Gamma-ray Burst 140330A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

none

Results of Observations

GCN Circular #16048
G. Vianello (Stanford U.), D. Kocevski (NASA/Goddard), and J. Racusin (NASA/Goddard) report on behalf of the Fermi-LAT team:
At 04:19:54.47 UT on March 30, 2014, Fermi-LAT detected high-energy emission from GRB 140330AA, which was also detected by Fermi-GBM (trigger 417845997).
The best LAT on-ground location is found to be
RA, Dec 325.59, -64.30 (J2000)
with an error radius of 0.2 deg (90% containment, statistical error only). This was within 15 deg from the LAT boresight at the time of the trigger. More than 10 photons above 100 MeV and 2 photons above 1 GeV are observed within 6000 seconds after the GBM trigger. The highest-energy photon is a 4.5 GeV event, which is observed 252 seconds after the GBM trigger.
A Swift ToO has been requested and accepted for this burst.
The Fermi-LAT point of contact for this burst is Daniel Kocevski (daniel.kocevski@nasa.gov<http://nasa.gov>).
The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN Circular #16051
K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,
I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team,
S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline, on behalf of the Konus-Wind team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and
V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM team, report:
The long-duration GRB 140330A (LAT detection: Vianello, Kocevski, and Racusin, GCN 16048) has been observed by Fermi (GBM: trigger 417845997), Konus-Wind, INTEGRAL (SPI-ACS), MESSENGER (GRNS), and Mars Odyssey (HEND), so far, at about 15594 s UT (04:19:54).
We have triangulated it to a preliminary, 3 sigma error box whose coordinates are:
```
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   328.068 (21h 52m 16s) -57.745 (-57d 44' 42")
  Corners:
   326.549 (21h 46m 12s) -57.180 (-57d 10' 46")
   327.145 (21h 48m 35s) -57.662 (-57d 39' 43")
   329.617 (21h 58m 28s) -58.274 (-58d 16' 25")
   328.989 (21h 55m 57s) -57.817 (-57d 49' 00")
  ---------------------------------------------
```
The error box area is 1482 sq. arcmin, and its maximum dimension is 1.97 deg (the minimum one is 17 arcmin).
The center of the LAT position (Vianello, Kocevski, and Racusin, GCN 16048) is 6.6 deg from the center of the box and, hence, this position is incorrect (or the LAT source is unrelated to this GRB).
This box may be improved.
A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB140330_T15594/IPN/
GCN Circular #16056
S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, and T. Cline on behalf of the Konus-Wind team, report:
The long-duration GRB 140330AA (Fermi LAT detection: Vianello, Kocevski, & Racusin, GCN 16048; IPN triangulation: Hurley at al., GCN 16051) triggered Konus-Wind at T0=15594.217 s UT (04:19:54.217).
The burst light curve shows a single pulse from ~T0-3 s to ~T0+15 s. The emission is seen up to ~10 MeV.
As observed by Konus-Wind, the burst had a fluence of 3.9(-0.5,+0.6)x10-6 erg/cm2, and a 64-ms peak flux, measured from T0+0.320 s, of 1.5(-0.4,+0.4)x10-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum (measured from T0 to T0+16.640 s) is best fit in the 20 keV - 18 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -0.60(-0.45,+0.55), and the peak energy Ep = 158(-24,+34) keV, chi2 = 105/96 dof. Fitting this spectrum with the Band model yields the same values of alpha and Ep with an upper limit on beta of -3.3.
The spectrum near the maximum count rate (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 18 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -0.18(-0.45,+0.55), and the peak energy Ep = 172(-21,+28) keV, chi2 = 89.2/95 dof.
The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB140330A_T15594/
All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN Circular #16058
