A&A 449, 89-100 (2006)
DOI: 10.1051/0004-6361:20054457
M. R. Goad1 - G. Tagliaferri2 - K. L. Page1 - A. Moretti2 - J. P. Osborne1 - S. Kobayashi3 - P. Kumar3 - P. I. Mészáros3 - G. Chincarini2,6 - T. Sakamoto4 - B. Zhang5 - S. D. Barthelmy4 - A. P. Beardmore1 - D. N. Burrows3 - S. Campana2 - M. Capalbi7 - L. Cominsky4 - G. Cusumano8 - N. Gehrels4 - P. Giommi7 - O. Godet1 - J. E. Hill3,4,9 - J. A. Kennea3 - H. Krimm4 - V. La Parola8 - V. Mangano8 - T. Mineo8 - D. C. Morris3 - K. Mukerjee1 - J. A. Nousek4 - P. T. O'Brien1 - C. Pagani2,3 - M. Perri7 - P. Romano2 - A. A. Wells1
1 - Department of Physics and Astronomy, University of Leicester,
LE1 7RH, UK
2 - INAF - Osservatorio Astronomica di Brera, via Bianchi 46, 23807
Merate, Italy
3 - Department of Astronomy & Astrophysics, 525 Davey Lab.,
Pennsylvania State University, University Park, PA 16802, USA
4 - NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
5 - Department of Physics,
University of Nevada, BOX 454002, Las Vegas, NV 891, USA
6 - Universita degli studi di Milano-Bicocca, P.za dell Scienze 3, 20126 Milano, Italy
7 - ASI Science Data Center, via Galileo Galilei, 00044 Frascati,
Italy
8 - INAF - Instituto di Astrofisica Spaziale e Cosmica, via Ugo La
Malfa 153, 90146, Palermo, Italy
9 - Universities Space Research Association, 10211 Wincopin Circle,
Suite 500, Columbia, MD, 21044-3432, USA
Received 1 November 2005 / Accepted 23 November 2005
Abstract
We report on the temporal and spectral characteristics of the early
X-ray emission from the Gamma Ray Bursts GRB050126 and GRB050219A as observed
by Swift. The X-ray light-curves of these 2 bursts both show
remarkably steep early decays (
), breaking to flatter
slopes on timescales of a few hundred seconds. For GRB050126 the burst shows
no evidence of spectral evolution in the 20-150 keV band, and the spectral
index of the
-ray and X-ray afterglows are significantly different
suggesting a separate origin. By contrast the BAT spectrum of GRB050219A
displays significant spectral evolution, becoming softer at later times, with
evolving toward the XRT photon index seen in the early X-ray
afterglow phase. For both bursts, the 0.2-10 keV spectral index pre- and
post-break in the X-ray decay light-curve are consistent with no spectral
evolution. We suggest that the steep early decline in the X-ray decay
light-curve is either the curvature tail of the prompt emission; X-ray flaring
activity; or external forward shock emission from a jet with high density
regions of small angular size (
). The late slope we associate
with the forward external shock.
Key words: gamma rays: bursts - gamma rays: observations - black hole physics
The Swift Gamma-Ray Burst Explorer (Gehrels et al. 2004), launched 2004 November 20 is now routinely observing the prompt gamma-ray and afterglow emission of Gamma-Ray Bursts (GRBs) in the astrophysically important minutes to hours timescale after the burst trigger. With its unique autonomous pointing capability, Swift is able to slew its narrow-field instruments, the X-Ray Telescope (XRT, Burrows 2005a) and UltraViolet-Optical Telescope (UVOT, Roming et al. 2005) to the burst position on timescales of less than 100 s, opening up to scrutiny a largely unexplored region of parameter space.
Table 1: Swift BAT spectral fits. Quoted errors are 90% confidence on 1 interesting parameter.
The greater sensitivity over previous gamma-ray missions of the Burst Alert
Telescope (hereafter BAT, Barthelmy 2004) together with Swift's rapid
pointing capability, allows prompt localisations (a few arcseconds) of
relatively faint GRB afterglows, essential for ground-based follow-up. Swift can therefore not only study fainter bursts, but also the early
afterglows during a phase in which they are many orders of magnitude brighter.
During the course of its 3-year mission Swift will deliver unique
insights as to the nature of the prompt and early afterglow emission as well
as probing the faint end of the GRB luminosity function.
Here we report on Swift observations of GRB050126 and GRB050219A (see
also Tagliaferri et al. 2005; Nousek et al. 2005; and Chincarini et al. 2005,
for a discussion of the average early X-ray light-curve behaviour of a sample
of Swift detected GRBs), two bursts for which we have early observations
(within 100 s) in the XRT and which show similar behaviour in their
prompt X-ray light-curves. In Sect. 2 we describe the data taken for each burst
in succession and present in detail a temporal and spectral analysis of the
BAT and XRT data. In Sect. 3 we place the observations in the context of
theoretical models of the GRB and afterglow emission. Our conclusions are
presented in Sect. 4.
