A statistical analysis of circumstellar material in Type Ia supernovae

Maguire, K.; Sullivan, M.; Patat, F.; Gal‐Yam, A.; Hook, I. M.; Dhawan, Suhail; Howell, D. A.; Mazzali, P. A.; Nugent, P.; Pan, Y.-C.; Podsiadlowski, Philipp; Simon, Joshua D.; Sternberg, A.; Valenti, S.; Baltay, C.; Bersier, D.; Blagorodnova, N.; Chen, Ting-Wan; Ellman, N.; Feindt, U.; Förster, F.; Fraser, M.; González–Gaitán, S.; Graham, M. L.; Gutiérrez, C. P.; Hachinger, Stephan; Hadjiyska, E.; Inserra, C.; Knapic, C.; Laher, Russ R.; Leloudas, G.; Margheim, S.; McKinnon, R.; Molinaro, M.; Morrell, N.; Ofek, E. O.; Rabinowitz, D.; Rest, A.; Sand, David J.; Smareglia, R.; Smartt, S. J.; Taddia, F.; Walker, E. S.; Walton, N. A.; Young, D. R.

doi:10.1093/mnras/stt1586

Cited by 109 publications

(124 citation statements)

References 111 publications

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“…Observations of these NaI doublet absorption features in SN Ia by Maguire et al (2013, see also Sternberg et al 2011 suggests that at least 20% of SN Ia have a contribution from a circumstellar medium. Notably, none of the SNe Ia with such absorption features in their sample were found in early-type galaxies.…”

Section: Discussionmentioning

confidence: 90%

On the Progenitors of Local Group Novae. Ii. The Red Giant Nova Rate of M31

Williams

Darnley

Bode

et al. 2016

ApJ

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In our preceding paper, Liverpool Telescope data of M31 novae in eruption were used to facilitate a search for their progenitor systems within archival Hubble Space Telescope data, with the aim of detecting systems with red giant secondaries (RG-novae) or luminous accretion disks. From an input catalog of 38 spectroscopically confirmed novae with archival quiescent observations, likely progenitors were recovered for 11 systems. Here we present the results of the subsequent statistical analysis of the original survey, including possible biases associated with the survey and the M31 nova population in general. As part of this analysis, we examine the distribution of optical decline times (t 2 ) of M31 novae, how the likely bulge and disk nova distributions compare, and how the M31 t 2 distribution compares to that of the Milky Way. Using a detailed Monte Carlo simulation, we determine that 30 % 10 13 -+ of all M31 nova eruptions can be attributed to RG-nova systems, and at the 99% confidence level, 10% > of all M31 novae are RG-novae. This is the first estimate of a RG-nova rate of an entire galaxy. Our results also imply that RG-novae in M31 are more likely to be associated with the M31 disk population than the bulge; indeed, the results are consistent with all RG-novae residing in the disk. If this result is confirmed in other galaxies, it suggests that any Type Ia supernovae that originate from RG-nova systems are more likely to be associated with younger populations and may be rare in old stellar populations, such as early-type galaxies.

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Section: Discussionmentioning

confidence: 90%

On the Progenitors of Local Group Novae. Ii. The Red Giant Nova Rate of M31

Williams

Darnley

Bode

et al. 2016

ApJ

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“…Maguire et al 2013). At one extreme are events that are luminous, have broad light curves, red intrinsic colors, high-velocity ejecta, large velocity gradients, redshifted and broad nebular lines, no carbon signatures, and star-forming hosts.…”

Section: Spectral and Light Curve Modelingmentioning

confidence: 99%

“…However, as already discussed, explosion energy and host galaxy type are correlated, which could provide an indirect link between explosion energy and ISM (rather than CSM) absorption. Maguire et al (2013) have re-analyzed spectra for 16 of the Sternberg et al (2011) events, together with new data for 16 additional SN Ia, while defining differently the zero absorption velocity. In this combined sample, the excess of blueshifted over redshifted Na I D absorptions is 11 versus 4, again suggesting ∼ 20% CSM-related absorption.…”

Section: Intervening Absorptionmentioning

confidence: 99%

Observational Clues to the Progenitors of Type Ia Supernovae

Maoz

Mannucci

Nelemans

2014

Annu. Rev. Astron. Astrophys.

926

894

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Type-Ia supernovae (SNe Ia) are important distance indicators, element factories, cosmic-ray accelerators, kinetic-energy sources in galaxy evolution, and endpoints of stellar binary evolution. It has long been clear that a SN Ia must be the runaway thermonuclear explosion of a degenerate carbon-oxygen stellar core, most likely a white dwarf (WD). However, the specific progenitor systems of SNe Ia, and the processes that lead to their ignition, have not been identified. Two broad classes of progenitor binary systems have long been considered: single-degenerate (SD), in which a WD gains mass from a non-degenerate star; and doubledegenerate (DD), involving the merger of two WDs. New theoretical work has enriched these possibilities with some interesting updates and variants. We review the significant recent observational progress in addressing the progenitor problem. We consider clues that have emerged from the observed properties of the various proposed progenitor populations, from studies of their sites -pre-and post-explosion, from analysis of the explosions themselves, and from the measurement of event rates. The recent nearby and well-studied event, SN 2011fe, has been particularly revealing. The observational results are not yet conclusive, and sometimes prone to competing theoretical interpretations. Nevertheless, it appears that DD progenitors, long considered the underdog option, could be behind some, if not all, SNe Ia. We point to some directions that may lead to future progress.

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“…Detection of interaction based on variable Na I features (e.g., Patat et al 2007;Blondin et al 2009;Sternberg et al 2011;Foley et al 2012b;Maguire et al 2013), and measurements of high velocity features (HVF) from multiple spectral lines (e.g., Marion et al 2013;Silverman et al 2015) have all been used to investigate potential SD systems. See Maoz et al (2014) for a more thorough discussion of work in this area.…”

Section: Introductionmentioning

confidence: 99%

SN 2012cg: EVIDENCE FOR INTERACTION BETWEEN A NORMAL SN Ia AND A NON-DEGENERATE BINARY COMPANION

Marion

Brown

Vinkó

et al. 2016

ApJ

153

202

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We report evidence for excess blue light from the Type Ia supernova (Sn Ia) SN2012cg at 15 and 16 days before maximum B-band brightness. The emission is consistent with predictions for the impact of the supernova on a nondegenerate binary companion. This is the first evidence for emission from a companion to a normal SNIa. Sixteen days before maximum light, the B V -color of SN2012cg is 0.2 mag bluer than for other normal SNIa. At later times, this supernova has a typical SNIa light curve, with extinction-corrected M 19.62 0.02 B = - mag and m B 0.86 0.02 15 ( ) D =  . Our data set is extensive, with photometry in seven filters from five independent sources. Early spectra also show the effects of blue light, and high-velocity features are observed at early times. Near maximum, the spectra are normal with a silicon velocity v Si =−10,500 km s −1 . Comparing the early data with models by Kasen favors a main-sequence companion of about six solar masses. It is possible that many other SN Ia have main-sequence companions that have eluded detection because the emission from the impact is fleeting and faint.

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A statistical analysis of circumstellar material in Type Ia supernovae

Cited by 109 publications

References 111 publications

On the Progenitors of Local Group Novae. Ii. The Red Giant Nova Rate of M31

On the Progenitors of Local Group Novae. Ii. The Red Giant Nova Rate of M31

Observational Clues to the Progenitors of Type Ia Supernovae

SN 2012cg: EVIDENCE FOR INTERACTION BETWEEN A NORMAL SN Ia AND A NON-DEGENERATE BINARY COMPANION

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