- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Sat 19 Mar 05 09:31:38 UT
NOTICE_TYPE: Swift-BAT GRB Position
TRIGGER_NUM: 111622, Seg_Num: 0
GRB_RA: 154.157d {+10h 16m 38s} (J2000),
154.236d {+10h 16m 57s} (current),
153.399d {+10h 13m 36s} (1950)
GRB_DEC: +43.566d {+43d 33' 56"} (J2000),
+43.539d {+43d 32' 22"} (current),
+43.815d {+43d 48' 55"} (1950)
GRB_ERROR: 4.00 [arcmin radius, statistical only]
GRB_INTEN: 5336 [cnts] Peak=263 [cnts/sec]
TRIGGER_DUR: 1.024 [sec]
TRIGGER_INDEX: 138 E_range: 15-50 keV
BKG_INTEN: 35176 [cnts]
BKG_TIME: 34264.00 SOD {09:31:04.00} UT
BKG_DUR: 8 [sec]
GRB_DATE: 13448 TJD; 78 DOY; 05/03/19
GRB_TIME: 34278.44 SOD {09:31:18.44} UT
GRB_PHI: 158.06 [deg]
GRB_THETA: 37.09 [deg]
SOLN_STATUS: 0x3
RATE_SIGNIF: 11.57 [sigma]
IMAGE_SIGNIF: 10.00 [sigma]
MERIT_PARAMS: +1 +0 +0 +0 +1 +3 +0 +0 +66 +1
SUN_POSTN: 358.97d {+23h 55m 54s} -0.44d {-00d 26' 39"}
SUN_DIST: 131.58 [deg]
MOON_POSTN: 108.30d {+07h 13m 13s} +27.61d {+27d 36' 52"}
MOON_DIST: 40.00 [deg]
MOON_ILLUM: 65 [%]
GAL_COORDS: 174.81, 54.84 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 139.15, 30.44 [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.
- red DSS finding chart
ps-file
- GCN/SWIFT NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Sat 19 Mar 05 09:33:17 UT
NOTICE_TYPE: Swift-XRT Position
TRIGGER_NUM: 111622, Seg_Num: 0
GRB_RA: 154.2016d {+10h 16m 48s} (J2000),
154.2804d {+10h 17m 07s} (current),
153.4438d {+10h 13m 47s} (1950)
GRB_DEC: +43.5463d {+43d 32' 47"} (J2000),
+43.5202d {+43d 31' 13"} (current),
+43.7962d {+43d 47' 46"} (1950)
GRB_ERROR: 5.8 [arcsec radius, statistical plus systematic]
GRB_INTEN: 4984.24 [arb]
GRB_SIGNIF: 8.94 [sigma]
GRB_DATE: 13448 TJD; 78 DOY; 05/03/19
GRB_TIME: 34365.53 SOD {09:32:45.53} UT
TAM[0-3]: 327.61 237.22 261.34 242.42
AMPLIFIER: 2
WAVEFORM: 134
SUN_POSTN: 358.98d {+23h 55m 54s} -0.44d {-00d 26' 38"}
SUN_DIST: 131.62 [deg]
MOON_POSTN: 108.32d {+07h 13m 16s} +27.61d {+27d 36' 47"}
MOON_DIST: 40.02 [deg]
MOON_ILLUM: 65 [%]
GAL_COORDS: 174.83, 54.87 [deg] galactic lon,lat of the burst
ECL_COORDS: 139.19, 30.44 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Coordinates.
COMMENTS: WARNING: XRT alignment calibration is on-going, and there may be
COMMENTS: residual systematic offsets of several arcseconds not accounted for yet
COMMENTS: by our on-board position determination algorithm. We have increased
COMMENTS: the estimated error circle radius to take this into account.
- GCN/SWIFT NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Sat 19 Mar 05 09:35:20 UT
NOTICE_TYPE: Swift-BAT GRB Lightcurve
TRIGGER_NUM: 111622, Seg_Num: 0
GRB_RA: 154.157d {+10h 16m 38s} (J2000),
154.236d {+10h 16m 57s} (current),
153.399d {+10h 13m 36s} (1950)
GRB_DEC: +43.566d {+43d 33' 56"} (J2000),
+43.539d {+43d 32' 22"} (current),
+43.815d {+43d 48' 55"} (1950)
GRB_DATE: 13448 TJD; 78 DOY; 05/03/19
GRB_TIME: 34278.44 SOD {09:31:18.44} UT
TRIGGER_INDEX: 138
GRB_PHI: 158.06 [deg]
GRB_THETA: 37.09 [deg]
DELTA_TIME: 52.00 [sec]
LC_URL: sw00111622000msb.lc
SUN_POSTN: 358.97d {+23h 55m 54s} -0.44d {-00d 26' 39"}
SUN_DIST: 131.58 [deg]
MOON_POSTN: 108.30d {+07h 13m 13s} +27.61d {+27d 36' 52"}
MOON_DIST: 40.00 [deg]
MOON_ILLUM: 65 [%]
GAL_COORDS: 174.81, 54.84 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 139.15, 30.44 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-BAT GRB Lightcurve.
