GRB 060614
GCN Circular 15560
Subject
GRB 060614: theoretical derivation of the redshift and need for deeper search of the host galaxy
Date
2013-12-02T17:16:04Z (13 years ago)
From
Remo Rufinni at ICRA <ruffini@icra.it>
R. Ruffini, C.L. Bianco, M. Enderli, M. Kovacevic, M. Muccino, A.V. Penacchioni, G.B. Pisani, J.A. Rueda, Y. Wang report:
The late X-ray observations of GRB 060614 (A. M. Parsons et al., GCN 5252) by Swift-XRT clearly evidence a pattern typical of a family of GRBs associated to supernova (SN) following the Induced Gravitational Collapse (IGC) paradigm (1,2). By overlapping the X-ray (0.3-10 keV in rest-frame) luminosity light curve of GRB 060614 with the one of GRB 090618, namely the IGC GRB-SN prototype (3), we estimate a theoretical redshift of z=1.2 (see�Fig. 1�http://www.icranet.org/images/GCN/GRB060614_Fig1.pdf), much higher than z=0.125 of the purported host galaxy (Price et al., GCN 5275; Fugazza et al., GCN 5276). This leads to the explanation of the absence of a visible SN (4,5,6), settling a long lasting dispute of a possible wrong redshift estimation given by a chance superposition of GRB 060614 with its purported host galaxy (7). GRB 060614 is therefore a canonical IGC GRB-SN system. We note that this new value of the redshift still marginally fulfills the Amati relation (see Fig. 2 http://www.icranet.org/images/GCN/GRB060614_Fig2.pdf), and that it is in agreement with z=1.45+/-0.85 given by the Atteia relation (A. Pelangeon & J-L. Atteia, GCN 5265) and with the observational limit of z<1.3 (99.99% CL) given by the combined ultraviolet/optical and X-ray spectra (8).
More optical observations in the GRB field are encouraged for the investigation of the actual host galaxy.
References:
(1) J. A. Rueda & R. Ruffini, ApJLett, 758, L7 (2012)
(2) G. B. Pisani et al., A&A, 552, L5 (2013)
(3) L. Izzo et al., A&A, 548, L5 (2012)
(4) M. Della Valle et al., Nature, 444, 1050-1052 (2006)
(5) J. P. U. Fynbo et al., Nature, 444, 1047-1049 (2006)
(6) A. Gal-Yam et al., Nature, 444, 1053-1055� (2006)
(7) B. E. Cobb et al., ApJ, 651, L85-L88 (2006)
(8) N. Gehrels et al., Nature, 444, 1044-1046 (2006)
GCN Circular 5359
Subject
GRB060614 ATCA Radio Limits
Date
2006-07-28T05:00:54Z (20 years ago)
From
Mark Wieringa at ATNF/CSIRO <Mark.Wieringa@csiro.au>
Diana Londish, Mark H. Wieringa (Australia Telescope National Facility)
and Dale A. Frail (NRAO) report on behalf of a larger collaboration:
"We observed a region covering the Swift burst GRB 060614 (GCN#5252)
using the Australia Telescope Compact Array for two 10 minute scans at
June 24 11:44 UT and 12:29 UT. At frequencies of 4.8 and 8.6 GHz no
emission was detected within a 30" error circle of the OT position
(GCN#5255). The 3-sigma detection limits are 0.9 mJy at both
frequencies. Beam size was 2.6"x20" and 1.5"x11" at 4.8 and 8.6 GHz
respectively"
The Australia Telescope Compact Array is part of the Australia Telescope
which is funded by the Commonwealth of Australia for operation as a
National Facility managed by CSIRO.
GCN Circular 5286
Subject
GRB060614: Possible SN Bump in UVOT U Band Light Curve
Date
2006-07-07T22:44:25Z (20 years ago)
From
Peter Brown at PSU <pbrown@astro.psu.edu>
Peter J. Brown (Penn State) & Stephen T. Holland (NASA/GSFC & USRA)
report on behalf of the Swift UVOT team:
Swift has been continuing to monitor the counterpart to
GRB060614 (Parsons et al. GCN 5252). The UVOT U band light curve,
which was nearly flat during the period of 2-10 days after the
burst at U~22.5 (Holland GCN 5281) has faded to U~24.0 +/- 0.7
(this last point being a 2.7 sigma detection from data taken
between 15-23 days after the burst).
