Issue |
A&A
Volume 508, Number 1, December II 2009
|
|
---|---|---|
Page(s) | 173 - 180 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200912788 | |
Published online | 15 October 2009 |
A&A 508, 173-180 (2009)
Extremely energetic Fermi gamma-ray bursts obey spectral energy correlations
L. Amati1 - F. Frontera1,2 - C. Guidorzi2
1 - INAF - IASF Bologna, via P. Gobetti 101, 40129 Bologna, Italy
2 - University of Ferrara, Department of Physics, via Saragat 1, 44100
Ferrara (FE), Italy
Received 29 June 2009 / Accepted 10 September 2009
Abstract
The origin, reliability, and dispersion of the
-
and other
spectral energy correlations is a highly debated topic in
GRB astrophysics. GRB 080916C, with its enormous
radiated energy (
1055 erg in the
1 keV-10 GeV cosmological rest-frame energy band) and
its intense GeV emission measured by Fermi,
provides a unique opportunity to investigate this issue.
In our analysis, we also study another extremely energetic
event, GRB 090323, more recently detected and localized by Fermi/LAT,
whose radiated energy is comparable to that of GRB 080916C in
the 1 keV-10 MeV energy range. Based on Konus/WIND
and Fermi spectral measurements,
we find that both events are fully consistent with the
-
correlation
(updated to include 95 GRBs with the data available as of
April 2009), thus further confirming and
extending it, and providing evidence against a possible
flattening or increased dispersion at very high energies.
This also suggests that the physics behind the emission of peculiarly
bright and hard GRBs is the same as for medium-bright and soft-weak
long events (XRFs), which all follow the correlation.
In addition, we find that the normalization of the correlation obtained
by considering these two GRBs and the other long ones for which
was measured to high accuracy by the Fermi/GBM are
fully consistent with those obtained by other instruments (e.g., BeppoSAX,
Swift, Konus/WIND), thus
indicating that the correlation is not affected significantly by ``data
truncation'' because of detector thresholds and limited energy bands.
A Fermi/GBM accurate estimate of the peak
energy of a
very bright and hard short GRB with a measured redshift,
GRB 090510, provides robust evidence that short GRBs do not
follow the
-
correlation
and that the
-
plane
can be used to discriminate between, and understand, the two classes of
events. Prompted by the extension of the spectrum of
GRB 080916C to several GeV (in the
cosmological rest-frame) without any excess or cut-off, we also
investigated whether the evaluation of
in the commonly adopted 1 keV-10 MeV energy band may
bias the
-
correlation
and/or contribute to its scatter.
By computing
from 1 keV to 10 GeV, the slope of the correlation
becomes slightly flatter, while its dispersion does not change
significantly. Finally, we find that GRB 080916C is also
consistent with most of the other spectral energy correlations derived
from it, with the possible exception of the
-
-
correlation.
Key words: gamma rays: bursts - gamma rays: observations
1 Introduction
Despite the enormous amount of observational and theoretical advances,
several open issues cloud
our understanding of the GRB phenomenon. Among these, the
correlation between the photon energy at which the
spectrum
(in the cosmological rest-frame) of the prompt emission
reaches its peak,
,
and the total radiated energy computed by assuming isotropic emission,
,
in long GRBs remains one of the most debated and intriguing. Discovered
in 2002 based on a sample of BeppoSAX GRBs with known redshift (Amati et al. 2002), the
-
correlation
was then confirmed and shown to hold for all GRBs, soft or bright, with
known z and constrained values of
and fluence, with the only exception of the peculiar sub-energetic
GRB 980425 (Amati
et al. 2007; Amati 2006a). This correlation was
also proposed by Lloyd et al.
(2000) based on the analysis of a sample of bright BATSE GRBs
without measured redshift. The implications of this observational
evidence involve the physics and geometry of the prompt emission, the
identification and understanding of different subclasses of GRBs (e.g.,
short, sub-energetic), and the use of GRBs to estimate cosmological
parameters (Amati
et al. 2008; Ghirlanda et al. 2006;
Amati 2006a;
Amati
et al. 2007).