COMMENTS: This does not match any source in the ground catalog.
- GCN notice #3116
E. Rykoff (Umich), B. Schaefer (LSU), R. Quimby (UTexas) report on
behalf of the ROTSE collagoration:
ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
050319 (Swift 11162) in 9.2 s, 27 s after the burst. Our unfiltered
images detect a 16th magnitude, fading source at:
10:16:47.9 +43:32:54.5
Continuing observations are in progress. The object is at ~18th
magnitude, around 940 seconds after the burst.
- GCN notice #3117
Swift Detection of GRB 050319
H. Krimm (GSFC/USRA), M. Still (GSFC/USRA), S. Barthelmy, L. Barbier (GSFC),
S. Campana (INAF-OAB), M. Capalbi (ASDC), M. Chester (PSU),
J. Cummings (GSFC/NRC), E. Fenimore (LANL),
N. Gehrels (GSFC), M. R. Goad, O. Godet (U.Leicester), J. Greiner (MPE),
D. Grupe (PSU), D. Hullinger (GSFC/UMD), V. La Parola , V. Mangano
(INAF-IASF/Palermo),
C. Markwardt (GSFC/UMD), P. Meszaros, D. C. Morris,
J. A. Nousek (PSU), K. Page (U.Leicester), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/NRC), G. Sato (ISAS), M. Suzuki (Saitama),
G.Tagliaferri (INAF-OAB),
J. Tueller (GSFC)
report on behalf of the Swift-BAT and Swift-XRT teams:
At 09:31:18.44 UT, the Swift Burst Alert Telescope (BAT) triggered and
located on-board GRB 050319. The burst was 37 degrees off the BAT
boresight. The spacecraft executed an immediate slew and was on
target by 09:32:45.53 UT at which time the XRT began taking data in
Auto State. On-board software recognized a bright source at location
RA 154.2016d {+10h 16m 48s} (J2000),
Dec +43.5463d {+43d 32' 47"} (J2000)
We estimate an uncertainty of 7 arcseconds.
The burst lightcurve as seen in the BAT has a single peak with a fast
rise, exponential decay. The estimated duration is 15 seconds. The
peak count rate is 2,000 counts/second (15-350 KeV)
- GCN notice #3118
S.Maeno,E.Sonoda,Y.Matsuo,M.Yamauchi
(University of Miyazaki)
"We have observed the field covering the error box of
GRB 050319 (GCN 3117;Swift-BAT Trigger time is 09:31:18.44 UT)
with the unfiltered CCD camera on the 30-cm telescope
at University of Miyazaki.
The observation was started 10:45:01 UT on Mar.19.
Observed field of view is 43 arcmin centerd on
R.A.=10h 17m 01s
Dec.=+43d 31m 06s
After co-adding a set of 9 images of 30 sec exposures,
we have compared with the USNO-A2.0 catalog.
Preliminary analysis shows there is no new source brighter than
17.8mag. at the reported position by GCN3116(E.Rykoff et al.) "
- GCN notice #3119
H. Krimm (GSFC/USRA), T. Sakamoto (GSFC/NRC), S. Barthelmy,
L. Barbier (GSFC), J. Cummings (GSFC/NRC), E. Fenimore (LANL),
N. Gehrels (GSFC), D. Hullinger (GSFC/UMD), C. Markwardt (GSFC/UMD),
F. Marshall (GSFC), J. Nousek (PSU), D. Palmer (LANL), A. Parsons (GSFC),
G. Sato (ISAS), M. Still (GSFC/USRA), M. Suzuki (Saitama), J. Tueller (GSFC)
on behalf of the Swift-BAT team:
Analysis of the full data set for the Swift-BAT GRB 050319 (Krimm,
et al., GCN 3117) yields a fluence of 8 X 10^-7 erg/cm2 in the 15-350 keV
band and a peak flux of 1.7 ph/cm2/sec (also 15-350 keV). The photon index
of the 1-s peak spectrum ( starting at T0 +0.36 sec.) is 2.1 +- 0.3
(90% confidence). The time-averaged spectrum yields a photon index of
2.2 +- 0.2.
