CHARACTERIZING THE<i>V</i>-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE

Anderson, J. P.; González–Gaitán, S.; Hamuy, M.; Gutiérrez, C. P.; Stritzinger, M. D.; Olivares, E. F.; Phillips, M. M.; Schulze, S.; Antezana, R.; Bolt, Luis; Campillay, A.; Castellón, S.; Contreras, C.; Jaeger, Thomas de; Folatelli, G.; Förster, F.; Freedman, Wendy L.; González, L.; Hsiao, E. Y.; Krzemiński, W.; Krisciunas, K.; Maza, J.; McCarthy, Patrick J.; Morrell, N.; Persson, S. E.; Roth, M.; Salgado, Francisco; Suntzeff, Nicholas B.; Thomas-Osip, J. E.

doi:10.1088/0004-637x/786/1/67

Cited by 282 publications

(486 citation statements)

References 108 publications

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“…They are characterized by hydrogenrich spectra (e.g., Filippenko et al 1997), and their light curves exhibit a fast rise to peak (Rubin et al 2015, hereafter R15), followed by a long (∼90 d) plateau in the case of SNe IIP or by a linear decline (>1.4 mag/100 d) in the case of SNe IIL. Anderson et al (2014) show that these two subclasses may actually be the extremes of a continuum, with several objects showing intermediate light-curve slopes. The nature of the progenitors of SNe IIP is well established: pre-explosion images at their locations show extended (R 500 R ) red supergiants (RSGs) in the mass range between 8.5 and 17 M (Smartt 2009).…”

Section: Introductionmentioning

confidence: 91%

“…Based on the light curves and the spectra of each SN, we subclassified our SNe into SNe IIP or IIL. Objects with a decline rate (s 2 in Anderson et al 2014) >1.4 mag/100 d during the plateau phase and a low ratio between the EW of Hα in absorption and emission were classified as SNe IIL. In Table A.1 we label the SNe IIL with an asterisk "*".…”

Section: Introductionmentioning

confidence: 99%

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Metallicity from Type II supernovae from the (i)PTF

Taddia

Moquist

Sollerman

et al. 2016

A&A

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Type IIP supernovae (SNe IIP) have recently been proposed as metallicity (Z) probes. The spectral models of Dessart et al. (2014, MNRAS, 440, 1856 showed that the pseudo-equivalent width of Fe ii λ5018 (pEW 5018 ) during the plateau phase depends on the primordial Z, but there was a paucity of SNe IIP exhibiting pEW 5018 that were compatible with Z < 0.4 Z . This lack might be due to some physical property of the SN II population or to the fact that those SNe have been discovered in luminous, metal-rich targeted galaxies. Here we use SN II observations from the untargeted (intermediate) Palomar Transient Factory [(i)PTF] survey, aiming to investigate the pEW 5018 distribution of this SN population and, in particular, to look for the presence of SNe II at lower Z. We perform pEW 5018 measurements on the spectra of a sample of 39 (i)PTF SNe II, selected to have well-constrained explosion epochs and light-curve properties. Based on the comparison with the pEW 5018 spectral models, we subgrouped our SNe into four Z bins from Z ≈ 0.1 Z up to Z ≈ 2 Z . We also independently investigated the Z of the hosts by using their absolute magnitudes and colors and, in a few cases, using strong-line diagnostics from spectra. We searched for possible correlations between SN observables, such as their peak magnitudes and the Z inferred from pEW 5018 . We found 11 events with pEW 5018 that were small enough to indicate Z ≈ 0.1 Z . The trend of pEW 5018 with Z matches the Z estimates obtained from the host-galaxy photometry, although the significance of the correlation is weak. We also found that SNe with brighter peak magnitudes have smaller pEW 5018 and occur at lower Z.

