU) report on behalf of the Swift Team:
At 12:43:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 060614 (trigger=214805). Swift slewed immediately to
the burst. The BAT on-board calculated location is
RA,Dec 320.862, -53.034 {21h 23m 27s, -53d 02' 02"} (J2000)
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a duration of about 120 sec, with initial bright sharp
peak and a long, also bright, somewhat softer extended peak. The peak
count rate was ~10000 counts/sec (15-350 keV), at ~2 sec after the
trigger.
The XRT began observing the field at 12:45:19 UT, 91 seconds after the
BAT trigger. XRT found a very bright, fading and uncatalogued X-ray source
located at RA(J2000) = 21h 23m 32.3s, Dec(J2000) = -53d 01' 32.1", with an
estimated uncertainty of 5.0 arcseconds (90% confidence radius).
This location is 58 arcseconds from the BAT on-board position, within
the BAT error circle. The initial flux in the 0.1s image was
6.0e-08 erg/cm2/s (0.2-10 keV).
UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 102 seconds after the BAT trigger. There
is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image
at (RA,DEC) (J2000) of (320.8839,-53.0267) or
(21h23m32.14s,-53o01'36.1") with a 1-sigma error radius of about 0.5
arc sec. This position is 4.3 arc sec. from the center of the XRT
error circle. The estimated magnitude is 18.4 with a 1-sigma error of
about 0.5 mag. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.02.
- GCN Circular #5254
V. Mangano, V. La Parola, E. Troja, G. Cusumano,
T. Mineo (INAF-IASFPA), A. Parsons (GSFC), J. Kennea (PSU)
on behalf of the Swift-XRT team
We have analyzed the first two orbits of data of GRB060614
(Parsons et al 2006, GCN 5252).
The XRT data set consists of 370 s exposure in Windowed
Timing (WT) in the first orbit followed by 2.1 ks exposure
in Photon Counting (PC) mode in the second orbit.
The refined position of the source is
RA (2000) = 21h 23m 32.00s
Dec (2000) = -53d 01' 39.4"
with an uncertainty of 3.7 arcsec (90% containment).
This position is 7.7 arcsec from the on board
XRT position, 3.5 arcsec from the UVOT afterglow
position and 51.7 arcsec from the BAT position
(Parsons et al. 2006, GCN 5252).
The 0.2-10 keV X-ray light curve shows an
exponential decay with a characteristic decay time
of 75 s during all the first orbit, and a nearly
flat behaviour at the level of 0.2 counts/s during
the second orbit that starts 4500 s after the trigger.
The WT light curve is highly piled-up, with an initial
(corrected) count rate of about 1300 counts/s.
From the present data we cannot give any reliable prediction
for the light curve evolution in the next hours. Further
data will be avaliable after the end of the Malidi gap
(2006 June 15, 1:27 UT).
The WT data show strong spectral evolution with time,
with an average photon index of 1.65 +/- 0.04 in the
time interval 90-270 s from the trigger and an
average photon index of 2.95 +/- 0.11 in the time
interval 270-460 s. WT spectra show evidence of
absorption at the level of (1.3 +/- 0.3)e21 cm^-2,
in excess with respect to the Galactic N_H of 3.e20 cm^-2.
The PC spectrum extracted from the second orbit of data
is well fitted by an absorbed power law with photon index
1.8 +/- 0.2 and N_H consistent with the Galactic value.
The average 0.2-10 keV unabsorbed flux during the
second orbit is 9.3e-12 erg cm^-2 s^-1.
This Circular is an official product of the Swift XRT Team.
- GCN Circular #5255
GRB 060614: Swift/UVOT Observations
S. T. Holland (NASA/GSFC & USRA) reports on behalf of the Swift/UVOT
team:
The Swift/UVOT began observing the field of GRB 060614 at
12:45:29 on 2006-06-14, 101 s after the BAT trigger (Parsons et al.,
GCN Circular 5252). An optical counterpart was detected in the White
filter (160-650 nm) at a position (RA,Dec) = (21:23:32.08,
-53:01:36.2) (J2000) with a 90% confidence interval of 0.56
arcsec. The optical afterglow was detected in the White, V, B, U,
UVW1, UVM2, and UVW2 filters. The detection in all of the UVOT bands
suggests that the redshift is less than approximately 1.1.
The photometry results are given for the UVOT filters below:
Filter T_mid(s) Exposure(s) Mag Err
V 5753 189 19.54 0.30
B 5143 196 19.91 0.21
U 4937 193 18.81 0.14
UVW1 4730 189 18.35 0.17
UVM2 5959 193 18.06 0.23
UVW2 5552 195 18.26 0.17
White 147 92 18.30 0.14
The values quoted above are not corrected for the expected Galactic
extinction of E_{B-V}=0.02 (Schlegel et al. 1998).
- GCN Circular #5256
S. Barthelmy (GSFC), L. Barbier (GSFC), J. Cummings (GSFC/UMD),
E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (BYU-Idaho),
H. Krimm (GSFC/USRA), M. Koss (GSFC/UMD),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/ORAU), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), on behalf of the Swift-BAT team:
Using the data set from T-120 s to T+180 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 060614 (trigger #214805)
(Parsons et al 2006, GCN 5252). The BAT ground-calculated position is
(RA,Dec) = 320.88, -53.035 { 21h 23m 31.8s , -53d 02' 04.4" }
[deg; J2000]+-1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 16%.
The BAT mask-weighted light curve shows an unusual multi-peaked burst
structure that begins with an initial bright, ~ 6 second wide peak
followed by a set of 5 fainter and somewhat softer peaks that increase
in intensity. After about T+45s, the light curve shows a smooth slope
down to the baseline level for a total duration of T90 (15-350 keV) =
102 +/- 5 sec.
The power law index of the time-averaged spectrum is 2.13 +- 0.04. The
fluence in the 15-150 keV band is 2.17+- 0.04 x 10^-5 erg/cm2. The
1-sec peak photon flux measured from T - 1.3 sec in the 15-150 keV band
is 11.6 +- 0.7 ph/cm2/sec. All the quoted errors are at the 90%
confidence level.
- GCN Circular #5257
John French, Garry Melady, Lorraine Hanlon (UCD Dublin)
Martin Jel=EDnek (IAA CSIC Granada)
and Petr Kub=E1nek (ISDC Versoix, ASU AV CR Ondrejov)
on behalf of the Watcher Collaboration
"The Watcher 0.4m telescope, located in Boyden Observatory,
South Africa, observed the SWIFT error box for GRB 060614
(Parsons et al. GCN 5252, Mangano et al GCN 5254, Holland et
al GCN 5255, Barthelmy et al GCN 5256).