The timing and shape of the plateau and subsequent decay are
very similar to the U band light curve of GRB060218/SN2006aj
(Campana et al. Nature, in press, astro-ph/0603279).
At a redshift of 0.125 (Price, Berger, & Fox GCN 5275),
the possible SN component has an absolute U magnitude about
2 magnitudes fainter than SN2006aj.
We encourage observations at other wavelengths to determine
whether the flattening previously observed (Fynbo et al. GCN 5277;
Cobb & Bailyn GCN 5282) is from the host galaxy or whether a
contributing SN component has since faded.
GCN Circular 5282
Subject
GRB 060614: SMARTS host galaxy observations
Date
2006-06-28T19:09:48Z (20 years ago)
From
Bethany Cobb at Yale U <cobb@astro.yale.edu>
B. E. Cobb and C. D. Bailyn (Yale), part of the larger SMARTS consortium,
report:
Continuing ANDICAM observations (see GCN 5259 for observing details) of
the afterglow of GRB 060614 (GCN 5255, Holland et al.) reveal the host
galaxy of the GRB in the I-band. Preliminary photometry in comparison with
several USNO B1.0 stars reveals that the host galaxy maintains a constant
brightness of I = 21.9 +/- 0.2 magnitudes between observations at
2006-06-19 07:36 UT and 2006-06-27 09:31 UT.
Images from four separate epochs (mid-exposure times of 2006-06-19 07:36
UT, 2006-06-21 07:22 UT, 2006-06-25 09:43 UT and 2006-06-27 09:31 UT) were
combined to produce a single J-band image but the host galaxy of GRB
060614 is not detected in this image down to a limiting magnitude of
J > 20.3+/-0.2 (based on two 2MASS standard stars).
Such a combined image was also produced in the I-band. The centroid of
the host galaxy was then compared to the centroid of the afterglow (imaged
at 2006-06-15 04:16 UT). The centroid of the afterglow appears 0.32" South
and 0.09" East of the host galaxy centroid. At a redshift of z=0.125
(GCN 5276, Fugazza et al.), and assuming H_o=71 km s^-1 Mpc^-1,
Omega_M=0.27 and Omega_Lambda=0.73, the projected distance between the
afterglow and the center of the host galaxy is 0.73 kpc.
Our 2006-06-27 09:31 UT observations correspond to ~13 days post-burst, or
~12 days in the host galaxy rest-frame. By this time post-burst in the
case of several other low-redshift GRBs (GRB 980425/SN 1998bw, GRB
031203/SN 2003lw and GRB 060218/SN 2006aj), the light from the associated
SNe was already clearly visible, yet no brightening is yet observed in the
host galaxy of GRB 060614 (see also GCN 5277, Fynbo et al.). Based on SN
1998bw and SN 2006aj, the expected absolute magnitude for a SN associated
with GRB 060614 would be I~-19.0. There is only a negligible amount of
Galactic extinction toward GRB 060614, so if a SN associated with GRB
060614 is not intrinsically underluminous but is being masked by
extinction, then that extinction must be due to dust in the host galaxy.
If we conservatively assume that half a magnitude increase in the
brightness of the host galaxy would have been detected in our I image,
then the absolute magnitude (uncorrected for absorption) of the SN must be
less than approximately -16.3. If this SN is not intrinsically
significantly dimmer than SN 1998bw or SN 2006aj, then this implies an
extinction in the host galaxy of at least 2.7 magnitudes in I, or A_V=5.6
assuming standard reddening with R_V=3.1.
GCN Circular 5281
Subject
GRB 060614: Detection of a Possible, Late-Time Rebrightening
Date
2006-06-28T15:50:46Z (20 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <sholland@milkyway.gsfc.nasa.gov>
GRB 060614: Detection of a Possible, Late-Time Rebrightening
S. T. Holland (NASA/GSFC & USRA) reports on behalf of the Swift/UVOT
team:
We report the possible detection of a source at the location of
the optical afterglow of GRB 060614((Parsons et al., 2006, GCN
Circular 5252) at approximately 9.5 days after the BAT trigger. The
putative source has a U-band magnitude of U = 22.8 +/- 0.3 (1-sigma
error) and was detected in coadded exposures taken between 7.4 and 12.4
days after the burst. This is a 4.2-sigma detection. Our detection
is approximately 3 mag brighter than the power-law extrapolation of
the early-time U-band decay predicts. We are not able to determine
if this source is a rebrightening of the afterglow of GRB 060614 or
a detection of the host galaxy (Fynbo et al., 2006, GCN Circular 5277).
