- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Tue 15 Mar 05 20:59:58 UT
NOTICE_TYPE: Swift-BAT GRB Position
TRIGGER_NUM: 111063, Seg_Num: 0
GRB_RA: 306.472d {+20h 25m 53s} (J2000),
306.560d {+20h 26m 14s} (current),
305.624d {+20h 22m 30s} (1950)
GRB_DEC: -42.587d {-42d 35' 13"} (J2000),
-42.570d {-42d 34' 11"} (current),
-42.751d {-42d 45' 03"} (1950)
GRB_ERROR: 4.00 [arcmin radius, statistical only]
GRB_INTEN: 6165 [cnts] Peak=260 [cnts/sec]
TRIGGER_DUR: 1.024 [sec]
TRIGGER_INDEX: 146 E_range: 25-100 keV
BKG_INTEN: 38180 [cnts]
BKG_TIME: 75568.00 SOD {20:59:28.00} UT
BKG_DUR: 8 [sec]
GRB_DATE: 13444 TJD; 74 DOY; 05/03/15
GRB_TIME: 75582.51 SOD {20:59:42.51} UT
GRB_PHI: -27.29 [deg]
GRB_THETA: 39.52 [deg]
SOLN_STATUS: 0x3
RATE_SIGNIF: 17.14 [sigma]
IMAGE_SIGNIF: 8.00 [sigma]
MERIT_PARAMS: +1 +0 +0 +3 +2 +7 +0 +0 -50 +1
SUN_POSTN: 355.76d {+23h 43m 02s} -1.84d {-01d 50' 12"}
SUN_DIST: 59.82 [deg]
MOON_POSTN: 61.14d {+04h 04m 33s} +24.29d {+24d 17' 08"}
MOON_DIST: 123.88 [deg]
MOON_ILLUM: 32 [%]
GAL_COORDS: 358.19,-34.82 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 298.31,-22.67 [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: Tue 15 Mar 05 21:03:19 UT
NOTICE_TYPE: Swift-BAT GRB Lightcurve
TRIGGER_NUM: 111063, Seg_Num: 0
GRB_RA: 306.472d {+20h 25m 53s} (J2000),
306.560d {+20h 26m 14s} (current),
305.624d {+20h 22m 30s} (1950)
GRB_DEC: -42.587d {-42d 35' 13"} (J2000),
-42.570d {-42d 34' 11"} (current),
-42.751d {-42d 45' 03"} (1950)
GRB_DATE: 13444 TJD; 74 DOY; 05/03/15
GRB_TIME: 75582.51 SOD {20:59:42.51} UT
TRIGGER_INDEX: 146
GRB_PHI: -27.29 [deg]
GRB_THETA: 39.52 [deg]
DELTA_TIME: 45.00 [sec]
LC_URL: sw00111063000msb.lc
SUN_POSTN: 355.76d {+23h 43m 02s} -1.84d {-01d 50' 12"}
SUN_DIST: 59.82 [deg]
MOON_POSTN: 61.14d {+04h 04m 33s} +24.29d {+24d 17' 08"}
MOON_DIST: 123.88 [deg]
MOON_ILLUM: 32 [%]
GAL_COORDS: 358.19,-34.82 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 298.31,-22.67 [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 #3094
A. Parsons, S. Barthelmy, L. Barbier (GSFC), J. Cummings (GSFC/NRC),
E. Fenimore (LANL), R. Fink, N. Gehrels (GSFC), S. Holland (GSFC/USRA),
D. Hullinger (GSFC/UMD), K. Hurley (UCB), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), S. Piranomonte (ASDC),
T. Sakamoto (GSFC/NRC), G. Sato (ISAS), A. Smale (NASA HQ), M. Suzuki
(Saitama),
J. Tueller (GSFC)
on behalf of the Swift-BAT team:
At 20:59:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located on-board GRB 050315. The spacecraft automatically slewed
to the burst location, and UVOT began automated observations. XRT was
not in a mode suitable for immediate position determination.
Using the time interval of the trigger of the burst, the
ground-calculated
location is RA,Dec 306.476,-42.591 (J2000) with an uncertainty of 3
arcmin
(radius, including a systematic uncertainty, 90% containment).
The burst was 40 degrees off the BAT boresight (60% coding).
The burst lightcurve has 2 overlapping FRED-like peaks. The duration
is ~40 sec. There is no further emmission out to T+180 sec, where the
end
of the real-time TDRSS data ends. The peak count rate is ~2500
counts/sec.