Thus, testing the -
correlation
and the other ``spectral energy'' correlations derived
from it, understanding their origin, and investigating their
dispersion and the existence of possible outliers are relevant issues
for GRB physics and cosmology. These issues can be approached in three
ways: a) by adding new data for GRBs with known redshift
detected by different instruments, each one having its own sensitivity
and spectral response and thus covering different regions of the
- fluence
plane (Ghirlanda
et al. 2008; Amati 2006a,b); b) by verifying its
validity with large samples of GRBs with no measured redshift (Ghirlanda
et al. 2005a,2008); and c) by
studying the behaviour in the
-
plane
of peculiar GRBs (Amati et al.
2007). Selection effects on this correlation have also been
investigated with contrasting results (Ghirlanda et al. 2005a;
Shahmoradi
& Nemiroff 2009; Butler et al. 2009; Ghirlanda
et al. 2008; Band & Preece 2005; Butler
et al. 2007).
In this article, the -
correlation
and its related spectral energy correlations are studied for the most
energetic GRBs yet detected, GRB 080916C (Abdo et al.
2009; Greiner
et al. 2009) and GRB 090323 (van der Horst
2009; Golenetskii
et al. 2009b). In particular, GRB 080916C,
with its enormous energy release, the extended spectrum of its prompt
emission up to tens of GeV without any excess or cut-off, and the
accurate measurements of its spectral parameters provided by Fermi/GBM
and Konus/WIND, provide a unique opportunity to
test the robustness and extension of these correlations and investigate
their properties. We also revise the
-
correlation
by including the newly detected GRBs with known redshift and
,
and compare the estimate of its normalization obtained
by using only GRBs detected by Fermi/GBM with those
estimated by other instruments. Our study is based on published
spectral results by Konus/WIND, Fermi/GBM,
Swift, and on specific data analyses of publicly
available data.
![]() |
Figure 1:
Light curve of the prompt emission of GRB 080916C as measured
by the Fermi/GBM - n3 detector ( |
Open with DEXTER |
2 Observations and data analysis
GRB 080916C was detected by the Fermi/GBM
on 16 September 2008 at 00:12:45 UT as a
long, multi-peak structured GRB of duration T90 66 s
in 50-300 keV (Goldstein
& van der Horst 2008). The light curve of the prompt
emission measured by one of the Fermi/GBM
NaI detectors that triggered the event is shown in
Fig. 1.
The burst was also observed by AGILE (MCAL, SuperAGILE, and ACS),
RHESSI, INTEGRAL (SPI-ACS), Konus/Wind, and
MESSENGER (Hurley et al. 2008).
Remarkably, very high energy photons from GRB 080916C were
detected by Fermi/LAT up to
10 GeV, more than
145 photons having energies of above 100 MeV and
14 photons above 1 GeV (Tajima et al. 2008; Abdo et al.
2009).
Because of the prompt dissemination of the Fermi/LAT
and IPN positions, GRB 080916C was followed-up by Swift
and other ground telescopes, leading to the detection of both the X-ray
and optical fading counterparts. Of particular interest are the
afterglow measurements by Swift/XRT and GROND. The
X-ray afterglow light curve (Fig. 2) shows the canonical
shape: a steep decay followed by a flat decay and than a
steeper power-law decay of index 1.4 and no break-up
until
1.3 Ms
from the GRB onset (Stratta
et al. 2008). The optical afterglow light curve
shows a different behaviour, with strong evidence of a simple power-law
decay (Greiner et al. 2009).
A photometric redshift of 4.35
0.15 was later reported by the GROND team (Greiner
et al. 2009). By combining this value with the
fluence and spectral parameters of the prompt emission provided by Fermi/GBM
and Konus/WIND, 080916C was found to be the most
energetic GRB ever, with an
of
4
1054 erg in the standard
1-10 000 keV cosmological rest-frame energy band.
Moreover, the joint spectral analysis of Fermi/GBM
and LAT data published by the Fermi team (Abdo et al. 2009) showed
that the spectrum extends up to
1-10 GeV without any
excess or cut-off, and that the
computed by integrating up to 10 GeV is as high as
1055 erg.
