PRE-DISCOVERY AND FOLLOW-UP OBSERVATIONS OF THE NEARBY SN 2009nr: IMPLICATIONS FOR PROMPT TYPE Ia SUPERNOVAE

Khan, R.; Prieto, J. L.; Pojmański, G.; Stanek, K. Z.; Beacom, J. F.; Szczygiel, D.; Pilecki, B.; Mogren, K.; Eastman, Jason D.; Martini, Paul; Stoll, R.

doi:10.1088/0004-637x/726/2/106

Cited by 15 publications

(15 citation statements)

References 65 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is thus important to take into account not just the integrated metallicity of the galaxy, but the value at the birthplace of the progenitor. Such a bias may already be seen in the number of cases in which a SN Ia occurred in the outer halo of a star-forming galaxy (Prieto et al 2008;Khan et al 2011). Using the location of the explosion as a proxy in such a differential study would be cleanest performed by considering "prompt" SNe Ia and/or small, more metallicity-homogeneous galaxies.…”

Section: Discussionmentioning

confidence: 99%

THE IMPACT OF METALLICITY ON THE RATE OF TYPE Ia SUPERNOVAE

Kistler

Stanek

Kochanek

et al. 2013

ApJ

Self Cite

View full text Add to dashboard Cite

The metallicity of a star strongly affects both its evolution and the properties of the stellar remnant that results from its demise. It is generally accepted that stars with initial masses below ∼ 8 M ⊙ leave behind white dwarfs and that some sub-population of these lead to Type Ia supernovae. However, it is often tacitly assumed that metallicity has no effect on the rate of SNe Ia. We propose that a consequence of the effects of metallicity is to significantly increase the SN Ia rate in lower-metallicity galaxies, in contrast to previous expectations. This is because lower-metallicity stars leave behind higher-mass white dwarfs, which should be easier to bring to explosion. We first model SN Ia rates in relation to galaxy masses and ages alone, finding that the elevation in the rate of SNe Ia in lower-mass galaxies measured by LOSS is readily explained. However, we then see that models incorporating this effect of metallicity agree just as well. Using the same parameters to estimate the cosmic SN Ia rate, we again find good agreement with data up to z ≈ 2. We suggest that this degeneracy warrants more detailed examination of host galaxy metallicities. We discuss additional implications, including for hosts of high-z SNe Ia, the SN Ia delay time distribution, super-Chandrasekhar SNe, and cosmology.

show abstract

Section: Discussionmentioning

confidence: 99%

THE IMPACT OF METALLICITY ON THE RATE OF TYPE Ia SUPERNOVAE

Kistler

Stanek

Kochanek

et al. 2013

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Performing comparisons at larger distances with more CCSNe and galaxies will dramatically improve the situation since even an increase in factor of two in distance would give a factor ∼ 8 increase in the rate. Presently running observation programs such as the All-Sky Automated Survey for the Brightest Supernovae (ASAS-SN; e.g., Khan et al 2011) will find CCSNe in a volume-limited sample of nearby galaxies, and the Palomar Transient Factory will collect larger numbers of CCSNe in survey mode (Law et al 2009;Lien & Fields 2009). Issues such as completeness should therefore improve dramatically in the near future.…”

Section: Discussion and Summarymentioning

confidence: 99%

Effects of Stellar Rotation on Star Formation Rates and Comparison to Core-Collapse Supernova Rates

Horiuchi

Beacom

Bothwell

et al. 2013

ApJ

View full text Add to dashboard Cite

We investigate star formation rate (SFR) calibrations in light of recent developments in the modeling of stellar rotation. Using new published non-rotating and rotating stellar tracks, we study the integrated properties of synthetic stellar populations and find that the UV to SFR calibration for the rotating stellar population is 30% smaller than for the non-rotating stellar population, and 40% smaller for the Hα to SFR calibration. These reductions translate to smaller SFR estimates made from observed UV and Hα luminosities. Using the UV and Hα fluxes of a sample of ∼ 300 local galaxies, we derive a total (i.e., sky-coverage corrected) SFR within 11 Mpc of 120-170 M ⊙ yr −1 and 80-130 M ⊙ yr −1 for the non-rotating and rotating estimators, respectively. Independently, the number of core-collapse supernovae discovered in the same volume requires a total SFR of 270 +110−80 M ⊙ yr −1 , suggesting a tension with the SFR estimates made with rotating calibrations. More generally, when compared with the directly estimated SFR, the local supernova discoveries strongly constrain any physical effects that might increase the energy output of massive stars, including, but not limited to, stellar rotation. The cosmic SFR and cosmic supernova rate data on the other hand show the opposite trend, with the cosmic SFR higher than that inferred from cosmic supernovae, constraining a significant decrease in the energy output of massive stars. Together, these lines of evidence suggest that the true SFR calibration factors cannot be too far from their canonical values.

show abstract

“…Foley et al (2012) presented light-curve parameters for SN 2009ig, which we also use here. For SN 2009nr, we use the light-curve properties reported by Khan et al (2011). Light curves of SNe 2007on, 2008C, 2008fp, 2008hv, and 2008ia were presented in Stritzinger et al (2011; we derive light-curve parameters for these SNe by fitting the light curves with the SNooPy Python package (Burns et al 2011).…”

Section: Datamentioning

confidence: 99%

“…d All measurements were originally reported byFoley et al (2012). e Light-curve parameters were originally reported byKhan et al (2011).…”

mentioning

confidence: 99%

LINKING TYPE Ia SUPERNOVA PROGENITORS AND THEIR RESULTING EXPLOSIONS

Foley

Simon

Burns

et al. 2012

ApJ

View full text Add to dashboard Cite

Comparing the ejecta velocities at maximum brightness and narrow circumstellar/interstellar Na D absorption line profiles of a sample of 23 Type Ia supernovae (SNe Ia), we determine that the properties of SN Ia progenitor systems and explosions are intimately connected. As demonstrated by Sternberg et al. (2011), half of all SNe Ia with detectable Na D absorption at the host-galaxy redshift in high-resolution spectroscopy have Na D line profiles with significant blueshifted absorption relative to the strongest absorption component, which indicates that a large fraction of SN Ia progenitor systems have strong outflows. In this study, we find that SNe Ia with blueshifted circumstellar/interstellar absorption systematically have higher ejecta velocities and redder colors at maximum brightness relative to the rest of the SN Ia population. This result is robust at a 98.9-99.8% confidence level, providing the first link between the progenitor systems and properties of the explosion. This finding is further evidence that the outflow scenario is the correct interpretation of the blueshifted Na D absorption, adding additional confirmation that some SNe Ia are produced from a single-degenerate progenitor channel. An additional implication is that either SN Ia progenitor systems have highly asymmetric outflows that are also aligned with the SN explosion or SNe Ia come from a variety of progenitor systems where SNe Ia from systems with strong outflows tend to have more kinetic energy per unit mass than those from systems with weak or no outflows.

show abstract

PRE-DISCOVERY AND FOLLOW-UP OBSERVATIONS OF THE NEARBY SN 2009nr: IMPLICATIONS FOR PROMPT TYPE Ia SUPERNOVAE

Cited by 15 publications

References 65 publications

THE IMPACT OF METALLICITY ON THE RATE OF TYPE Ia SUPERNOVAE

THE IMPACT OF METALLICITY ON THE RATE OF TYPE Ia SUPERNOVAE

Effects of Stellar Rotation on Star Formation Rates and Comparison to Core-Collapse Supernova Rates

LINKING TYPE Ia SUPERNOVA PROGENITORS AND THEIR RESULTING EXPLOSIONS

Contact Info

Product

Resources

About