C. Pittori, F. Verrecchia (ASDC and INAF/OAR), A. Bulgarelli (INAF/IASF-Bo), A. Giuliani (INAF/IASF-Mi), M. Tavani (INAF/IAPS Rome, and Univ. Roma Tor Vergata), P. Caraveo (INAF/IASF-Mi), F. Lucarelli (ASDC and INAF/OAR), M. Marisaldi (INAF/IASF-Bo), F. Longo (Univ. of Trieste and INFN Trieste), E. Del Monte, F. Lazzarotto, I. Donnarumma, Y. Evangelista, M. Feroci, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda (INAF/IAPS Rome), G. Barbiellini, (INFN Trieste), F. Fuschino, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, V. Fioretti, M. Galli (INAF/IASF-Bo), S. Mereghetti, F. Perotti (INAF/IASF-Mi), M. Cardillo, E. Striani, (INAF/IAPS Rome, and Univ. Roma Tor Vergata), A. Argan, G. Piano, S. Sabatini, V. Vittorini (INAF/IAPS Rome), G. Pucella (ENEA Frascati), A. Pellizzoni, A. Trois (INAF/OA Cagliari), M. Pilia (ASTRON), S. Vercellone (INAF/IASF-Pa), P. W. Cattaneo, A. Rappoldi (INFN Pavia), A. Morselli, P. Picozza (INFN Roma-2), M. Prest, E. Vallazza (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), A. Chen (Wits University), S. Colafrancesco (INAF/OAR and Wits University), P. Giommi, and G. Valentini (ASI), on behalf of the AGILE Team, report:
The AGILE Gamma Ray Imaging Detector (GRID) observed an intense and prolonged high-energy emission above 100 MeV from GRB 140330AA (Fermi-LAT detection: G. Vianello et al., GCN 16048).
Despite a data telemetry gap of about 30 minutes occurring during the prompt emission of this GRB, a maximum likelihood analysis of the AGILE-GRID data integrated from 2014-03-30 04:50 UT (1805 s since trigger time) to 2014-03-31 08:00 UT yields a detection at a significance level larger than 4 sigma, with an average flux of F=(2.30 +/- 0.98) 10-6 ph/cm2/s (E > 100 MeV).
Due to the high fluence of this burst at E>100 MeV, comparable only to the one of GRB 130427A as recorded in the AGILE database, it was possible to derive its properties using the maximum likelihood techniques routinely used in the standard data analysis of AGILE-GRID point sources.
This measurement was obtained with AGILE observing a large portion of the sky in spinning mode.
GCN Circular #16062
G. Vianello (Stanford U.), D. Kocevski (NASA/Goddard), J. Racusin (NASA/Goddard), R. Ojha (NASA/GSFC/UMBC/CRESST) , and S. Ciprini (ASDC) report on behalf of the Fermi-LAT team:
The analysis of new data downloaded from Fermi has shown that emission from the proposed high-energy counterpart of GRB 140330A (Vianello et al., GCN 16048; Pittori et al., GCN 16058) has continued up to at least 40 ks after the GBM trigger. This is very unusual for a faint burst such as GRB 130330A. Also, our localization of the LAT excess has improved, and it is now:
R.A., Dec. = 325.40, -64.13 with an error radius of 0.14 (90 % c.l., statistical only),
which is well outside the IPN error box (Hurley et al., GCN 16051).
Moreover, a search in Fermi archival data has shown a variable emission from a source compatible with our position, which was detected in several occasions in 2012 and 2013, and also detected on March 28 and 29, 2014. This source has been tentatively associated with the extra-galactic radio source PKS 2136-642 in the past (ATel #5695; Mauch et al. 2003, MNRAS, 342, 1117).
Therefore, we believe that the high-energy source detected by Fermi and by AGILE (Pittori et al., GCN 16058) is unrelated to GRB 130330A.
Further analysis is ongoing.
GCN Circular #16066
V. Pelassa (UAH), G. Fitzpatrick (UCD), C. Meegan and N. Bhat (UAH) report on behalf of the Fermi GBM Team:
"At 04:19:54.47 UT on 30 March 2014, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 140330AA (trigger 417845997 / 140330A180), which was also detected by Konus-Wind (S. Golenetskii et al, GCN 16056) and localized by the Interplanetary Network (K. Hurley et al, GCN 16051). The GBM on-ground location is consistent with the IPN location. The angle from the Fermi LAT boresight is 13.6 degrees.
The GBM light curve consists of a FRED pulse with a duration (T90) of about 34 s (50-300 keV).
The time-averaged spectrum from T0-0.768 s to T0+35.073 s is well fit by a power law function with an exponential high-energy cutoff. The power law index is -0.66 +/- 0.10 and the cutoff energy, parameterized as Epeak, is 197 +/- 17 keV. (Castor statistics 578.62 for 486 d.o.f.). A Band function fits the spectrum equally well (Castor statistics 577.22 for 485 d.o.f.) with Epeak= 172 +/- 23 keV, alpha = -0.57 +/- 0.13 and beta = -2.4 +/- 0.3. This result is consistent with the analysis of the Konus observation (S. Golenetskii et al, GCN 16056).
The event fluence (10-1000 keV) in this time interval is (5.6 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.640 s in the 10-1000 keV band is 4.3 +/- 0.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."

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Jochen Greiner, last update: 05-Apr-2014 [Disclaimer]