![]() |
Figure 2:
X-ray afterglow light curve of GRB 080916C measured by the
Swift/XRT in 0.3-10 keV. The continuous line shows
the best-fit double broken power-law; the dashed line shows the triple
broken power-law obtained by fixing the last slope to 2.4 and
corresponding to the 90% c.l. lower limit to |
Open with DEXTER |
More recently, another very bright event, GRB 090323, has been
detected and localized by the Fermi/LAT (Ohno et al. 2009).
Follow-up observations were performed by Swift and
other ground-based facilities, leading to the discovery of X-ray,
optical, and radio counterparts (Harrison et al. 2009; Updike
et al. 2009; Kennea et al. 2009).
A spectroscopic redshift of 3.57 was measured by
Gemini south (Chornock
et al. 2009). Spectral parameters and fluence for
GRB 090323 were provided by both the Fermi/GBM
(van der Horst 2009) and Konus/WIND
(Golenetskii et al.
2009b). Based on the spectrum and fluence measured by Konus/WIND
and the redshift of 3.57 measured by Gemini south, the
value
of this event in the 1-10 000 keV cosmological
rest-frame energy band can be inferred to be
4
1054 erg, thus comparable to that of
GRB 080916C. No refined analysis of the
VHE emission measured by the LAT from this event has been
published.
![]() |
Figure 3:
Location in the |
Open with DEXTER |
In our analysis, we used results published in the above references and
specific data analysis of the public Fermi/GBM and Swift/XRT
data. In particular, for
GRB 080916C we extracted the light curve of each Fermi/GBM
detection unit that triggered the event (n3, n4
and b0) by using the gtbin tool included
in the data reduction and analysis tools
.
The Swift/XRT data of this burst were processed
using the heasoft package (v.6.4). We ran the task
xrtpipeline (v.0.11.6) by applying calibration and standard
filtering and screening criteria
.
Radiated energies and luminosities are computed by assuming a
standard CDM cosmology
with H0=
70 km s-1 Mpc-1,
= 0.27, and
=
0.73. The quoted uncertainties are at 68% c.l., unless stated
otherwise.
Table 1:
The 25 GRBs with known redshift and measured
added to the sample of Amati
et al. (2008) in our analysis of the
-
correlation,
providing a total of 95 GRBs.
3 The
correlation: update and comparison among different instruments
In Fig. 3
(right panel), we show the -
correlation
for long GRBs (short GRBs and the peculiar sub-energetic
GRB 980425 are not included) obtained by adding to the sample
of 70 events of Amati
et al. (2008) 25 more GRBs for which
measurements of the redshift and/or of the
spectral parameters have in the meantime become available
(as of April 2009). As in previous
evaluations,
was
derived in the 1-10 000 keV energy band. The
and
of these events, together with their redshift and relevant references,
are reported in Table 1.
These values and their uncertainties were computed based on published
spectral parameters and fluences, and following the methods and
criteria reported, e.g., in Amati
(2006a) and Amati
et al. (2008). As can be seen, this updated
sample of 95 GRBs is fully consistent with the
-
correlation
and its dispersion as derived by Amati
et al. (2008). This is quantitatively confirmed by
the fit with both
the classical
method
and the adopted maximum likelihood method by Amati
(2006a) and Amati
et al. (2008), which allows us to quantify the
extrinsic scatter in the correlation (
). We obtain a slope of m =
0.57
0.01 and a
of 594, by means of a linear fit to the log(
) versus
log(
) data
points with the
method,
and m = 0.54
0.03 and
=
0.18
0.02 (68% c.l.) with the maximum likelihood method. These
values are fully consistent with those obtained by Amati et al. (2008).