The value quoted above is not corrected for the expected Galactic
extinction of E_{B-V} = 0.02 (Schlegel et al. 1998).
GCN Circular 5277
Subject
GRB060614: Detection of the host galaxy but no supernova emission
Date
2006-06-22T21:09:09Z (20 years ago)
From
Johan U. Fynbo at U.Copenhagen <jfynbo@astro.ku.dk>
J. P.U. Fynbo, C. C. Thoene, B. L. Jensen, J. Hjorth,
J. Sollerman, D. Watson, D. Xu (DARK Cosmology Centre), J.-E. Ovaldsen
(Oslo University), U. G. Joergensen, T. Hinse, K. Woller
(NBI Copenhagen) report:
We have obtained further imaging of the optical afterglow of GRB060614
(GCN 5252) with the Danish 1.54m telescope and DFOSC on La Silla in the
R-band at June 19-21. The afterglow has flattened from the power-law
decay reported by Thoene et al. (GCN 5272). Also, the source is clearly
resolved in the latest images. Hence, the host galaxy is most likely now
contributing most of the detected flux. There is not yet any sign of
an emerging supernova. Given the low redshift of GRB060614 (GCN 5275,
GCN 5276) we can conclude that if there is a supernova associated with
GRB060614 it is either intrinsically about 2 magnitudes fainter than
SN2006aj (associated with GRB060218) at a similar time or there is
substantial dust absorption along the line of sigth to the afterglow.
A plot of the data and fit is available at:
http://www.astro.ku.dk/~brian_j/grb/grb060614/
GCN Circular 5276
Subject
GRB 060614: redshift confirmation
Date
2006-06-21T17:21:33Z (20 years ago)
From
Daniele Malesani at SISSA-ISAS,Trieste,Italy <malesani@sissa.it>
D. Fugazza (INAF/OABr), D. Malesani (SISSA), P. Romano, G. Tagliaferri,
S. Covino (INAF/OABr), G. Chincarini (INAF/OABr & Univ. Milano-Bicocca),
M. Della Valle (INAF/OAA), F. Fiore, & L. Stella (INAF/OAR), report on
behalf of the MISTICI collaboration:
We observed the afterglow of GRB 060614 (Parsons et al., GCN 5252;
Mangano et al., GCN 5254; Brown et al., GCN 5262) with VLT+FORS2. A
spectrum was taken with the grism 300V (resolution ~10 A, wavelength
coverage 4500-9500 A). The total exposure time was 50 min, with mean
time Jun 21.365 UT.
Based on the identification of several emission lines, among which
Halpha, weak Hbeta, [OIII] 4959, [OIII] 5007, we confirm the redshift
z=0.125 reported by Price et al. (GCN 5275).
We acknowledge the excellent support from the ESO staff, in particular
Riccardo Scarpa.
This message can be cited.
GCN Circular 5275
Subject
GRB 060614: Redshift
Date
2006-06-20T02:56:46Z (20 years ago)
From
Paul Price at IfA,UH <price@ifa.hawaii.edu>
P.A. Price (IfA, Hawaii), E. Berger (OCIW) and D.B. Fox (Penn. State)
report on behalf of a larger collaboration:
We observed the afterglow of GRB 060614 (GCN #5254) with the Gemini
South telescope + GMOS. Our observations consisted of 4x1800 sec
exposures with the R400 grating and 1 arcsec slit, commencing at June
19.3 UTC. In each image we identify a single emission line at 7388A
superposed on a continuum emission with no apparent absorption
features. If this line is due to [O II], the redshift is z = 0.98.
However, there is a hint of a line at 5634A which suggests that the line
is actually due to Halpha at z = 0.13.
In addition to the bright emission line due to the GRB host galaxy,
there is a brighter emission line at the same wavelength from the galaxy
17 arcsec North of the GRB. A spectrum from the Magellan telescope
reveals the presence of the [N II] doublet flanking the Halpha line for
this galaxy, with a secure redshift of z = 0.125. Based on the
identical wavelength of the lines, the two galaxies are likely related,
at a redshift of z = 0.125; in this case, the separation in the plane of
the sky is 38 kpc.