We detected the object quoted by Parsons et al. (GCN 5252) and
estimated its brightness as R=19.0+-0.3 on the 20min image
obtained at 20:50UT (ie. 7.1h after the GRB). Further we
observe fading with a power law decay index of ~-1.0.
We encourage spectroscopic observations of this object.
This message is quotable".
- GCN Circular #5258
Brian Schmidt, Bruce Peterson, and Karen Lewis (RSAA, The Australian National University) report
"The 1m telescope, located at Siding Spring Observatory,
observed the SWIFT error box for GRB 060614 (Parsons et al. GCN 5252, Mangano et al GCN 5254, Holland et al GCN 5255, Barthelmy et al GCN 5256) starting 20 minutes after burst trigger. Our photometry shows the OT rising in brightness from R=20.2 to R=18.8 in the 5 hours following the burst. Observations presented below are referenced to UCAC2 star of R=15.74 located at RA=21:23:31.573, DEC=-53:02:21.528 J2000.0
UT + 2006Jun14 R err
===============================
0.5483 20.2 (0.3)
0.5525 19.9 (0.2)
0.5566 19.9 (0.2)
0.5607 19.9 (0.2)
0.6017 19.1 (0.1)
0.6492 19.2 (0.1)
0.6912 19.1 (0.1)
0.7272 19.0 (0.1)
0.7731 18.8 (0.1)
- GCN Circular #5259
B. E. Cobb (Yale), part of the larger SMARTS consortium, reports:
Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 060614
(GCN 5252, Parsons et al.) with a mid-exposure time of
2006-06-15 04:16 UT (~15.5 hours post-burst).
Total summed exposure times for each observation amounted
to 36 minutes in I and 30 minutes in J.
The afterglow of GRB 060614 (GCN 5255, Holland et al.) is visible in
each combine image. The preliminary magnitudes reported below were
calibrated using several USNO-B1.0 stars in the I-band and three
2MASS standards in J.
time
post-burst I magnitude J magnitude
------------------------------------------------------
15.5 hours 18.9 +/- 0.1 18.2 +/- 0.1
Given that the afterglow was also reported to have an R magnitude
of ~19 at approximately 5.8 and 7.1 hours post-burst (GCN 5258, Schmidt et
al. & GCN 5257, French et al.), it is clear that the behavior of this
afterglow continues to deviate from a typical smoothly decaying
power-law.
- GCN Circular #5261
D. Malesani (SISSA), S. Covino, S. Campana, D. Fugazza, G. Tagliaferri
(INAF/OABr), G. Chincarini (Univ. Milano-Bicocca), and L. Stella
(INAF/OAR), report on behalf of the MISTICI collaboration:
We have observed the afterglow of GRB 060614 (Parsons et al., GCN 5252)
with the ESO VLT-UT1 equipped with the FORS2 instrument.
The optical afterglow is well detected in the R filter, and shows a
dimming by 0.45+-0.03 mag between 14.4 and 21.6 hr after the GRB.
Assuming a power-law decay, this corresponds to a decay slope alpha ~ 1,
consistent with what found by French et al. (GCN 5257). Compared with
several nearby USNO-B1 stars (R1 magnitudes), the afterglow has R~19.3
on Jun 14.12892, with a calibration uncertainty of ~0.2 mag.
We note an overall similarity between the early optical light curves of
GRB 060614 and GRB 060218 (Campana et al., astro-ph/0603279), both
presenting a maximum ~0.5 d after the burst. GRB 060614 is however
peaking earlier. We encourage further follow-up of this interesting event.
We acknowledge excellent support from the ESO staff at Paranal, in
particular Rachel Gilmour and Leonardo Vanzi.
- GCN Circular #5262
The Unusually Long-Lived Afterglow of GRB 060614
P. J. Brown (Penn State), S. T. Holland (NASA/GSFC & USRA),
V. Mangano (INAF-IASFPA), A. M. Parsons (NASA/GSFC),
& N. Gehrels (NASA/GSFC) report on behalf of the Swift Team:
Swift/UVOT observations of the optical afterglow of
GRB 060614 (trigger=214805; Parsons et al. GCN 5252) show
that the V-band light from the afterglow remains approximately
constant at V ~ 19.8 until at least 80,000 s after the
BAT trigger (the latest data presently available). Similar
behaviour is seen in the B-, U-, and UVW1-bands.
There is weak evidence that the UVM2 and UVW2
fluxes decrease after approximately 10,000 s. The UV-optical
colors are similar to GRB060218/SN2006aj, whose shock breakout
peaked at about 40,000 s in the UV and optical and then
began fading before being overtaken by the rising SN
(Campana et al. Nature, in press, astro-ph/0603279).
Though we do not see as prominent of a rise in the UVOT
data for GRB060614, other observers have noted rising and
fading in the R band (Schmidt, Peterson, & Lewis GCN 5258;
French et al. GCN 5257), and Malesani et al. (GCN 5261) have
also noted the similarity to GRB060218.
The BAT lightcurve of GRB 060614 (Barthelmy et al. GCN 5256)
shows a hard, bright initial flare followed by softer,
extended prompt emission. The T90 duration of the prompt
emission was 108 s. The prompt fluence was the greatest
of all Swifts burst that have been located by the BAT.
The X-ray light curve (Mangano et al. GCN 5254) was
unusually bright and decayed rapidly with a strong hard to
soft evolution. This was followed by an extended period
of near-constant emission, that shows evidence for small-scale
flares, out to approximately 70,000 s. The hardness ratio of
the flat part of the light curve is nearly constant, and the
power law fit of the spectrum gives a standard afterglow
photon index of 1.8 with no absorption in excess the
Galactic N_H.
In light of the peculiar characteristics observed by all
three Swift instruments and ground based observers,
we encourage further observations of this unusual afterglow.
- GCN Circular #5264
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline on behalf of the Konus-Wind team report:
The long GRB 060614 (Swift-BAT trigger #214805;
Parsons et al., GCN 5252; Barthelmy et al., GCN 5256)
triggered Konus-Wind at T0=45831.590 s UT (12:43:51.590).