In their study of the selection effects, Butler et al. (2009)
claim that the dispersion and significance of the
-
correlation
in the intrinsic plane is comparable to that of the
- fluence
in the observer plane, and that the normalization of the
-
correlation
depends on the instrument used to detect GRBs. In Fig. 3 (left panel), we
show the distribution of these 95 GRBs in the
- fluence
observer plane. To allow a reliable comparison, the X and
Y scales of this plot cover the same orders of magnitude as
the
-
plane shown in
Fig. 3
(right panel). As can be seen, when we move from the observer
to the intrinsic plane the dispersion the correlation between spectral
peak photon energy and fluence (radiated energy) decreases
significantly (
from
0.31 to
0.18, and
from 3110 to 594), its extension covers more orders of
magnitudes, and its significance increases (Spearman's correlation
coefficient
from
0.75 to
0.88). In
Fig. 4,
we compare the normalization of the
-
correlation
obtained with all the most relevant instruments with that derived by Amati et al. (2008).
As can be seen, no significant (i.e. above
1
)
change is evident. In particular, the
-
correlation
derived using the Swift GRB data for
which, unlike those considered by Butler
et al. (2009),
is
really measured with BAT (from the official Swift team
catalog by Sakamoto et al.
(2008), and/or GCNs) or with broad-band instruments (mainly Konus/WIND),
is fully consistent with that determined with other instruments. The
-
correlation
derived from GRBs detected with Fermi/GBM is fully
consistent with the correlation determined by other instruments with
narrower energy ranges. Given the unprecedented broad energy coverage
of the GBM (from
8 keV
up to more than 30 MeV), the derived
-
correlation
is certainly not affected by biases in the estimate of the spectral
parameters (the so-called ``data truncation'' effect,
see e.g., Lloyd
et al. 2000).
We also tested the effect of redshift on the versus
fluence dependence. Starting from
versus fluence data,
we derived 10 000
-
simulated correlations by
randomly exchanging the z values
among the 95 GRBs, and we computed for each sample the
Spearman's correlation coefficient
between the
and
values
so obtained. We found a
distribution that is fully consistent
with a Gaussian of centroid
0.75,
which is exactly the value obtained for the
versus
fluence correlation in the observer plane, and of dispersion
0.035, extending up to
0.85.
For comparison, the
value
of the true
-
correlation,
as we have seen, is
0.88
which is
3.8
away from that obtained from the simulation and corresponds to a chance
probability of less than 1 over 1000, that the true
-
correlation
is randomly extracted from the simulated ones.
An exhaustive paper devoted to the discussion of the selection
effects affecting the -
correlation
is in preparation.
4 Fermi
highly energetic GRBs in the
plane
Based on Fermi/GBM observations, the fluence of
GRB 080916C in 8 keV-30 MeV was measured to
be 1.9
10-4 erg cm-2
and its time-averaged spectrum in the same energy band can be fit by a
Band function (Band et al. 1993)
with
=
-0.91
0.02,
=
-2.08
0.06, and
=
424
24 keV (van der Horst
& Goldstein 2008). For the
20 keV-10 MeV energy band, the Konus/WIND team
reported a fluence of (1.24
0.17)
10-4 erg cm-2,
a 256-ms peak flux of (1.19
0.30)
10-5 erg cm-2 s-1
and a time-averaged spectrum with
= -1.04
0.06,
=
-2.26
0.3, and
=
505
75 keV (Golenetskii
et al. 2008f).
By taking into account these fluences and spectral parameters,
with their uncertainties, the redshift, with its uncertainty, provided
by GROND, and by integrating the cosmological rest-frame spectrum in
the commonly adopted 1 keV-10 MeV energy band (Amati 2006a;
Amati
et al. 2002), we derive
=
(3.8
0.8)
1054 erg, and
=
2646
566 keV. As can be seen in Fig. 3, these parameters
imply that the location of GRB 080916C in the
-
plane
is very close to the best-fit power-law obtained for a sample of
70 long GRBs considered by Amati
et al. (2008). This confirms that
GRB 080916C follows the
-
correlation
and extends its range of validity along
by a factor of
2.
If GRB 080916C is excluded from the fit to
the correlation, the values of the parameters and their uncertainties
do not change significantly with respect to those reported in the
previous section, which is however the case when the
softest/weakest events are excluded. This confirms that both the
significance and the characterization of the
-
correlation
do not depend on events at the most extreme ranges of the ranges of
and
values.
