Environment-derived constraints on the progenitors of low-luminosity Type I supernovae★

Lyman, J.; James, P. A.; Perets, Hagai B.; Anderson, J. P.; Gal‐Yam, A.; Mazzali, P. A.; Percival, S. M.

doi:10.1093/mnras/stt1038

Cited by 80 publications

(113 citation statements)

References 40 publications

Supporting

Mentioning

102

Contrasting

Order By: Relevance

“…Investigations into their environments seem to imply relatively young progenitors. Lyman et al (2013) showed that SNe Iax have a similar degree of association to host galaxy on-going SF as SNe IIP, and used this to argue for progenitors with delay times of less than 50 Myrs. It is interesting to note that Foley et al (2014) constrained the progenitor lifetime of the extreme SN Iax SN 2008ha to be less than 80 Myrs.…”

Section: Sne Iaxmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

Mapping the diversity of supernovae (SNe) to progenitor properties is key to our understanding of stellar evolution and explosive stellar death. Investigations of the immediate environments of SNe allow statistical constraints to be made on progenitor properties such as mass and metallicity. Here we review the progress that has been made in this field. Pixel statistics using tracers of e.g. star formation within galaxies show intriguing differences in the explosion sites of, in particular SNe types II and Ibc (SNe II and SNe Ibc respectively), suggesting statistical differences in population ages. Of particular interest is that SNe Ic are significantly more associated with host galaxy Hα emission than SNe Ib, implying shorter lifetimes for the former. In addition, such studies have shown (unexpectedly) that the interacting SNe IIn do not explode in regions containing the most massive stars, which suggests that at least a significant fraction of their progenitors arise from the lower end of the core-collapse SN mass range. Host H ii region spectroscopy has been obtained for a significant number of core-collapse events, however definitive conclusions on differences between distinct SN types have to-date been elusive. Single stellar evolution models predict that the relative fraction of SNe Ibc to SNe II should increase with increasing metallicity, due to the dependence of mass-loss rates on progenitor metallicity. We present a meta-analysis of all current host H ii region oxygen abundances for CC SNe. It is concluded that the SN II to SN Ibc ratio shows little variation with oxygen abundance, with only a suggestion that the ratio increases in the lowest bin. Radial distributions of different SNe are discussed, where a central excess of SNe Ibc has been observed within disturbed galaxy systems, which is difficult to ascribe to metallicity or selection effects. Environment studies are also being undertaken for SNe Ia, where constraints can be made on the shortest delay times of progenitor systems. It is shown that 'redder' SNe Ia are more often found within star-forming regions. Environment studies are evolving to enable studies at higher spatial resolutions than previously possible, while in addition the advent of widefield integral field unit instruments allows galaxy-wide spectral analyses which will provide fruitful results to this field. Some example contemporary results are shown in that direction.

show abstract

Section: Sne Iaxmentioning

confidence: 99%

Statistical Studies of Supernova Environments

Anderson

James

Habergham

et al. 2015

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

show abstract

“…Nevertheless, the undisputed presence of spectral lines due to hydrogen in these type II-Plateau SNe, and the conspicuous absence of these in SNe Iax, including SN 2008ha, poses problems for this scenario. Recent studies that have considered the location of SNe Iax within their host galaxies have shown that SNe Iax tend to favour late-type galaxies with higher local star formation rates, which could indicate that they result from younger stars (Lyman et al 2013). Some progenitor channels involving WDs in binary systems are, however, consistent with the relatively young ages inferred for SNe Iax progenitors (Wang et al 2014;Kromer et al 2015) implying that environmental factors alone cannot be used as a discriminating factor.…”

Section: Introductionmentioning

confidence: 96%

The type Iax supernova, SN 2015H

Magee

Kotak

Sim

et al. 2016

A&A

Self Cite

View full text Add to dashboard Cite

We present results based on observations of SN 2015H which belongs to the small group of objects similar to SN 2002cx, otherwise known as type Iax supernovae. The availability of deep pre-explosion imaging allowed us to place tight constraints on the explosion epoch. Our observational campaign began approximately one day post-explosion, and extended over a period of about 150 days post maximum light, making it one of the best observed objects of this class to date. We find a peak magnitude of M r = −17.27 ± 0.07, and a (∆m 15 ) r = 0.69 ± 0.04. Comparing our observations to synthetic spectra generated from simulations of deflagrations of Chandrasekhar mass carbon-oxygen white dwarfs, we find reasonable agreement with models of weak deflagrations that result in the ejection of ∼0.2 M of material containing ∼0.07 M of 56 Ni. The model light curve however, evolves more rapidly than observations, suggesting that a higher ejecta mass is to be favoured. Nevertheless, empirical modelling of the pseudobolometric light curve suggests that 0.6 M of material was ejected, implying that the white dwarf is not completely disrupted, and that a bound remnant is a likely outcome.

show abstract

“…Even more striking, many are found at substantial offsets from their presumed host galaxies, suggesting either that they originate in extremely faint systems (such as globular clusters; Yuan et al 2013), or alternatively that the progenitor has traveled from its birth site. Increasingly deep limits at the transient locations have failed to detect an underlying host system, favoring the latter interpretation (Lyman et al 2013(Lyman et al , 2014(Lyman et al , 2016.…”

Section: Introductionmentioning

confidence: 99%

Two New Calcium-rich Gap Transients in Group and Cluster Environments

Lunnan

Kasliwal

Cao

et al. 2017

ApJ

Self Cite

111

View full text Add to dashboard Cite

We present the Palomar Transient Factory discoveries and the photometric and spectroscopic observations of PTF11kmb and PTF12bho. We show that both transients have properties consistent with the class of calcium-rich gap transients, specifically lower peak luminosities and rapid evolution compared to ordinary supernovae, and a nebular spectrum dominated by [Ca II] emission. A striking feature of both transients is their host environments: PTF12bho is an intracluster transient in the Coma Cluster, while PTF11kmb is located in a loose galaxy group, at a physical offset ∼150 kpc from the most likely host galaxy. Deep Subaru imaging of PTF12bho rules out an underlying host system to a limit of > -M 8.0 mag R , while Hubble Space Telescope imaging of PTF11kmb reveals a marginal counterpart that, if real, could be either a background galaxy or a globular cluster. We show that the offset distribution of Ca-rich gap transients is significantly more extreme than that seen for SNe Ia or even short-hard gamma-ray bursts (sGRBs). Thus, if the offsets are caused by a kick, they require higher kick velocities and/or longer merger times than sGRBs. We also show that almost all Ca-rich transients found to date are in group and cluster environments with elliptical host galaxies, indicating a very old progenitor population; the remote locations could partially be explained by these environments having the largest fraction of stars in the intragroup/ intracluster light following galaxy-galaxy interactions.

show abstract

Environment-derived constraints on the progenitors of low-luminosity Type I supernovae★

Cited by 80 publications

References 40 publications

Statistical Studies of Supernova Environments

Statistical Studies of Supernova Environments

The type Iax supernova, SN 2015H

Two New Calcium-rich Gap Transients in Group and Cluster Environments

Contact Info

Product

Resources

About