The delay-time distribution of Type Ia supernovae from Sloan II

By D. Maoz, F. Mannucci, Timothy D. Brandt. 2012

217 citations recorded by the source corpus.

We derive the delay-time distribution (DTD) of Type Ia supernovae (SNe Ia) using a sample of 132 SNe Ia, discovered by the Sloan Digital Sky Survey II (SDSS2) among 66 000 galaxies with spectral-based star formation histories (SFHs). To recover the best-fitting DTD, the SFH of every individual galaxy is compared, using Poisson statistics, to the number of SNe that it hosted (zero or one), based on the method introduced in Maoz et al. This SN sample differs from the SDSS2 SN Ia sample analysed by Brandt et al., using a related, but different, DTD recovery method. Furthermore, we use a simulation-based SN detection-efficiency function, and we apply a number of important corrections to the galaxy SFHs and SN Ia visibility times. The DTD that we find has 4σ detections in all three of its time bins: prompt (τ 2.4 Gyr), indicating a continuous DTD, and it is among the most accurate and precise among recent DTD reconstructions. The best-fitting power-law form to the recovered DTD is t−1.07 ± 0.07, consistent with generic ∼t−1 predictions of SN Ia progenitor models based on the gravitational-wave-induced mergers of binary white dwarfs. The time-integrated number of SNe Ia per formed stellar mass is NSN/M = 0.00130 ± 0.00015 M⊙−1, or about 4 per cent of the stars formed with initial masses in the 3 - 8 M⊙ range. This is lower than, but largely consistent with, several recent DTD estimates based on SN rates in galaxy clusters and in local-volume galaxies, and is higher than, but consistent with NSN/M estimated by comparing volumetric SN Ia rates to cosmic SFH.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cd78c578840fe0d30d384915225e71e33e6b3ed5

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium (2017, methodology): “(3) where the power law index s = 1.12 is taken as our fiducial value (Maoz et al. 2012), the normalization constant is N0 = 1.3 × 10−3 M−1 (Maoz et al. 2012), and t ≥ τ8 M = 40 Myr is the delay time, here corresponding to the main sequence lifetime of an ∼ 8M star, the upper mass limit for the…”
Theoretical uncertainties of the Type Ia supernova rate (2014, background): “Different groups find an integrated rate between 0.33·10−3 and 2.9·10−3 M⊙−1 (Maoz et al. 2011, 2012; Graur et al. 2011; Graur & Maoz 2013; Perrett et al. 2012).”
Neutron Star Mergers Might Not Be the Only Source of r-process Elements in the Milky Way (2018, result): “Regardless of the different methodologies, most studies point toward a DTD in the form of t−1 (Totani et al. 2008; Maoz et al. 2010, 2012; Graur et al. 2011, 2014; Perrett et al. 2012), which is consistent with the predictions of population synthesis models (e.g., Ruiter et al. 2009).”
OBSERVING THE NEXT GALACTIC SUPERNOVA (2013, unknown): “We note that recent work has advocated a continuous delay time distribution (Horiuchi & Beacom 2010; Maoz et al. 2012), but this extra complication seemed unnecessary for our present models.”
DEMOGRAPHICS OF THE GALAXIES HOSTING SHORT-DURATION GAMMA-RAY BURSTS (2013, result): “We note that this result is similar to Type Ia supernovae which have n ≈ −1.1 (Maoz et al. 2010, 2012), and is in contrast to previous short GRB results which claimed substantially longer average delay times of∼ 4−8 Gyr for lognormal lifetime distributions based on smaller numbers of events (Nakar…”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, methodology): “We take s = 1.12 as the fiducial value (Maoz et al. 2012), which is consistent with theoretical expectations that relate the Type Ia rate to the loss of energy and angular momentum to gravitational radiation in a binary system (e.g., Greggio 2005).”
CONFIRMATION OF A STAR FORMATION BIAS IN TYPE Ia SUPERNOVA DISTANCES AND ITS EFFECT ON THE MEASUREMENT OF THE HUBBLE CONSTANT (2014, background): “Thus, if SNe Ia do indeed have a rapidly falling—1/t—delay time distribution (see, e.g., Maoz et al. 2012), then only a minority of SNe Ia would be superimposed on a geometrical region of their host that is unrelated to their birth environment.”
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, background): “This is a reasonable choice, given that, after 50 Myr, almost all of the energy is liberated via Type Ia SNe that have time delays between several hundred Myrs to a few Gyrs (e.g. Maoz et al. 2012).”
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, background): “…focus on the delay time of type Ia supernovae (SNe Ia), which are thought to arise from the thermonuclear explosion of a white dwarf (e.g., Totani et al. 2008; Maoz et al. 2010, 2011, 2012; Maoz & Badenes 2010; Graur & Maoz 2013; Graur et al. 2014); we refer to Maoz et al. (2014) for a review.”
An Open Catalog for Supernova Data (2016, background): “Examples include: estimating the number of supernovae of a given type discovered and/or observed per year, and its dependence on redshift (cf. Maoz et al. 2012); determining the frequency of supernova type by galaxy type, and its relation to galactocentric distances assuming a volume limited sample…”