The spectral analysis performed by Abdo
et al. (2009) indicates that the time-resolved
spectra of this event can be fit with the simple Band function from 8 keV
up to more than 1 GeV. This implies that the
above 10 MeV should not be negligible. Indeed, by extending
the integration up to 10 GeV (cosmological rest-frame) and
using the
value
provided by Fermi/GBM (which, given the extension
of the energy band of this instrument, is expected to be more accurate
than that provided by Konus/WIND), we obtain a
value of
of (1.1
0.2)
1055 erg, which is higher than the
value obtained by integrating up to 10 MeV by a factor
of
2.5.
As can be seen in Fig. 3, for this (enormous)
value of
,
GRB 080916C remains still consistent with the
-
correlation
to within 2
and extends its dynamic range along
by about half an order of magnitude.
![]() |
Figure 4:
Location in the |
Open with DEXTER |
In Fig. 3,
we also show the location in the
-
plane
of data for the other ultra-energetic GRB detected by Fermi,
GRB 090323. For this event, no refined analysis of
the VHE emission measured by the LAT has been published, thus
no reliable extrapolation and integration of the spectrum up to the GeV
range can be made. Hence, we restrict the analysis to the standard
1 keV-10 MeV energy band. In addition, the published
GBM spectral analysis concerns only the first
70 s
of the event (which shows a total duration of
120 s), and thus
these data do not provide a reliable estimate of
and
.
By using the spectral parameters
= -0.96
-0.09+0.12,
=
-2.09
-0.22+0.16,
and
=
416
-73+76 keV,
the fluence of (2.0
0.3)
10-4 erg cm-2
(20 keV-10 MeV) provided by Konus/WIND
(Golenetskii et al.
2009b), and the redshift of 3.57 measured by Gemini
south, we find that
=
(4.1
0.5)
1054 erg and
=
1901
343 keV. These values are very close to those of
GRB 080916C and also make this event fully consistent with the
-
correlation.
This provides additional evidence that the newly discovered class of
extremely energetic GRBs follows the correlation. The detection of more
GRBs with photons at GeV energies (e.g., from Fermi/LAT)
will strengthen this result.
The extension of the spectrum of GRB 080916C supports
the possibility that, at least for a fraction of long GRBs,
the commonly adopted 1 keV-10 MeV cosmological
rest-frame energy band for the computation of
may underestimate this quantity and be a source of systematic errors
and extra-scatter in the
-
correlation.
To test this, we again considered the sample of Amati et al. (2008) in
addition to the 25 GRBs reported in Table 1. For each event,
we re-computed the
value
by extending the integration up to 10 GeV using the
and
values
reported in the literature. For those events without a reported value
of
,
e.g., in the case of a fit with a cut-off power-law, we adopted a Band
function with
.
The fit with the
method
provides m = 0.55
0.01 with a best-fit
of 619, while the maximum likelihood method provides m =
0.51
0.03 and
=
0.18
0.02 (68% c.l.).
We conclude that extending the computation of
up to 10 GeV slightly flattens the slope of the
-
correlation
but does not significantly change its scatter.
Finally, the Fermi/LAT detected and
localized GeV emission from the bright short (0.5 s)
GRB 090510 Ohno &
Pelassa (2009). This event was also detected by AGILE at
energies above 100 MeV (Longo
et al. 2009). By combining the VLT redshift
estimate of z = 0.903 Rau
et al. (2009) and the spectral parameters and
fluence obtained with the Fermi/GBM Guiriec et al. (2009),
the parameters
and
of this event are found to be (4
1)
1052 erg and 8370
760 keV, respectively. With these values, GRB 090510
is located in the
-
plane
significantly above the region populated by long GRBs (Fig. 3, right panel),
helping to confirm that short GRBs do not follow the
-
correlation.
