Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae
21 Mar 2016-Monthly Notices of the Royal Astronomical Society (Oxford University Press)-Vol. 457, Iss: 1, pp 328-350
TL;DR: In this article, the bolometric light curve of 38 stripped-envelope core-collapse supernovae (SE SNe) is recovered and template light curves provided.
Abstract: Literature data are collated for 38 stripped-envelope core-collapse supernovae (SE SNe; i.e. SNe IIb, Ib, Ic and Ic-BL) that have good light curve coverage in more than one optical band. Using bolometric corrections derived in previous work, the bolometric light curve of each SN is recovered and template bolometric light curves provided. Peak light distributions and decay rates are investigated; SNe subtypes are not cleanly distinguished in this parameter space, although some grouping of types does occur and there is a suggestion of a Phillips-like relation for most SNe Ic-BL. The bolometric light curves are modelled with a simple analytical prescription and compared to results from more detailed modelling. Distributions of the explosion parameters shows the extreme nature of SNe Ic-BL in terms of their 56Ni mass and the kinetic energy, however ejected masses are similar to other subtypes. SNe Ib and Ic have very similar distributions of explosion parameters, indicating a similarity in progenitors. SNe~IIb are the most homogeneous subtype and have the lowest average values for 56Ni mass, ejected mass, and kinetic energy. Ejecta masses for each subtype and SE SNe as a whole are inconsistent with those expected from very massive stars. The majority of the ejecta mass distribution is well described by more moderately massive progenitors in binaries, indicating these are the dominant progenitor channel for SE SNe.
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TL;DR: The Zwicky Transient Facility (ZTF) as discussed by the authors is a new time domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg$^2$ field of view and 8 second readout time.
Abstract: The Zwicky Transient Facility (ZTF), a public-private enterprise, is a new time domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg$^2$ field of view and 8 second readout time. It is well positioned in the development of time domain astronomy, offering operations at 10% of the scale and style of the Large Synoptic Survey Telescope (LSST) with a single 1-m class survey telescope. The public surveys will cover the observable northern sky every three nights in g and r filters and the visible Galactic plane every night in g and r. Alerts generated by these surveys are sent in real time to brokers. A consortium of universities which provided funding ("partnership") are undertaking several boutique surveys. The combination of these surveys producing one million alerts per night allows for exploration of transient and variable astrophysical phenomena brighter than r $\sim$ 20.5 on timescales of minutes to years. We describe the primary science objectives driving ZTF including the physics of supernovae and relativistic explosions, multi-messenger astrophysics, supernova cosmology, active galactic nuclei and tidal disruption events, stellar variability, and Solar System objects.
501 citations
Cites background from "Bolometric light curves and explosi..."
...…supernovae (SE SNe) samples currently available in the literature are mainly targeted (i.e., 34 SE SNe in Taddia et al. 2018b, CSP), and non-homogenous (i.e. collections by Cano 2013, Lyman et al. 2016, and Prentice et al. 2016), or rather small (i.e., 20 SNe in Taddia et al. 2015, SDSS II)....
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TL;DR: In this paper, a new grid of presupernova models of massive stars extending in mass between 13 and 120 Msun, covering four metallicities (Fe/H]=0, -1, -2 and -3) and three initial rotation velocities (i.e. 0, 150 and 300 km/s).
Abstract: We present a new grid of presupernova models of massive stars extending in mass between 13 and 120 Msun, covering four metallicities (i.e. [Fe/H]=0, -1, -2 and -3) and three initial rotation velocities (i.e. 0, 150 and 300 km/s). The explosion has been simulated following three different assumptions in order to show how the yields depend on the remnant mass - initial mass relation. An extended network from H to Bi is fully coupled to the physical evolution of the models. The main results can be summarized as follows. a) At solar metallicity the maximum mass exploding as Red Super Giant (RSG) is of the order of 17 Msun in the non rotating case, all the more massive stars exploding as WR stars. All rotating models, vice versa, explode as Wolf-Rayet (WR) stars. b) The interplay between the core He burning and the H burning shell, triggered by the rotation induced instabilities, drives the synthesis of a large primary amount of all the products of the CNO, not just N14. A fraction of them enriches enormously the radiative part of the He core (and is responsible of the large production of F) and a fraction enters the convective core leading therefore to an important primary neutron flux able to synthesize heavy nuclei up to Pb. c) In our scenario, remnant masses of the order of those inferred by the first detections of the gravitational waves (GW150914, GW151226, GW170104, GW170814) are predicted at all metallicities for none or moderate initial rotation velocities.
328 citations
Cites background from "Bolometric light curves and explosi..."
...…3 − 4 M⊙ estimated from the SNIb light curve fitting 34 Limongi,Chieffi (Wheeler & Levreault 1985; Ensman & Woosley 1988; Dessart et al. 2011, 2015, 2016; Lyman et al. 2016); (d) a limiting mass between SNIIP and SNIb corresponding to MIIP ∼ 17 M⊙ implies a fraction of SNIb of ∼ 26 % of all the…...
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TL;DR: In this article, the authors present a review of the supernova community's efforts to identify progenitor stars of core-collapse supernovae in high resolution archival images of their galaxies.
Abstract: Over the last 15 years, the supernova community has endeavoured to identify progenitor stars of core-collapse supernovae in high resolution archival images of their galaxies.This review compiles results (from 1999 - 2013) in a distance limited sample and discusses the implications. The vast majority of the detections of progenitor stars are of type II-P, II-L or IIb with one type Ib progenitor system detected and many more upper limits for progenitors of Ibc supernovae (14). The data for these 45 supernovae progenitors illustrate a remarkable deficit of high luminosity stars above an apparent limit of Log L ~= 5.1 dex. For a typical Salpeter IMF, one would expect to have found 13 high luminosity and high mass progenitors. There is, possibly, only one object in this time and volume limited sample that is unambiguously high mass (the progenitor of SN2009ip). The possible biases due to the influence of circumstellar dust and sample selection methods are reviewed. It does not appear likely that these can explain the missing high mass progenitor stars. This review concludes that the observed populations of supernovae in the local Universe are not, on the whole, produced by high mass (M > ~18Msun) stars. Theoretical explosions of model stars also predict that black hole formation and failed supernovae tend to occur above M > ~18Msun. The models also suggest there are islands of explodability for stars in the 8-120Msun range. The observational constraints are quite consistent with the bulk of stars above M > ~18Msun collapsing to form black holes with no visible supernovae. (Abridged).
317 citations
California Institute of Technology1, University of Washington2, Stockholm University3, University of Maryland, College Park4, Auburn University5, University of Wisconsin–Milwaukee6, Goddard Space Flight Center7, National Central University8, University of California, Santa Barbara9, University of Michigan10, Northwestern University11, Adler Planetarium12, Lawrence Berkeley National Laboratory13, University of California, Berkeley14, Weizmann Institute of Science15, Radboud University Nijmegen16, Humboldt University of Berlin17, Macau University of Science and Technology18, Tel Aviv University19, Soka University of America20, Centre national de la recherche scientifique21, Los Alamos National Laboratory22
TL;DR: The Zwicky Transient Facility (ZTF) as mentioned in this paper is a new time-domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg^2 field of view and an 8 second readout time.
Abstract: The Zwicky Transient Facility (ZTF), a public–private enterprise, is a new time-domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg^2 field of view and an 8 second readout time. It is well positioned in the development of time-domain astronomy, offering operations at 10% of the scale and style of the Large Synoptic Survey Telescope (LSST) with a single 1-m class survey telescope. The public surveys will cover the observable northern sky every three nights in g and r filters and the visible Galactic plane every night in g and r. Alerts generated by these surveys are sent in real time to brokers. A consortium of universities that provided funding ("partnership") are undertaking several boutique surveys. The combination of these surveys producing one million alerts per night allows for exploration of transient and variable astrophysical phenomena brighter than r ~ 20.5 on timescales of minutes to years. We describe the primary science objectives driving ZTF, including the physics of supernovae and relativistic explosions, multi-messenger astrophysics, supernova cosmology, active galactic nuclei, and tidal disruption events, stellar variability, and solar system objects.
280 citations
TL;DR: In this paper, a detailed report of the connection between long-duration gamma-ray bursts (GRBs) and their accompanying supernovae (SNe) is presented, with a focus on how observations, and the modelling of observations, have constrained what we know about GRB-SNe.
Abstract: We present a detailed report of the connection between long-duration gamma-ray bursts (GRBs) and their accompanying supernovae (SNe). The discussion presented here places emphasis on how observations, and the modelling of observations, have constrained what we know about GRB-SNe. We discuss their photometric and spectroscopic properties, their role as cosmological probes, including their measured luminosity–decline relationships, and how they can be used to measure the Hubble constant. We present a statistical summary of their bolometric properties and use this to determine the properties of the “average” GRB-SN. We discuss their geometry and consider the various physical processes that are thought to power the luminosity of GRB-SNe and whether differences exist between GRB-SNe and the SNe associated with ultra-long-duration GRBs. We discuss how observations of their environments further constrain the physical properties of their progenitor stars and give a brief overview of the current theoretical paradigms of their central engines. We then present an overview of the radioactively powered transients that have been photometrically associated with short-duration GRBs, and we conclude by discussing what additional research is needed to further our understanding of GRB-SNe, in particular the role of binary-formation channels and the connection of GRB-SNe with superluminous SNe.
212 citations
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TL;DR: In this paper, the uncertainty inherent in any observational estimate of the IMF is investigated by studying the scatter introduced by Poisson noise and the dynamical evolution of star clusters, and it is found that this apparent scatter reproduces quite well the observed scatter in power-law index determinations, thus defining the fundamental limit within which any true variation becomes undetectable.
Abstract: A universal initial mass function (IMF) is not intuitive, but so far no convincing evidence for a variable IMF exists. The detection of systematic variations of the IMF with star-forming conditions would be the Rosetta Stone for star formation.
In this contribution an average or Galactic-field IMF is defined, stressing that there is evidence for a change in the power-law index at only two masses: near 0.5 M⊙ and near 0.08 M⊙. Using this supposed universal IMF, the uncertainty inherent in any observational estimate of the IMF is investigated by studying the scatter introduced by Poisson noise and the dynamical evolution of star clusters. It is found that this apparent scatter reproduces quite well the observed scatter in power-law index determinations, thus defining the fundamental limit within which any true variation becomes undetectable. The absence of evidence for a variable IMF means that any true variation of the IMF in well-studied populations must be smaller than this scatter.
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6,784 citations
"Bolometric light curves and explosi..." refers methods in this paper
...The lack of large Mej events is somewhat at odds from predictions of stellar models with a simple weighting from the IMF....
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...Thus, although the spread of model Mej values are good representations of the observed distribution, the quantitative divide between low- and high-Mej events is inconsistent with expectations from the IMF, and something must act to suppress the observability of SNe from progenitors that would otherwise produce large Mej explosions....
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...In order to determine the fraction of SNe producing each bin of Mej, the models were weighted by the IMF (Kroupa 2001)....
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...Rates of SE SNe compared to SNe II appear too high to only arise from the most massive stars, when considering the stellar initial mass function (IMF)....
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...One may expect very low Mej systems to be more abundant, given some proportionality between the initial mass of the star and the exploding core mass, and considering the shape of the stellar IMF....
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TL;DR: In this paper, a cosmological model for gamma-ray bursts is explored in which the radiation is produced as a broadly beamed pair fireball along the rotation axis of an accreting black hole.
Abstract: A cosmological model for gamma-ray bursts is explored in which the radiation is produced as a broadly beamed pair fireball along the rotation axis of an accreting black hole. The black hole may be a consequence of neutron star merger or neutron star-black hole merger, but for long complex bursts, it is more likely to come from the collapse of a single Wolf-Rayet star endowed with rotation ('failed' Type Ib supernova). The disk is geometrically thick and typically has a mass inside 100 km of several tenths of a solar mass. In the failed supernova case, the disk is fed for a longer period of time by the collapsing star. At its inner edge the disk is thick to its own neutrino emission and evolves on a viscous time scale of several seconds. In a region roughly 30 km across, interior to the accretion disk and along its axis of rotation, a pair fireball is generated by neutrino annihilation and electron-neutrino scattering which deposit approximately 10 exp 50 ergs/s.