The overall measures of burst duration give T90 = 10 +- 2 seconds (including
systematics).
- GCN notice #3120
GRB 050319 : Confirmation of optical afterglow decay
T. Yoshioka (Naogya Univ.), C.W. Chen (NCU), S.Nishiura (Tokyo Gakugei
Univ.), M. Isogai (Tokyo Univ.), T. Soyano(Tokyo Univ.), W.P. Chen (NCU)
Y. Urata, T. Tamagawa (RIKEN), K.Y. Huang, W.H. Ip (NCU), Y. Qiu (BAO)
and Y.Q. Lou(THCA)
on behalf of the East Asian collaboration report:
" We have observed the afterglow candidate of GRB 050319 (Rykoff et al.
# 3116, Krimm et al. # 3117) using Kiso 1.05-m and Lulin 1-m
telescopes starting at 2005 Mar. 19, 10:45 UTC (after end of
twilight). We have imaged the optical candidate (Rykoff et al. # 3116)
clearly in BVRI bands. Based on our preliminary photometry for R-band
images, we have confirmed the decay of the optical candidate.
Observation time and magnitudes are:
Filter Exposure UT Mag. site
R 300s 10:45 19.5 Kiso
R 300s 11:28 19.5 Lulin
R 300s 13:29 20.0 Kiso
Further observations are in progress, this message may be cite."
- GCN notice #3121
K. Torii (Osaka U.) reports
"The error region of GRB 050319 (GCN 3117) was observed by the
ART 14-inch telescope. BVRcIc imaging started at 2005 March 19, 11:24
UT and 60-s exposure in each filter was repeated.
By stacking twenty Rc and twenty Ic frames obtained between 11:36 UT
and 13:05 UT (Mean Epoch 12:20 UT), we note an enhancement of
2.3-sigma level at the position of the optical afterglow (GCN
3116). The enhancement in the stacked frame corresponds to 19.6 mag
with reference to USNO-A2.0 red magnitude.
Combining this magnitude and those reported in GCN 3116 and GCN 3120,
the early optical afterglow of GRB 050319 decays with relatively
shallow power-law index of t^(-0.6)."
- GCN notice #3124
D. Sharapov, M. Ibrahimov, R. Karimov, B. Kahharov (UBAI), A.Pozanenko
(IKI), V.Rumyantsev (CrAO), G.Beskin (SAO) report:
We observed afterglow candidate of Swift GRB050319 (Rykoff et al. GCN
3116, Krimm et al. GCN 3117) with 1.5m telescope of Mt.Maidanak
high-altitude observatory. BR-band images were taken in two sets of
observation on (UT) March 19, 17:14 --17:58 and 19:18 -- 21:45. We confirm
a fading afterglow (Yoshioka et al. GCN 3120). Preliminary photometry
against of USNO-B1.0 Catalog is following:
Mean time Exposure Filter Mag.
(UT) (s)
Mar.19 17:28 900 B 20.85
Mar.19 17:31 1500 R 20.12
Mar.19 20:17 1800 B 21.29
Mar.19 20:16 4800 R 20.17
with typical magnitude error of less than 0.10.
B-R at the two epochs marginally indicate color variation which is not
typical for this phase of afterglow.
This message may be cited.
- GCN notice #3125
Koshy George,Jinesh Jain,N.M.Ashok,T.Chandrasekhar
(Physical Research Laboratory,India)
We report on the detection of near infrared afterglow of GRB 050319 using
NICMOS camera coupled with 1.2m telescope of Physical Research Laboratory
at Gurushikar, Mt.Abu, India.
The observations started at 15:41:00 UT on 19 March in J-band filter at
a 4'* 4' field of view shows a probable Infrared candidate at the error
region of optical afterglow candidate (GCN 3116 & 3117).
We had taken a net fourty minute exposure and the source which was present
in our first 20s frame was found to be faded down to our observational
limits with in 4min (four frames of each 60s exposure).
Preliminary analysis and on comparison with two near by stars present in
our field shows that the near infrared afterglow candidate corresponds to
a J-band magnitude ~ 13 at 15:41:20 UT
- GCN notice #3126
Koshy George, Jinesh Jain, N.M.Ashok, T.Chandrasekhar
(Physical Research Laboratory, India)
We report on the detection of near infrared afterglow of GRB 050319 using
NICMOS camera coupled with 1.2m telescope of Physical Research Laboratory
at Gurushikar, Mt.Abu, India.