![]() |
Figure 5:
a) Correlation between
|
Open with DEXTER |
5 GRB 080916C and other spectral energy correlations
After the discovery and first studies of the
-
correlation,
it was pointed out that
also correlates with other GRB intensity indicators, such as the peak
luminosity,
,
(Ghirlanda
et al. 2005b; Yonetoku et al. 2004)
or the average luminosity,
,
(Ghirlanda
et al. 2009; Lamb et al. 2004). In
addition, it was found that by including the break time of the
afterglow light curve,
,
either directly (Ghirlanda
et al. 2007; Liang & Zhang 2005; Nava et al.
2006) or by using it to derive the jet opening angle and thus
compute the collimation-corrected radiated energy
(Ghirlanda
et al. 2004; Nava et al. 2006), the
extrinsic scatter decreases significantly. As discussed, e.g.,
by Amati (2008), given the
strong correlation between
,
,
and
,
the two-parameter spectral energy correlations are equivalent. In
addition, in the light of the Swift results
on X-ray afterglow light curves, the measurement of
and its use to derive the jet opening angle are questionable (Ghirlanda
et al. 2007; Campana et al. 2007).
It was also proposed that the inclusion of the ``high signal
timescale'', T0.45,
introduced and used for variability studies, reduces the dispersion in
the
-
correlation (Firmani et al. 2006),
but this property was not confirmed by later studies (Collazzi
& Schaefer 2008; Rossi et al. 2008).
Finally, there is evidence that, at least for a significant fraction of
GRBs, the correlation between
and luminosity also holds for the time-resolved spectra of individual
events (Liang
et al. 2004; Firmani et al. 2008;
Frontera et al., in prep.). Given its extreme
energetics and the good sampling of its optical and X-ray afterglow
light curve, GRB 080916C can also be used to test these
correlations.
For the -
correlation,
the 256 ms peak flux measured by Konus, by
assuming the best-fit model of the time-averaged spectrum, allows us to
infer that
=
(1.9
0.6)
1054 erg s-1.
This value, combined with the
value
of 2646
566 keV
derived above, gives a data point fully consistent with this
correlation (Fig. 5a).
For the
-
-
T0.45 correlation, the
background subtracted 8-1000 keV light curves obtained with
the two (n3 and n4) Fermi/GBM NaI
detectors (see Fig. 1)
allow us to estimate T0.45
(19.5
0.6 s for n3 and 19.2
0.5 s for n4) following the same approach as Rossi et al. (2008). The
result is that GRB 080916C is also consistent with this
correlation (Fig. 5a).
From the time-resolved spectral analysis reported by Abdo et al. (2009), an
accurate estimate of
was obtained. By using these results, we computed the
for each of the corresponding time intervals and reconstructed the
track of GRB 080916C in the
-
plane
(Fig. 5b).
As can be seen, the spectral and luminosity evolution of this
GRB is fully consistent with the
-
correlation,
as typically observed for bright events (Liang et al. 2004; Firmani
et al. 2008; Frontera et al.,
in prep.). The slope of the power-law that best fits the
6 GRB 080916C data points is
0.4, slightly flatter than the
commonly found value of
0.5.
This is mostly due to the data point corresponding to the first time
interval (A) (Fig. 1),
which deviates slightly from the
-
correlation.
For the -
correlation,
no evidence of a jet break
is found either in
the X-ray light curve (see Fig. 2) until the end of
the XRT observations (
1.3 Ms
from the trigger) or in the optical light curve up to the end of the
GROND (Greiner et al. 2009)
observations (
0.5 Ms
from the trigger). A 90% lower limit to the jet break time of
about 0.5 Ms is inferred from the X-ray light curve when
assuming a typical post-break slope of 2.4 (see Fig. 2).
By adopting a lower limit to
of 0.5 Ms, standard assumptions about the conversion
efficiency of the fireball kinetic energy into radiated energy, on the
ISM density and profile, and on the ratio of mass loss rate to
wind velocity (Ghirlanda
et al. 2007; Nava et al. 2006), we
obtain
>
8.8
1051 erg in the case of a homogeneous
circumburst medium, and
>
1.6
1051 erg in the case of a wind medium.