2,399 citations
"Bolometric light curves and explosi..." refers background in this paper
...Fall-back SNe, in which little or none of the mass is ejected or direct collapse to a black hole for very massive pre-SN progenitors could be possible solutions (e.g. Woosley 1993; Fryer 1999; Heger et al. 2003; Fryer et al. 2009; Kochanek 2014)....
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TL;DR: In this article, the authors discuss how metallicity affects the evolution and final fate of massive stars, and derive the relative populations of stellar populations as a function of metallity.
Abstract: How massive stars die-what sort of explosion and remnant each produces-depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are the only means of mass loss, and these are a function of the metallicity of the star. We discuss how metallicity, and a simplified prescription for its effect on mass loss, affects the evolution and final fate of massive stars. We map, as a function of mass and metallicity, where black holes and neutron stars are likely to form and where different types of supernovae are produced. Integrating over an initial mass function, we derive the relative populations as a function of metallicity. Provided that single stars rotate rapidly enough at death, we speculate on stellar populations that might produce gamma-ray bursts and jet-driven supernovae.
2,007 citations
"Bolometric light curves and explosi..." refers background in this paper
...Fall-back SNe, in which little or none of the mass is ejected or direct collapse to a black hole for very massive pre-SN progenitors could be possible solutions (e.g. Woosley 1993; Fryer 1999; Heger et al. 2003; Fryer et al. 2009; Kochanek 2014)....
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TL;DR: In this paper, absolute magnitudes in the B, V, and I bands were derived for nine well-observed Type Ia supernovae, using host galaxy distances estimated via the surface brightness fluctuations or Tully-Fisher methods.
Abstract: Absolute magnitudes in the B, V, and I bands are derived for nine well-observed Type Ia supernovae, using host galaxy distances estimated via the surface brightness fluctuations or Tully-Fisher methods. These data indicate that there is a significant intrinsic dispersion in the absolute magnitudes at maximum light of Type Ia supernovae, amounting to +/- 0.8 mag in B, +/- 0.6 mag in V, and +/- 0.5 mag in I. Moreover, the absolute magnitudes appear to be tightly correlated with the initial rate of decline of the B light curve, with the slope of the correlation being steepest in B and becoming progressively flatter in the V and I bands. This implies that the intrinsic B - V colors of Type Ia supernovae at maximum light are not identical, with the fastest declining light curves corresponding to the intrinsically reddest events. Certain spectroscopic properties may also be correlated with the initial decline rate. These results are most simply interpreted as evidence for a range of progenitor masses, although variations in the explosion mechanism are also possible. Considerable care must be exercised in employing Type Ia supernovae as cosmological standard candles, particularly at large redshifts where Malmquist bias could be an important effect.
1,991 citations
"Bolometric light curves and explosi..." refers background in this paper
...2 is akin to the suggestion of a possible Phillips’ relation (i.e. brighter SNe have wider light curves; Phillips 1993) for GRB-SNe that is discussed in Schulze et al. (2014)....
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Abstract: The discovery of afterglows associated with gamma-ray bursts at X-ray, optical and radio wavelengths and the measurement of the redshifts of some of these events has established that gamma-ray bursts lie at extreme distances, making them the most powerful photon-emitters known in the Universe. Here we report the discovery of transient optical emission in the error box of the gamma-ray burst GRB980425, the light curve of which was very different from that of previous optical afterglows associated with gamma-ray bursts. The optical transient is located in a spiral arm of the galaxy ESO 184-GS2, which has a redshift velocity of only 2,550 km/ s. Its optical spectrum and location indicate that it is a very luminous supernova, which has been identified as SN1998bw. If this supernova and GRB980425 are indeed associated, the energy radiated in gamma-rays is at least four orders of magnitude less than in other gamma-ray bursts, although its appearance was otherwise unremarkable: this indicates that very different mechanisms can give rise to gamma-ray bursts. But independent of this association, the supernova is itself unusual, exhibiting an unusual light curve at radio wavelengths that requires that the gas emitting the radio photons be expanding relativistically.
1,823 citations