The Type Ia Supernova Rate

By Evan Scannapieco, L. Bildsten. 2005

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We explore the idea that the Type Ia supernova (SN Ia) rate consists of two components: a prompt piece that is proportional to the star formation rate (SFR), and an extended piece that is proportional to the total stellar mass. We fit the parameters of this model to the local observations by Mannucci and collaborators and then study its impact on three important problems. On cosmic scales, the model reproduces the observed SN Ia rate density below z = 1 and predicts that it will track the measured SFR density at higher redshift, reaching a value of (1-3.5) × 10-4 yr-1 Mpc-3 at z = 2. In galaxy clusters, a large prompt contribution helps explain the Fe content of the intracluster medium. Within the Galaxy, the model reproduces the observed stellar [O/Fe] abundance ratios if we allow a short (≈0.7 Gyr) delay in the prompt component. Ongoing medium-z SN surveys will yield more accurate parameters for our model.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7fa582c992a2d3c2aa6b95edc1ff0f828f0d8926

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Citations in the corpus

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, methodology): “…earlier found that SNe Ia occur in spiral arms with a frequency similar to that of SNe II).8 As discussed in §4.2, the rates used to derive the twocomponent model by M05 and Scannapieco & Bildsten (2005) have not been corrected for the rate-size relation, and thus are for the average galaxy sizes.”
Evidence of Environmental Dependencies of Type Ia Supernovae from the Nearby Supernova Factory indicated by Local H$\alpha$ (2013, background): “On the other hand, the wide range of observed ΣHα is an indication of SNe from both passive and star-forming regions, i.e. from both young and old progenitors (Scannapieco & Bildsten 2005; Mannucci et al. 2005, 2006; Sullivan et al. 2006).”
GIANT SPARKS AT COSMOLOGICAL DISTANCES? (2014, background): “…[1] Guetta & Della Valle 2007; [2] Soderberg et al. 2006; [3a] Nakar, Gal-Yam & Fox 2006; [3b] Coward et al. 2012; [4] Kalogera et al. 2004; [5] Ofek 2007; [6] Scannapieco & Bildsten 2005; [7] Li et al. 2011 [8] Lorimer et al. 2007; [9] Thornton et al. 2013. tion of short hard bursts is wider.”
THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, methodology): “…a proportionality between star-formation rate (SFR) and SN Ia rate per unit stellar mass in star forming galaxies, and on the other hand, a non-zero SN Ia rate in early-type galaxies with no current star formation (Mannucci et al. 2005, 2006; Scannapieco & Bildsten 2005; Sullivan et al. 2006).”
Nearby Supernova Factory Observations of SN 2005gj: Another Type Ia Supernova in a Massive Circumstellar Envelope (2006, background): “…to low-redshift SNe Ia to deduce cosmological parameters—is the question of whether or not SNe Ia may arise from multiple channels (e.g., Howell 2001; Scannapieco & Bildsten 2005), acting on significantly different timescales, and in particular whether the relative contributions of multiple…”
The Progenitors of Type Ia Supernovae (2008, background): “Finally, it should be noted that the predictions of SN Ia rate in this paper provide a better match to observations than does the empirical A · M + B · SFR formula (Scannapieco & Bildsten 2005; Sullivan et al. 2006).”
Characterizing Supernova Progenitors via the Metallicities of their Host Galaxies, from Poor Dwarfs to Rich Spirals (2007, background): “…delayed (SNe Ia explode >109 yr after star formation)—were suggested to explain the high rates of SNe Ia in actively starforming galaxies (late-type spirals and irregulars) compared with SNe Ia in old, elliptical galaxies (e.g., Mannucci et al. 2005; Scannapieco & Bildsten 2005; Neill et al. 2006).”
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): “A prompt component to the supernova Ia rate has been claimed by a number of authors (e.g., Scannapieco & Bildsten 2005; Mannucci et al. 2006; Aubourg et al. 2008; Brandt et al. 2010; Maoz & Badenes 2010; Maoz et al. 2010; Maoz et al. 2011).”