The Swift BAT triggered on GRB050126 at 12:00:54 UT Jan. 26th 2005 (Sato et al. 2005). The spacecraft autonomously slewed to the burst location and was settled on target at 12:03:04 UT. Before the slew, the XRT was in manual state taking calibration observations of Mkn 876 in Photon Counting (PC) mode. Thus the first 278 s of observations were taken in PC mode only. Ground analysis of the early PC mode data identified a new bright source at position RA(J2000) 18:32:27.0, Dec(J2000) +42:22:13.5 with an estimated uncertainty of 8 arcsec (Kennea et al. 2005; Campana et al. 2005a,b).
Analysis of BAT calibration targets during the mission verification phase
shows that the early BAT response matrix (build 11) under-predicts the flux by
20-30% at energies below 20 keV and predicts an excess of emission at
energies above 100 keV. The BAT event data described here were re-analysed
using the standard BAT analysis software (build 14) as described in the Swift
BAT Ground Analysis Software Manual (Krimm et al. 2004), which
incorporates post-launch updates to the BAT spectral response and effective
area and includes the systematic error vector which must be applied to all
BAT spectra.
![]() |
Figure 1: 15-350 keV mask-weighted (i.e. background subtracted) BAT lightcurve of GRB050126. The x-axis indicates the elapsed time in seconds from the BAT rate trigger. |
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GRB050126 is characterised by a single broad peak with fast rise ( s),
and exponential decay (FRED) and total duration
s
(
s; Fig. 1). The total fluence is
(
erg cm-2 (15-350 keV) and the peak five
second flux is 0.4 ph cm-2 s-1. The spectrum is
consistent with an unabsorbed power-law with photon index
(where
)
in the 20-150 keV band,
for
53 d.o.f. (Sato et al. 2005). A cut-off powerlaw does not significantly
improve the fit (
for 52 d.o.f.), and the high-energy cut-off is
unconstrained by the data (Table 1). We find no evidence for
spectral evolution in the BAT data for this source. From 12:02:32 UT onward
(i.e. 98 s after the BAT trigger), there is no detectable gamma-ray emission
with an approximate
upper limit of
erg cm-2 s-1 (15-350 keV).
Because the XRT was in Manual State before the slew, the standard set of XRT observations was not implemented and thus the image mode (IM) observations normally taken once the spacecraft has settled were not taken in this instance. Furthermore, in Manual State automatic mode-switching is disabled hence only photon counting (PC) mode observations were taken for this source.
The PC mode event lists were processed using the standard xrtpipeline
data reduction software, version 12, within FTOOLS v5.3.1, screening for
hot-pixels, bad columns and selecting event grades 0-12 for light-curves and
grade 0 for spectra. Early calibration observations show that XRT can suffer
from a high optical background light that dominates the spectrum at low
energies (<0.2 keV), and which is particularly strong near the bright Earth
limb. In the analysis presented here, the low energy photons have been removed
by filtering out PHA values below 0.2 keV. Bad columns, and channels above
10 keV have also been excluded. Finally, frames with spacecraft pointing
directions greater than 4.8 arcmin from the nominal GRB position, and with
CCD temperatures >-50 degrees Celsius have also been
excluded. For light-curve and spectral extraction we define both an annular
source region of inner radius 3 pixels and outer radius 30 pixels to account
for the moderate pile-up at early times, and a circular source region of
radius 30 pixels (
)
at later times, both centred on the XRT
position as determined from the XRT analysis task xrtcentroid. For the
background we define an annular region of inner radius 80 pixels and outer
radius 120 pixels centred on the same position. Our selection criteria
yielded a total on-source time of 8076 s from 9 orbits of PC mode data, with a
mean background count-rate of 0.0019 ct s-1.
Figure 2 shows the XRT light-curve for GRB050126. For the first 2 orbits of data, the light-curve points were grouped to a minimum of 20 counts/bin, while, at later times, we bin data into a single bin for each orbit. The source and background lightcurves were then simultaneously fitted within XSPEC, using Cash Statistics since many of the latter data points do not contain the minimum number of counts required for Gaussian statistics.
Here we chose to use XSPEC for light-curve fitting as it provides a ready-made
suite of models with which to fit the data.
The 0.2-10.0 keV XRT light-curve of GRB050126 shows a steep early decline
breaking to a flatter decay slope on relatively short timescales (a few
hundred seconds). A single power-law fit to the XRT light-curve
(
), with
,
Cash
statistic = 62.0 for 20 data points, provides a poor fit to the data. A
broken power-law provides an improved fit to the data (Cash statistic = 26.1
for 20 data points) yielding an initial slope
,
flattening to
after a time
s (Table 2, Col. 1),
where
is the rate trigger time and all errors are 90%
confidence for 1 interesting parameter. We note that because of a gap in the
data coverage due to an early SAA passage, only the lower limit to the break
timescale is well-constrained. A single powerlaw fit to the data which allows
for differences between the burst rate trigger and the onset of afterglow
,
(i.e.