The Konus-Wind light shows an intense multipeaked
initial pulse with a duration of ~6 sec,
followed by a weaker softer highly variable emission
seen up to T-T0 ~110 sec.
The spectrum of the initial intense pulse
(accumulated from T-T0=0 to T-T0=8.448 sec)
can be fitted (in the 20 keV - 2 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ E^(-alpha) * exp(-(2-alpha)*E/Ep)
with alpha = 1.57(-0.14, +0.12)
and Ep = 302(-85, +214) keV (chi2 = 73/59 dof).
The fluence of this part is 8.19(-2.52, +0.56)x10^-6 erg/cm2
(in the 20 keV - 2 MeV range).
The spectrum of the remaining part of the burst
(accumulated from T-T0=8.448 to T-T0=106.752 sec)
can be fitted (in the 20 keV - 1 MeV range)
by a simple power law with photon index
2.13 +/- 0.05 (chi2 = 63/49 dof).
The fluence of this part is 3.27(-0.23,+0.17)x10^-5 erg/cm2
(in the 20 keV - 2 MeV range).
We note that because the derived photon index is ~2,
this fluence value is very sensitive to the upper boundary
of the energy range.
The burst total fluence is 4.09(-0.34, +0.18)x10^-5 erg/cm2
and peak flux on 64-ms time scale measured from T-T0=0.032 sec
4.50(-1.53, +0.72)x10^-6 erg/cm2/sec
(both in the 20 keV - 2 MeV energy range).
All the quoted errors are at the 90% confidence level.
The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB060614_T45831/
- GCN Circular #5265
A. Pelangeon & J-L. Atteia (LATT-OMP) report:
We have used the spectral parameters of GRB 060614
provided by Golenetskii et al. (GCNC 5264) to
compute the spectral pseudo-redshift** of this burst
detected by SWIFT-BAT (Parsons et al., GCNC 5252).
We find a pseudo-redshift pz= 1.45 +/- 0.85 (90% error)
This is a typical value for a GRB.
** cf. http://www.ast.obs-mip.fr/grb/pz
- GCN Circular #5271
D. Fugazza (INAF/OABr), M. Della Valle (INAF/OAA), D. Malesani (SISSA),
P. Romano (INAF/OABr), F. Fiore (INAF/OAR), S. Covino (INAF/OABr), G.
Tagliaferri (INAF/OABr), G. Chincarini (Univ. Milano-Bicocca), P.
D'Avanzo (INAF/OABr & Univ. Insubria), S. Piranomonte (INAF/OAR), and L.
Stella (INAF/OAR) report on behalf of the MISTICI collaboration:
We observed the afterglow of GRB 060614 (Parsons et al., GCN 5252;
Mangano et al., GCN 5254; Brown et al., GCN 5262) with the ESO-VLT UT1
and UT2 equipped with FORS2 and FORS1, respectively. Spectra were taken
around Jun 15.416 and Jun 16.313 UT (0.88 and 1.78 days after the burst,
respectively). Despite the bright, closeby Moon, both spectra have a
good signal-to-noise ratio, and cover the wavelenght range 4500-9500 A.
We detect no significant features, neither in absorption nor in
emission. On Jun 15.4, the continuum is well described by a power law
with spectral index beta=0.60 (F_nu propto nu^-beta) in the range
5000-9000 A (where the flux calibration is solid).
The lack of emission features may suggest that the host galaxy is
relatively faint with respect to the afterglow (which had R~20.8 at the
second epoch). For comparison, the spectra of the lowest-redshift GRBs
(e.g. GRB 031203 and GRB 060218) revealed already in the earliest stages
the nebular emission lines from the galaxy. Our observations, therefore,
may imply a redshift larger than ~0.1.
We acknowledge significant support from the VLT staff.
This message can be cited.
- GCN Circular #5272
Christina C. Thoene, Johan P.U. Fynbo, Brian L. Jensen, J. Hjorth, D. Xu
(DARK Cosmology Centre), Uffe G. Joergensen, Kristian Woller
(NBI Copenhagen) report:
We observed the OT of GRB060614 (GCN 5252) with the Danish 1.54m
telescope and
DFOSC on La Silla in the R-band at several epochs on June 15-18. A
fit to our
data leads to a powerlaw decay with a temporal decay index of 1.50.
Compared to
other data reported in the GCNs is seems that the afterglow in the R-
band had a rising
lightcurve during the first about 12 hours after the burst and then
started the
more regular powerlaw decay. In this way the burst qualitatively
resemples
GRB970508 (Pedersen et al. 1998, ApJ 496, 311).
A plot of the data and fit is available at:
http://www.astro.ku.dk/~brian_j/grb/grb060614/
- GCN Circular #5275
P.A. Price (IfA, Hawaii), E. Berger (OCIW) and D.B. Fox (Penn. State)
report on behalf of a larger collaboration:
We observed the afterglow of GRB 060614 (GCN #5254) with the Gemini
South telescope + GMOS. Our observations consisted of 4x1800 sec
exposures with the R400 grating and 1 arcsec slit, commencing at June
19.3 UTC. In each image we identify a single emission line at 7388A
superposed on a continuum emission with no apparent absorption
features. If this line is due to [O II], the redshift is z = 0.98.
However, there is a hint of a line at 5634A which suggests that the line
is actually due to Halpha at z = 0.13.
In addition to the bright emission line due to the GRB host galaxy,
there is a brighter emission line at the same wavelength from the galaxy
17 arcsec North of the GRB. A spectrum from the Magellan telescope
reveals the presence of the [N II] doublet flanking the Halpha line for
this galaxy, with a secure redshift of z = 0.125. Based on the
identical wavelength of the lines, the two galaxies are likely related,
at a redshift of z = 0.125; in this case, the separation in the plane of
the sky is 38 kpc.
Using the fluence of 2.17 x 10^-5 erg/cm^2 (GCN #5254), a redshift of z
= 0.125 corresponds to an isotropic energy release of Eiso = 8.4 x 10^50
erg.
We thank the Gemini South observing team for obtaining these
observations.
- GCN Circular #5276
D. Fugazza (INAF/OABr), D. Malesani (SISSA), P. Romano, G. Tagliaferri,
S. Covino (INAF/OABr), G. Chincarini (INAF/OABr & Univ. Milano-Bicocca),
M. Della Valle (INAF/OAA), F. Fiore, & L. Stella (INAF/OAR), report on
behalf of the MISTICI collaboration:
We observed the afterglow of GRB 060614 (Parsons et al., GCN 5252;
Mangano et al., GCN 5254; Brown et al., GCN 5262) with VLT+FORS2. A
spectrum was taken with the grism 300V (resolution ~10 A, wavelength
coverage 4500-9500 A). The total exposure time was 50 min, with mean
time Jun 21.365 UT.