- GCN notice #3095
S. Rosen, K. McGowan, M. De Pasquale (MSSL), 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, S. Koch (PSU), M. Carter,
H. Huckle (MSSL), P. Broos (PSU), T. Kennedy, P. Smith, B. Hancock
(MSSL), A. Parsons (GSFC), J. Nousek (PSU), N. Gehrels (GSFC), on
behalf of the Swift UVOT team.
The Swift Ultra-Violet/Optical Telescope (UVOT) began observing
the field of GRB 050315 (GCN 3094) at 21:01:13 UT, approximately 90
seconds after the BAT trigger. The first image was sent down via the
TDRSS link approximately 200 seconds after the trigger. This image
was a 100 second exposure taken with the V filter. It was centred on
the BAT position, and had a size of 5 x 5 arcminutes, which covered
88% of the BAT error circle. The middle of the exposure was 140.19
seconds after the BAT trigger. The image was binned 8 x 8 to reduce
the bandwidth required for transmission. A comparison against the DSS
showed no new sources down to a 5-sigma limiting magnitude of
approximately V = 18.5. We stress that this limiting magnitude is
based on ground calibrations and may be uncertain by approximately 0.5
mag. The full-resolution version of this image will be transmitted to
the ground during the next Malindi pass, which will occur at
approximately 0000 UTC March 16, 2005.
- GCN notice #3097
D. C. Morris, D. N. Burrows, J. E. Hill, J. A. Kennea, J. A. Nousek (PSU),
C. Pagani, G. Chincarini (INAF-OAB), A. F. Abbey, P. T. O'Brien (U.
Leicester), G. Cusumano, T. Mineo (INAF-IASF/Palermo), M. Capalbi (ASDC),
A. Parsons, S. Holland, N. White, N. Gehrels (GSFC), K. Mason (MSSL), and
K. Hurley (UCB) report on behalf of the Swift XRT team:
The Swift BAT instrument detected GRB 050315 at 20:59:42 UT on 15 March
2005 (Parsons et al 2005, GCN 3094). The observatory executed an automated
slew to the BAT position and the XRT began taking data at 21:01:05.5
UT. The XRT was in Manual state and made observations in Photon Counting
mode. Data were dumped to the ground at about 00:00 UT on 16 March 2005
and a preliminary analysis was performed by the XRT team. We find a bright
uncataloged, rapidly fading X-ray source located at:
RA(J2000) = 20:25:54,
Dec(J2000) = -42:36:0.2
We estimate an uncertainty of about 6 arcseconds. This source is 32
arcseconds from the BAT position reported in GCN 3094.
- GCN notice #3098
Mark H Wieringa (Australia Telescope National Facility), Brian P Schmidt
(Australian National University)
and Alicia Soderberg (CalTech) report on behalf of a larger collaboration:
"We observed a region covering the Swift burst GRB 050315 (GCN#3094)
using the Australia Telescope Compact Array for 1 hour centered on
March 16.02 UT. At frequencies of 4.8 and 8.6 GHz no emission was
detected within the 6 arcsec diameter error circle of the XRT position
(GCN#3097). The 3-sigma detection limits are 0.6 and 0.8 mJy at 4.8 and
8.6 GHz respectively. No detections above these limits are present
in a larger area (1 arcmin diameter) around the XRT position."
We thank the ATNF Director for making this rapid response possible.
- GCN notice #3099
T. Sakamoto (GSFC/NRC), S. Barthelmy, L. Barbier (GSFC),
J. Cummings (GSFC/NRC), E. Fenimore (LANL), R. Fink,
N. Gehrels (GSFC), S. Holland (GSFC/USRA),
D. Hullinger (GSFC/UMD), K. Hurley (UCB), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
S. Piranomonte (ASDC), G. Sato (ISAS), A. Smale (NASA HQ),
M. Suzuki (Saitama), J. Tueller (GSFC)
on behalf of the Swift-BAT team:
Analysis of the available data for the Swift-BAT GRB050315
(Parsons et al., GCN Circ 3094) yields a fluence of > 2.8x10^-6
erg/cm2 in the 15-350 keV band and a peak flux of 2.5 ph/cm2/sec
(also 15-350 keV). The photon index of the 1-s peak spectrum (T0+25 sec.)
is 2.5 +- 0.3 (90% confidence). Although there is a data gap,
the time averaged spectrum also shows a soft spectrum.
This appears to be a soft X-ray-rich GRB.
We are planning a further circular when more complete data
are avaliable.
- GCN notice #3100
Dan Kelson and Edo Berger (Carnegie Observatories) report:
"On 2005, March 16.347 UT we imaged the XRT error circle of GRB 050315
(GCN 3097) with the newly-comissioned LDSS3 instrument on Magellan/Clay in
the r-band filter. Within the 6" radius error circle we find a single
bright object which is not present in the DSS at coordinates (J2000):
RA = 20:25:54.1
DEC = -42:36:02.2
with an uncertainty of about 0.5" in each coordinate. We consider this
object to be the optical afterglow of GRB 050315."