), provides an acceptable
fit to the data with
,
,
Cash statistic = 31.7 for 20 data points.
![]() |
Figure 2:
The XRT
0.2-10.0 keV decay light-curve for GRB050126. All data were taken in PC
mode. The decay curve is well-fit by a broken power-law (solid line) with
slope
2.52+0.50-0.22 at early times flattening to a slope of 1.0 after 424 s (Cash statistic = 26.1 for 20 data points). Also shown is a
powerlaw fit to the decay light-curve accounting for the onset of the X-ray
afterglow ![]() ![]() ![]() ![]() ![]() |
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Table 2: Swift XRT temporal decay fits. Quoted errors are 90% confidence on 1 interesting parameter.
Table 3: Swift XRT spectral fits. Quoted errors are 90% confidence on 1 interesting parameter.
Ancillary response files were created using the XRT analysis task xrtmkarf (version 12). The XRT spectrum is well fit by an
absorbed
power-law, photon index
,
with the column fixed
at the Galactic value of
cm-2, yielding
for 8 degrees of freedom. An excess column above the Galactic
value is not required by the data. We have also formed time-averaged spectra
before and after the measured break in the XRT decay light-curve
(Table 3). With the column fixed at the Galactic value, and
photon index
pre- and post-break tied together we find a marginally
steeper (though consistent within the errors) mean photon index of
,
for 6 degrees of
freedom. Untying
pre- and post-break, we find marginal evidence (90%
confidence) for spectral hardening in the 0.2-10.0 keV band following the
break in the decay light-curve, with
decreasing from
2.59+0.38-0.35 pre-break to
1.72+0.65-0.60 post-break.
Furthermore, by fixing
to the post-break value of 1.72, a fit to
the pre-break data reveals an additional soft excess, which may be modelled as
a blackbody with temperature
keV,
for 3 d.o.f., or a powerlaw with photon index
,
for 3 d.o.f. We emphasise that while indicative of a possible
excess in emission at low energies, the quality of the statistics is poor (only
3 degrees of freedom), therefore we prefer not to draw any firm conclusions
based on this finding.
In Fig. 3 we show the combined BAT and XRT flux
light-curves corrected for absorption. The BAT photon index is insensitive to
the Galactic column for energies above 20 keV. Therefore to derive the BAT
flux light-curve we have simply extrapolated the BAT spectrum into the XRT
band (0.2-10 keV) adopting the average photon index of the pre-slew BAT and
pre-break XRT spectra (
).
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Figure 3: BAT-XRT decay light-curve for GRB050126 (0.2-10 keV, see text for details). Note that the early steep decline phase in the XRT light-curve joins smoothly with the late-time BAT data. |
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Taken at face value, the pre-break XRT light-curve appears to point toward the
late-time BAT data indicating that the early X-ray emission may be associated
with the end of the initial explosion. A combined powerlaw fit to the BAT
(20-150 keV) and pre-break XRT (0.2-10 keV) spectra
(Fig. 4), covering the time interval
s to
s for the BAT spectrum and
s to
s for the XRT spectrum, however, is inconsistent with a single
powerlaw slope at >99% confidence, with the XRT spectrum being
significantly softer. This does not preclude an association between the prompt
and early X-ray emission since these observations are non-simultaneous, and
the prompt emission may evolve at later times, though we note that there is no
evidence for spectral evolution in the BAT data.
Due to the close proximity of GRB050126 to the bright star Vega, UVOT was unable to observe this field. Ground based observations with Keck/NIRC obtained on Jan. 26th, 4.5 h after the burst (Berger & Gonzalez 2005) revealed a new infra-red (Ks band) source 1.9 arcsec from the XRT position with a subsequent redshift determination for the host galaxy of z=1.29.
![]() |
Figure 4: Combined power-law fit to the BAT (20-150 keV) and pre-break XRT (0.2-10 keV) spectra of GRB050126. The data are inconsistent with a single powerlaw fit at greater than >99% confidence. Inset: 68%, 90%, 95%, and 99% confidence contours indicating the Photon indices for BAT and XRT PC mode data in a combined fit to the BAT and XRT spectra for GRB050126. The data are inconsistent with a single power-law fit to the BAT and XRT spectra at >99%confidence. |
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The Swift BAT triggered on GRB050219A at 12:40:01 UT Feb. 19th 2005
(Hullinger et al. 2005). The spacecraft autonomously slewed to the burst
location starting at
s and was on target at
s. Following
the slew Swift began an automated sequence of observations with
XRT and UVOT.
