Maqola

Deep Photometry of GRB 041006 Afterglow: Hypernova Bump at Redshift <i>z</i> = 0.716

K. Z. StanekHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]P. GarnavichDepartment of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556P. A. NutzmanHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]J. D. HartmanHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]Arti GargHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]Kurt L. AdelbergerCarnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101Z. BenkhaldounF. L. Whipple Observatory, 670 Mount Hopkins Road, P.O. Box 97, Amado, AZ 85645A. Z. BonanosHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]M. CalkinsF. L. Whipple Observatory, 670 Mount Hopkins Road, P.O. Box 97, Amado, AZ 85645P. ChallisHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]B. Scott GaudiHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]M. J. HolmanHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]R. KirshnerHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]B. A. McLeodHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]D. J. OsipCarnegie Institution of Washington, Las Campanas Observatory, Casilla 601, La Serena, ChileT. PimenovaDepartment of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556T. H. ReiprichInstitut für Astrophysik und Extraterrestrische Forschung, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, GermanyW. RomanishinDepartment of Physics and Astronomy, University of Oklahoma, 440 West Brooks, Norman, OK 73019T. B. SpahrHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; [email protected]S. C. TeglerDepartment Physics and Astronomy, Northern Arizona University, Box 6010, Flagstaff, AZ 86011Xiaohong ZhaoDepartment of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556

2005en

ABI

Annotatsiya

We present deep optical photometry of the afterglow of gamma-ray burst (GRB) 041006 and its associated hypernova obtained over 65 days after detection (55 R-band epochs on 10 different nights). Our early data (t<4 days) joined with published GCN data indicates a steepening decay, approaching F_nu ~t^{-0.6} at early times (<<1 day) and F_nu ~t^{-1.3} at late times. The break at t_b=0.16+-0.04 days is the earliest reported jet break among all GRB afterglows. During our first night, we obtained 39 exposures spanning 2.15 hours from 0.62 to 0.71 days after the burst that reveal a smooth afterglow, with an rms deviation of 0.024 mag from the local power-law fit, consistent with photometric errors. After t~4 days, the decay slows considerably, and the light curve remains approximately flat at R~24 mag for a month before decaying by another magnitude to reach R~25 mag two months after the burst. This ``bump'' is well-fitted by a k-corrected light curve of SN1998bw, but only if stretched by a factor of 1.38 in time. In comparison with the other GRB-related SNe bumps, GRB 041006 stakes out new parameter space for GRB/SNe, with a very bright and significantly stretched late-time SN light curve. Within a small sample of fairly well observed GRB/SN bumps, we see a hint of a possible correlation between their peak luminosity and their ``stretch factor'', broadly similar to the well-studied Phillips relation for the type Ia supernovae.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1086/431361

Iqtiboslar va manbalar

2 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar