The Host Galaxies of Fast-Ejecta Core-Collapse Supernovae

Kelly, Patrick L.; Filippenko, A. V.; Modjaz, M.; Kocevski, D.

doi:10.1088/0004-637x/789/1/23

Cited by 64 publications

(97 citation statements)

References 73 publications

(102 reference statements)

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“…Our limit on the environment density around SN 2014J strongly argues against this progenitor scenario (Figure 4). From the analysis of the complete set of pre-explosion images (near UV to NIR) at the SN site acquired with the Hubble Space Telescope, Kelly et al (2014) exclude SD progenitor systems with a bright red giant donor star. Consistent with these results, the mass-loss limit we derived from deep X-ray observations of the SN environment firmly and independently rules out this possibility and extends the conclusion to the entire class of red giant secondary stars.…”

Section: Sd With Quasi-steady Mass Lossmentioning

confidence: 99%

“…However, no stellar progenitor has ever been directly identified in pre-explosion images, not even for the two closest Type Ia SNe discovered in the last 25 yr: SN 2011fe (Li et al 2011) and, more recently, SN 2014J (Kelly et al 2014;Goobar et al 2014). As a result, the nature of their progenitor system is still a matter of debate (e.g., Howell 2011;Di Stefano et al 2013;Maoz et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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NO X-RAYS FROM THE VERY NEARBY TYPE Ia SN 2014J: CONSTRAINTS ON ITS ENVIRONMENT

Margutti

Parrent

Kamble

et al. 2014

ApJ

125

156

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Deep X-ray observations of the post-explosion environment around the very nearby Type Ia SN 2014J (d L = 3.5 Mpc) reveal no X-ray emission down to a luminosity L x < 7 × 10 36 erg s −1 (0.3-10 keV) at δt ∼ 20 days after the explosion. We interpret this limit in the context of inverse Compton emission from upscattered optical photons by the supernova shock and constrain the pre-explosion mass-loss rate of the stellar progenitor system to beṀ < 10 −9 M yr −1 (for wind velocity v w = 100 km s −1 ). Alternatively, the SN shock might be expanding into a uniform medium with density n CSM < 3 cm −3 . These results rule out single-degenerate (SD) systems with steady mass loss until the terminal explosion and constrain the fraction of transferred material lost at the outer Lagrangian point to be 1%. The allowed progenitors are (1) white dwarf-white dwarf progenitors, (2) SD systems with unstable hydrogen burning experiencing recurrent nova eruptions with recurrence time t < 300 yr, and (3) stars where the mass loss ceases before the explosion.

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Section: Sd With Quasi-steady Mass Lossmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

NO X-RAYS FROM THE VERY NEARBY TYPE Ia SN 2014J: CONSTRAINTS ON ITS ENVIRONMENT

Margutti

Parrent

Kamble

et al. 2014

ApJ

125

156

View full text Add to dashboard Cite

show abstract

“…Some of these systems may produce unusually rapid rotators even within the framework of the Tayler-Spruit dynamo, but more detailed evolutionary studies are needed to make a meaningful conclusion on this. The fact that host galaxies of broad-lined SNe Ic and GRBs are found to be systematically overdense compared to other galaxies of the Sloan Digital Sky Survey might be an indication for the importance of the binary channel for producing rapidly rotating progenitors to produce these events (Kelly et al 2014).…”

Section: Rotationmentioning

confidence: 99%

Evolutionary Models for Type Ib/c Supernova Progenitors

Yoon

2015

Publ. Astron. Soc. Aust.

107

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SNe Ib/c mark the deaths of hydrogen-deficient massive stars. The evolutionary scenarios for SNe Ib/c progenitors involve many important physical processes including mass loss by winds and its metallicity dependence, stellar rotation, and binary interactions. This makes SNe Ib/c an excellent test bed for stellar evolution theory. We review the main results of evolutionary models for SN Ib/c progenitors available in the literature and their confrontation with recent observations. We argue that the nature of SN Ib/c progenitors can be significantly different for single and binary systems, and that binary evolution models can explain the ejecta masses derived from SN Ib/c light curves, the distribution of SN Ib/c sites in their host galaxies, and the optical magnitudes of the tentative progenitor candidate of iPTF13bvn. We emphasise the importance of early-time observations of light curves and spectra, accurate measurements of helium mass in SN Ib/c ejecta, and systematic studies about the metallicity dependence of SN Ib/c properties, to better constrain theories.

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“…However, metallicity may not be the only factor affecting the LGRB production efficiency (e.g. Kelly et al 2014;Perley et al 2015). Even though a number of studies have addressed this issue, no self-consistent study has been performed simultaneously on stellar masses, SFRs and metallicities of a complete sample of LGRBs hosts.…”

Section: Introductionmentioning

confidence: 99%

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

Japelj

Vergani

Salvaterra

et al. 2016

A&A

100

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Aims. Long gamma-ray bursts (LGRBs) are associated with the deaths of massive stars and might therefore be a potentially powerful tool for tracing cosmic star formation. However, especially at low redshifts (z < 1.5) LGRBs seem to prefer particular types of environment. Our aim is to study the host galaxies of a complete sample of bright LGRBs to investigate the effect of the environment on GRB formation. Methods. We studied host galaxy spectra of the Swift/BAT6 complete sample of 14 z < 1 bright LGRBs. We used the detected nebular emission lines to measure the dust extinction, star formation rate (SFR), and nebular metallicity (Z) of the hosts and supplemented the data set with previously measured stellar masses M . The distributions of the obtained properties and their interrelations (e.g. mass-metallicity and SFR-M relations) are compared to samples of field star-forming galaxies. Results. We find that LGRB hosts at z < 1 have on average lower SFRs than if they were direct star formation tracers. By directly comparing metallicity distributions of LGRB hosts and star-forming galaxies, we find a good match between the two populations up to 12 + log O H ∼ 8.4−8.5, after which the paucity of metal-rich LGRB hosts becomes apparent. The LGRB host galaxies of our complete sample are consistent with the mass-metallicity relation at similar mean redshift and stellar masses. The cutoff against high metallicities (and high masses) can explain the low SFR values of LGRB hosts. We find a hint of an increased incidence of starburst galaxies in the Swift/BAT6 z < 1 sample with respect to that of a field star-forming population. Given that the SFRs are low on average, the latter is ascribed to low stellar masses. Nevertheless, the limits on the completeness and metallicity availability of current surveys, coupled with the limited number of LGRB host galaxies, prevents us from investigating more quantitatively whether the starburst incidence is such as expected after taking into account the high-metallicity aversion of LGRB host galaxies.

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The Host Galaxies of Fast-Ejecta Core-Collapse Supernovae

Cited by 64 publications

References 73 publications

NO X-RAYS FROM THE VERY NEARBY TYPE Ia SN 2014J: CONSTRAINTS ON ITS ENVIRONMENT

NO X-RAYS FROM THE VERY NEARBY TYPE Ia SN 2014J: CONSTRAINTS ON ITS ENVIRONMENT

Evolutionary Models for Type Ib/c Supernova Progenitors

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

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