The observations started at 15:41:00 UT on 19 March in J-band filter at
a 4'* 4' field of view shows a probable Infrared candidate at the error
region of optical afterglow candidate (GCN 3116 & 3117).
We had taken a net fourty minute exposure and the source which was present
in our first 20s frame was found to be faded down to our observational
limits with in 4min (four frames of each 60s exposure).
Preliminary analysis and on comparison with two near by stars present in
our field shows that the near infrared afterglow candidate corresponds to
a J-band magnitude ~ 13 at 15:41:20 UT
- GCN notice #3127
A. M. Soderberg (Caltech) reports on behalf of the
Caltech-NRAO-Carnegie GRB collaboration:
"Using the Very Large Array at 8.5 GHz, we observed the
field of GRB050319 (GCN 3117) on 2005 Mar 20.03 UT.
We do not detect a radio source at the position of the optical
afterglow (GCN 3116). We place a (2-sigma) limit of 115 uJy.
Further observations are planned."
- GCN notice #3129
P. Boyd (GSFC/UMBC), S. T. Holland, M. Still (GSFC/USRA), W. Landsman
(GSFC), S. Hunsberger (PSU), A. Breeveld (MSSL), P. Roming (PSU), K.
Mason, P. Schady (MSSL), M. Ivanushkina (PSU), T. Poole (MSSL), C.
Gronwall (PSU) A. Blustin (MSSL), P. Brown (PSU), S. Rosen, K. McGowan
(MSSL), S. Koch (PSU), M. Carter, H. Huckle, M. De Pasquale (MSSL), P.
Broos (PSU), T. Kennedy, P. Smith, B. Hancock (MSSL), H. Krimm
(GSFC/USRA), J. Nousek (PSU), N. Gehrels (GSFC), on behalf of the Swift
UVOT team.
The Swift Ultra-Violet/Optical Telescope (UVOT) began
settled observations of the field of GRB 050319 (Krimm
et al; GCN 3117) at 09:32:48 UT, 90 after the BAT
trigger. A comparison of the 100s finding chart (with
mid-exposure 140s after the trigger) against the
Digitized Sky Survey reveals a new source inside the BAT
and XRT error circles at:
RA = 10h 16m 47.76(3)s Dec = +43d 32m 54.9(5)s J2000
and consistent with the ROTSE-IIIb position reported by
Rykoff et al. (GCN 3116) The V band magnitude is V =
17.5(1).
The UVOT obtained a series of images of this burst with
a variety of integration times. Mid-exposure times,
Delta-T, with respect to the BAT trigger at 09:31:18 UT
are measured in seconds. Observations with the V and B
filters are listed below:
Delta-T Exposure(s) Filter Mag
140 100 V 17.5 (Finding Chart)
380 80 B 18.8
600 80 V 18.4
1030 100 B 18.9
1250 100 V 19.2
5400 900 B 20.9
7080 700 V 20.2
17000 900 B 21.2
18700 700 V 20.6
No signal was detected in the U band in a total exposure
time of 90s centered approximately 600s after the
trigger with an upper limit of U = 19.
We caution that the absolute magnitude scale is based on
ground calibration and will require confirmation in
flight.
- GCN notice #3130
Kuntal Misra, Atish P. Kamble and S. B. Pandey (ARIES Naini Tal), on
behalf of larger Indian GRB collaboration
We observed the optical afterglow candidate (GCN 3116) localized by
Swift-BAT (GCN 3117) using the 1.04-m telescope at ARIES, Naini Tal
starting around 2005 March 19, 16:09 UT. We acquired BVRI images
under thin passing clouds. Our preliminary R-band photometry
gives a magnitude of 19.92 +/- 0.08 at 2005 March 19, 17:16 UT after
comparing with near by USNO-A2.0 stars. Further observations are in
progress.
This message may be cited.
- GCN notice #3131
Guy Pooley (MRAO, Cavendish Astrophysics, Cambridge) reports:
Using the Ryle Telescope at 15 GHz in an observation of the field of
GRB050319 (GCN3117) centred on 2005 Mar 21.0, we do not detect
any radio emission; the formal measurement is 0.21 +- 0.23 (sigma)
at the position of the optical afterglow (GCN3116).