Table 4: GRB050219a BAT time-resolved spectral fits.
![]() |
Figure 5: 15-350 keV mask-weighted BAT lightcurve of GRB050219a. The dotted lines (segments 1-5) indicate the time-slices used for the BAT spectral evolution analysis. Zero represents the BAT rate trigger time. |
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The BAT light-curve for GRB050219A is characterised by two overlapping peaks,
with a duration
s (Fig. 5). The
peak flux is 5.5 ph cm-2 s-1 for a 1-s interval (15-350 keV),
15 s after the onset of the burst. The burst fluence is
erg cm-2 in the 15-350 keV band. In the
20-150 keV energy range, the BAT spectrum is well-fit by a cut-off power-law
with photon index
,
high energy cut-off
40.61+12.5-8.2 keV,
for 52 d.o.f. A single power-law
fit to the 20-150 keV spectrum is significantly worse (
for
53 d.o.f., Table 1). A Band model (Band et al. 1993) fit to the
data is poorly constrained due to the limited range and low BAT effective area
at high energies.
A cross-correlation analysis of the 4 channel, 1 s, BAT light-curves
(15-25 keV, 25-50 keV, 50-100 keV, 100-350 keV) shows that the 4-channel
light-curves are highly correlated, and display evidence for inter-band
delays, with the lowest energy bands delayed with respect to the higher energy
bands (Fig. 6). This is confirmed by a simple hardness ratio plot,
which shows the BAT spectrum is indeed significantly softer at later times.
The highest energy band 100-350 keV precedes the 50-100 keV band by
s, the 50-100 keV precedes the 25-50 keV band by
s and
the 25-50 keV band precedes the 15-25 keV band by
s, all
measurements determined from a Gaussian fit to the peak (correlation
coefficient >0.5) of the cross-correlation function.
![]() |
Figure 6:
Cross-correlation functions indicating the interband delays in 4 BAT
channels for GRB050219a. The light-curves are highly correlated with the
hardest bands leading the softer bands by ![]() ![]() ![]() |
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To determine the rate at which the photon index evolves, we have divided the
15-350 keV light-curve into 5 segments, fitting the spectrum in each segment
with a cut-off powerlaw (Table 4). A single cut-off
powerlaw fit to all 5 segments is not a good fit to the data, with
,
keV,
for 272 d.o.f. Keeping
the photon index tied between each segment and allowing the cutoff energy to
freely vary, provides a significant improvement, with
,
and
increasing from 77.5 keV to 139.2 keV through segments 1-3
before decreasing in the final 2 segments to 59.6 keV,
for 268 d.o.f. Finally, allowing the photon index to freely vary provides
further improvement,
.
In Table 4 we show cut-off
powerlaw fits to individual segments only. Table 4 confirms our earlier
finding that the BAT photon index steepens at later times. As with the
combined fit we find that the peak energy in the cut-off powerlaw appears to
increase through segments 1-3, peaking in segment 3, when the burst was
brightest, before shifting back to lower energies in the final segment. The
observed decrease in peak energy at later times is a feature common to many
burst afterglows (Ford et al. 1995; Norris et al. 1986).
Figure 7 shows the evolution of the BAT photon index
(15-350 keV) with time together with the measured photon index in the XRT
0.2-10 keV during the early steep decline phase of the burst (see Sects. 2.2.2
and 2.2.3).
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Figure 7: Evolution of the BAT photon index 15-150 keV (black points) for GRB050219a during segments 1-5 (see text for details). The red triangle indicates the 0.2-10 keV XRT photon index during the steep early decline phase of the burst. The BAT and XRT errors are 90% confidence limits on the spectral fit. |
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The XRT was in Auto-State when Swift slewed to the burst. During the
slew XRT was in Low rate PhotoDiode (LrPD) mode and the early frames are
vignetted (Fig. 8). After settling, a single exposure (2.5 s
duration) Image Mode frame was taken, truncating the final LrPD mode
frame. XRT then cycled through Windowed Timing (WT) mode and PC mode
observations, with the mode determined by the count-rate and the on-board
switch thresholds (Hill et al. 2005). The first usable data, an un-vignetted
LrPD frame, was taken 86.5 s after the burst trigger. The LrPD data indicate
an initial increase in the observed count rate over and above that of the
background count rate, which we assume to be due to the source moving into the
field of view of the XRT (see Fig. 8). GRB050219A was observed for a total
of
s. XRT returned to the target in the following orbit for
a second pointed observation in PC mode (total duration 2170 s). No further
observations of GRB050219A were taken during the next few weeks as GRB050219b
(Cummings et al. 2005) became the new priority target. Observations taken in
March did not detect the source.
The event lists for the various XRT observing modes were processed using the
standard xrtpipeline calibration software, version 12, screening for
hot-pixels, bad columns and using grade selection: PC mode 0-12,
WT mode 0-2, LrPD mode 0-5. We note that for the first
s the CCD
temperature was marginally above -50 Celsius. However, as far as we can
tell, there do not appear to be any temperature-dependent artefacts in the
data.
