The diversity of Type II supernova versus the similarity in their progenitors

Valenti, S.; Howell, D. A.; Stritzinger, M. D.; Graham, M. L.; Hosseinzadeh, G.; Arcavi, I.; Bildsten, Lars; Jerkstrand, A.; McCully, C.; Pastorello, A.; Piro, Anthony L.; Sand, David J.; Smartt, S. J.; Terreran, G.; Baltay, C.; Benetti, S.; Brown, P. J.; Filippenko, A. V.; Fraser, M.; Rabinowitz, D.; Sullivan, M.; Yuan, F.

doi:10.1093/mnras/stw870

Cited by 290 publications

(435 citation statements)

References 135 publications

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“…Global fitting of all observations removes manual procedures such as correction for reddening and construction of L bol , and replaces them with functions that are consistently and mechanically applied to all objects. The observational uncertainties can thus be propagated Childress et al (2016); Valenti et al (2016) through these functions revealing covariances between quantities of interest. The global part of the model is an empirical description of the evolution of the supernova spectral energy distribution (SED), which is separated in achromatic changes of photospheric radius constrained by the expansion velocities, and chromatic changes in the SED arising from the temperature evolution constrained by photometry.…”

Section: Modelmentioning

confidence: 99%

“…The success of amateur and professional supernova surveys (e.g., Calán/Tololo, Hamuy et al 1993;LOSS, Li et al 2011;CHASE, Pignata et al 2009; PTF/iPTF, Rau et al 2009;Pan-Starrs, Kaiser et al 2002;ASAS-SN, Shappee et al 2014) has been paramount for follow-up studies that have uncovered the full range of observed and physical properties of normal SN II as well as significant correlations between some of their properties (e.g. Hamuy 2003;Arcavi et al 2012;Anderson et al 2014;Faran et al 2014;Gutiérrez et al 2014;Sanders et al 2015;Pejcha & Prieto 2015a,b;Holoien et al 2016;Valenti et al 2016;Rubin et al 2016). Hydrodynamical models of explosions of hydrogen-rich massive stars explain relatively well most of the main features of the light curves and spectra * tmuller@astro.puc.cl of normal SN II (e.g.…”

Section: Introductionmentioning

confidence: 99%

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The Nickel Mass Distribution of Normal Type II Supernovae

Müller

Prieto

Pejcha

et al. 2017

ApJ

107

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Core-collapse supernova explosions expose the structure and environment of massive stars at the moment of their death. We use the global fitting technique of Pejcha & Prieto (2015a,b) to estimate a set of physical parameters of 19 normal Type II SNe, such as their distance moduli, reddenings, 56 Ni masses M Ni , and explosion energies E exp from multicolor light curves and photospheric velocity curves. We confirm and characterize known correlations between M Ni and bolometric luminosity at 50 days after the explosion, and between M Ni and E exp . We pay special attention to the observed distribution of M Ni coming from a joint sample of 38 Type II SNe, which can be described as a skewed-Gaussian-like distribution between 0.005 M ⊙ and 0.280 M ⊙ , with a median of 0.031 M ⊙ , mean of 0.046 M ⊙ , standard deviation of 0.048 M ⊙ and skewness of 3.050. We use twosample Kolmogorov-Smirnov test and two-sample Anderson-Darling test to compare the observed distribution of M Ni to results from theoretical hydrodynamical codes of core-collapse explosions with the neutrino mechanism presented in the literature. Our results show that the theoretical distributions obtained from the codes tested in this work, KEPLER and Prometheus Hot Bubble, are compatible with the observations irrespective of different pre-supernova calibrations and different maximum mass of the progenitors.

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Section: Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Nickel Mass Distribution of Normal Type II Supernovae

Müller

Prieto

Pejcha

et al. 2017

ApJ

107

View full text Add to dashboard Cite

show abstract

“…After the images are taken, they are automatically ingested and processed by the LCOGTSNpipe pipeline (Valenti et al 2016) and displayed on a webpage for manual scanning, next to SDSS (if available) and DSS images of the field for comparison. Image subtraction can then be performed in order to detect faint transients using SDSS templates when available or subtracting the different LCO epochs off of each other to search for changing sources, otherwise.…”

