The Supernova rate per unit mass

By F. Mannucci, M. Della Valle, N. Panagia, E. Cappellaro, G. Cresci, R. Maiolino, A. Petrosian, M. T. C. -. I. Firenze, I. -. O. Arcetri, STScI - Esa and 6 more. 2004

423 citations recorded by the source corpus.

We compute the rate of supernovae (SNe) of different types along the Hubble sequence normalized to the near- infrared luminosity and to the stellar mass of the parent galaxies. This is made possible by the new complete catalog of near- infrared galaxy magnitudes obtained by 2MASS. We find that the rates of all SN types, including Ia, Ib/c and II, show a sharp dependence on both the morphology and the (B − K) colors of the parent galaxies and, therefore, on the star formation activity. In particular we find, with a high statistical significance, that the type Ia rate in late type galaxies is a factor ∼20 higher than in E/S0. Similarly, the type Ia rate in the galaxies bluer than B − K = 2.6 is about a factor of 30 larger than in galaxies with B − K > 4.1. These findings can be explained by assuming that a significant fraction of Ia events in late spirals/irregulars originates in a relatively young stellar component.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5b10bc269b7f79bfeb9260952cdb1e9840102fcc

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

In Nuclear and High Energy Physics

Citations in the corpus

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).”
The 511 keV emission from positron annihilation in the Galaxy (2010, methodology): “The work of Mannucci et al. (2005), corrected for various observational biases, offers a valuable database for such an estimate and can be used, along with the stellar masses of the various Galactic components (Sec.”
DO HOT HALOS AROUND GALAXIES CONTAIN THE MISSING BARYONS? (2010, methodology): “1 This is estimated by integrating over a Chabrier (2003) initial mass function, letting stars with M > 8 M explode in a core-collapse supernova, and applying a 20% correction (Mannucci et al. 2005) to include type Ia supernovae.”
SUB-CHANDRASEKHAR WHITE DWARF MERGERS AS THE PROGENITORS OF TYPE Ia SUPERNOVAE (2010, background): “The rate has been suggested to depend on both mass and star-formation rate (Mannucci et al. 2005), or to simply 2 be a roughly constant fraction, of∼1%, of the instantaneous WD formation rate (Pritchet et al. 2008; but see Maoz et al. 2010a, whose data suggest a break beyond∼ 2Gyr [their Fig.”
Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries (2007, background): “If every AM CVn gives a visibly explosive last flash, this would give 1 event every 5000-15000 years in a 1011M⊙ E/S0 galaxy, 2− 6% of the Type Ia SN rate in E/SO galaxies (Mannucci et al. 2005; Scannapieco & Bildsten 2005; Sullivan et al. 2006).”
THE LONG-TERM EVOLUTION OF DOUBLE WHITE DWARF MERGERS (2011, result): “As a result, population synthesis calculations (Branch et al. 1995; Yungelson & Livio 1998, 2000; Ruiter et al. 2009) predict SN Ia rates from the SDS channel that are ∼ 10 times lower than the observed rate (Mannucci et al. 2005; Scannapieco & Bildsten 2005; Dilday et al. 2008).”
The all-sky distribution of 511 keV electron-positron annihilation emission (2005, background): “Furthermore, it is suggested that different SN Ia explosion mechanisms exist in different types of galaxy (e.g. Della Valle & Livio 1994b; Howell 2001; Mannucci et al. 2005) making the proposed extrapolation even more uncertain.”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, neutral): “Whether there are two channels that produce SNe Ia (e.g., Mannucci et al. 2005), or lower metallicity at high redshift reduces the efficiency of accretion (Kobayashi & Nomoto 2009), or there is more host extinction at high redshift than previously believed (Greggio et al. 2008) are hypotheses we…”
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).”
OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, background): “Thus, they include well-known and, inevitably, more luminous galaxies (e.g., Li et al. 2001; Gallagher et al. 2005; Mannucci et al. 2005).”
DOUBLE-DETONATION SUB-CHANDRASEKHAR SUPERNOVAE: SYNTHETIC OBSERVABLES FOR MINIMUM HELIUM SHELL MASS MODELS (2010, background): “Moreover, there is growing observational evidence that there are different populations of SNe Ia (Mannucci et al. 2005; Scannapieco & Bildsten 2005).”
Nearby supernova rates from the Lick Observatory Supernova Search - IV. A recovery method for the delay-time distribution (2010, methodology): “Thus, our results will be comparable to other SN rate studies, such as Mannucci et al. (2005, 2006), that have assumed the diet-Salpeter IMF.”
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).”
The Type Ia Supernova Rate (2005, positive): “We show here, that in addition to explaining the Ia rates seen in nearby galaxies as described in Mannucci et al. 2005 (hereafter M05), such a simple two-component model also resolves a wide range of outstanding issues surrounding these ob- jects.”
Short-Duration Gamma-Ray Bursts (2013, background): “The Type Ia SNe also exhibit a clear increase in the rate per unit stellar mass from early- to late-type galaxies, ranging from about 0.044 (E/SO) to 0.065 (Sa/b) to 0.17 (Sc/d) per 1010 M⊙ per century (Mannucci et al. 2005), similar to the inference for short GRBs (§6.3; Leibler & Berger 2010).”
Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “…SN rates vs. color and Hubble type The first observational indications for the existence of a range of SN Ia delay times (i.e. a DTD) was found by Mannucci et al. (2005) and Mannucci, Della Valle & Panagia (2006) who, analyzing a local SN sample (Cappellaro, Evans & Turatto 1999), demonstrated…”
Massive stars exploding in a He-rich circumstellar medium. I. Type Ibn (SN 2006jc-like) events (2008, background): “Some basic properties of SN progenitors (such as their interval of initial mass) can be estimated through the measurement of the local SN rates (e.g. Cappellaro et al. 1997, 1999; Mannucci et al. 2005, 2006; Botticella et al. 2008).”
RATES AND DELAY TIMES OF TYPE Ia SUPERNOVAE (2009, background): “For the Model 2 elliptical galaxy, we find a low SN Ia rate of ∼ 0.001 SNuM at 10 Gyr, which is over an order of magnitude below the rate for E/S0 galaxies in Mannucci et al. (2005) (0.044+0.016−0.014 SNuM).”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, background): “They cite the dependence of the SNIa rate on galaxy colour observed in the local universe (Mannucci et al. 2005)as well as a dependence on radio loudness observed by Della Valle et a. (2005).”