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The hydrogen-poor superluminous supernova iPTF 13ajg and its host galaxy in absorption and emission

Vreeswuk, Paul M. and Perley, Daniel A. and Cao, Yi and Kulkarni, Shrinivas R. and Laher, Russ and Surace, Jason (2014) The hydrogen-poor superluminous supernova iPTF 13ajg and its host galaxy in absorption and emission. Astrophysical Journal, 797 (1). Art. No. 24. ISSN 0004-637X.

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We present imaging and spectroscopy of a hydrogen-poor superluminous supernova (SLSN) discovered by the intermediate Palomar Transient Factory, iPTF 13ajg. At a redshift of z = 0.7403, derived from narrow absorption lines, iPTF 13ajg peaked at an absolute magnitude of M_(u,AB) = –22.5, one of the most luminous supernovae to date. The observed bolometric peak luminosity of iPTF 13ajg is 3.2 × 10^(44) erg s^(–1), while the estimated total radiated energy is 1.3 × 10^(51) erg. We detect narrow absorption lines of Mg I, Mg II, and Fe II, associated with the cold interstellar medium in the host galaxy, at two different epochs with X-shooter at the Very Large Telescope. From Voigt profile fitting, we derive the column densities log N(Mg I) =11.94 ± 0.06, log N(Mg II) =14.7 ± 0.3, and log N(Fe II) =14.25 ± 0.10. These column densities, as well as the Mg I and Mg II equivalent widths of a sample of hydrogen-poor SLSNe taken from the literature, are at the low end of those derived for gamma-ray bursts (GRBs) whose progenitors are also thought to be massive stars. This suggests that the environments of hydrogen-poor SLSNe and GRBs are different. From the nondetection of Fe II fine-structure absorption lines, we derive a lower limit on the distance between the supernova and the narrow-line absorbing gas of 50 pc. The neutral gas responsible for the absorption in iPTF 13ajg exhibits a single narrow component with a low velocity width, ΔV = 76 km s^(–1), indicating a low-mass host galaxy. No host galaxy emission lines are detected, leading to an upper limit on the unobscured star formation rate (SFR) of SFR_([OII]) < 0.07 M_☉ yr^(-1). Late-time imaging shows the iPTF 13ajg host galaxy to be faint, with g_(AB) ≈ 27.0 and R_(AB) ≥ 26.0 mag, corresponding to M_(B,Vega) ≳ –17.7 mag.

Item Type:Article
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URLURL TypeDescription Paper
Perley, Daniel A.0000-0001-8472-1996
Cao, Yi0000-0002-8036-8491
Kulkarni, Shrinivas R.0000-0001-5390-8563
Surace, Jason0000-0001-7291-0087
Additional Information:© 2014 American Astronomical Society. Received 2014 August 15; accepted 2014 September 23; published 2014 November 21. This paper is based on observations collected at the Palomar 48 and 60 inch telescopes, the Nordic Optical Telescope (NOT), the Discovery Channel Telescope (DCT), the Very Large Telescope (VLT) under proposal No. 291.D-5009, and the Keck-I and Keck-II telescopes. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA); it was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful to Ori D. Fox, Isaac Shivvers, Patrick L. Kelly, WeiKang Zheng, Sumin Tang, W. Kao, and Joel Johansson for performing part of the Keck observations presented in this paper, and to ESO’s User Support Department and Paranal observing staff for arranging and securing the VLT DDT observations. These results made use of Lowell Observatory’s Discovery Channel Telescope; Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. The LMI at the DCT was built by Lowell Observatory using funds from the NSF grant AST–1005313. We wish to thank Sylvain Veilleux, Antonino Cucchiara, Suvi Gezari, and Eleonora Troja for assistance in obtaining the DCT data. It is a pleasure to thank Daniele Malesani for providing his handy finder-chart routine, and Melina Bersten for interesting discussions. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, GIF, Minerva, and ISF grants, WIS-UK “making connections,” and Kimmel and ARCHES awards. A.V.F.’s supernova group at UC Berkeley is supported through NSF grant AST–1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. M.S. acknowledges support from the Royal Society. Support for D.A.P.was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute,which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The Dark Cosmology Centre is funded by the DNRF. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project.
Group:IPTF, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
Discovery CommunicationsUNSPECIFIED
European Research Council (ERC)307260
Israeli Committee for planning and funding Quantum Universe I-Core programUNSPECIFIED
Israel Science FoundationUNSPECIFIED
German-Israeli Foundation for Research and DevelopmentUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
NASA Hubble FellowshipHST-HF-51296.01-A
NASANAS 5-26555
Danish National Research FoundationUNSPECIFIED
Department of Energy (DOE)DE-AC02-05CH11231
Subject Keywords:ISM: atoms; supernovae: general; supernovae: individual (iPTF 13ajg)
Record Number:CaltechAUTHORS:20151204-072412759
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Official Citation:Paul M. Vreeswijk et al 2014 ApJ 797 24
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:62595
Deposited By: Ruth Sustaita
Deposited On:04 Dec 2015 16:44
Last Modified:27 Oct 2017 23:48

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