Using the fluence of 2.17 x 10^-5 erg/cm^2 (GCN #5254), a redshift of z
= 0.125 corresponds to an isotropic energy release of Eiso = 8.4 x 10^50
erg.
We thank the Gemini South observing team for obtaining these
observations.
GCN Circular 5272
Subject
GRB060614: Optical observations
Date
2006-06-18T14:41:30Z (20 years ago)
From
Johan U. Fynbo at U.Copenhagen <jfynbo@astro.ku.dk>
Christina C. Thoene, Johan P.U. Fynbo, Brian L. Jensen, J. Hjorth, D. Xu
(DARK Cosmology Centre), Uffe G. Joergensen, Kristian Woller
(NBI Copenhagen) report:
We observed the OT of GRB060614 (GCN 5252) with the Danish 1.54m telescope and
DFOSC on La Silla in the R-band at several epochs on June 15-18. A fit to our
data leads to a powerlaw decay with a temporal decay index of 1.50. Compared to
other data reported in the GCNs is seems that the afterglow in the R-band had a rising
lightcurve during the first about 12 hours after the burst and then started the
more regular powerlaw decay. In this way the burst qualitatively resemples
GRB970508 (Pedersen et al. 1998, ApJ 496, 311).
A plot of the data and fit is available at:
http://www.astro.ku.dk/~brian_j/grb/grb060614/
GCN Circular 5271
Subject
GRB 060614: spectroscopy
Date
2006-06-17T21:28:58Z (20 years ago)
From
Daniele Malesani at SISSA-ISAS,Trieste,Italy <malesani@sissa.it>
D. Fugazza (INAF/OABr), M. Della Valle (INAF/OAA), D. Malesani (SISSA),
P. Romano (INAF/OABr), F. Fiore (INAF/OAR), S. Covino (INAF/OABr), G.
Tagliaferri (INAF/OABr), G. Chincarini (Univ. Milano-Bicocca), P.
D'Avanzo (INAF/OABr & Univ. Insubria), S. Piranomonte (INAF/OAR), and L.
Stella (INAF/OAR) report on behalf of the MISTICI collaboration:
We observed the afterglow of GRB 060614 (Parsons et al., GCN 5252;
Mangano et al., GCN 5254; Brown et al., GCN 5262) with the ESO-VLT UT1
and UT2 equipped with FORS2 and FORS1, respectively. Spectra were taken
around Jun 15.416 and Jun 16.313 UT (0.88 and 1.78 days after the burst,
respectively). Despite the bright, closeby Moon, both spectra have a
good signal-to-noise ratio, and cover the wavelenght range 4500-9500 A.
We detect no significant features, neither in absorption nor in
emission. On Jun 15.4, the continuum is well described by a power law
with spectral index beta=0.60 (F_nu propto nu^-beta) in the range
5000-9000 A (where the flux calibration is solid).
The lack of emission features may suggest that the host galaxy is
relatively faint with respect to the afterglow (which had R~20.8 at the
second epoch). For comparison, the spectra of the lowest-redshift GRBs
(e.g. GRB 031203 and GRB 060218) revealed already in the earliest stages
the nebular emission lines from the galaxy. Our observations, therefore,
may imply a redshift larger than ~0.1.
We acknowledge significant support from the VLT staff.
This message can be cited.
GCN Circular 5265
Subject
GRB 060614: pseudo-z from spectral parameters of the prompt emission
Date
2006-06-16T15:01:22Z (20 years ago)
From
Jean-Luc Atteia at Lab d Astrophys.,OMP,Toulouse <atteia@ast.obs-mip.fr>
A. Pelangeon & J-L. Atteia (LATT-OMP) report:
We have used the spectral parameters of GRB 060614
provided by Golenetskii et al. (GCNC 5264) to
compute the spectral pseudo-redshift** of this burst
detected by SWIFT-BAT (Parsons et al., GCNC 5252).
We find a pseudo-redshift pz= 1.45 +/- 0.85 (90% error)
This is a typical value for a GRB.
** cf. http://www.ast.obs-mip.fr/grb/pz
GCN Circular 5264
Subject
Konus-Wind observation of GRB 060614
Date
2006-06-16T13:21:45Z (20 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline on behalf of the Konus-Wind team report:
The long GRB 060614 (Swift-BAT trigger #214805;
Parsons et al., GCN 5252; Barthelmy et al., GCN 5256)
triggered Konus-Wind at T0=45831.590 s UT (12:43:51.590).
The Konus-Wind light shows an intense multipeaked
initial pulse with a duration of ~6 sec,
followed by a weaker softer highly variable emission
seen up to T-T0 ~110 sec.
The spectrum of the initial intense pulse
(accumulated from T-T0=0 to T-T0=8.448 sec)
can be fitted (in the 20 keV - 2 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ E^(-alpha) * exp(-(2-alpha)*E/Ep)
with alpha = 1.57(-0.14, +0.12)
and Ep = 302(-85, +214) keV (chi2 = 73/59 dof).
The fluence of this part is 8.19(-2.52, +0.56)x10^-6 erg/cm2
(in the 20 keV - 2 MeV range).
The spectrum of the remaining part of the burst
(accumulated from T-T0=8.448 to T-T0=106.752 sec)
can be fitted (in the 20 keV - 1 MeV range)
by a simple power law with photon index
2.13 +/- 0.05 (chi2 = 63/49 dof).
The fluence of this part is 3.27(-0.23,+0.17)x10^-5 erg/cm2
(in the 20 keV - 2 MeV range).
We note that because the derived photon index is ~2,
this fluence value is very sensitive to the upper boundary
of the energy range.
The burst total fluence is 4.09(-0.34, +0.18)x10^-5 erg/cm2
and peak flux on 64-ms time scale measured from T-T0=0.032 sec
4.50(-1.53, +0.72)x10^-6 erg/cm2/sec
(both in the 20 keV - 2 MeV energy range).
All the quoted errors are at the 90% confidence level.
The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB060614_T45831/
GCN Circular 5262
Subject
The Unusually Long-Lived Afterglow of GRB 060614
Date
2006-06-15T17:31:08Z (20 years ago)
From
Peter Brown at PSU <pbrown@astro.psu.edu>
The Unusually Long-Lived Afterglow of GRB 060614
P. J. Brown (Penn State), S. T. Holland (NASA/GSFC & USRA),
V. Mangano (INAF-IASFPA), A. M. Parsons (NASA/GSFC),
& N. Gehrels (NASA/GSFC) report on behalf of the Swift Team:
Swift/UVOT observations of the optical afterglow of
GRB 060614 (trigger=214805; Parsons et al. GCN 5252) show
that the V-band light from the afterglow remains approximately
constant at V ~ 19.8 until at least 80,000 s after the
BAT trigger (the latest data presently available). Similar
behaviour is seen in the B-, U-, and UVW1-bands.
There is weak evidence that the UVM2 and UVW2
fluxes decrease after approximately 10,000 s. The UV-optical
colors are similar to GRB060218/SN2006aj, whose shock breakout
peaked at about 40,000 s in the UV and optical and then
began fading before being overtaken by the rising SN
(Campana et al. Nature, in press, astro-ph/0603279).
Though we do not see as prominent of a rise in the UVOT
data for GRB060614, other observers have noted rising and
fading in the R band (Schmidt, Peterson, & Lewis GCN 5258;
French et al. GCN 5257), and Malesani et al. (GCN 5261) have
also noted the similarity to GRB060218.
The BAT lightcurve of GRB 060614 (Barthelmy et al. GCN 5256)
shows a hard, bright initial flare followed by softer,
extended prompt emission. The T90 duration of the prompt
emission was 108 s. The prompt fluence was the greatest
of all Swifts burst that have been located by the BAT.
The X-ray light curve (Mangano et al. GCN 5254) was
unusually bright and decayed rapidly with a strong hard to
soft evolution. This was followed by an extended period
of near-constant emission, that shows evidence for small-scale
flares, out to approximately 70,000 s. The hardness ratio of
the flat part of the light curve is nearly constant, and the
power law fit of the spectrum gives a standard afterglow
photon index of 1.8 with no absorption in excess the
Galactic N_H.
In light of the peculiar characteristics observed by all
three Swift instruments and ground based observers,
we encourage further observations of this unusual afterglow.