Based on the identification of several emission lines, among which
Halpha, weak Hbeta, [OIII] 4959, [OIII] 5007, we confirm the redshift
z=0.125 reported by Price et al. (GCN 5275).
We acknowledge the excellent support from the ESO staff, in particular
Riccardo Scarpa.
This message can be cited.
- GCN Circular #5277
J. P.U. Fynbo, C. C. Thoene, B. L. Jensen, J. Hjorth,
J. Sollerman, D. Watson, D. Xu (DARK Cosmology Centre), J.-E. Ovaldsen
(Oslo University), U. G. Joergensen, T. Hinse, K. Woller
(NBI Copenhagen) report:
We have obtained further imaging of the optical afterglow of GRB060614
(GCN 5252) with the Danish 1.54m telescope and DFOSC on La Silla in the
R-band at June 19-21. The afterglow has flattened from the power-law
decay reported by Thoene et al. (GCN 5272). Also, the source is clearly
resolved in the latest images. Hence, the host galaxy is most likely now
contributing most of the detected flux. There is not yet any sign of
an emerging supernova. Given the low redshift of GRB060614 (GCN 5275,
GCN 5276) we can conclude that if there is a supernova associated with
GRB060614 it is either intrinsically about 2 magnitudes fainter than
SN2006aj (associated with GRB060218) at a similar time or there is
substantial dust absorption along the line of sigth to the afterglow.
A plot of the data and fit is available at:
http://www.astro.ku.dk/~brian_j/grb/grb060614/
-
LEFT:
Lightcurve for GRB 060614 - Jul.14 to Jul.21
RIGHT:
R:2700s smoothed image (ca. 1x1 arcmin, N up/left, E left/down) taken with DK-1.5m+DFOSC at June 21, 2006 UT. Seeing is ~1".
The marked position is: (RA,Dec)(J2000.0) = (21:23:32.13, -53:01:36.5).
The circle indicates the refined 3.7" XRT error circle Mangano et al. (GCN 5254).
- GCN Circular #5281
GRB 060614: Detection of a Possible, Late-Time Rebrightening
S. T. Holland (NASA/GSFC & USRA) reports on behalf of the Swift/UVOT
team:
We report the possible detection of a source at the location of
the optical afterglow of GRB 060614((Parsons et al., 2006, GCN
Circular 5252) at approximately 9.5 days after the BAT trigger. The
putative source has a U-band magnitude of U = 22.8 +/- 0.3 (1-sigma
error) and was detected in coadded exposures taken between 7.4 and 12.4
days after the burst. This is a 4.2-sigma detection. Our detection
is approximately 3 mag brighter than the power-law extrapolation of
the early-time U-band decay predicts. We are not able to determine
if this source is a rebrightening of the afterglow of GRB 060614 or
a detection of the host galaxy (Fynbo et al., 2006, GCN Circular 5277).
The value quoted above is not corrected for the expected Galactic
extinction of E_{B-V} = 0.02 (Schlegel et al. 1998).
- GCN Circular #5282
B. E. Cobb and C. D. Bailyn (Yale), part of the larger SMARTS consortium,
report:
Continuing ANDICAM observations (see GCN 5259 for observing details) of
the afterglow of GRB 060614 (GCN 5255, Holland et al.) reveal the host
galaxy of the GRB in the I-band. Preliminary photometry in comparison with
several USNO B1.0 stars reveals that the host galaxy maintains a constant
brightness of I = 21.9 +/- 0.2 magnitudes between observations at
2006-06-19 07:36 UT and 2006-06-27 09:31 UT.
Images from four separate epochs (mid-exposure times of 2006-06-19 07:36
UT, 2006-06-21 07:22 UT, 2006-06-25 09:43 UT and 2006-06-27 09:31 UT) were
combined to produce a single J-band image but the host galaxy of GRB
060614 is not detected in this image down to a limiting magnitude of
J > 20.3+/-0.2 (based on two 2MASS standard stars).
Such a combined image was also produced in the I-band. The centroid of
the host galaxy was then compared to the centroid of the afterglow (imaged
at 2006-06-15 04:16 UT). The centroid of the afterglow appears 0.32" South
and 0.09" East of the host galaxy centroid. At a redshift of z=0.125
(GCN 5276, Fugazza et al.), and assuming H_o=71 km s^-1 Mpc^-1,
Omega_M=0.27 and Omega_Lambda=0.73, the projected distance between the
afterglow and the center of the host galaxy is 0.73 kpc.
Our 2006-06-27 09:31 UT observations correspond to ~13 days post-burst, or
~12 days in the host galaxy rest-frame. By this time post-burst in the
case of several other low-redshift GRBs (GRB 980425/SN 1998bw, GRB
031203/SN 2003lw and GRB 060218/SN 2006aj), the light from the associated
SNe was already clearly visible, yet no brightening is yet observed in the
host galaxy of GRB 060614 (see also GCN 5277, Fynbo et al.). Based on SN
1998bw and SN 2006aj, the expected absolute magnitude for a SN associated
with GRB 060614 would be I~-19.0. There is only a negligible amount of
Galactic extinction toward GRB 060614, so if a SN associated with GRB
060614 is not intrinsically underluminous but is being masked by
extinction, then that extinction must be due to dust in the host galaxy.
If we conservatively assume that half a magnitude increase in the
brightness of the host galaxy would have been detected in our I image,
then the absolute magnitude (uncorrected for absorption) of the SN must be
less than approximately -16.3. If this SN is not intrinsically
significantly dimmer than SN 1998bw or SN 2006aj, then this implies an
extinction in the host galaxy of at least 2.7 magnitudes in I, or A_V=5.6
assuming standard reddening with R_V=3.1.
- GCN Circular #5286
Peter J. Brown (Penn State) & Stephen T. Holland (NASA/GSFC & USRA)
report on behalf of the Swift UVOT team:
Swift has been continuing to monitor the counterpart to
GRB060614 (Parsons et al. GCN 5252). The UVOT U band light curve,
which was nearly flat during the period of 2-10 days after the
burst at U~22.5 (Holland GCN 5281) has faded to U~24.0 +/- 0.7
(this last point being a 2.7 sigma detection from data taken
between 15-23 days after the burst).
