Delay Time Distribution Measurement of Type Ia Supernovae by the Subaru/XMM-Newton Deep Survey and Implications for the Progenitor

By P. Astron, Soc., Japan., T. Totani, T. Morokuma, T. Oda, M. Doi, N. Yasuda. 2008

204 citations recorded by the source corpus.

The delay time distribution (DTD) of type Ia supernovae (SNe Ia) from star formation is an important clue to reveal the still unknown progenitor system of SNe Ia. Here we report on a measurement of the SN Ia DTD in a delay time range of t_Ia = 0.1-8.0 Gyr by using the faint variable objects detected in the Subaru/XMM-Newton Deep Survey (SXDS) down to i' ~ 25.5. We select 65 SN candidates showing significant spatial offset from nuclei of the host galaxies having old stellar population at z ~ 0.4-1.2, out of more than 1,000 SXDS variable objects. Although spectroscopic type classification is not available for these, we quantitatively demonstrate that more than ~80% of these should be SNe Ia. The DTD is derived using the stellar age estimates of the old galaxies based on 9 band photometries from optical to mid-infrared wavelength. Combined with the observed SN Ia rate in elliptical galaxies at the local universe, the DTD in t_Ia ~ 0.1-10 Gyr is well described by a featureless power-law as f_D(t_Ia) \propto t_Ia^{-1}. The derived DTD is in excellent agreement with the generic prediction of the double-degenerate scenario, giving a strong support to this scenario. In the single-degenerate (SD) scenario, although predictions by simple analytic formulations have broad DTD shapes that are similar to the observation, DTD shapes calculated by more detailed binary population synthesis tend to have strong peaks at characteristic time scales, which do not fit the observation. This result thus indicates either that the SD channel is not the major contributor to SNe Ia in old stellar population, or that improvement of binary population synthesis theory is required. Various sources of systematic uncertainties are examined and tested, but our main conclusions are not affected significantly.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4bf8ebf9300402da1103da28d0a10e1bb17b39b7

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In Astronomy and Astrophysics

1. D. Maoz
2. F. Mannucci
3. A. Filippenko
4. Michela Mapelli
5. R. Kirshner
6. S. Jha
7. Robert G. Izzard
8. N. Smith

In Instrumentation

1. R. Bouwens
2. F. Mannucci
3. D. Maoz
4. M. Franx
5. H. C. Ford
6. Selma de Mink
7. Richard S. Ellis
8. G. Illingworth

Citations in the corpus

• Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, background): “6 where we show the DTD of SNe Ia derived by Totani et al. (2008) and Maoz et al. (2010) from extragalactic surveys (blue triangles and circles, respectively).”
• 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).”
• Supernova Type Ia progenitors from merging double white dwarfs - Using a new population synthesis model (2012, background): “Overplotted with black circles are the observed values of the SNIa rate of Totani et al. (2008), Maoz etal.”
• Gravitationally lensed quasars and supernovae in future wide-field optical imaging surveys (2010, methodology): “In this paper, we use the result of Totani et al. (2008) who constrained the distribution of tD assuming a power law f (tD) ∝ t−1.08D (tD > 0.1 Gyr).”
• Type-Ia Supernova Rates and the Progenitor Problem: A Review (2011, methodology): “…described previously: the DTD based on galaxy-cluster SN Ia rates (Maoz et al. 2010); the DTD from the ages of high-z field ellipticals (Totani et al. 2008); the DTD from the nearby LOSS galaxies with their SDSS-based SFHs, and the SNe they hosted (Maoz et al. 2011); the DTD from all…”
• Observational Clues to the Progenitors of Type Ia Supernovae (2013, methodology): “A related approach to DTD recovery was taken by Totani et al. (2008), using field elliptical galaxies instead of galaxy clusters.”
• Theoretical uncertainties of the Type Ia supernova rate (2014, background): “More recent observations show that the DTD is best described by a continuous power-law function with an index of−1 (Totani et al. 2008; Maoz et al. 2010, 2011; Maoz & Mannucci 2012; Graur et al. 2011; Graur & Maoz 2013), more specifically (Maoz & Mannucci 2012) DTD(t) ≈ 0.4 (t/Gyr)−1 SNuM,…”
• The delay-time distribution of Type Ia supernovae from Sloan II (2012, methodology): “Our new result provides the strongest support to date for previous indications for a continuous DTD (Mannucci et al. 2006; Totani et al. 2008; Maoz et al. 2010).”
• THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “However, a number of more recent measurements and analyses point to a DTD that is a power law of index ≈ −1 (Totani et al. 2008; Maoz et al. 2010; Maoz & Badenes 2010; Brandt et al. 2010; Horiuchi & Beacom 2010; Maoz et al. 2011; Graur et al. 2011).”
• RATES AND DELAY TIMES OF TYPE Ia SUPERNOVAE (2009, result): “The DDS DTD, following a power law, is consistent with the findings of Totani et al. (2008), whose observationallyderived delay time of SNe Ia in intermediate-redshift elliptical galaxies follows a featureless power law ∝ t−1 for 0.1 < t < 10 Gyr.”
• 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).”
• THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, methodology): “…DTD agrees remarkably well, both in shape and in absolute normalization, with DTDs recently recovered using different techniques, in different environments: in field ellipticals (Totani et al. 2008); in nearby galaxies (Maoz et al. 2010); and in the Magellanic Clouds (Maoz & Badenes 2010).”
• The dependence of Type Ia Supernovae luminosities on their host galaxies (2010, background): “…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 al. 2009) with some…”
• SNLS3: CONSTRAINTS ON DARK ENERGY COMBINING THE SUPERNOVA LEGACY SURVEY THREE-YEAR DATA WITH OTHER PROBES (2011, background): “…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. 2007).”
• Nearby supernova rates from the Lick Observatory Supernova Search - IV. A recovery method for the delay-time distribution (2010, background): “…rates per unit stellar mass in galaxies of particular types (star forming, quiescent, etc.), and to attempt to assign to each type a “formation age,” or some generic, simple, SFH (e.g., Mannucci et al. 2005, 2006; Sullivan et al. 2006; Totani et al. 2008; Pritchet et al. 2008; Raskin et al. 2009b).”
• 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): “The delay-time distribution of Ia supernovae implies that many systems explode on 1-10 Gyr timescales (e.g., Totani et al. 2008), and this fact implies a certain number density of progenitor systems in the Galaxy.”