If
>
1 Ms, these values become
>
1.5
1052 erg (homogeneous circumburst
medium),
>
2.4
1051 erg (wind medium). These lower
limits take into account the uncertainty both in
and the GRB redshift. As can be seen in Fig. 5c, the lower limits
to
obtained with
1 Ms are around 1.5-2
from the best-fit function reported by Ghirlanda
et al. (2007), while for
0.5 Ms they are fully consistent with the fit.
Intriguingly, we find that GRB 080916C is a possible
outlier of the -
-
correlation
(Fig. 5d).
Indeed, its deviation from the best-fit power-law (determined by Ghirlanda et al. 2007)
is >
3.5
,
for
>
1 Ms, and more than
2.2
,
for
> 0.5 Ms.
6 Discussion
Prompt emission GRB models are challenged by both the extreme
energetics of GRB 080916C and its spectrum following the
simple Band function without any break or excess up to several tens
of GeVs (in the cosmological rest-frame). For
instance, Abdo et al. (2009)
and Wang et al. (2009)
suggest that the most probable emission mechanism is the standard
non-thermal synchrotron radiation from shock-accelerated electrons
within a fireball of bulk Lorentz factor >
600-1000 (Abdo
et al. 2009; Li 2009; Greiner et al. 2009).
Nevertheless, the lack of a synchrotron self-Compton component cannot
be explained by this scenario, and inverse Compton process in residual
collisions may be needed to explain the time-delayed
GeV photons (Li 2009).
That GRB 080916C is fully consistent with the
-
correlation
(Sect. 4 and Fig. 3)
and most of its related correlations (Fig. 5), provides
additional support to the hypothesis that, despite its huge
isotropic-equivalent radiated energy and the extension to its emission
up to VHE, the physics behind the emission of this event is not unusual
compared to that governing less energetic long GRBs and XRFs. We note
that the
-
correlation
itself can be explained by the non-thermal synchrotron radiation
scenario, e.g., by assuming that the minimum Lorentz factor,
,
and the normalization of the power-law distribution of the radiating
electrons do not vary significantly from burst to burst or when
imposing limits on the slope of the correlation between the fireball
bulk Lorentz factor,
,
and the burst luminosity (Zhang
& Mészáros 2002; Lloyd et al. 2000). The
consistency of time-resolved spectra of GRB 080916C with the
-luminosity
correlation (Fig. 5)
confirms that the prompt emission is dominated by a single emission
mechanism. However, the slight deviation from this correlation of the
peak energy and luminosity measured
during the first time interval (Fig. 5b) may suggest that
during the rise phase of the GRB, the main emission mechanism is still
not fully operating and other mechanisms may play a relevant role.
In turn, the results for GRB 080916C confirm the
robustness of the -
correlation
at least
in the range of intrinsically medium-bright GRBs and, when integrating
the spectrum up
to 10 GeV, extend its range in
by
half an
order of magnitude (Fig. 3).
The flattening of the slope predicted in some scenarios, e.g., the
multiple sub-jet model
by Toma et al. (2005)
or an increase in the dispersion at very high energies is not observed.
The above considerations are also supported by another
extremely energetic GRB 090323 detected by the Fermi/LAT,
which shows
and
values
similar to those of GRB 080916C and is thus also consistent
with the
-
correlation
(Fig. 3).
The measurement by Fermi of the
and GeV emission of the short bright GRB 090510,
combined with a redshift measurement by VLT, provides additional strong
evidence that short GRBs do not follow the correlations that hold for
long GRBs, and that the
-
plane
is a powerful tool for discriminating between the two classes and
understanding their different emission mechanisms and origins.
