Pair-instability supernovae via collision runaway in young dense star clusters

Pan, Tony; Loeb, Abraham; Kasen, Daniel

doi:10.1111/j.1365-2966.2012.21030.x

Cited by 46 publications

(35 citation statements)

References 59 publications

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“…While spherically symmetric star formation models fail to produce stars more massive than about 20 M⊙ (Kahn 1974;Wolfire & Cassinelli 1987) recent multidimensional simulations have succeeded in obtaining ⋆ E-mail:a.jerkstrand@qub.ac.uk much higher masses (Krumholz et al 2009;Kuiper et al 2010;Cunningham et al 2011). There is also a possibility that some very massive stars are formed via mergers (Bonnell, Bate & Zinnecker 1998;Portegies Zwart et al 1999;Pan, Loeb & Kasen 2012).…”

Section: Introductionmentioning

confidence: 99%

Nebular spectra of pair-instability supernovae

Jerkstrand

Smartt

Heger

2015

Mon. Not. R. Astron. Soc.

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If very massive stars (M 100 M ⊙ ) can form and avoid too strong mass loss during their evolution, they are predicted to explode as pair-instability supernovae (PISNe). One critical test for candidate events is whether their nucleosynthesis yields and internal ejecta structure, being revealed through nebular-phase spectra at t 1 yr, match those of model predictions. Here we compute theoretical spectra based on model PISN ejecta at 1-3 years post-explosion to allow quantitative comparison with observations. The high column densities of PISNe lead to complete gamma-ray trapping for t 2 years which, combined with fulfilled conditions of steady state, leads to bolometric supernova luminosities matching the 56 Co decay. Most of the gamma-rays are absorbed by the deep-lying iron and silicon/sulphur layers. The ionization balance shows a predominantly neutral gas state, which leads to emission lines of Fe I, Si I, and S I. For low-mass PISNe the metal core expands slowly enough to produce a forest of distinct lines, whereas high-mass PISNe expand faster and produce more featureless spectra. Line blocking is complete below ∼5000Å for several years, and the model spectra are red. The strongest line is typically [Ca II] λλ7291, 7323, one of few lines from ionized species. We compare our models with proposed PISN candidates SN 2007bi and PTF12dam, finding discrepancies for several key observables and thus no support for a PISN interpretation. We discuss distinct spectral features predicted by the models, and the possibility of detecting pair-instability explosions among non-superluminous supernovae.

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Section: Introductionmentioning

confidence: 99%

Nebular spectra of pair-instability supernovae

Jerkstrand

Smartt

Heger

2015

Mon. Not. R. Astron. Soc.

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“…Detections of Pop III SNe will be the most direct probe of the first stars in the near term because they are thousands of times brighter than their progenitors and the primitive galaxies that host them Kitayama & Yoshida 2005;Greif et al 2007;Whalen et al 2008c;de Souza et al 2011a;Vasiliev et al 2012;Pan et al 2012b). PI SNe in particular are ideal candidates for finding Pop III stars because of their extreme luminosities.…”

Section: Introductionmentioning

confidence: 99%

Finding the First Cosmic Explosions. I. Pair-Instability Supernovae

Whalen

Even

Frey

et al. 2013

ApJ

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The first stars are the key to the formation of primitive galaxies, early cosmological reionization and chemical enrichment, and the origin of supermassive black holes. Unfortunately, in spite of their extreme luminosities, individual Population III stars will likely remain beyond the reach of direct observation for decades to come. However, their properties could be revealed by their supernova explosions, which may soon be detected by a new generation of NIR observatories such as JWST and WFIRST. We present light curves and spectra for Pop III pair-instability supernovae calculated with the Los Alamos radiation hydrodynamics code RAGE. Our numerical simulations account for the interaction of the blast with realistic circumstellar envelopes, the opacity of the envelope, and Lyman absorption by the neutral IGM at high redshift, all of which are crucial to computing the NIR signatures of the first cosmic explosions. We find that JWST will detect pair-instability supernovae out to z 30, WFIRST will detect them in all-sky surveys out to z ∼ 15 -20 and LSST and Pan-STARRS will find them at z 7 − 8. The discovery of these ancient explosions will probe the first stellar populations and reveal the existence of primitive galaxies that might not otherwise have been detected.

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“…The energy-injection model involves a rapidly rotating central engine similar in nature to the central engine of gamma-ray bursts (GRBs; e.g., Usov 1992); if this model explains some or all SLSNe, then it would be reasonable to expect similarities between the hosts of SLSNe and the hosts of long-duration GRBs, which are observed to avoid high-metallicity galaxies and occur predominantly at low to intermediate metallicity in the local universe (Stanek et al 2006;Modjaz et al 2008;Graham & Fruchter 2013;Krühler et al 2015;Japelj et al 2016;Perley et al 2016). Other models invoke dynamical interactions and stellar mergers in dense environments (Pan et al 2012;van den Heuvel & Portegies Zwart 2013), which would favor particularly intense starbursts. In any case, regardless of the underlying theoretical model, the degree of similarity or dissimilarity between the hosts of Type I versus Type II events (or between subclasses of these events, or between these events and other classes of SNe) might help establish whether these explosions are closely related or fundamentally different.…”

Section: Introductionmentioning

confidence: 99%

Host-Galaxy Properties of 32 Low-Redshift Superluminous Supernovae From the Palomar Transient Factory

Perley

Quimby

Yan

et al. 2016

ApJ

248

346

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We present ultraviolet through near-infrared photometry and spectroscopy of the host galaxies of all superluminous supernovae (SLSNe) discovered by the Palomar Transient Factory prior to 2013 and derive measurements of their luminosities, star formation rates, stellar masses, and gas-phase metallicities. We find that TypeI (hydrogen-poor) SLSNe (SLSNe I) are found almost exclusively in low-mass ( * <´ M M 2 10 9) and metal-poor (12+log 10 [O/ H] < 8.4) galaxies. We compare the mass and metallicity distributions of our sample to nearby galaxy catalogs in detail and conclude that the rate of SLSNe I as a fraction of all SNe is heavily suppressed in galaxies with metallicities   Z 0.5 . Extremely low metallicities are not required and indeed provide no further increase in the relative SLSN rate. Several SLSN I hosts are undergoing vigorous starbursts, but this may simply be a side effect of metallicity dependence: dwarf galaxies tend to have bursty star formation histories. TypeII (hydrogen-rich) SLSNe (SLSNe II) are found over the entire range of galaxy masses and metallicities, and their integrated properties do not suggest a strong preference for (or against) low-mass/low-metallicity galaxies. Two hosts exhibit unusual properties: PTF 10uhf is an SLSN I in a massive, luminous infrared galaxy at redshift z=0.29, while PTF 10tpz is an SLSN II located in the nucleus of an early-type host at z=0.04.

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Pair-instability supernovae via collision runaway in young dense star clusters

Cited by 46 publications

References 59 publications

Nebular spectra of pair-instability supernovae

Nebular spectra of pair-instability supernovae

Finding the First Cosmic Explosions. I. Pair-Instability Supernovae

Host-Galaxy Properties of 32 Low-Redshift Superluminous Supernovae From the Palomar Transient Factory

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