GCN Circular 5261
Subject
GRB 060614: optical observations
Date
2006-06-15T16:22:59Z (20 years ago)
From
Daniele Malesani at SISSA-ISAS,Trieste,Italy <malesani@sissa.it>
D. Malesani (SISSA), S. Covino, S. Campana, D. Fugazza, G. Tagliaferri
(INAF/OABr), G. Chincarini (Univ. Milano-Bicocca), and L. Stella
(INAF/OAR), report on behalf of the MISTICI collaboration:
We have observed the afterglow of GRB 060614 (Parsons et al., GCN 5252)
with the ESO VLT-UT1 equipped with the FORS2 instrument.
The optical afterglow is well detected in the R filter, and shows a
dimming by 0.45+-0.03 mag between 14.4 and 21.6 hr after the GRB.
Assuming a power-law decay, this corresponds to a decay slope alpha ~ 1,
consistent with what found by French et al. (GCN 5257). Compared with
several nearby USNO-B1 stars (R1 magnitudes), the afterglow has R~19.3
on Jun 14.12892, with a calibration uncertainty of ~0.2 mag.
We note an overall similarity between the early optical light curves of
GRB 060614 and GRB 060218 (Campana et al., astro-ph/0603279), both
presenting a maximum ~0.5 d after the burst. GRB 060614 is however
peaking earlier. We encourage further follow-up of this interesting event.
We acknowledge excellent support from the ESO staff at Paranal, in
particular Rachel Gilmour and Leonardo Vanzi.
GCN Circular 5259
Subject
GRB 060614, SMARTS optical/IR afterglow observation
Date
2006-06-15T15:51:23Z (20 years ago)
From
Bethany Cobb at Yale U <cobb@astro.yale.edu>
B. E. Cobb (Yale), part of the larger SMARTS consortium, reports:
Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 060614
(GCN 5252, Parsons et al.) with a mid-exposure time of
2006-06-15 04:16 UT (~15.5 hours post-burst).
Total summed exposure times for each observation amounted
to 36 minutes in I and 30 minutes in J.
The afterglow of GRB 060614 (GCN 5255, Holland et al.) is visible in
each combine image. The preliminary magnitudes reported below were
calibrated using several USNO-B1.0 stars in the I-band and three
2MASS standards in J.
time
post-burst I magnitude J magnitude
------------------------------------------------------
15.5 hours 18.9 +/- 0.1 18.2 +/- 0.1
Given that the afterglow was also reported to have an R magnitude
of ~19 at approximately 5.8 and 7.1 hours post-burst (GCN 5258, Schmidt et
al. & GCN 5257, French et al.), it is clear that the behavior of this
afterglow continues to deviate from a typical smoothly decaying
power-law.
GCN Circular 5258
Subject
GRB060614: SSO 1m observations
Date
2006-06-15T07:26:06Z (20 years ago)
From
Brian Schmidt at RSAA, ANU (MSSSO) <brian@mso.anu.edu.au>
Brian Schmidt, Bruce Peterson, and Karen Lewis (RSAA, The Australian National University) report
"The 1m telescope, located at Siding Spring Observatory,
observed the SWIFT error box for GRB 060614 (Parsons et al. GCN 5252, Mangano et al GCN 5254, Holland et al GCN 5255, Barthelmy et al GCN 5256) starting 20 minutes after burst trigger. Our photometry shows the OT rising in brightness from R=20.2 to R=18.8 in the 5 hours following the burst. Observations presented below are referenced to UCAC2 star of R=15.74 located at RA=21:23:31.573, DEC=-53:02:21.528 J2000.0
UT + 2006Jun14 R err
===============================
0.5483 20.2 (0.3)
0.5525 19.9 (0.2)
0.5566 19.9 (0.2)
0.5607 19.9 (0.2)
0.6017 19.1 (0.1)
0.6492 19.2 (0.1)
0.6912 19.1 (0.1)
0.7272 19.0 (0.1)
0.7731 18.8 (0.1)
GCN Circular 5257
Subject
GRB060614: Watcher observation
Date
2006-06-14T22:32:48Z (20 years ago)
Edited On
2024-11-18T09:45:08Z (2 years ago)
From
Martin Jelinek at Inst.Astrophys.Andalucia,Granada <mates@iaa.es>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
John French, Garry Melady, Lorraine Hanlon (UCD Dublin)
Martin Jelínek (IAA CSIC Granada)
and Petr Kubánek (ISDC Versoix, ASU AV CR Ondrejov)
on behalf of the Watcher Collaboration
"The Watcher 0.4m telescope, located in Boyden Observatory,
South Africa, observed the SWIFT error box for GRB 060614
(Parsons et al. GCN 5252, Mangano et al GCN 5254, Holland et
al GCN 5255, Barthelmy et al GCN 5256).