The timing and shape of the plateau and subsequent decay are
very similar to the U band light curve of GRB060218/SN2006aj
(Campana et al. Nature, in press, astro-ph/0603279).
At a redshift of 0.125 (Price, Berger, & Fox GCN 5275),
the possible SN component has an absolute U magnitude about
2 magnitudes fainter than SN2006aj.
We encourage observations at other wavelengths to determine
whether the flattening previously observed (Fynbo et al. GCN 5277;
Cobb & Bailyn GCN 5282) is from the host galaxy or whether a
contributing SN component has since faded.
- GCN Circular #5359
Diana Londish, Mark H. Wieringa (Australia Telescope National Facility)
and Dale A. Frail (NRAO) report on behalf of a larger collaboration:
"We observed a region covering the Swift burst GRB 060614 (GCN#5252)
using the Australia Telescope Compact Array for two 10 minute scans at
June 24 11:44 UT and 12:29 UT. At frequencies of 4.8 and 8.6 GHz no
emission was detected within a 30" error circle of the OT position
(GCN#5255). The 3-sigma detection limits are 0.9 mJy at both
frequencies. Beam size was 2.6"x20" and 1.5"x11" at 4.8 and 8.6 GHz
respectively"
The Australia Telescope Compact Array is part of the Australia Telescope
which is funded by the Commonwealth of Australia for operation as a
National Facility managed by CSIRO.
- astro-ph/0608322 from
Valle: GRB 060614: an enigmatic long-duration gamma-ray burst not due to a hypernova
Gamma-ray bursts (GRBs) are short, intense flashes of soft gamma radiation
coming from the distant Universe. There is now convincing evidence that
long-duration GRBs (those lasting more than ~2 s) originate from the deaths of
massive stars. This conclusion is mostly based on a handful of outstanding
associations between GRBs and supernovae (SNe) of type Ib/c. In particular, the
GRB-associated SNe belong to a peculiar subclass, characterized by high
luminosity at maximum light (M_V ~ -19, with a dispersion of ~1 mag) and high
expansion velocity of the ejecta (v_max ~ 30000 km/s). Such SNe are often
labelled "hypernovae". Here we report deep optical observations of GRB 060614
showing no emerging SN brighter than M_V = -13.9, up to 50 days after the
burst. Any SN associated with this GRB was therefore at least 100 times fainter
at optical wavelengths than the other SNe associated with GRBs. This fact
allows us to set a stringent upper limit to the expansion velocity of the SN
ejecta v < 3500 km/s. This is exceptionally low, about an order of magnitude
smaller than all GRB-associated SNe discovered so far. This is the first clear
evidence that long-duration GRBs can be either associated with SNe which do not
have hypernova properties or they can be produced by different phenomena.
- astro-ph/0608257 from 11 Aug 2006
Gal: The gamma-ray burst GRB060614 requires a novel explosive process
Over the past decade our physical understanding of gamma-ray bursts (GRBs)
has progressed rapidly thanks to the discovery and observation of their
long-lived afterglow emission. Long-duration (T < 2 s) GRBs are associated
with the explosive deaths of massive stars (``collapsars''), which produce
accompanying supernovae, while the short-duration (T > 2 s) GRBs arise from
a different origin, which has been argued to be the merger of two compact
objects, either neutron stars or black holes. Here we present observations of
GRB060614, a 100-s long burst discovered by the Swift satellite, which require
the invocation of a new explosive process: either a massive ``collapsar'' that
powers a GRB without any associated supernova, or a new type of engine, as
long-lived as the collapsar but without any such massive stellar host. We also
discuss the properties of this burst's redshift z=0.125 host galaxy, which
distinguish it from other long-duration GRBs and suggest that an entirely new
type of GRB progenitor may be required.
- astro-ph/0608678 from
Cobb: Could GRB 060614 and its presumed host galaxy be a chance superposition?
The lack of an observed supernova associated with GRB 060614 appears to
require a new paradigm for the formation of (a subset of) long-duration GRBs.
This requirement is based on the presumed low redshift of the burst, which was
inferred from the spatial coincidence of the afterglow with a z=0.125 galaxy.
We explore the possibility that this low-redshift galaxy is a chance
superposition along the line of sight to GRB 060614. We examine the galaxy
distribution of the field of GRB 060614 and find that the probability of a
chance association with a galaxy at least as bright as the putative host is
only ~2%. However, for the current ensemble of ~180 Swift GRBs it is likely
that several such coincidences have occurred, and given the "non-standard"
nature of GRB 060614 it is not implausible that this is one such occurrence.
Thus the conclusion that GRB 060614 requires a revision to the formation
paradigm for long-duration GRBs should be approached with caution.
- astro-ph/0610635 from 20 Oct 2006
Gehrels: Swift detects a remarkable gamma-ray burst, GRB 060614, that introduces a new classification scheme
Gamma ray bursts (GRBs) are known to come in two duration classes, separated
at ~2 s. Long bursts originate from star forming regions in galaxies, have
accompanying supernovae (SNe) when near enough to observe and are likely caused
by massive-star collapsars. Recent observations show that short bursts
originate in regions within their host galaxies with lower star formation rates
consistent with binary neutron star (NS) or NS - black hole (BH) mergers.
Moreover, although their hosts are predominantly nearby galaxies, no SNe have
been so far associated with short GRBs. We report here on the bright, nearby
GRB 060614 that does not fit in either class. Its ~102 s duration groups it
with long GRBs, while its temporal lag and peak luminosity fall entirely within
the short GRB subclass. Moreover, very deep optical observations exclude an
accompanying supernova, similar to short GRBs. This combination of a long
duration event without accompanying SN poses a challenge to both a collapsar
and merging NS interpretation and opens the door on a new GRB classification
scheme that straddles both long and short bursts.