- GCN notice #3132
A. M. Soderberg (Caltech) reports on behalf of the
Caltech-NRAO-Carnegie GRB collaboration:
"Using the Very Large Array at 8.5 GHz, we observed again the
field of GRB050319 (GCN 3117) on 2005 Mar 21.4 UT.
We still do not detect a radio source at the position of the optical
afterglow (GCN 3116). We place a (2-sigma) limit of 133 uJy at
that position. Combining these data with those of our previous
epoch (GCN 3127), we derive a deeper limit of 70 uJy (2-sigma rms)
for the field."
- GCN notice #3133
A. P. Beardmore, K. L. Page (U. Leicester), V. Mangano (INAF-IASF/Palermo),
P. Romano (INAF-OAB), M. R. Goad, O. Godet, J. P. Osborne (U. Leicester),
G. Chincarini, S. Campana (INAF-OAB), D. N. Burrows, J. L. Racusin
(PSU), G. Cusumano, T. Mineo (INAF-IASF/Palermo), M. Perri, F. Tamburelli
(ASDC), L. Angelini, F. Marshall, N. Gehrels (GSFC) report on behalf of the
Swift XRT team:
We report refined XRT source positions for GRB 050315 (GCN3094, GCN3097),
GRB 050318 (GCN3111, GCN3113), and GRB 050319 (GCN3117), based on improved
ground-based analysis of extended data sets from these three bursts. We
find the following afterglow positions:
GRB 050315: RA(J2000) = 20:25:53.9, Dec(J2000) = -42:36:01.4 (P. Romano),
which is 2.3" from the optical counterpart (GCN3100).
GRB 050318: RA(J2000) = 03:18:51.1, Dec(J2000) = -46:23:44.7 (V. Mangano),
which is 1.1" from the optical counterpart (GCN3123).
GRB 050319: RA(J2000) = 10:16:48.1, Dec(J2000) = +43:32:52.3 (K. Page),
which is 3.1" from the optical counterpart (GCN3116).
- GCN notice #3135
R. M. Quimby, E. S. Rykoff, B. E. Schaefer, T. McKay, and S. A. Yost
report on behalf of the ROTSE collaboration:
ROTSE-IIIb, located at the McDonald Observatory, Texas, responded
automatically to Swift GRB 050319 (Krimm et al., GCN 3117, GCN 3119)
with the first 5-second exposure beginning Mar 19, 09:31:45.56 UT
(Rykoff et al., GCN 3116), 27.1 seconds after the BAT trigger. The
observing sequence consisted of ten 5-second and ten 20-second images
followed by about 70 60-second exposures before clouds set in. All
images are unfiltered and the average time between exposures was 9.5
seconds.
We measured the afterglow flux in circular apertures relative to our
deepest image, and calibrated the magnitude scale by adopting SDSS
r-band values for our fiducial reference stars. Magnitudes on this
system for our first 5, 20, and 60-second images are given below.
Time (UT) mag +/-
09:31:45.56 16.16 0.17
09:34:09.95 17.22 0.20
09:39:05.24 17.58 0.18
The afterglow is detected in the first 30 images, and coadding the
later exposures in groups of 5 to 10 also results in detections,
making this one of the best sampled early light curves for any
GRB. The afterglow is well fit by a t^(-alpha) power law with
alpha=0.59 +/- 0.05, consistent with later R band observations
reported in the GCN Circulars (GCNs 3120, 3121, 3124). Continuing this
trend predicts the afterglow is currently brighter than 22nd
magnitude.
No host is present in the SDSS data at the location of the afterglow,
which implies the redshift for this GRB is larger than 0.3. We also
note the IR detection reported by George et al. (GCN 3125) gives a J-R
color of about 7, and could suggest a high-z source. Spectral
observations are encouraged to accurately determine the GRB redshift.
- GCN notice #3136
GRB 050319: Absorption redshift from the Nordic Optical Telescope
Johan P. U. Fynbo, Jens Hjorth, Brian L. Jensen, Pall Jakobsson
(Niels Bohr Institute), Palle Moller (ESO), Jyri N=E4r=E4nen (Nordic=20
Optical Telescope) report:
"Using ALFOSC on the Nordic Optical Telescope (NOT) we have obtained=20
spectra of the afterglow of GRB 050319 (GCN 3116, 3117) on 2005,=20
March 20 UT. We find several absorption features, including strong=20
Lyman-alpha, OI+SiII, SiIV and CIV, corresponding to a redshift of
z=3.24."