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Figure 8:
Timeline showing the LrPD count-rate during the slew, settling and
early pointing phase observations of GRB050219a. The object enters the XRT
field of view
![]() ![]() ![]() |
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Figure 9:
The XRT 0.2-10.0 keV decay light-curve for GRB050219a. Colours
indicate LrPD data (blue), IM data (magenta), WT data (red), and PC mode data
(green). The best-fit broken power-law fit to the decay curve after 100 s has a decay slope
![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 9 shows the XRT light-curve constructed from the standard grade selections for all modes, and grouped for a minimum of 40 counts/bin. Note we do not bin across gaps in the light-curves caused by orbital viewing constraints, nor do we include data taken within different modes within the same bin.
The prompt X-ray emission, detected within 86 s of the BAT rate trigger, is
one of the earliest X-ray detections of a GRB made by Swift. If we
include the LrPD data taken during the slew, the XRT lightcurve indicates an
initial rise, possibly due to an X-ray flare, followed by a steep decline from
a peak near the time of the Image Mode exposure. Flaring behaviour has been
detected in approximately half of the Swift GRB population (see e.g. Burrows
et al. 2005b; Barthelmy et al. 2005). For the decline phase, we measure an
initial decay slope for the XRT light-curve (excluding the PC mode data)
relative to the BAT rate trigger of
at early
times, breaking to a slope of
,
332+26-22 s later, with
for 36 d.o.f.
(Fig. 9). A single powerlaw fit to the data with the
afterglow coincident with the onset of the burst provides a poor fit to the
data with a best-fit slope of
2.50+0.16-0.16,
for 38 d.o.f. Fitting for the onset of the afterglow, we obtain a decay slope
,
s (90% confidence)
after the BAT rate trigger with
.
We note that this fit
is a poor approximation to the late-time data.
![]() |
Figure 10: BAT-XRT light-curve for GRB050219a (0.2-10 keV, see text for details). Note that the early steep decline in the XRT data does not appear to join up smoothly with the late time BAT data. |
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Fitting the time-averaged spectra for the LrPD, WT and PC mode data together
yields a best-fit powerlaw model with photon index
with an excess absorption above the Galactic
value (
cm-2) of
cm-2,
for 52 d.o.f. We find no evidence for
spectral hardening following the break in the decay light-curve
(Table 3) and applying the post-break spectral fit to the
pre-break data does not in this case reveal any excess emission at soft
energies. Figure 10 shows the BAT and XRT decay
light-curves. Count rates have been converted to fluxes using the spectral
fits to the BAT and XRT data and assuming no spectral evolution pre- and
post-break in the XRT light-curve. The BAT data have been extrapolated into
the XRT 0.2-10.0 keV band using an average of the photon index of the BAT and
XRT data for each of the 4 segments of the BAT light-curve. For GRB050219A the
XRT light-curve does not appear to join smoothly with the late-time BAT data.
This apparent mismatch in the BAT/XRT light-curves is most likely due to
flaring behaviour in the early XRT data, although the strong spectral
evolution in the BAT data could also have some influence.
Figure 11 shows a combined fit to the BAT and
pre-break XRT spectra. A single powerlaw fit to the combined BAT-XRT spectrum
is a poor (
)
description of the data, again indicative
of strong spectral evolution in the GRB spectrum. We note that GRB flares
observed by Swift have generally harder canonical photon indices than spectra
derived from the underlying powerlaw decay curve and soften with time,
reminiscent of the behaviour of the prompt emission (see
e.g. Burrows et al. 2005b).
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Figure 11: Combined power-law fit to the BAT (20-150 keV) and XRT (0.2-10 keV) spectra of GRB050219a. Inset: 68.3%, 90%, 95.4% and 99% confidence contours indicating the relative Photon indices for BAT and XRT in a combined fit to the BAT and XRT spectra of GRB050219a. The data are inconsistent with a single power-law fit to the BAT and XRT spectra at greater than 99% confidence. |
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The XRT decay light-curves of GRB050126 and GRB050219A are both characterised
by an initial steep decline breaking to a flatter slope on timescales of a few
hundred seconds (Table 2). A similar break, though less well-defined has also
been seen in GRB050117A (Hill et al. 2005) and GRB050319 (Cusumano
et al. 2005), while possibly the most convincing early break is seen in the
prompt X-ray light-curve of GRB050315 (Vaughan et al. 2005). If these temporal
variations do indeed represent breaks in the afterglow light-curves, then they
are amongst the earliest breaks yet seen. A single powerlaw fit to the data
with the onset of the afterglow, ,
set to the BAT trigger time, is
in both cases a poor fit to the data (Table 2). A broken
powerlaw fit is a significant improvement in both cases, with derived break
timescales of
s (all errors 90% confidence
on 1 interesting parameter), and
s for GRB050126
and GRB050219A respectively (Table 2). For GRB050126 we can also find an
acceptable fit to the data by fitting a single powerlaw together with an offset (
)
for the onset of the afterglow relative to the BAT trigger.