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Section: Introductionmentioning

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Metallicity from Type II supernovae from the (i)PTF

Taddia

Moquist

Sollerman

et al. 2016

A&A

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“…Although type II-L SNe generally exhibit a weaker P Cygni absorption profile at the Hα line than type II-P SNe (Schlegel 1996), separating these types can be difficult without light curves which are not always available -not to mention that e.g. Anderson et al (2014) argue that there is no unambiguous borderline between types II-P and II-L at all. The A12 SN subsamples may therefore be affected by mixing between the subtypes (for example, one type Ib/IIb SN was included as half a type Ib and half a type IIb).…”

Section: Sn Samplesmentioning

confidence: 99%

“…Barbon, Ciatti & Rosino 1979), types II-P and II-L are now more commonly thought to occupy a continuum of different levels of mass loss primarily influenced by the initial mass of the progenitor (e.g. Anderson et al 2014;Sanders et al 2015;González-Gaitán et al 2015). Type IIn ('narrow lines') SNe are characterized by the presence of a dense circumstellar medium (CSM) at the time of explosion, resulting in strong interaction between the SN ejecta and the CSM (e.g.…”

Section: Introductionmentioning

confidence: 99%

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

Kangas

Portinari

Mattila

et al. 2017

A&A

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We study the spatial correlations between the H α emission and different types of massive stars in two local galaxies, the Large Magellanic Cloud (LMC) and Messier 33. We compare these to correlations derived for core-collapse supernovae (CCSNe) in the literature to connect CCSNe of different types with the initial masses of their progenitors and to test the validity of progenitor mass estimates which use the pixel statistics method. We obtain samples of evolved massive stars in both galaxies from catalogues with good spatial coverage and/or completeness, and combine them with coordinates of main-sequence stars in the LMC from the SIMBAD database. We calculate the spatial correlation of stars of different classes and spectral types with H α emission. We also investigate the effects of distance, noise and positional errors on the pixel statistics method. A higher correlation with H α emission is found to correspond to a shorter stellar lifespan, and we conclude that the method can be used as an indicator of the ages, and therefore initial masses, of SN progenitors. We find that the spatial distributions of type II-P SNe and red supergiants of appropriate initial mass ( 9 M ) are consistent with each other. We also find the distributions of type Ic SNe and WN stars with initial masses 20 M consistent, while supergiants with initial masses around 15 M are a better match for type IIb and II-L SNe. The type Ib distribution corresponds to the same stellar types as type II-P, which suggests an origin in interacting binaries. On the other hand, we find that luminous blue variable stars show a much stronger correlation with H α emission than do type IIn SNe.

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“…SNe II-P show a plateau of ∼100 days duration, while SNeII-L show a more linear (in magnitude) decay. The distinction between Types II-L and II-P is somewhat controversial Anderson et al 2014;Faran et al 2014;Sanders et al 2015).…”

Section: Introductionmentioning

confidence: 99%

FLASH SPECTROSCOPY: EMISSION LINES FROM THE IONIZED CIRCUMSTELLAR MATERIAL AROUND <10-DAY-OLD TYPE II SUPERNOVAE

Khazov

Yaron

Gal‐Yam

et al. 2016

ApJ

212

223

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Supernovae (SNe) embedded in dense circumstellar material (CSM) may show prominent emission lines in their early-time spectra ( 10 days after the explosion), owing to recombination of the CSM ionized by the shockbreakout flash. From such spectra ("flash spectroscopy"), we can measure various physical properties of the CSM, as well as the mass-loss rate of the progenitor during the year prior to its explosion. Searching through the Palomar Transient Factory (PTF and iPTF) SN spectroscopy databases from 2009 through 2014, we found 12 SNe II showing flash-ionized (FI) signatures in their first spectra. All are younger than 10 days. These events constitute 14% of all 84 SNe in our sample having a spectrum within 10 days from explosion, and 18% of SNeII observed at ages <5 days, thereby setting lower limits on the fraction of FI events. We classified as "blue/featureless" (BF) those events having a first spectrum that is similar to that of a blackbody, without any emission or absorption signatures. It is possible that some BF events had FI signatures at an earlier phase than observed, or that they lack dense CSM around the progenitor. Within 2 days after explosion, 8 out of 11 SNe in our sample are either BF events or show FI signatures. Interestingly, we found that 19 out of 21 SNe brighter than an absolute magnitude M R =−18.2 belong to the FI or BF groups, and that all FI events peaked above M R =−17.6 mag, significantly brighter than average SNeII.

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CHARACTERIZING THEV-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE

Cited by 282 publications

References 108 publications

Metallicity from Type II supernovae from the (i)PTF

Metallicity from Type II supernovae from the (i)PTF

Core-collapse supernova progenitor constraints using the spatial distributions of massive stars in local galaxies

FLASH SPECTROSCOPY: EMISSION LINES FROM THE IONIZED CIRCUMSTELLAR MATERIAL AROUND <10-DAY-OLD TYPE II SUPERNOVAE

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