Late-time spectroscopy of Type Iax Supernovae. Issue 1 (7th June 2016)

• Record Type: Journal Article
• Authors: Foley, Ryan J.; Jha, Saurabh W.; Pan, Yen-Chen; Zheng, WeiKang; Bildsten, Lars; Filippenko, Alexei V.; Kasen, Daniel
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 461:Issue 1(2016)
• Page Start: 433
• Page End: 457
• Publication Date: 2016-06-07
• Subjects: supernovae: general -- supernovae: individual: PTF09ego, PTF09eiy, PTF10bvr, SN 2002cx, SN 2004cs, SN 2005P, SN 2005hk, SN 2007J, SN 2008A, SN 2008ge, SN 2008ha, SN 2010ae, SN 2011ay, SN 2011ce, SN 2012Z, SN 2014dt; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stw1320
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We examine the late-time ( t ≳ 200 d after peak brightness) spectra of Type Iax supernovae (SNe Iax), a low-luminosity, low-energy class of thermonuclear stellar explosions observationally similar to, but distinct from, Type Ia supernovae. We present new spectra of SN 2014dt, resulting in the most complete late-time spectral sequence of an SN Iax. At late times, SNe Iax have generally similar spectra, all with a similar continuum shape and strong forbidden-line emission. However, there is also significant diversity where some SN Iax spectra display narrow P-Cygni features from permitted lines and a continuum indicative of a photosphere at late times in addition to strong narrow (FWHM < 3500 km s −1 ) forbidden lines, others have no obvious P-Cygni features, strong broad (FWHM > 6000 km s −1 ) forbidden lines, and weak narrow forbidden lines, and some SNe Iax have spectra intermediate to these two varieties. We find that SNe Iax with strong broad forbidden lines are more luminous and have higher velocity ejecta at peak brightness. We estimate blackbody and kinematic radii of the late-time photosphere, finding the latter significantly larger than the former. We propose a two-component model that solves this discrepancy and explains the diversity of the late-time spectra of SNe Iax. In this model, the broad forbidden lines originate from the SN ejecta, while the photosphere, P-Cygni lines, and narrow forbidden lines originate from a wind launched from the remnant of the progenitor white dwarf and is driven by the radioactive decay of newly synthesized material left in the remnant. The relative strength of the two components accounts for the diversity of late-time SN Iax spectra. This model also solves the puzzle of a long-lived photosphere and the slow late-time decline of SNe Iax.