The Progenitors of Type Ia Supernovae

By C. Pritchet, D. Howell, Mark Sullivan. 2008

178 citations recorded by the source corpus.

Type Ia supernovae (SNe Ia) occur in both old, passive galaxies and active, star-forming galaxies. This fact, coupled with the strong dependence of SN Ia rate on star formation rate, suggests that SNe Ia form from stars with a wide range of ages. Here we show that the rate of SN Ia explosions is about 1% of the stellar death rate, independent of star formation history. The dependence of SN Ia rate on star formation rate implies a delay time distribution proportional to t−0.5 ± 0.2. The single-degenerate channel for SNe Ia can be made to match the observed SN Ia rate-SFR relation, but only if white dwarfs are converted to SNe Ia with a uniform efficiency of ~1%, independent of mass. Since low-mass progenitors are expected to have lower conversion efficiencies than high-mass progenitors, we conclude that some other progenitor scenario must be invoked to explain some, or perhaps all, SNe Ia.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a8ea2869037d78a8c8236473d14a8b283d3b6f8c

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In Astronomy and Astrophysics

1. D. Maoz
2. F. Mannucci
3. L. Hernquist
4. P. Hopkins
5. A. Filippenko
6. R. Bouwens
7. M. Franx
8. A. Riess

In Electrical and Electronic Engineering

1. D. Maoz
2. F. Mannucci
3. R. Bouwens
4. A. Filippenko
5. A. Gal-yam
6. H. C. Ford
7. Ryan Chornock
8. A. Riess

In Instrumentation

1. D. Maoz
2. F. Mannucci
3. R. Bouwens
4. M. Franx
5. Richard S. Ellis
6. H. C. Ford
7. P. V. van Dokkum
8. G. Illingworth

Citations in the corpus

• The dependence of Type Ia Supernovae luminosities on their host galaxies (2010, background): “…and “delayed” components, or with a wide range of delay-times, match most observational datasets well (Mannucci et al. 2006; Sullivan et al. 2006; Pritchet et al. 2008; Totani et al. 2008), though the minimum age for the prompt systems remains controversial (Aubourg et al. 2008; Raskin et…”
• THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, background): “Pritchet et al. (2008) have argued that such a t−1/2 form for the DTD can explain the trend of SN Ia rate versus specific starformation rate of the host population in the Supernova Legacy Survey.”
• SNLS3: CONSTRAINTS ON DARK ENERGY COMBINING THE SUPERNOVA LEGACY SURVEY THREE-YEAR DATA WITH OTHER PROBES (2011, background): “…SN Ia progenitor population (Mannucci et al. 2005, 2006; Sullivan et al. 2006b; Brandt et al. 2010), or at least a wide-range in the SN delay-times (Pritchet et al. 2008; Totani et al. 2008), a natural prediction is a subtle change in the mix of SN light curve shapes with redshift (Howell et al.…”
• The helium star donor channel for the progenitors of Type Ia supernovae (2009, background): “It is generally believed that SNe Ia are thermonuclear explosions of carbon–oxygen white dwarfs (CO WDs) in binaries (Nomoto et al. 1997; Livio 2000).”
• Nearby supernova rates from the Lick Observatory Supernova Search – III. The rate–size relation, and the rates as a function of galaxy Hubble type and colour (2010, background): “…been discussed in numerous subsequent studies of SN rates (e.g., Neill et al. 2006; Sullivan et al. 2006; Mannucci et al. 2006; Dahlen et al. 2008; Pritchet et al. 2008; see also Bartunov, Tsvetkov, & Filimonova 1994, who over a decade earlier found that SNe Ia occur in spiral arms with a…”
• THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “Observations have suggested various different forms for the DTD (e.g., (Dahlen et al. 2004, 2008; Mannucci et al. 2006; Pritchet et al. 2008)).”
• Type-Ia Supernova Rates and the Progenitor Problem: A Review (2011, methodology): “A different power-law DTD dependence, with different physical motivation, has been proposed by Pritchet et al. (2008), by way of interpreting volumetric SN rates in the SNLS (but see Greggio 2010).”
• Unveiling the gravitational universe at μ-Hz frequencies (2019, background): “angular momentum loss and binary merger products [143, 176, 276].”
• Delay Time Distribution Measurement of Type Ia Supernovae by the Subaru/XMM-Newton Deep Survey and Implications for the Progenitor (2008, result): “Recently, Pritchet et al. (2008) reported that DTD proportional to t 0:5˙0:2Ia is implied based on the SNLS data (Sullivan et al. 2006), which seems to be inconsistent with our results.”
• Nearby supernova rates from the Lick Observatory Supernova Search - IV. A recovery method for the delay-time distribution (2010, methodology): “We find that the relative uncertainty in the DTD amplitude in the jth bin scales roughly as one would expect from Poisson statistics, considering the number of SNe that contribute to every bin in the DTD.”
• ACCELERATING COMPACT OBJECT MERGERS IN TRIPLE SYSTEMS WITH THE KOZAI RESONANCE: A MECHANISM FOR “PROMPT” TYPE Ia SUPERNOVAE, GAMMA-RAY BURSTS, AND OTHER EXOTICA (2010, background): “In this case, one expects a delay-time distribution of∼ t−1/2 (Pritchet et al. 2008).”
• On the Progenitors of Type Ia Supernovae (2018, unknown): “For a recent, excellent review from an observational perspective see Maoz, Mannucci and Nelemans (2014), and see also the more theoretically flavored review of Wang & Han (2012).”
• Production of dust by massive stars at high redshift (2011, background): “2.5 Type Ia supernovae Type Ia SNe are characterized by the absence of hydrogen and presence of silicon in their spectra and are believed to result from a thermonuclear explosion of a carbon-oxygen white dwarf (e.g., Livio, 2000; Hillebrandt and Niemeyer, 2000).”
• SUB-CHANDRASEKHAR WHITE DWARF MERGERS AS THE PROGENITORS OF TYPE Ia SUPERNOVAE (2010, background): “Quantitatively, the scale factor is∼0.01 (Pritchet et al. 2008), while the fraction of WDs formed in double degenerates is aboutfbin f10<P<2000fwide ≃ 0.04.”
• Holographic dark energy (2016, background): “Type Ia Supernova Type Ia supernova (SNIa) is a sub-category of cataclysmic variable stars that result from the thermonuclear explosions of white dwarfs, when these white dwarfs reach the Chandrasekhar limit and ignite carbon at their centers [54, 55].”
• Theoretical uncertainties of the Type Ia supernova rate (2014, background): “Some groups find a different slope, e.g. Pritchet et al. (2008) find at−0.5±0.2 relation.”