The n ature of submillimetre galaxies in cosmological hydrodynamic simulations (2009, methodology): “Type Ia modelling is based on the fit to data by Scannapieco & Bildsten (2005), as a prompt component tracing the star formation rate and a delayed component (with a 0.7 Gyr delay) tracking stellar mass. Stellar mass loss is derived from Bruzual & Charlot (2003) population synthesis modelling…”
Comparative Direct Analysis of Type Ia Supernova Spectra. I. SN 1994D (2005, methodology): “In recent years it has been shown (Mannucci et al. 2005, 2006; Scannapieco & Bildsten 2005; Sullivan et al. 2006) that some SNe Ia, called prompt, are produced by a young (∼108 yr) stellar population while others, called tardy, are produced by an older population (several Gyr).”
Nearby supernova rates from the Lick Observatory Supernova Search – I. The methods and data base (2010, background): “The implications of the two-component model on the progenitors of SNe Ia and the impact on their use as calibratable candles to derive cosmological parameters are further discussed by Scannapieco & Bildsten (2005), Sullivan et al. (2006), and Dahlen et al. (2008).”
Feedback and recycled wind accretion: assembling the z= 0 galaxy mass function (2009, methodology): “We input the Type Ia SNe rates of Scannapieco & Bildsten (2005), where an instantaneous component is tied to the SFR, and a delayed component is proportional to the stellar mass as described in OD08.”
The Progenitors of Type Ia Supernovae (2012, background): “Many works involve the observational DTDs (e.g. Scannapieco and Bildsten, 2005; Mannucci et al., 2006, 2008; Förster et al., 2006; Aubourg et al., 2008; Botticella et al., 2008; Totani et al., 2008; Schawinski, 2009; Maoz et al., 2011).”
IMPROVED DARK ENERGY CONSTRAINTS FROM ∼100 NEW CfA SUPERNOVA TYPE Ia LIGHT CURVES (2009, background): “Scannapieco & Bildsten (2005), Mannucci, Della Valle, & Panagia (2006) and Sullivan et al. (2006) find two populations of SN Ia progenitors, one “prompt”, that follows the star-formation rate, and one “tardy”, that follows the mass distribution.”
Two populations of progenitors for type ia supernovae (2005, methodology): “These aspects have recently been discussed in some detail by Scannapieco & Bildsten (2005) who for their model calculations adopted the simplified description of the SN Ia rates as derived by Mannucci et al. (2005) in terms of a component proportional to the star formation rate (SFR) and another…”
VARIABLE SODIUM ABSORPTION IN A LOW-EXTINCTION TYPE Ia SUPERNOVA, (2009, background): “…both a prompt (∼ 108 yr) component that is closely associated with recent star formation and a much more extended component with a characteristic timescale of several Gyr (Scannapieco & Bildsten 2005; Mannucci, Della Valle, & Panagia 2006, although see Totani et al. 2008 for a conflicting view).”
TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE (2014, methodology): “The construction of our bifurcated DTD model is reminiscent of the two-component “A+B” model (Mannucci et al. 2005; Scannapieco & Bildsten 2005), but it has closer ties to recent theoretical predictions from binary population synthesis models.”
Gravitationally lensed quasars and supernovae in future wide-field optical imaging surveys (2010, background): “…sometimes been assumed that SNe Ia are drawn from two populations, ‘prompt’ (tracing star formation rates) and ‘old’ (tracing stellar masses of host galaxies) SNe (Mannucci et al. 2005; Scannapieco & Bildsten 2005; Mannucci, Della Valle & Panagia 2006; Sullivan et al. 2006b; Aubourg et al. 2008).”
On the Normalization of the Cosmic Star Formation History (2006, methodology): “To explore a more physically motivated connection between SNIa generation and the underlying stellar populations, Scannapieco & Bildsten (2005) introduced a two component model, dependent on both SFR and stellar mass densities, to derive the SNIa rate density.”