- GCN notice #3101
Dan Kelson and Edo Berger (Carnegie Observatories) report:
"Using LDSS3 on Magellan we also obtained a 20-minute spectrum of the
afterglow candidate (GCN 3100). We find several absorption features which
we identify as AlIII (1854.7 and 1862.8) and SiII (1808.0) at a redshift
of z=1.949. We conclude that this is the redshift of GRB 050315.
Given a fluence of >2.8e-6 erg/cm^2 (GCN 3099), the isotropic-equivalent
gamma-ray energy is > 2.6e52 erg."
- GCN notice #3102
A. M. Soderberg (Caltech) and D. A. Frail (NRAO) report
on behalf of the Caltech-NRAO-Carnegie GRB collaboration:
"Using the Very Large Array at 8.5 GHz, we observed the
field of GRB050315 (GCN 3094) on 2005 Mar 16.68 UT (t=0.80 d).
Within the XRT localization (GCN 3097), we detect a radio
source at the following coordinates:
RA: 20:25:54.17 Dec: -42:36:01.0 (J2000)
with a positional uncertainty of ~0.5 arcsec. Noting that
this source is roughly coincident with the optical afterglow position
reported by Kelson and Berger (GCN 3100), we interpret this as the radio
afterglow of GRB050315.
Further observations are planned."
- GCN notice #3103
D. Bersier, J. Rhoads, A. Fruchter (STScI), D. Gilbank (Toronto)
report on behalf of the NOAO GRB collaboration:
We have observed the field of GRB 050315 (GCN 3094) with the MOSAIC II
wide-field camera on the CTIO 4m Blanco telescope, starting 0.47d after
the burst.
The afterglow seen in the optical and radio (GCNs 3100, 3101 and 3102)
is well detected in our I-band data, taken at a mean time of 0.484d
after the burst. A preliminary reduction, using an average zero point
for this camera, yields mI=20.7.
- GCN notice #3104
B. E. Cobb and C. D. Bailyn (Yale), part of the larger SMARTS
consortium, report:
Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 050315
(GCN 3094, Parsons et al.) beginning ~11.6 hours post-burst
(2005-03-16 08:35:09 UT). Total summed exposure times amounted
to 180s in BRIYJK and 120s in H and V.
An optical source is detected in R and I at the coordinates of the
reported optical afterglow candidate (GCN 3100, Kelson & Berger). This
source is, however, only slightly brighter than our detection limits.
Preliminary comparison with Landolt Standard PG 1047+003 and USNO B1.0
stars yields the following approximate afterglow magnitudes:
R = 20.9
I = 20.3
No source was detected in B or V with upper limits of B > 22.3 and V > 21.4.
Additionally, the afterglow candidate is not detected in the IR images to
the following detection limits (obtained by comparison with 2MASS):
J > 18.0
H > 17.4
K > 16.3
- GCN notice #3105
H. Krimm (GSFC/USRA), S. Barthelmy, L. Barbier (GSFC), J. Cummings (GSFC/NRC),
E. Fenimore (LANL), R. Fink, N. Gehrels (GSFC), S.T. Holland (GSFC/USRA),
D. Hullinger (GSFC/UMD), K. Hurley (UCB), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
S. Piranomonte (ASDC), T. Sakamoto (GSFC/NRC), G. Sato (ISAS),
A. Smale (NASA HQ), M. Suzuki (Saitama), J. Tueller (GSFC)
on behalf of the Swift-BAT team:
Continued analysis of the full data set (now with telemetry gaps
filled in) for the Swift-BAT GRB050315 (Parsons et al., GCN Circ
3094, Sakamoto et al., GCN Circ 3099) yields a fluence of 4.2 x 10^-6
erg/cm2 in the 15-350 keV band and a peak flux of 2.4 ph/cm2/sec
(also 15-350 keV). The photon index of the 1-s peak spectrum (T0+24.6
sec.) is 2.4 +- 0.3 (90% confidence). The time averaged spectrum
also shows a soft spectrum with a power law index of 2.3 +- 0.1 (90%
confidence). The Swift mission is still in its early orbit phase
and the BAT spectral response continues to be refined. Further
spectral analysis is in progress. In particular, since there is an
uncertainty in the energy response at the lowest energies at the
current time, it is not possible to conclude that this event is an
X-ray flash.