- astro-ph/0612238 from 8 Dec 2006
Zhang: Making a Short Gamma-Ray Burst from a Long one: Implications for the Nature of GRB 060614
The absence of a supernova accompanying the nearby long GRB 060614 poses a
great puzzle about the progenitor of this event and challenges the current GRB
classification scheme. This burst displays a short-hard emission episode
followed by extended soft emission with strong spectral evolution. Noticing
that this burst has an isotropic gamma-ray energy only ~8 times that of GRB
050724, a good candidate of merger-type short GRBs, we generate a ``pseudo''
burst that is ~8 times less energetic than GRB 060614 based on the spectral
properties of GRB 060614 and the Ep ~ Eiso^{1/2} (Amati) relation. We find that
this pseudo-burst would have been detected by BATSE as a marginal
short-duration GRB, and would have properties in the Swift BAT and XRT bands
similar to GRB 050724. This suggests that GRB 060614 is likely a more intense
event in the traditional short-hard GRB category as would be detected by BATSE.
Events like GRB 060614 that seem to defy the traditional short vs. long
classification of GRBs may require modification of our classification
terminology for GRBs. By analogy with supernova classifications, we suggest
that GRBs be classified into Type I (typically short and associated with old
populations) and Type II (typically long and associated with young
populations). We propose that GRB 060614 belongs to Type I, and predict that
similar events will be detected in elliptical galaxies.
- 0801.2419from 21 Jan 2008
Lu: A tidal disruption model for the gamma-ray burst of GRB 060614
Abstract: The combination of a long duration and the absence of any accompanying
supernova clearly shows that GRB 060614 can not be grouped into the two
conventional classes of gamma-ray bursts, i.e. the long/soft bursts deemed to
be collapsars and the short/hard bursts deemed to be merging binary compact
stars. A new progenitor model is required for this anomalous gamma-ray burst.
We propose that GRB 060614 might be produced through the tidal disruption of a
star by an intermediate mass black hole. In this scenario, the long duration
and the lack of any associated supernova are naturally expected. The
theoretical energy output is also consistent with observations.
- 0810.4855from 27 Oct 2008
Caito: GRB060614: a "fake" short GRB from a merging binary system
Abstract: (Shortened) CONTEXT: [...]
GRB060614 is the first nearby long duration GRB
clearly not associated to a bright Ib/c supernova. Moreover, its duration
(T_{90} ~ 100s) makes it hardly classifiable as a short GRB. It presents strong
similarities with GRB970228, the prototype of the new class of "fake" short
GRBs that appear to originate from the coalescence of binary neutron stars or
white dwarfs spiraled out into the galactic halo. AIMS: Within the "canonical"
GRB scenario based on the "fireshell" model, we test if GRB060614 can be a
"fake", or, better, "disguised" short GRB. [...] METHODS: We fit GRB060614
light curves in Swift's BAT (15-150keV) and XRT (0.2-10keV) energy bands.
Within the fireshell model, light curves are formed by two well defined and
different components: the Proper-GRB (P-GRB), emitted at the fireshell
transparency, and the afterglow, due to the interaction between the leftover
accelerated baryonic shell and the CBM. RESULTS: We determine the two free
parameters describing the GRB source within the fireshell model. [...] A small
average CBM density [...] is inferred, typical of galactic halos. The first
spikelike emission is identified with the P-GRB and the following prolonged
emission with the peak of the afterglow.[...] CONCLUSIONS: The anomalous
GRB060614 finds a natural interpretation within our canonical GRB scenario: it
is a "disguised" short GRB. [...] This result points to an old binary system,
likely formed by a white dwarf and a neutron star, as the progenitor of
GRB060614 and well justify the absence of an associated supernova Ib/c.
Particularly important for further studies of the final merging process are the
temporal structures in the P-GRB down to 0.1s.
- 1210.2399 from 10 Oct 12
Zahide Funda Bostanci et al.: Gamma Ray Bursts with Extended Emission Observed with BATSE
We present the results of our systematic search for extended emission components following initial short gamma-ray burst (GRB) spikes, using
Burst and Transient Source Experiment (BATSE) observations. We performed the extended emission search for both short- and long-duration GRBs to
unveil the BATSE population of new hybrid class of GRBs similar to GRB 060614. For the identified bursts, we investigate temporal and spectral
characteristics of their initial spikes as well as their extended emission. Our results reveal that the fraction of GRBs with extended emission
is ~7% of the total number of our BATSE sample. We find that the spectrum of the extended emission is, in general, softer than that of the
initial spike, which is in accord with what has been observed in the prototypical bursts, GRB 060614. We also find that the energy fluence of
the extended emission varies on a broad range from 0.1 to 40 times of the fluence of the initial spike. We discuss our results in the context
of existing physical models, in particular within the two-component jet model.
- GCN Circular #15560
R. Ruffini, C.L. Bianco, M. Enderli, M. Kovacevic, M. Muccino, A.V. Penac=
chioni, G.B. Pisani, J.A. Rueda, Y. Wang report:
The late X-ray observations of GRB 060614 (A. M. Parsons et al., GCN 5252)
by Swift-XRT clearly evidence a pattern typical of a family of GRBs
associated to supernova (SN) following the Induced Gravitational Collapse
(IGC) paradigm (1,2). By overlapping the X-ray (0.3-10 keV in rest-frame)
luminosity light curve of GRB 060614 with the one of GRB 090618, namely the
IGC GRB-SN prototype (3), we estimate a theoretical redshift of z=3D1.2
(see=A0Fig. 1=A0http://www.icranet.org/images/GCN/GRB060614_Fig1.pdf),
much higher than z=3D0.125 of the purported host galaxy (Price et al., GCN
5275; Fugazza et al., GCN 5276). This leads to the explanation of the
absence of a visible SN (4,5,6), settling a long lasting dispute of a possible
wrong redshift estimation given by a chance superposition of GRB 060614
with its purported host galaxy (7). GRB 060614 is therefore a canonical
IGC GRB-SN system. We note that this new value of the redshift still
marginally fulfills the Amati relation (see Fig. 2
http://www.icranet.org/images/GCN/GRB060614_Fig2.pdf),
and that it is in agreement with z=3D1.45+/-0.85 given by the Atteia
relation (A. Pelangeon & J-L. Atteia, GCN 5265) and with the
observational limit of z<1.3 (99.99% CL) given by the combined
ultraviolet/optical and X-ray spectra (8).
More optical observations in the GRB field are encouraged for the
investigation of the actual host galaxy.