We find a best-fit model of
,
,
Cash statistic = 31.7 for 20 data points. For
GRB050219A, a single powerlaw fit with offset
significantly
under-predicts the late-time (post-break) data, though the derived
for GRB050219A is consistent within the errors with the observed rise in the
light curve seen in the LrPD frames (Fig. 8) taken during the
final stages of settling in the first orbit. Taking the observed rise in count
rates in the pre-slew LrPD mode frames at face value, we may well have
observed the onset of the afterglow in this burst. Since the peak count-rate
in the Image Mode frame is consistent with the sharp decline at early times,
the peak afterglow emission may have occurred prior to the Image Mode
observation.
In the previous discussion we have assumed that the early X-ray data
are entirely due to the onset of the afterglow.
In order to quantify the relationship, if any, between the -ray
emission and the early X-ray light-curve, we show in Table 2
the results of fitting a Gaussian+powerlaw model to the XRT decay
light-curve. For both, we initially fix the late-time powerlaw decay slope to
the best-fit model for the late-time data and then fit a Gaussian assuming that
the location of the peak of the Gaussian
is coincident with the
burst trigger time. For both GRB050126 and GRB050219A, freeing
produces no improvement in the fit to the data, suggesting
is
indeed coincident with the BAT trigger.
The spectral indices measured for the -ray emission and prompt X-ray
emission immediately following the burst (i.e. during the steep decline phase)
are significantly different in both sources (>99% confidence), suggesting a
separate origin. However, we note that the BAT spectral index for GRB050219A
evolves during the course of the burst toward the measured XRT photon index
(see e.g. Fig. 7, and Table 4).
Fitting the XRT 0.2-10 keV band either side of the break in the light-curve
is only marginally suggestive of spectral hardening at later times,
and
for GRB050126 and
GRB050219A respectively. While we stress that in both cases the slopes pre-
and post-break are entirely consistent within the errors with no temporal
spectral evolution, we remark in passing that unlike GRB050219A, GRB050126
shows evidence of a soft excess consistent with either a thermal blackbody
with temperature
kT=0.11+0.04-0.03 keV,
for 3 d.o.f., or a
powerlaw with
,
for 3 d.o.f.; when
applying the spectral fit for the post-break XRT data to the pre-break XRT
data.
The X-ray afterglow emission from these two bursts consists of an early
steeply declining phase,
,
lasting approximately
five minutes, followed by the more typically observed less steeply declining
phase with
(see Table 2 for their observational
properties). The broken powerlaw light-curve is likely
produced by two distinct X-ray components.
The interpretation for the less steeply falling X-ray light-curve is
straightforward - it is synchrotron radiation in the external forward
shock. The spectral index
(where
)
and the temporal
index
(
)
are both related to
the electron powerlaw index p. When the observed energy band
(0.2-10 keV) is above the synchrotron cooling frequency, the most
likely possibility for these bursts at early times, then
and
.
The values of
and
for these two bursts
(see Table 5) are consistent within the errors with this expectation;
for GRB050126 and
for GRB050219A.
Table 5:
The relationship between temporal decay index ,
and spectral
slopes
,
for internal and external shock models.
If the onset of the afterglow phase ()
is unrelated to the burst
trigger time, then the entire X-ray afterglow light-curve for GRB050126 can be
fitted with a single power law of index
(Table 2) i.e.,
with
s (see Kobayashi et al. 2005, for a
detailed discussion of the choice of the onset of
)
. The X-ray light-curves and the spectra in
this case are entirely consistent with synchrotron radiation in the external
forward shock. However, in the internal-external shock model
cannot simply be chosen arbitrarily. According to this model the outer-most
shell, that is farthest from the central explosion, is the first to interact
with the circumstellar medium and produces the forward shock emission we see
whereas the burst itself is produced in internal shocks at smaller
radii. Therefore, we expect
to lie between the gamma-ray burst
trigger time and the reverse shock crossing time (afterglow peak time). This
suggests that the break in the X-ray light-curve for GRB050219A is real and we
consider various models that can give rise to this break.
A rapidly falling X-ray light-curve at early times could be due to emisson from a hot cocoon accompanying a relativistic jet (Mészáros & Rees 2001; Ramirez-Ruiz et al. 2002), and from the photosphere associated with the outflow from the explosion (e.g. Mészáros & Rees 2000; Mészáros et al. 2002; Rees & Mészáros 2004). However, in the simplest versions of these models the spectrum of the emergent radiation is thermal which is inconsistent with the non-thermal powerlaw spectrum for the two bursts (again we emphasise that the evidence for a soft excess with a thermal spectrum in GRB050126 is marginal at best). Some modifications to these models, for example, Comptonisation of the powerlaw tail of the thermal radiation, might produce the observed behaviour.
