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

Vreeswijk, PM and Savaglio, S and Gal-Yam, A and De Cia, A and Quimby, RM and Sullivan, M and Cenko, SB and Perley, DA and Filippenko, AV and Clubb, KI and Taddia, F and Sollerman, J and Leloudas, G and Arcavi, I and Rubin, A and Kasliwal, MM and Cao, Y and Yaron, O and Tal, D and Ofek, EO and Capone, J and Kutyrev, AS and Toy, V and Nugent, PE and Laher, R and Surace, J and Kulkarni, SR (2014) The hydrogen-poor superluminous supernova iPTF 13ajg and its host galaxy in absorption and emission. The Astrophysical Journal, 797 (1). ISSN 1538-4357

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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 × 1044 erg s-1, while the estimated total radiated energy is 1.3 × 1051 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. 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. © 2014. The American Astronomical Society. All rights reserved..

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences, 0305 Organic Chemistry, 0306 Physical Chemistry (Incl. Structural)
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Q Science > QD Chemistry
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society
Date Deposited: 22 Feb 2017 09:40
Last Modified: 07 Sep 2017 20:38
DOI or Identification number: 10.1088/0004-637X/797/1/24
URI: http://researchonline.ljmu.ac.uk/id/eprint/5697

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