Improved Standardization of Type Ii-P Supernovae: Application to an Expanded Sample

Poznanski, D.; Butler, Nathaniel R.; Filippenko, A. V.; Ganeshalingam, M.; Li, Weidong; Bloom, J.; Chornock, R.; Foley, R. J.; Nugent, P.; Silverman, J. M.; Cenko, S. B.; Gates, E. L.; Leonard, Douglas C.; Miller, A. A.; Modjaz, M.; Serduke, F. J. D.; Smith, Nathan; Swift, B.; Wong, D. S.

doi:10.1088/0004-637x/694/2/1067

Cited by 157 publications

(252 citation statements)

References 76 publications

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“…To conclude, we find that the match to the photometric redshifts of the potential host galaxy and the supernova lightcurves, along with the fitted peak magnitude being consistent with a type IIP supernova (reddened by dust with R V similar to that found for the nearby sample of type IIP SNe in Poznanski et al 2009) to represent the most compelling fit to the transient behind A1689.…”

Section: A Transient Candidatesupporting

confidence: 65%

“…All available SN templates and a grid of redshifts (z = [0, 3]) and reddening parameters were tested (allowing for an intrinsic variation in the brightness) and the best fit was found for a type IIP template based on lightcurves of SN2001cy from Poznanski et al (2009), redshifted to z SN = 0.59. Moreover, the best fit of the transient colors was found by assuming that the SN is highly reddened, with a low total-to-selective extinction ratio (A V = 1.27, R V = 1.5), as shown in Fig.…”

Section: A Transient Candidatementioning

confidence: 99%

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Near-IR search for lensed supernovae behind galaxy clusters

Goobar

Paech

Stanishev³

et al. 2009

A&A

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Aims. Powerful gravitational telescopes in the form of massive galaxy clusters can be used to enhance the light collecting power over a limited field of view by about an order of magnitude in flux. This effect is exploited here to increase the depth of a survey for lensed supernovae at near-IR wavelengths. Methods. We present a pilot supernova search programme conducted with the ISAAC camera at VLT. Lensed galaxies behind the massive clusters A1689, A1835, and AC114 were observed for a total of 20 h divided into 2, 3, and 4 epochs respectively, separated by approximately one month to a limiting magnitude J < ∼ 24 (Vega). Image subtractions including another 20 h worth of archival ISAAC/VLT data were used to search for transients with lightcurve properties consistent with redshifted supernovae, both in the new and reference data. Results. The feasibility of finding lensed supernovae in our survey was investigated using synthetic lightcurves of supernovae and several models of the volumetric type Ia and core-collapse supernova rates as a function of redshift. We also estimate the number of supernova discoveries expected from the inferred star-formation rate in the observed galaxies. The methods consistently predict a Poisson mean value for the expected number of supernovae in the survey of between N SN = 0.8 and 1.6 for all supernova types, evenly distributed between core collapse and type Ia supernovae. One transient object was found behind A1689, 0.5 from a galaxy with photometric redshift z gal = 0.6 ± 0.15. The lightcurve and colors of the transient are consistent with being a reddened type IIP supernova at z SN = 0.59. The lensing model predicts 1.4 mag of magnification at the location of the transient, without which this object would not have been detected in the near-IR ground-based search described in this paper (unlensed magnitude J ∼ 25). We perform a feasibility study of the potential for lensed supernovae discoveries with larger and deeper surveys and conclude that the use of gravitational telescopes is a very exciting path for new discoveries. For example, a monthly rolling supernova search of a single very massive cluster with the HAWK-I camera at VLT would yield > ∼ 10 lensed supernova lightcurves per year, where type Ia supernovae would constitute about half of the expected sample. Conclusions.

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Section: A Transient Candidatesupporting

confidence: 65%

Section: A Transient Candidatementioning

confidence: 99%

Near-IR search for lensed supernovae behind galaxy clusters

Goobar

Paech

Stanishev³

et al. 2009

A&A

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“…If the above trend holds over all type II-P, L SNe, then objects such as SNe 2000dc and 2001do appear to be true intermediates in the sense that they are brighter at peak and have longer rise times than the average SN II-P, while they are fainter, and have shorter rise times than the average II-L. Interestingly, these very objects were culled by Poznanski et al (2009) from their sample of type II-P SNe to be used as distance indicators owing to their larger-than-average post-peak decline rates, while Faran et al (2014b) classified these as type II-L SNe for their study of type II SNe. Another case in point is SN 2013ej: dubbed a "slow-rising" type II-P SN by Valenti et al (2014), while Bose et al (2015) favour a "Type II-L" classification based on its post-peak decline rate.…”

Section: Rise Time Correlationsmentioning

confidence: 96%

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

A&A

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We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P.

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“…Recently, Dessart et al (2010) have provided an extensive grid of radiation-hydrodynamics simulations of artificial 0.1-3 B explosions driven by a piston at the base of nonrotating (Woosley et al 2002) expl More recently, Poznanski (2013) compiled a list of 23 SN IIP events whose progenitors had been determined from their presence in archival images of the host galaxy, or through upper limits to M ZAMS implied by non-detection in archival progenitor images. For 17 of these supernovae, Poznanski (2013) determined expansion velocities at the photosphere using the minimum of the 5169 Å Fe II spectral feature (Poznanski et al 2009) and propagated to day 50, v , p,50d on the plateau using Equation (2) of Nugent et al (2006). Poznanski (2013) found an approximately linear relation (albeit with substantial error bars) between v p,50d and the progenitor ZAMS masses, implying a strong dependence of the explosion energy on M ZAMS , such that E v .…”

Section: Introductionmentioning

confidence: 99%

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

Bruenn

Lentz

Hix

et al. 2016

ApJ

205

300

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We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M  zero-age main sequence progenitors. All of the simulations yield explosions and havebeen evolved for at least 1.2 s after core bounce and 1 s after material first becomes unbound. These simulations were computed with our CHIMERA code employing RbR spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 s after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident. We compute explosion energy estimates, including the negative gravitational binding energy of the stellar envelope outside the expanding shock, of 0.34, 0.88, 0.38, and 0.70 Bethe (B≡10 51 erg) and increasing at 0.03, 0.15, 0.19, and 0.52 B s 1 -, respectively, for the 12, 15, 20, and 25 M  models at the endpoint of this report. We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows. We discuss how the explosion energies may be subject to stochastic variations as exemplfied by the effect of the explosion geometry of the 20 M  model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. We compare our results for the explosion energies and ejected Ni 56 masses against some observational standards despite the large error bars in both models and observations.

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Improved Standardization of Type Ii-P Supernovae: Application to an Expanded Sample

Cited by 157 publications

References 76 publications

Near-IR search for lensed supernovae behind galaxy clusters

Near-IR search for lensed supernovae behind galaxy clusters

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

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