We detected the object quoted by Parsons et al. (GCN 5252) and
estimated its brightness as R=19.0+-0.3 on the 20min image
obtained at 20:50UT (ie. 7.1h after the GRB). Further we
observe fading with a power law decay index of ~-1.0.
We encourage spectroscopic observations of this object.
This message is quotable".
GCN Circular 5256
Subject
GRB 060614: Swift-BAT refined analysis
Date
2006-06-14T20:10:49Z (20 years ago)
From
Hans Krimm at NASA-GSFC <krimm@milkyway.gsfc.nasa.gov>
S. Barthelmy (GSFC), L. Barbier (GSFC), J. Cummings (GSFC/UMD),
E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (BYU-Idaho),
H. Krimm (GSFC/USRA), M. Koss (GSFC/UMD),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/ORAU), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), on behalf of the Swift-BAT team:
Using the data set from T-120 s to T+180 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 060614 (trigger #214805)
(Parsons et al 2006, GCN 5252). The BAT ground-calculated position is
(RA,Dec) = 320.88, -53.035 { 21h 23m 31.8s , -53d 02' 04.4" }
[deg; J2000]+-1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 16%.
The BAT mask-weighted light curve shows an unusual multi-peaked burst
structure that begins with an initial bright, ~ 6 second wide peak
followed by a set of 5 fainter and somewhat softer peaks that increase
in intensity. After about T+45s, the light curve shows a smooth slope
down to the baseline level for a total duration of T90 (15-350 keV) =
102 +/- 5 sec.
The power law index of the time-averaged spectrum is 2.13 +- 0.04. The
fluence in the 15-150 keV band is 2.17+- 0.04 x 10^-5 erg/cm2. The
1-sec peak photon flux measured from T - 1.3 sec in the 15-150 keV band
is 11.6 +- 0.7 ph/cm2/sec. All the quoted errors are at the 90%
confidence level.
GCN Circular 5255
Subject
GRB 060614: Swift/UVOT Observations
Date
2006-06-14T19:16:39Z (20 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <sholland@milkyway.gsfc.nasa.gov>
GRB 060614: Swift/UVOT Observations
S. T. Holland (NASA/GSFC & USRA) reports on behalf of the Swift/UVOT
team:
The Swift/UVOT began observing the field of GRB 060614 at
12:45:29 on 2006-06-14, 101 s after the BAT trigger (Parsons et al.,
GCN Circular 5252). An optical counterpart was detected in the White
filter (160-650 nm) at a position (RA,Dec) = (21:23:32.08,
-53:01:36.2) (J2000) with a 90% confidence interval of 0.56
arcsec. The optical afterglow was detected in the White, V, B, U,
UVW1, UVM2, and UVW2 filters. The detection in all of the UVOT bands
suggests that the redshift is less than approximately 1.1.
The photometry results are given for the UVOT filters below:
Filter T_mid(s) Exposure(s) Mag Err
V 5753 189 19.54 0.30
B 5143 196 19.91 0.21
U 4937 193 18.81 0.14
UVW1 4730 189 18.35 0.17
UVM2 5959 193 18.06 0.23
UVW2 5552 195 18.26 0.17
White 147 92 18.30 0.14
The values quoted above are not corrected for the expected Galactic
extinction of E_{B-V}=0.02 (Schlegel et al. 1998).
/
\
/
GCN Circular 5254
Subject
GRB060614: Swift-XRT refined analysis
Date
2006-06-14T18:31:49Z (20 years ago)
From
Vanessa Mangano at INAF-IASFPA <vanessa@ifc.inaf.it>
V. Mangano, V. La Parola, E. Troja, G. Cusumano,
T. Mineo (INAF-IASFPA), A. Parsons (GSFC), J. Kennea (PSU)
on behalf of the Swift-XRT team
We have analyzed the first two orbits of data of GRB060614
(Parsons et al 2006, GCN 5252).