- GCN notice #3139
U. Kiziloglu, S. Balman, A. Baykal (METU), Z. Aslan, I. Khamitov,
K. Uluc (TUG), S. Evren (EgeU), A. Alpar (Sabanci U.), R. Burenin,
M. Pavlinsky (IKI), R. Sunyaev (IKI, MPA), I, Bikmaev (KSU) report :
We observed the field centered on the Swift GRB 041006 (Rykoff et al.
GCN 3116, Krimm et al., GCN 3117, GCN 3119) with the TUG (TUBITAK
National Observatory, Turkey) 1.5-m Russian-Turkish Telescope (RTT150).
We obtained 8x300s 6x120s 3x60s R band images on 2005.03.19 starting
at 17:26:36 UT using the imaging ANDOR CCD. The seeing was 1.8"-2.1".
We further obtained 6x300 s R band images on 2005.03.20 and 2005.03.21
with RTT150. The seeing was poor with Moon.
We calculated the R magnitudes below using the USNO B1.0 Catalog.
Observation (UT) R_mag
-------------------- ----------------------
2005 March 19, 18:12 20.14 +/- 0.09
2005 March 21, 00:16 21.3 +/- 0.6 1 Sigma frame upper limit
2005 March 21, 17:58 21.1 +/- 0.3
This message can be cited.
- GCN notice #3140
D. Sharapov, M. Ibrahimov, R. Karimov, B. Kahharov (UBAI), A.Pozanenko
(IKI), V.Rumyantsev (CrAO), G.Beskin (SAO) report:
We continue observation (Sharapov et al. GCN 3124) of GRB050319 afterglow
(Rykoff et al. GCN 3116, Krimm et al. GCN 3117) with 1.5m telescope of
Maidanak Astronomical Observatory, Mt.Maidanak, Uzbekistan. R-band images
were taken in several sets of observation on March 19-22. Preliminary
photometry against of USNO-B1.0 Catalog is following:
Mean time Exposure Filter Mag.
(UT) (s)
Mar.20 21:49 2640 R 21.62 (0.07)
Mar.21 21:34 1560 R 21.67 (0.09)
Mar.22 18:41 1260 R 21.27 (0.13)
Observations obtained on March 22 are not compatible with power law index
decay 1.59 (.05) for early and first day afterglow observations (Torii et
al. GCN 3132, Quimby, GCN 3135) suggesting a presence of knee or
re-brightening of the afterglow light curve.
Excellent seeing conditions during the observations on Mar. 22 (~0.7") allow
us to investigate some details of the field objects. In particular IDs
(USNO-B1.0) 1335-0213759 and 1335-0213777 seem to be galaxies, and ID
1335-0213724 is a variable star. All above is leaving a few field stars for
calibration.
Deep field photometry for correct calibration would be encouraged.
This message may be cited.
- GCN notice #3141
<> V. Simon, R. Hudec (Astronomical Institute AV CR, Ondrejov, Czech
Republic) and G. Pizzichini, N. Masetti (INAF/IASF Bologna, Italy) report:
We have determined the color indices of the optical afterglow (OA) of
GRB050319 in its very early phase from the available data (GCN 3124,
3129). The interpolation method described in Simon et al. (2001, A&A,
377, 450) was used. Since the Swift UVOT magnitudes need a confirmation
of their calibration, we determined the indices separately for UVOT and
ground-based observations. The indices of the OA from UVOT are:
t-To=0.0044 d: B-V=0.68; 0.0119: -0.10; 0.0625: 0.85; 0.1968: 0.64,
while those of the ground-based observations (GCN 3124) are: t-To(d)=
0.331 d: B-R=0.73; 0.448: 1.12. The typical error of these indices is
about 0.10 mag.
The Galactic reddening E(B-V)=0.011, determined from the maps by
Schlegel et al. (1998, ApJ, 500, 525), is comparable to the errors
of the measurements.
We note that the variations in B-V, with a peak at t-To=0.01 days,
are caused by a plateau in B while the V magnitude was already
steadily decreasing. The last two measurements from UVOT can
suggest that B-V reached the value roughly consistent with the
typical one for the ensemble of 23 OAs, defined by Simon et al.
(2001; 2004, AIP Conf. Proc., Vol.727, p.487), not later than at
t-To=0.06 days.
