Fermi/gamma-ray burst monitor observations of SGR J0501+4516 bursts
View/ Open
Author
Lin, Lin
Kouveliotou, Chryssa
Baring, Matthew G.
van der Horst, Alexander J.
Guiriec, Sylvain
Woods, Peter M.
Gogus, Ersin
Kaneko, Yuki
Scargle, Jeffrey
Granot, Jonathan
Preece, Robert
von Kienlin, Andreas
Chaplin, Vandiver
Watts, Anna L.
Wijers, Ralph A. M. J.
Zhang, Shuang Nan
Bhat, Narayan
Finger, Mark H.
Gehrels, Neil
Harding, Alice
Kaper, Lex
Kaspi, Victoria
Mcenery, Julie
Meegan, Charles A.
Paciesas, William S.
Pe'er, Asaf
Ramirez-Ruiz, Enrico
van der Klis, Michiel
Wachter, Stefanie
Wilson-Hodge, Colleen
Attention
2299/6612
Abstract
We present our temporal and spectral analyses of 29 bursts from SGR J0501+4516, detected with the gamma-ray burst monitor on board the Fermi Gamma-ray Space Telescope during 13 days of the source's activation in 2008 (August 22-September 3). We find that the T-90 durations of the bursts can be fit with a log-normal distribution with a mean value of similar to 123 ms. We also estimate for the first time event durations of soft gamma repeater (SGR) bursts in photon space (i.e., using their deconvolved spectra) and find that these are very similar to the T-90 values estimated in count space (following a log-normal distribution with a mean value of similar to 124 ms). We fit the time-integrated spectra for each burst and the time-resolved spectra of the five brightest bursts with several models. We find that a single power law with an exponential cutoff model fits all 29 bursts well, while 18 of the events can also be fit with two blackbody functions. We expand on the physical interpretation of these two models and we compare their parameters and discuss their evolution. We show that the time-integrated and time-resolved spectra reveal that E-peak decreases with energy flux (and fluence) to a minimum of similar to 30 keV at F = 8.7 x 10(-6) erg cm(-2) s(-1), increasing steadily afterward. Two more sources exhibit a similar trend: SGRs J1550-5418 and 1806-20. The isotropic luminosity, L-iso, corresponding to these flux values is roughly similar for all sources (0.4-1.5 x 10(40) erg s(-1)).