Our preferred production mechanism for the rapidly decaying X-ray light-curves is through internal or external shocks (see e.g. Zhang et al. 2005, for a thorough review of the theoretical implications of X-ray afterglow light-curves). We discuss each of these possibilities in detail below.
One possible explanation for the steeply falling X-ray light-curve at early
times is a high degree of angular fluctuation in the relativistic outflow
(Kumar & Piran 2000) or a mini-jet (Yamazaki et al. 2004). If the angular
size of the high energy density regions, or "bright spots'', in the blast wave
is less than
,
the early X-ray light-curve will decline as
t-p, as in a spreading jet case, and the spectrum is given by
when the X-ray band is above the cooling frequency;
is
the Lorentz factor of the jet. For GRB050126 this provides a reasonable fit
to the early X-ray light-curve:
,
and
.
However, for the steeply falling part of the X-ray
light-curve of GRB050219A
and
,
are
inconsistent with this picture (Table 5). When the bright region along our
line of sight spreads and merges with other bright regions the subsequent
light-curve decline is the same as in the standard external forward shock
model, i.e.,
.
A possible weakness of this model is that the
probability of a random observer line of sight passing through a bright region
is smaller than the probability of that passing through the darker,
inter-bright, regions. We should therefore see many more X-ray light-curves
with
at early times, or even
,
a conclusion which
is not supported by the data. However, it is possible that the dark regions
are very faint in
-rays and therefore do not trigger the
BAT.
A rapidly falling X-ray light-curve could also arise if the source activity
ends abruptly, as might be expected in the internal shock or in the reverse
shock heated GRB ejecta. In this situation the observed flux will not drop
suddenly but will have a non-zero value for some period of time as the
observer will continue to receive radiation from those parts of the
relativistic source that lie at angles ()
greater than
with respect to the observers line-of-sight, the so-called "curvature
effect'' (see e.g. Kumar & Panaitescu 2000; Dermer 2004; Fan & Wei
2005). For the simplest case of a uniform source the observed radiation in a
fixed observer energy band will decline with time as
;
the
observed spectrum is
(Kumar & Panaitescu 2000). The values
of
and
for the steeply falling part of the X-ray light-curve
for GRB 050219A are compatible with this expectation. However, if the source
for X-rays is the same as the
-ray burst photons, which is the most
natural explanation in this model, then we expect the spectrum during the
X-ray afterglow to be the same as during the
-ray burst. This
requirement is violated for both of the bursts. The emission from
from the
-ray source provides a lower limit to
the flux we must detect at 5 min in the X-ray band. This limit is also
violated for GRB050219A, suggesting that the comoving energy flux for the
-ray source is decreasing with increasing
.
In this case the
spectrum at
is likely to be softer than we see during the
burst, and the inconsistency between spectra during the
-ray burst and
the X-ray afterglow could be resolved. In this scenario the rapidly falling
X-ray light-curve is from the same source as the
-ray burst, with the
forward shock emission dominating after a few hundred seconds.
A rapidly falling X-ray light-curve is also expected from the reverse shock
heated ejecta. The synchrotron emission from the reverse shock is thought
usually to peak in the infrared or optical band (Mészáros & Rees
1993; Panaitescu et al. 1998; Sari & Piran 1999), and the optical light-curve
after the deceleration time decays as
.
However, the optical
synchrotron photons when inverse Compton scattered in the ejecta, may emerge
in the X-ray band. The inverse Compton light-curve declines faster than the
synchrotron light-curve by a factor of
;
where
is the optical depth of the
ejecta to Thomson scattering, and
for
.
Thus, the inverse Compton X-ray light-curve decline is
expected to be
which is consistent with the steeply declining
early X-ray observations for these two bursts. The optical depth of the
ejecta at deceleration is
,
where
is the number of
pairs per proton, R is
the deceleration radius, and a numerical subscript x means the variable
divided by 10x. The optical flux at deceleration is larger than the X-ray
flux by a factor
and violates the upper limit on the optical
flux from these bursts unless
.
If the -rays are generated through internal shocks, we expect the
ejecta to undergo adiabatic expansion and cool down with time once shell
collisions have ended. As time goes by, the adiabatically expanding shells
will produce radiation that is shifted to lower and lower energies, and could
ultimately be responsible for the early rapidly declining X-ray light-curve we
observe for these two bursts. The influence of a magnetic field could enhance
this possibility. A tangled magnetic field in the ejecta decreases with
radius as r-2, and the electron thermal energy decreases as
r-1. Since the Lorentz factor of the shell is not changing with time,
,
and the flux in a fixed observer band above the peak of the
spectrum, decays as
where
,
and
is the
spectral index. For a transverse magnetic field in the ejecta,
,
and the light-curve in a fixed observer band decays as
when the burst energy is carried by matter, or
when the magnetic field dominates the energy in the outflow (Mészáros
& Rees 1999). We note that
can be no larger than
,
if
the shells are homogeneous in the angular direction, because radiation from
will always contribute to the observed flux.