References:
(1) J. A. Rueda & R. Ruffini, ApJLett, 758, L7 (2012)
(2) G. B. Pisani et al., A&A, 552, L5 (2013)
(3) L. Izzo et al., A&A, 548, L5 (2012)
(4) M. Della Valle et al., Nature, 444, 1050-1052 (2006)
(5) J. P. U. Fynbo et al., Nature, 444, 1047-1049 (2006)
(6) A. Gal-Yam et al., Nature, 444, 1053-1055=A0 (2006)
(7) B. E. Cobb et al., ApJ, 651, L85-L88 (2006)
(8) N. Gehrels et al., Nature, 444, 1044-1046 (2006)
- 1503.07761 from 27 Mar 15
Bin Yang et al.: A possible Macronova in the late afterglow of the `long-short' burst GRB 060614
GRB 060614 was a unique burst straddling both long and short duration gamma-ray bursts and its physical origin is still debated. Here we
re-examine the afterglow data of GRB 060614 and find a significant F814W-band excess at $t\sim 13.6$ day after the burst observed by the {\it
Hubble Space Telescope (HST)}. This corresponds to an extremely-low luminosity $\sim 3\times 10^{40}~{\rm erg~s^{-1}}$. The excess component
has a very red spectrum and a rapid decline, both unexpected within the present theoretical framework of afterglow. We examine two possible
sources of this signal$-$a very weak supernova and a Li-Paczynski Macronova/kilonova. We find that the observed signal is incompatible with a
weak supernova. However, it is compatible with the ejection of $\sim 0.03-0.1~M_\odot$ of $r-$process material. If this interpretation is
correct GRB 060614 arose from a compact binary (most likely a black hole$-$neutron star but also possibly a double neutron star) merger.
- 1506.05899 from 22 Jun 15
Y. Kaneko et al.: Short Gamma-Ray Bursts with Extended Emission Observed with Swift/BAT and Fermi/GBM
Some short GRBs are followed by longer extended emission, lasting anywhere from ~10 to ~100 s. These short GRBs with extended emission (EE) can
possess observational characteristics of both short and long GRBs (as represented by GRB 060614), and the traditional classification based on
the observed duration places some of them in the long GRB class. While GRBs with EE pose a challenge to the compact binary merger scenario,
they may therefore provide an important link between short and long duration events. To identify the population of GRBs with EE regardless of
their initial classifications, we performed a systematic search of short GRBs with EE using all available data (up to February 2013) of both
Swift/BAT and Fermi/GBM. The search identified 16 BAT and 14 GBM detected GRBs with EE, several of which are common events observed with both
detectors. We investigated their spectral and temporal properties for both the spikes and the EE, and examined correlations among these
parameters. Here we present the results of the systematic search as well as the properties of the identified events. Finally, their properties
are also compared with short GRBs with EE observed with BATSE, identified through our previous search effort. We found several strong
correlations among parameters, especially when all of the samples were combined. Based on our results, a possible progenitor scenario of
two-component jet is discussed.
- 1507.07206 from 28 Jul 15
Zhi-Ping Jin et al.: The lightcurve of the macronova associated with the long-short burst GRB 060614
GRB 060614 was a unique burst straddling both long- and short-duration gamma-ray bursts (GRBs) and its physical origin was heavily debated over
the years. Recently, a distinct very-soft F814W-band excess at $t\sim 13.6$ days after the burst was identified in a joint-analysis of VLT and
HST optical afterglow data of GRB~060614, which has been interpreted as evidence for an accompanying macronova (also called a kilonova). Under
the assumption that the afterglow data in the time interval of $1.7-3$ days after the burst are due to the external forward shock emission it
is found that there is an excess of flux in several multi-band photometric observations, not dissimilar to the flux excess interpreted as
supernovae associated to GRBs. Taken at face value, these bumps represent the first time that a light curve of a macronova has been obtained
(opposed to the single-epoch observation of GRB~130603B). The macronova associated with GRB 060614 peaked at $t<4$ days after the burst, which
is significantly earlier than that ever observed for a GRB-associated supernova. Due to the limited data, no strong evidence for evolution of
the temperature is found. A conservative estimate of the macronova rate is $\sim 14.8^{+14.8}_{-7.4}~{\rm Gpc^{-3}}{\rm yr^{-1}}$, implying a
promising prospect for detecting the gravitational wave radiation from compact object mergers by upcoming Advanced LIGO/VIRGO/KAGRA detectors
(i.e., the rate is ${\cal R}_{\rm GW} \sim 1.7^{+1.7}_{-0.85}(D/300~{\rm Mpc})^{3}~{\rm yr^{-1}}$).
- 1508.05093 from 24 Aug 15
Shota Kisaka et al.: X-ray-powered macronovae
A macronova (or kilonova) was observed as an infrared excess several days after short gamma-ray burst, GRB 130603B. Although the $r$-process
radioactivity is widely discussed as an energy source, it requires huge mass of ejecta from a neutron star (NS) binary merger. We propose that
the X-ray excess simultaneously observed with the infrared excess can naturally heat the ejecta, leading to the thermal re-emission as observed
in infrared. This X-ray-powered model explains both the X-ray and infrared excesses with a single energy source by the central engine like a
black hole, and allows for broader parameter region, in particular smaller ejecta mass $\sim10^{-3}-10^{-2}M_{\odot}$ with iron mixed as
suggested by general relativistic simulations for typical NS-NS mergers, than the previous models. We also discuss the other macronova
candidates in GRB 060614 and GRB 080503, and implications for the search of electromagnetic counterparts to gravitational waves.
- 1512.04192 from 15 Dec 15
Zhi-Ping Jin et al.: An $r-$process macronova/kilonova in GRB 060614: evidence for the merger of a neutron star-black hole binary
After the jet break at $t\sim 1.4$ days, the optical afterglow emission of the long-short burst GRB 060614 can be divided into two components.
One is the power-law decaying forward shock afterglow emission. The other is an excess of flux in several multi-band photometric observations,
which emerges at $\sim$4 days after the burst, significantly earlier than that observed for a supernova associated with a long-duration GRB. At
$t>13.6$ days, the F814W-band flux drops faster than $t^{-3.2}$. Moreover, the spectrum of the excess component is very soft and the luminosity
is extremely low. These observed signals are incompatible with those from weak supernovae, but the ejection of $\sim 0.1~M_\odot$ of
$r-$process material from a black hole-neutron star merger, as recently found in some numerical simulations, can produce it. If this
interpretation is correct, it represents the first time that a multi-epoch/band lightcurve of a Li-Paczynski macronova (also known as kilonova)
has been obtained and black hole-neutron star mergers are sites of significant production of $r-$process elements.
