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6 results on '"Postigo, ADU"'

1. THE NEEDLE in the 100 deg2 HAYSTACK: UNCOVERING AFTERGLOWS of FERMI GRBs with the PALOMAR TRANSIENT FACTORY

Author

Singer, LP, Kasliwal, MM, Cenko, SB, Perley, DA, Anderson, GE, Anupama, GC, Arcavi, I, Bhalerao, V, Bue, BD, Cao, Y, Connaughton, V, Corsi, A, Cucchiara, A, Fender, RP, Fox, DB, Gehrels, N, Goldstein, A, Gorosabel, J, Horesh, A, Hurley, K, Johansson, J, Kann, DA, Kouveliotou, C, Huang, K, Kulkarni, SR, Masci, F, Nugent, P, Rau, A, Rebbapragada, UD, Staley, TD, Svinkin, D, Thöne, CC, Postigo, ADU, Urata, Y, and Weinstein, A

Subjects
gamma-ray burst: individual, gravitational waves, methods: observational, supernovae: general, surveys, astro-ph.HE, astro-ph.CO, astro-ph.IM, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts' host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z = 0.145 and 0.384, respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron star mergers that may soon be detected by Advanced LIGO and Virgo.

Published
2015

3. The origin of the early time optical emission of Swift GRB 080310

Author

Littlejohns, OM, Willingale, R, O'Brien, PT, Beardmore, AP, Covino, S, Perley, DA, Tanvir, NR, Rol, E, Yuan, F, Akerlof, C, D'Avanzo, P, Bersier, DF, Castro-Tirado, AJ, Christian, P, Cobb, BE, Evans, PA, Filippenko, AV, Flewelling, H, Fugazza, D, Hoversten, EA, Kamble, AP, Kobayashi, S, Li, W, Morgan, AN, Mundell, CG, Page, K, Palazzi, E, Quimby, RM, Schulze, S, Steele, IA, Postigo, ADU, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, QC, QB
Abstract

We present broadband multi-wavelength observations of GRB 080310 at redshift z = 2.43. This burst was bright and long-lived, and unusual in having extensive optical and near IR follow-up during the prompt phase. Using these data we attempt to simultaneously model the gamma-ray, X-ray, optical and IR emission using a series of prompt pulses and an afterglow component. Initial attempts to extrapolate the high energy model directly to lower energies for each pulse reveal that a spectral break is required between the optical regime and 0.3 keV to avoid over predicting the optical flux. We demonstrate that afterglow emission alone is insufficient to describe all morphology seen in the optical and IR data. Allowing the prompt component to dominate the early-time optical and IR and permitting each pulse to have an independent low energy spectral indices we produce an alternative scenario which better describes the optical light curve. This, however, does not describe the spectral shape of GRB 080310 at early times. The fit statistics for the prompt and afterglow dominated models are nearly identical making it difficult to favour either. However one enduring result is that both models require a low energy spectral index consistent with self absorption for at least some of the pulses identified in the high energy emission model., 24 pages, 12 figures, 12 tables. Accepted to MNRAS

Published
2012

4. Grb 030913: hunting the afterglow

Author

Postigo, Adu, Guziy, S., Gorosabel, J., Castro-Tiradol, Aj, Ceron, Jmc, Sanguino, Tjm, Jelinek, M., Petr Kubánek, Hudec, R., Pata, P., Amado, P., Fathkullin, T., Herreria, A., Mendez, J., Ruiz-Lapuente, P., Sokolov, Vv, Zurita, A., Grace, Collaboration, and Battrick, B.

5. BOOTES: Recent technical developments and scientific results

Author

Sanguino, Tjm, La Morena, Ba, Riera, Jt, Castro-Tirado, Aj, Postigo, Adu, Gorosabel, J., Ceron, Jcm, Dabo, Ceg, Galiano, Jab, Pata, P., Vitek, S., Bernas, M., Jelinek, M., Petr Kubánek, Hudec, R., Mcbreen, S., Soria, T., Feroci, M., Frontera, F., Masetti, N., and Piro, L.

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