Section: The Triggering Processmentioning

confidence: 99%

Optical Follow-up of Gravitational-wave Events with Las Cumbres Observatory

Arcavi

McCully

Hosseinzadeh

et al. 2017

ApJ

111

106

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We present an implementation of the Gehrels et al. (2016) galaxy-targeted strategy for gravitationalwave (GW) follow-up using the Las Cumbres Observatory global network of telescopes. We use the Galaxy List for the Advanced Detector Era (GLADE) galaxy catalog, which we show is complete (with respect to a Schechter function) out to ∼ 300 Mpc for galaxies brighter than the median Schechter function galaxy luminosity. We use a prioritization algorithm to select the galaxies with the highest chance of containing the counterpart given their luminosity, their position, and their distance relative to a GW localization, and in which we are most likely to detect a counterpart given its expected brightness compared to the limiting magnitude of our telescopes. This algorithm can be easily adapted to any expected transient parameters and telescopes. We implemented this strategy during the second Advanced Detector Observing Run (O2) and followed the black hole merger GW170814 and the neutron star merger GW170817. For the latter, we identified an optical kilonova/macronova counterpart thanks to our algorithm selecting the correct host galaxy fifth in its ranked list among 182 galaxies we identified in the Laser Interferometer Gravitational-wave Observatory LIGO-Virgo localization. This also allowed us to obtain some of the earliest observations of the first optical transient ever triggered by a GW detection (as presented in a companion paper).

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“…The SN exhibited a peak absolute magnitude of~-17.5 and a nebular-phase decline rate consistent with a small mass of radioactive 56 Ni in the range 0.013-0.023 M e (Dhungana et al 2016;Yuan et al 2016). Although SN 2013ej was initially classified as an SN II-P (Leonard et al 2013;Valenti et al 2014), subsequent studies showed that the relatively fast decline rate during the recombination phase (∼1.2 mag in the first 50 days after rising up to the plateau; Valenti et al 2016) and some of the spectroscopic features appeared similar to those of SNe from the II-L class (Bose et al 2015;Huang et al 2015;Dhungana et al 2016;Valenti et al 2016). The distinction between SNII-L and II-P light curves is not always obvious (Anderson et al 2014;Sanders et al 2015); indeed, large samples have revealed a continuum of light-curve morphologies that are intermediate between sources classified as SNe II-P and SNe II-L.…”

Section: Introductionmentioning

confidence: 99%

Asphericity, Interaction, and Dust in the Type Ii-P/Ii-L Supernova 2013ej in Messier 74

Mauerhan

Dyk

Johansson

et al. 2017

ApJ

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SN 2013ej is a well-studied core-collapse supernova (SN) that stemmed from a directly identified red supergiant (RSG) progenitor in galaxy M74. The source exhibits signs of substantial geometric asphericity, X-rays from persistent interaction with circumstellar material (CSM), thermal emission from warm dust, and a light curve that appears intermediate between supernovae of Types II-P and II-L. The proximity of this source motivates a close inspection of these physical characteristics and their potential interconnection. We present multiepoch spectropolarimetry of SN 2013ej during the first 107 days and deep optical spectroscopy and ultraviolet through infrared photometry past ∼800 days. SN 2013ej exhibits the strongest and most persistent continuum and line polarization ever observed for a SN of its class during the recombination phase. Modeling indicates that the data are consistent with an oblate ellipsoidal photosphere, viewed nearly edge-on and probably augmented by optical scattering from circumstellar dust. We suggest that interaction with an equatorial distribution of CSM, perhaps the result of binary evolution, is responsible for generating the photospheric asphericity. Relatedly, our late-time optical imaging and spectroscopy show that asymmetric CSM interaction is ongoing, and the morphology of broad Hα emission from shock-excited ejecta provides additional evidence that the geometry of the interaction region is ellipsoidal. Alternatively, a prolate ellipsoidal geometry from an intrinsically bipolar explosion is also a plausible interpretation of the data but would probably require a ballistic jet of radioactive material capable of penetrating the hydrogen envelope early in the recombination phase. Finally, our latest space-based optical imaging confirms that the late interaction-powered light curve dropped below the stellar progenitor level, confirming the RSG star's association with the explosion.

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The diversity of Type II supernova versus the similarity in their progenitors

Cited by 290 publications

References 135 publications

The Nickel Mass Distribution of Normal Type II Supernovae

The Nickel Mass Distribution of Normal Type II Supernovae

Optical Follow-up of Gravitational-wave Events with Las Cumbres Observatory

Asphericity, Interaction, and Dust in the Type Ii-P/Ii-L Supernova 2013ej in Messier 74

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