For ,
as is the case for both GRB050126 and GRB050219A, the high
emission dominates when the magnetic field in the shock heated ejecta
is randomly oriented. In the other two cases considered above, high
emission dominates when
and
respectively. The
early X-ray spectral indices for GRB050126 and GRB050219A, during the
afterglow phase, were
and
respectively. These
values are significantly larger than the BAT spectral index during the burst
(
,
and
for GRB050126 and GRB050219A respectively)
even when we include the spectral steeping by 1/2 due to electron cooling. If
we assume that toward the end of the burst
increased and reached the
value we observe during the afterglow (as appears to be the case for
GRB050219A), then the above argument suggests that the high-angle emission
dominated the observed flux during the adiabatic expansion of shells in the
internal shock, and
.
Thus, the internal shock model for the
steep X-ray lightcurve has the same characteristic spectral and temporal
features as the model involving high-angle emission in external shocks
described above.
Adopting the host galaxy redshift z of 1.29 for GRB050126 (Berger &
Gonzalez 2005) and a BAT fluence of
erg cm-2we derive an isotropic gamma-ray energy of
erg in the 15-350 keV band (assuming a WMAP
Cosmology of
km s-1 Mpc-1,
,
and
). For GRB050219A there was no
ground-based optical/IR detection and hence no redshift estimate for this
source. However, we can estimate the redshift (with large uncertainty) using
the relationship
(Amati
et al. 2002; Moran et al. 2004). For GRB050219A (
)
we estimate a redshift of
1.94+0.69-0.49, which for a BAT fluence of
erg cm-2 implies an isotropic gamma-ray energy
erg in the 15-350 keV band.
Re-writing the Amati relation (Amati et al. 2002) in terms of the isotropic
energy,
,
and peak energy
,
i.e.
,
(Friedman & Bloom 2005), we
derive a rest-frame
keV for GRB050126. Using the
Ghirlanda relation (Ghirlanda et al. 2004; Friedman & Bloom
2005) which describes the dependence of the total energy radiated
in
-rays on
,
where
,
we derive an
erg. This implies a beaming fraction
.
For GRB050219A, we measure a mean rest-frame peak
energy of
keV using our adopted redshift of 1.94, close
to the predicted rest-frame
of 305.6 keV found using the
Ghirlanda relation. Using these estimates for
we derive
erg, and beaming fraction
.
As far as these relationships are applicable to GRBs in general, then both
and
for GRB050126
place it amongst the low-end of the
and
distributions given in Frail et al. (2001), while for GRB050219A
and
lie near the mean of these distributions. We note that the
derived beaming fraction for both sources is a factor of a few larger than the
mean beaming fraction (
)
found by Frail et al. for the same
sample. The predicted break timescales, 11.2 days and 2.4 days for GRB050126
and GRB050219A respectively, both occur later than the last XRT observation
for these sources and are consistent with the non-detection of a jet-break in
their lightcurves.
The early X-ray decay light-curves of GRB050126 and GRB050219A are
characterised by an unusually steep early decline (
), flattening to a more gradual decline on timescales of a few hundred
seconds.
The prompt -ray and the early X-ray afterglow emissions for GRB 050126
& 050219A require at least two, possibly three, distinct mechanisms. The
X-ray lightcurve after the break for these GRBs is produced in the forward
external shock. The early, steeply falling, X-ray lightcurve may be due to
synchrotron self-Comptonisation in the reverse shock. However, in order to
avoid early bright optical emission from these bursts, which was not seen in
the UVOT data, we require the GRB ejecta to be highly enriched with
pairs, and to have a Lorentz factor of at least a few hundred. Furthermore,
it is difficult to see how SSC can account for a steep decay over almost 2
orders of magnitude. An alternate possibility is that the early X-ray
light-curve was produced in the external shock from a jet consisting of narrow
regions (regions of angular size
)
of high energy density.
We suggest that the most plausible explanations for the steep early decay are
either high-latitude (
)
emission from a relativistic jet
arriving at the observer when emission from
has dropped
to zero (the curvature effect) or X-ray flares, indicative of late time
activity of the central engine.
Acknowledgements
MRG would like to thank the anonymous referee for a prompt and thorough reading of this manuscript. This work is supported at the University of Leicester by the Particle Physics and Astronomy Research Council (PPARC), at Penn State by NASA contract NAS5-00136, and in Italy by funding from ASI on contract number I/R/039/04.