High-Redshift Supernova Rates

By T. Dahlén, L. Strolger, A. Riess, B. Mobasher, R. Chary, Christopher J. Conselice, H. Ferguson, A. Fruchter, M. Giavalisco, M. Livio and 3 more. 2004

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We use a sample of 42 supernovae detected with the Advanced Camera for Surveys on board the Hubble Space Telescope as part of the Great Observatories Origins Deep Survey to measure the rate of core-collapse supernovae to z ~ 0.7 and Type Ia supernovae to z ~ 1.6. This significantly increases the redshift range at which supernova rates have been estimated from observations. The rate of core-collapse supernovae can be used as an independent probe of the cosmic star formation rate. Based on the observations of 17 core-collapse supernovae, we measure an increase in the core-collapse supernova rate by a factor of ~1.6 in the range 0.3 < z < 0.7 and an overall increase by a factor of ~7 to z ~ 0.7 in comparison with the local core-collapse supernova rate. The increase in the rate in this redshift range is consistent with recent measurements of the star formation rate derived from UV-luminosity densities and IR data sets. Based on 25 Type Ia supernovae, we find a Type Ia supernova rate that is a factor of 3-5 higher at z ~ 1 compared to earlier estimates at lower redshifts (z < 0.5), implying that the Type Ia supernova rate traces a higher star formation rate at redshifts z > 1 compared to low redshift. At higher redshift (z ≳ 1), we find a suggested decrease in the Type Ia rate with redshift. This evolution of the Ia rate with redshift is consistent with a Type Ia progenitor model, in which there is a substantial delay between the formation of the progenitor star and the explosion of the supernova. Assuming that the Type Ia progenitor stars have initial main-sequence masses 3 M☉ < M < 8 M☉, we find that 5%-7% of the available progenitors explode as Type Ia supernovae.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d03d05770a26b928121387c06d438b87ecf9d2df

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Citations in the corpus

CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “Prior HST surveys for SNe Ia at z > 1 suggest a long delay of ∼ 3 Gyr between star formation and SN Ia production (Dahlen et al. 2004; Kuznetsova et al. 2008; Strolger et al. 2004).”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, methodology): “Instead, a simple parameterisation of the Type Ia rate based on the delay time distribution (DTD) of Type Ia events (e.g., Dahlen et al. 2004; Strolger 2004; Greggio 2005; Mannucci et al. 2006; Matteucci et al. 2006) is often adopted.”
On the Normalization of the Cosmic Star Formation History (2006, methodology): “The uncertainties affecting thėρSNII measurements are treated in some detail by Dahlen et al. (2004), and the error bars shown are representative of the combination of both statistical and systematic uncertainties.”
The evolution of stellar mass and the implied star formation history (2008, background): “Supernova rates are filled red circles from Dahlen et al. (2004) and Cappellaro et al. (2005). star formation regions) can be used as tracers of the formation of massive stars.”
Rates and Properties of Type Ia Supernovae as a Function of Mass and Star Formation in Their Host Galaxies (2006, background): “The most deviant point is the ≃ 1 rate from Dahlen et al. (2004), but even this value differs from the model at only 1.8σ.”
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)).”
Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “Early on, Dahlen, Strolger & Riess (2008); Dahlen et al. (2004); Strolger et al. (2004) and Strolger, Dahlen & Riess (2010) argued for a DTD that is peaked at a delay of ∼ 3 Gyr, with little power at either shorter or longer delays.”
Short-hard gamma-ray bursts (2007, background): “The mean lifetime of a NS-BH binary in this scenario is ≈ 5 Gyr and the predicted rate (normalized to the supernova rate at a redshift of ≈ 0.7) is ∼ 104 Gpc−3 yr−1 (Bethe, Brown & Lee, 2007, this volume).”
THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT (2010, unknown): “In contrast, Dahlen et al. (2004, 2008) and Strolger (2004) have argued for a DTD that is peaked at a delay of ∼ 3 Gyr, with little power at short delays, based on a decrease in the SN Ia rate at z > 1.”
The illustris simulation: Public data release (2015, unknown): “Maoz+ (2012) Dahlen+ (2004) Wiersma+ (2009b)”
Nearby supernova rates from the Lick Observatory Supernova Search - IV. A recovery method for the delay-time distribution (2010, background): “As already noted, “A+B” is an oversimplification, but its measured values are seen to be consistent with our DTD. Strolger et al. (2004) and Dahlen et al. (2004) have deduced a Gaussian DTD centred at 4 Gyr with half-width 0.8 Gyr, as a best fit to their comparison of SN rates to cosmic SFH, out to…”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, methodology): “Using an improved compilation of modern cosmic SFR data, Hopkins & Beacom (2006) noted that the measured cosmic SNR (Cappellaro et al. 1999; Dahlen et al. 2004; Cappellaro et al. 2005) were somewhat lower than those predicted from the SFR. Similar conclusion were reached by Mannucci et al. (2007)…”
Nearby supernova rates from the Lick Observatory Supernova Search – I. The methods and data base (2010, background): “…have derived SN Ia rates at moderate to high redshifts (e.g., Hardin et al. 2000; Madgwick et al. 2003; Tonry et al. 2003; Blanc et al. 2004; Strolger et al. 2004; Dahlen et al. 2004, 2008; Neill et al. 2006; Poznanski et al. 2007; Botticella et al. 2008; Dilday et al. 2008; Horesh et al. 2008).”
The Hubble Higher z Supernova Search: Supernovae to z ≈ 1.6 and Constraints on Type Ia Progenitor Models (2004, methodology): “Elsewhere, we report on the rates of SNe Ia and core-collapse SNe and the comparison of these measured rates to those made by other surveys and to the predicted SN formation-rate history partly predicted from the analysis in this paper (Dahlen et al. 2004).”
TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE (2014, methodology): “First were the GOODS SN surveys, which used the HST ACS camera to measure the SN Ia rate to z ∼ 1.8 (GOODS Strolger et al. 2004; Dahlen et al. 2004).”
The evolution of massive black holes and their spins in their galactic hosts (2012, background): “A similar procedure can be followed with core-collapse supernova rates (see for instance Dahlen et al. (2004)), for these stars too are short-lived compared to star formation.”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, methodology): “…(filled square), Hardin (2000) (open diamond), Neill (2006) (filled diamond), Tonry (2003) (open black triangle), Pain (2002) (filled triangle), Dahlen et al. (2004) (crosses), Barris & Tonry (2006) (open circles), Poznanski et al. (2007) (upright triangles), andKuznetsova et al. (2008) (left…”