The burst shows considerable structure in its light curve. There is
a precursor starting ~60 seconds before the trigger and continuing up
until the main peak emission begins. The first of the two main peaks
has a slow rise of about ten seconds and a gradual decline
interrupted at TO ~22 seconds by a second peak with a much steeper
rise. The burst shows signs of spectral evolution (hard to soft)
from the precursor through the two main peaks. There is no
significant emission after the decay of the second peak. The overall
measures of burst duration give T90 = 96 +- 10 seconds and T50 = 25
+- 5 seconds. The errors in duration are estimated systematic errors.
- GCN notice #3110
B. E. Cobb and C. D. Bailyn (Yale), part of the larger SMARTS
consortium, report:
Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained additional optical/IR imaging of the reported optical afterglow
candidate (GCN 3100, Kelson & Berger) of GRB 050315
(GCN 3094, Parsons et al.) beginning ~35.6 hours post-burst.
Total summed exposure times amounted to 10 minutes R and I and
12.5 minutes in J.
The source identified as the afterglow candidate has dimmed
since our previous observations (GCN 3104, Cobb & Bailyn).
Preliminary comparison with Landolt Standards PG 1047+003 and RU 149
yields the following approximate afterglow magnitudes:
R = 21.6
I = 21.5
The counterpart was again not detected in the IR, with a
magnitude limit of J > 18.6.
Our R and I observations are summarized below:
time post-burst: R magnitude: I magnitude:
11.6 hours 20.9 20.3
35.6 hours 21.6 21.5
We note that the I-band observations are close to the detection
limit, and have measurement errors of >0.2 magnitudes, so the
evidence for a color change should be treated with caution.
The R-band magnitudes have errors of ~0.2, so assuming
a power-law afterglow decay (afterglow flux proportional to
t^alpha), then this corresponds to an alpha of -0.57 +\- 0.25.
- GCN notice #3128
GRB 050315: Variability Analysis of Swift BAT Time History
T. Q. Donaghy, T. Sakamoto, D. Q. Lamb, E. E. Fenimore, D. E. Reichart,
on behalf of the Swift BAT Team report:
We have calculated the variability measure V (Fenimore and Ramirez-Ruiz
2000; Reichart et al. 2001) for GRB 050315 (Parsons et al., GCN Circular
3094), using the Swift BAT time history data for this burst. We find
values V = 0.017 +/- 0.027, 0.068 +/- 0.022, 0.086 +/- 0.041, and 0.064
+/- 0.016 (68 percent confidence regions) in the 15-25 keV, 25-50 keV,
50-100 keV, and 25-100 keV energy bands, respectively. These values of
V are the same within the statistical uncertainties; this is consistent
with the results of Reichart et al. (2001), who found no significant
trend of V with energy for BATSE bursts.
Analyzing the Swift BAT spectral data for GRB 050315, we find a peak
photon energy flux in 1 s of (9.2 +/- 0.6) x 10-8 erg cm-2 s-1 (68%
confidence region) in the 33.9 - 339.1 keV energy band [which
corresponds to the 100-1000 keV energy band in the rest frame of the
source for a redshift of z = 1.949 (Kelson and Berger, GCN Circular
3101)]. This peak photon energy flux corresponds to an isotropic-
equivalent peak luminosity in the 100-1000 keV energy band in the rest
frame of the source of L_obs = (3.2 +/- 0.2) x 10^51 erg s-1.
Using V in the 25-100 keV energy band as a luminosity (and therefore a
redshift) estimator, we estimate an isotropic-equivalent luminosity in
100-1000 keV in the rest frame of the source of log L_V (erg s-1) =
51.46 +/- 0.747 and a redshift z_V = 1.94 (+2.02/-0.97) for the burst.
These values are consistent with the observed values log L_obs (erg s-1)
= 51.51 (+0.02/-0.04) (90% confidence region) and z = 1.949 (Kelson and
Berger, GCN Circular 3101).
These results are encouraging. They suggest that analyses of the Swift
BAT time history data for a large sample of bursts will provide a
decisive test of the validity of the variability measure V as a
luminosity (and therefore a redshift) estimator, and if the analyses
confirm its validity, they will make possible a better calibration of
the estimator.
- 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 #3294
J. Gorosabel (IAA-CSIC, Granada), P. Laursen, B.L. Jensen, J.P.U.
Fynbo, J. Hjorth, D. Watson, H. Pedersen, P. Jakobsson, J.M. Castro
Cer=A2n (NBI, Copenhagen), M.I. Andersen (AIP, Potsdam), report:
"We have obtained deep R-band imaging of the field of the GRB
050315 optical afterglow (GCN Circ. 3100) with the 1.54m Danish
telescope on La Silla. The observations were carried out during
five nights (8, 9, 11, 12 & 14 April 2005) with a total exposure
time of ~7 hours. In the stacked image, which has a 3 sigma
limiting magnitude of 24.2, an object is detected within an arcsec
of the afterglow position. This object, which we tentatively
identify as the GRB 050315 host galaxy, shows an elongated shape
in the E-W direction.