The indices of the OA of GRB050319 for t-To > 0.06 days thus appear
to be plausibly consistent with the mean values of the ensemble
(B-V)o=0.45+/-0.15, (B-R)o=0.86+/-0.17. This suggests that the shape
of the spectrum of the afterglow of GRB050319 is similar to the other
afterglows and that its intrinsic reddening (that is inside the host
galaxy) must be again small (Simon et al. 2001; 2004, AIP Conf.
Proc., Vol.727, p.487). Also the redshift of GRB050319 z=3.24 (GCN
3136) suggests that this GRB appears to be another member of the
above-mentioned ensemble of the OAs with z < 3.5.
The search for the host galaxy and the determination of its type
are also encouraged.
This message may be cited.
- GCN notice #3142
G. Greco, C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University),
P. Ferrero (Osservatorio e Universita' di Teramo), G. Pizzichini (IASF-CNR,
Sezione di Bologna) and I. Bruni (Osservatorio di Bologna) report:
We observed the error box of GRB050319 (SWIFT trigger 11162; Krimm et al.,
GCN 3117) in Rc light on March 20 in good sky conditions (seeing approx.
1.5 - 2 arcsec) but in presence of high contribution of moonlight with
the 152 cm G.D. Cassini telescope of Bologna University, equipped with the
BFOSC CCD imager.
We got 4X1200s images with the following results:
UT at start exposure Exposure (s) OT Rc mag
2005 March 20, 2:14 1200 19.58 (+- 0.18)
2005 March 20, 2:37 1200 19.66 (+- 0.16)
2005 March 20, 3:02 1200 19.67 (+- 0.16)
2005 March 20 3:25 1200 19.69 (+- 0.19)
obtained using as comparisons the following objects extracted from
the USNO A2 catalog:
ID: 1275-07685084
ID: 1275-07684473
ID: 1275-07683651
ID: 1275-07685059
ID: 1275-07684793
ID: 1275-07685268
ID: 1275-07684751
s
From our images, by comparison with the R magnitudes reported by CGN 3124,
3139 and 3140 we infer a substantial rebrightening. An image of the OT
is posted
into a public directory from where it can be retrieved by sftp using
hostname: ermione.bo.astro.it, username: publicGRB, password: GRB_bo and
directory: GRB050319.
- GCN notice #3153
A.Volvach (CrAO), A.Pozanenko (IKI) reports on behalf of CrAO-IKI-SAO GRB
collaboration:
We observed the error-box of GRB050319 (Krimm et al. GCN 3117) on March 21,
and 24 at 2.3 GHz and 8.4 GHz with RT-22 of Crimean Astrophysical
Observatory.
Upper limits obtained for the afterglow position (Rykoff et al. GCN 3116)
are approximately equal for both 2.3 GHz and 8.4 GHz frequencies:
Mar. 21.69 (UT) 2 mJy (2 sigma)
Mar. 24.67 (UT) 2 mJy (2 sigma)
Results of observations are in an agreement with GCN 3132 (A. M. Soderberg)
This message may be cited.
- GCN notice #3454
A. Henden (AAVSO/USNO) reports on behalf of the USNO GRB Team:
We have acquired BVRcIc all-sky photometry for 11x11arcmin
fields centered on the coordinates of recent GRB localizations
with the USNOFS 1.0-m telescope on one photometric night
but with bright moonlight. Stars brighter than V=12.0
are saturated and should be used with care. We have placed
the photometric data on our anonymous ftp site:
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb050319.dat
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb050401.dat
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb050408.dat
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb050416.dat
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb050502a.dat
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb050509b.dat
The astrometry in these files is based on linear plate solutions
with respect to UCAC2. The external errors are less than 100mas.
The estimated external photometric error is about 0.03mag.
Since these bursts had identified optical afterglows, we expect
to improve the photometric calibration on subsequent nights.
As always, you should check the dates on the .dat file prior to
final publication to get the latest photometry. There is
a README file on the ftp directory to give you information
about the procedures used to calibrate these fields.
- astro-ph/0511421 from 15 Nov 2005
Quimby: Early-Time Observations of the GRB 050319 Optical Transient
We present the unfiltered ROTSE-III light curve of the optical transient
associated with GRB 050319 beginning 4 s after the cessation of gamma-ray
activity. We fit a power-law function to the data using the revised trigger
time given by Chincarini et al. (2005), and a smoothly broken power-law to the
data using the original trigger disseminated through the GCN notices. Including
the RAPTOR data from Wozniak et al. (2005), the best fit power-law indices are
alpha=-0.854 (+/- 0.014) for the single power-law and alpha_1=-0.364 (+/-
0.020), alpha_2= -0.881 (+/- 0.030), with a break at t_b = 418 (+/- 30) s for
the smoothly broken fit. We discuss the fit results with emphasis placed on the
importance of knowing the true start time of the optical transient for this
multi-peaked burst. As Swift continues to provide prompt GRB locations, it
becomes more important to answer the question, "when does the afterglow begin"
to correctly interpret the light curves.