The XRT data set consists of 370 s exposure in Windowed
Timing (WT) in the first orbit followed by 2.1 ks exposure
in Photon Counting (PC) mode in the second orbit.
The refined position of the source is
RA (2000) = 21h 23m 32.00s
Dec (2000) = -53d 01' 39.4"
with an uncertainty of 3.7 arcsec (90% containment).
This position is 7.7 arcsec from the on board
XRT position, 3.5 arcsec from the UVOT afterglow
position and 51.7 arcsec from the BAT position
(Parsons et al. 2006, GCN 5252).
The 0.2-10 keV X-ray light curve shows an
exponential decay with a characteristic decay time
of 75 s during all the first orbit, and a nearly
flat behaviour at the level of 0.2 counts/s during
the second orbit that starts 4500 s after the trigger.
The WT light curve is highly piled-up, with an initial
(corrected) count rate of about 1300 counts/s.
From the present data we cannot give any reliable prediction
for the light curve evolution in the next hours. Further
data will be avaliable after the end of the Malidi gap
(2006 June 15, 1:27 UT).
The WT data show strong spectral evolution with time,
with an average photon index of 1.65 +/- 0.04 in the
time interval 90-270 s from the trigger and an
average photon index of 2.95 +/- 0.11 in the time
interval 270-460 s. WT spectra show evidence of
absorption at the level of (1.3 +/- 0.3)e21 cm^-2,
in excess with respect to the Galactic N_H of 3.e20 cm^-2.
The PC spectrum extracted from the second orbit of data
is well fitted by an absorbed power law with photon index
1.8 +/- 0.2 and N_H consistent with the Galactic value.
The average 0.2-10 keV unabsorbed flux during the
second orbit is 9.3e-12 erg cm^-2 s^-1.
This Circular is an official product of the Swift XRT Team.
GCN Circular 5252
Subject
GRB 060614: Swift detection of a burst with a bright optical and X-ray counterpart
Date
2006-06-14T13:04:09Z (20 years ago)
From
Ann M. Parsons at NASA/GSFC/Swift <parsons@milkyway.gsfc.nasa.gov>
A. M. Parsons (GSFC), J. R. Cummings (NASA/ORAU),
N. Gehrels (NASA/GSFC), M. R. Goad (U Leicester), C. Gronwall (PSU),
S. T. Holland (GSFC/USRA), J. A. Kennea (PSU),
V. La Parola (INAF-IASFPA), V. Mangano (INAF-IASFPA),
F. E. Marshall (NASA/GSFC), K. M. McLean (LANL/UTD), C. Pagani (PSU),
D. M. Palmer (LANL), P. Romano (INAF-OAB) and
M. Stamatikos (NASA/ORAU) report on behalf of the Swift Team:
At 12:43:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 060614 (trigger=214805). Swift slewed immediately to
the burst. The BAT on-board calculated location is
RA,Dec 320.862, -53.034 {21h 23m 27s, -53d 02' 02"} (J2000)
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a duration of about 120 sec, with initial bright sharp
peak and a long, also bright, somewhat softer extended peak. The peak
count rate was ~10000 counts/sec (15-350 keV), at ~2 sec after the
trigger.
The XRT began observing the field at 12:45:19 UT, 91 seconds after the
BAT trigger. XRT found a very bright, fading and uncatalogued X-ray source
located at RA(J2000) = 21h 23m 32.3s, Dec(J2000) = -53d 01' 32.1", with an
estimated uncertainty of 5.0 arcseconds (90% confidence radius).
This location is 58 arcseconds from the BAT on-board position, within
the BAT error circle. The initial flux in the 0.1s image was
6.0e-08 erg/cm2/s (0.2-10 keV).
UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 102 seconds after the BAT trigger. There
is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image
at (RA,DEC) (J2000) of (320.8839,-53.0267) or
(21h23m32.14s,-53o01'36.1") with a 1-sigma error radius of about 0.5
arc sec. This position is 4.3 arc sec. from the center of the XRT
error circle. The estimated magnitude is 18.4 with a 1-sigma error of
about 0.5 mag. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.02.