- 1601.00180 from 5 Jan 16
Xiang Li et al.: Long-short GRBs within the horizon of the advanced LIGO/VIRGO network and Time lag between compact object coalescence and GRB onset
Short duration GRBs (SGRBs) are widely believed to be powered by the mergers of compact binaries, like binary neutron stars or possibly neutron
star-black hole binaries. Though the prospect of detecting SGRBs with gravitational wave (GW) signals by the advanced LIGO/VIRGO network is
promising, no known SGRB has been found within the expected advanced LIGO/VIRGO sensitivity range. We argue, however, that the two long-short
GRBs (GRB 060505 and GRB 060614) may be within the horizon of advanced GW detectors. In the upcoming era of GW astronomy, the merger origin of
some long-short GRBs, as favored by the macronova signature displayed in GRB 060614, can be unambiguously tested. The model-dependent time-lags
between the merger and the onset of the prompt emission of GRB are estimated. The comparison of such time-lags between model prediction to the
real data expected in the era of the GW astronomy would be helpful in revealing the physical processes taking place at the central engine
(including the launch of the relativistic outflow, the emergence of the outflow from the dense material ejected during the merger and the
radiation of gamma-rays). The achievable accuracy of measuring the speed of GW in the advanced LIGO/VIRGO era is also examined.
- 1601.01692 from 11 Jan 16
Assaf Horesh et al.: Testing the Magnetar Model via Late Time Radio Observations of Two Macronova Candidates
Compact binary mergers may have already been observed as they are the leading model for short gamma-ray bursts (sGRBs). Radioactive decay
within the ejecta from these mergers is expected to produce an infra-red flare, dubbed macronova (or kilonova), on a time scale of a week.
Recently two such macronova candidates were identified in followup observations of sGRBs, strengthening the possibility that those indeed arise
from mergers. The same ejecta will also produce a long term (months to years) radio emission due to its interaction with the surrounding ISM.
In search for this emission, we observed the two macronova candidates, GRB 130603B and GRB 060614 with the Jansky very large array (VLA) and
the Australia Telescope Compact Array (ATCA). Our observations resulted in null-detections, putting strong upper limits on the kinetic energy
and mass of the ejecta. A possible outcome of a merger is a highly magnetized neutron star (a magnetar), which has been suggested as the
central engine for GRBs. Such a magnetar will deposit a significant fraction of its energy into the ejecta leading to a brighter radio flare.
Our results, therefore, rule out magnetars in these two events.
- 1603.07869 from 28 Mar 16
Zhi-Ping Jin et al.: The 050709 macronova and the GRB/macronova connection
We reanalyzed the publicly-available optical/near-infrared afterglow observations of GRB 050709, the first short GRB from which an optical
afterglow was detected. The $I$-band/F814W-band light curve is significantly shallower than the $R$-band light curve. This additional
low-luminosity soft component can be a signature of a Li-Paczy\'{n}ski macronova (also known as kilonova) arising from $\sim 0.05~M_\odot$
r-process material launched by a compact binary merger. As macronovae are relatively weak and soft they can be identified only within the
afterglows of relatively nearby ($z<0.4$) bursts that have sufficient near-infrared/optical data. There are five such events: GRBs 050709,
060505, 060614, 061201 and 130603B. However, the redshift of 061201 is unclear and there is doubt concerning the origin of GRB 060505.
Remarkably, evidence for a macronova signature is found in the afterglow of each one of the remaining three events. This demonstrates that
macronovae are ubiquitous. The significant mass ejection supports the suggestion that these events are significant and possible main sites of
heavy r-process nucleosynthesis. The identification of two of the three macronova candidates in the $I$-band implies a more promising detection
prospect for the ground-based survey.
- 1605.07235 from 25 May 16
Masaomi Tanaka: Kilonova/Macronova Emission from Compact Binary Mergers
We review current understanding of kilonova/macronova emission from compact binary mergers (mergers of two neutron stars or a neutron star and
a black hole). Kilonova/macronova is optical and near-infrared emission powered by radioactive decays of r-process nuclei. Emission from the
dynamical ejecta with ~0.01 Msun is likely to have a luminosity of ~10^{40}-10^{41} erg s^{-1} with a characteristic timescale of about 1 week.
The spectral peak is located in red optical or near-infrared wavelengths. A subsequent accretion disk wind may provide an additional
luminosity, or an earlier/bluer emission if it is not absorbed by the precedent dynamical ejecta. The detection of near-infrared excess in the
afterglow of short GRB 130603B and possible optical excess in GRB 060614 supports the concept of the kilonova/macronova scenario. At 200 Mpc
distance, a typical brightness of kilonova/macronova with 0.01 Msun ejecta is expected to be about 22 mag and the emission rapidly fades to >24
mag within ~10 days after the merger. Kilonova/macronova candidates can be distinguished from supernovae by (1) the faster time evolution, (2)
fainter absolute magnitudes, and (3) redder colors. To effectively search for such objects, follow-up survey observations with multiple visits
within <10 days and with multiple filters will be important. Since the high expansion velocity (v ~ 0.1-0.2c) is a robust outcome of compact
binary mergers, the detection of smooth spectra will be the smoking gun to conclusively identify the GW source.
- 1606.01983 from 8 Jun 16
Yuu Niino et al.: The redshifted selected sample of long gamma-ray burst host galaxies: the complete metallicity measurements at $z \leq 0.41$
We present the complete list of host galaxy metallicities for all long GRBs whose redshifts were determined to be $\leq 0.41$ before the end of
March 2014, including newly obtained spectroscopic datasets of the host galaxies of GRB 060614, 090417B, and 130427A. We compare the
metallicity distribution of the redshift selected complete sample to the model predictions, and constrain the relation between metallicity and
GRB occurrence. We take account of spatial variation of metallicities among star forming regions within a galaxy. We found that the models, in
which only low-metallicity stars produce GRBs with a sharp cutoff of GRB production efficiency around 12+log(O/H) $\sim$ 8.2, can well
reproduce the observed distribution, while the models with moderate (or no) metallicity dependence are not consitistent with the observations.
This is the first fair estimate of the metallicity distribution of GRB host galaxies based on the redshift selected complete sample in the {\it
Swift} era. We also discuss possible sampling biases we may suffer by collecting long GRBs whose redshifts are known, presenting the
photometric observations of the host galaxy of GRB 111225A at $z = 0.297$ whose redshift has been undetermined until $\sim$ 2.3 years after the
burst.
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