- astro-ph/0602384 from 17 Feb 2006
George: A late, infrared flash from the afterglow of GRB 050319
We report the detection of a bright, near-infrared flash from the afterglow
of GRB 050319, 6.15 hours after the burst. The IR flash faded rapidly from
J=13.12 mag. to J > 15.5 mag. in about 4 minutes. There are no reported
simultaneous observations at other wavelengths making it an unique event. We
study the implications of its late timing in the context of current theoretical
models for GRB afterglows.
- astro-ph/0609450 from 15 Sep 2006
Jakobsson et al: HI column densities of z > 2 Swift gamma-ray bursts
Context: Before the launch of the Swift satellite, the majority of the gamma-ray burst (GRB) afterglows for which Ly-alpha was redshifted into the observable spectrum showed evidence for a damped Ly-alpha absorber. This small sample indicated that GRBs explode either in galaxies, or regions within them, having high neutral hydrogen column densities.
Aims: To increase the spectroscopic sample of GRBs with z > 2 and hence establish the N(HI) distribution along GRB lines-of-sight.
Methods: We have obtained six z > 2 GRB afterglow spectra and fitted the Ly-alpha absorption line in each case to determine N(HI). This has been complemented with 12 other Swift N(HI) values from the literature.
Results: We show that the peak of the GRB N(HI) distribution is qualitatively consistent with a model where GRBs originate in Galactic-like molecular clouds. However, a systematic difference, in particular an excess of low column-density systems compared to the predictions, indicates that selection effects and conditions within the cloud (e.g. strong ionization) influence the observed N(HI) range. We also report the discovery of Ly-alpha emission from the GRB 060714 host, corresponding to a star-formation rate of approximately 0.8 M_Sun/year. Finally, we present accurate redshifts of the six bursts: z = 3.240 +/- 0.001 (GRB 050319), z = 2.198 +/- 0.002 (GRB 050922C), z = 3.221 +/- 0.001 (GRB 060526), z = 3.425 +/- 0.002 (GRB 060707), z = 2.711 +/- 0.001 (GRB 060714) and z = 3.686 +/- 0.002 (GRB 060906).
- astro-ph/0611323 from 10 Nov 2006
Huang: Multi-color Shallow Decay and Chromatic Breaks in the GRB 050319 Optical Afterglow
Multi-wavelength B, V, R, I observations of the optical afterglow of GRB
050319 were performed by the 1.05-m telescope at Kiso Observatory and the 1.0-m
telescope at Lulin Observatory from 1.31 hours to 9.92 hours after the burst.
Our R band lightcurves, combined with other published data, can be described by
the smooth broken power-law function, with $\alpha_1$ = -0.84 $\pm$0.02 to
$\alpha_2$ = -0.48$\pm$0.03, 0.04 days after the GRB. The optical lightcurves
are characterized by shallow decays-- as was also observed in the X-rays--
which may have a similar origin, related to energy injection. However, our
observations indicate that there is still a puzzle concerning the chromatic
breaks in the R band lightcurve (at 0.04 days) and the X-ray lightcurve (at
0.004 days) that remains to be solved.
- 0709.3561 from 22 Sep 2007
Kamble: Observations of the Optical Afterglow of GRB 050319 : Wind to ISM transition in view
Abstract: The collapse of a massive star is believed to be the most probable progenitor
of a long GRB. Such a star is expected to modify its environment by stellar
wind. The effect of such a circum-stellar wind medium is expected to be seen in
the evolution of a GRB afterglow, but has so far not been conclusively found.
We claim that a signature of wind to constant density medium transition of
circum-burst medium is visible in the afterglow of GRB 050319. Along with the
optical observations of the afterglow of GRB 050319 we present a model for the
multiband afterglow of GRB 050319. We show that the break seen in optical light
curve at $\sim$ 0.02 day could be explained as being due to wind to constant
density medium transition of circum-burst medium, in which case, to our
knowledge, this could be the first ever detection of such a transition at any
given frequency band. Detection of such a transition could also serve as a
confirmation of massive star collapse scenario for GRB progenitors, independent
of supernova signatures.
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