As a part of our study, we have shown (Sect. 3) that:
i) the distribution of the updated
sample of 95 long GRBs with firm estimates of
and z in the
-
plane
is fully consistent with the slope, normalization, and dispersion
determined for previous samples
(Fig. 3);
ii) moving from the observer frame (
- fluence)
to the intrinsic plane (
-
),
the dispersion in the correlation decreases and its significance
significantly increases (Fig. 3);
iii) if we randomly redistribute the redshift values among the
95 GRBs of the sample, the
versus
distribution
is similar to that of
versus
fluence; iv) not only all Fermi/GBM GRBs
but also all other long GRBs of known redshift (except
GRB 980425) detected with BeppoSAX,
HETE-2, and Swift, follow
-
correlations
that are fully consistent with both each other and the
-
correlation
derived by Amati et al. (2008)
(Fig. 4).
All this evidence conflicts with the conclusions of Butler et al. (2009))
that the -
correlation
is strongly affected by instrumental effects. In addition, since GRBs
detected and localized in different energy bands and by different
instruments all follow the
-
correlation,
the
spectral energy correlations do not appear to be strongly affected by
selection effects introduced in the observational process that lead to
the redshift estimate. An exhaustive analysis of instrumental and
selection effects on the
-
correlation
is underway and will be reported elsewhere.
Following the Band function without any cut-off up to a few
tens of GeVs (in the cosmological rest-frame), the
spectrum of GRB 080916C may suggest that the commonly adopted
1 keV-10 MeV energy band is too narrow for a correct
computation of ,
thus biasing the
-
correlation.
However, our analysis reported in Sect. 4 shows that the
extension of the energy band up to 10 GeV at which
is computed has a marginal impact on the slope and the dispersion of
the correlation, providing support for its robustness.
Finally, the testing of the consistency between data of very
high energy GRBs and both the -
and other
spectral energy correlations (Sect. 5) is important for their
potential use in cosmology (Amati et al. 2008; Ghirlanda
et al. 2006). Because of detector sensitivity
thresholds and possible evolutionary effects, more luminous GRBs are
those more easily detectable at high redshifts (e.g., Amati 2006a). Besides the
-
correlation,
which is fully satisfied by both GRB 080916C and
GRB 090323, the lack of accurate enough long-term monitoring
of the optical afterglow of these events (Kann et al. 2009; Greiner
et al. 2009) prevents a stringent test of
correlations involving the break-time
.
However, we find that GRB 080916C deviates by more than
2.5
from the best-fit function of the
-
-
correlation
(Fig. 5),
suggesting that the dispersion in this correlation either is higher
than understood previously or is not satisfied at very high energies.
This is an important issue, given that, with respect to the
-
correlation,
the
-
-
has the advantage, as for the simple
-
correlation,
of being model independent.
Due to Fermi and AGILE, we expect that the number of these extremely bright GRBs selected on the basis of their GeV emission will increase in the near future, giving us the possibility of improving our understanding of the physics of the prompt emission of GRBs and deriving important clues about the reliability and origin of spectral energy correlations.
We thank Guido Barbiellini and Francesco Longo at(Trieste, Italy) for discussions that prompted this work and Sara Cutini (at ASI/ASDC, Roma, Italy) for useful hints on the reduction of Fermi/GBM data.
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Footnotes
- ... data
- The Fermi/GBM data and analysis tools
are available at ftp://legacy.gsfc.nasa.gov/fermi/;
the Swift/XRT data are available at
http://swift.gsfc.nasa.gov/docs/swift/archive/ - ... tools
- Available at http://fermi.gsfc.nasa.gov/ssc/data/analysis/
- ... criteria
- See http://swift.gsfc.nasa.gov/docs/swift/analysis/
All Tables
Table 1:
The 25 GRBs with known redshift and measured
added to the sample of Amati
et al. (2008) in our analysis of the
-
correlation,
providing a total of 95 GRBs.
All Figures
![]() |
Figure 1:
Light curve of the prompt emission of GRB 080916C as measured
by the Fermi/GBM - n3 detector ( |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
X-ray afterglow light curve of GRB 080916C measured by the
Swift/XRT in 0.3-10 keV. The continuous line shows
the best-fit double broken power-law; the dashed line shows the triple
broken power-law obtained by fixing the last slope to 2.4 and
corresponding to the 90% c.l. lower limit to |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Location in the |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Location in the |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
a) Correlation between
|
Open with DEXTER | |
In the text |
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