The magnitude of the potential host galaxy is R=3D23.9+/-0.2. The
photometric calibration is based on observations of Landolt fields.
A finding chart can be found at:
http://www.dsri.dk/~jgu/grb050315/FCs/GRB050315.R.Danish.medianw.gif
Further sub-arsecond deep observations are necessary to clarify
the nature of this object."
This message can be cited.
- astro-ph/0510677 from 24 Oct 2005
Vaughan: Swift observations of the X-ray bright GRB 050315
This paper discusses Swift observations of the gamma-ray burst GRB 050315
(z=1.949) from 80 s to 10 days after the onset of the burst. The X-ray light
curve displayed a steep early decay (t^-5) for ~200 s and several breaks.
However, both the prompt hard X-ray/gamma-ray emission (observed by the BAT)
and the first ~ 300 s of X-ray emission (observed by the XRT) can be explained
by exponential decays, with similar decay constants. Extrapolating the BAT
light curve into the XRT band suggests the rapidly decaying, early X-ray
emission was simply a continuation of the fading prompt emission; this strong
similarity between the prompt gamma-ray and early X-ray emission may be related
to the simple temporal and spectral character of this X-ray rich GRB. The
prompt (BAT) spectrum was a steep down to 15 keV, and appeared to continue
through the XRT bandpass, implying a low peak energy, inconsistent with the
Amati relation. Following the initial steep decline the X-ray afterglow did not
fade for ~1.2*10^4 s, after which time it decayed with a temporal index of
alpha ~ 0.7, followed by a second break at ~2.5*10^5 s to a slope of alpha ~ 2.
The apparent `plateau' in the X-ray light curve, after the early rapid decay,
makes this one of the most extreme examples of the steep-flat-steep X-ray light
curves revealed by Swift. If the second afterglow break is identified with a
jet break then the jet opening angle was theta_0 ~ 5 deg, and implying E_gamma
> 10^50 erg.
- astro-ph/0601708 from 31 Jan 2006
Ruffini: GRB 050315: A step in the proof of the uniqueness of the overall GRB
Using the Swift data of GRB 050315, we progress in proving the uniqueness of
our theoretically predicted Gamma-Ray Burst (GRB) structure as composed by a
proper-GRB, emitted at the transparency of an electron-positron plasma with
suitable baryon loading, and an afterglow comprising the "prompt radiation" as
due to external shocks. Detailed light curves for selected energy bands are
theoretically fitted in the entire temporal region of the Swift observations
ranging over 10^6 seconds.
- astro-ph/0606030 from 1 Jun 2006
Ruffini: GRB 050315: A step toward the uniqueness of the overall GRB structure
Using the Swift data of GRB 050315, we progress on the uniqueness of our
theoretically predicted Gamma-Ray Burst (GRB) structure as composed by a
proper-GRB (P-GRB), emitted at the transparency of an electron-positron plasma
with suitable baryon loading, and an afterglow comprising the so called "prompt
emission" as due to external shocks. Thanks to the Swift observations, the
P-GRB is identified and for the first time we can theoretically fit detailed
light curves for selected energy bands on a continuous time scale ranging over
10^6 seconds. The theoretically predicted instantaneous spectral distribution
over the entire afterglow is presented, confirming a clear hard-to-soft
behavior encompassing, continuously, the "prompt emission" all the way to the
latest phases of the afterglow.
- 0705.2453from 16 May 2007
Ruffini: GRB 050315: A step toward the uniqueness of the overall GRB structure and the true nature of long GRBs
Abstract: Using the Swift data of GRB 050315, we progress on the uniqueness of our
theoretically predicted Gamma-Ray Burst (GRB) structure as composed by a
proper-GRB (P-GRB), emitted at the transparency of an electron-positron plasma
with suitable baryon loading, and an afterglow comprising the so called "prompt
emission" as due to external shocks. Thanks to the Swift observations, we can
theoretically fit detailed light curves for selected energy bands on a
continuous time scale ranging over 10^6 seconds. The theoretically predicted
instantaneous spectral distribution over the entire afterglow confirms a clear
hard-to-soft behavior encompassing, continuously, the "prompt emission" all the
way to the latest phases of the afterglow. Consequences of the instrumental
threshold on the definition of "short" and "long" GRBs are discussed.
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