The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations?

Phillips, M. M.; Li, Weidong; Frieman, Joshua A.; Блинников, С. И.; DePoy, D. L.; Prieto, J. L.; Milne, Peter; Contreras, C.; Folatelli, G.; Morrell, N.; Hamuy, M.; Suntzeff, Nicholas B.; Roth, M.; González, S.; Krzemiński, W.; Filippenko, A. V.; Freedman, Wendy L.; Chornock, R.; Jha, Saurabh W.; Madore, Barry F.; Persson, S. E.; Burns, C. R.; Wyatt, P.; Murphy, D. C.; Foley, R. J.; Ganeshalingam, M.; Serduke, F. J. D.; Krisciunas, K.; Bassett, Bruce A.; Becker, A. C.; Dilday, B.; Eastman, Jason D.; Garnavich, P.; Holtzman, Jon A.; Keßler, R.; Lampeitl, H.; Marriner, J.; Stephan, F.; Marshall, J. L.; Miknaitis, G.; Šako, M.; Schneider, Donald P.; Heyden, K. van der; Yasuda, Naoki

doi:10.1086/518372

Cited by 206 publications

(123 citation statements)

References 79 publications

(134 reference statements)

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“…Upon our request, Chris Burns has kindly calculated the ( ) -E B V , R V , and A V values and/or upper limits for the first two (SN 2002fk andSN 2003W). For the next two, SN2002bo and SN2014J, we rely on the values provided by Amanullah et al (2014) and Krisciunas et al (2004), and for SN2005hk we follow Phillips et al (2007). For SN2011ae there were no public photometric data.…”

Section: Observations and Ancillary Datamentioning

confidence: 99%

Continuum Foreground Polarization and Na i Absorption in Type Ia SNe*

Zelaya

Clocchiatti

Baade

et al. 2017

ApJ

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We present a study of the continuum polarization over the 400-600 nm range of 19 SNe Ia obtained with FORS at the VLT. We separate them into those that show Na ID lines at the velocity of their hosts and those that do not. Continuum polarization of the sodium sample near maximum light displays a broad range of values, from extremely polarized cases like SN2006X to almost unpolarized ones like SN2011ae. The non-sodium sample shows, typically, smaller polarization values. The continuum polarization of the sodium sample in the 400-600 nm range is linear with wavelength and can be characterized by the mean polarization (P mean ). Its values span a wide range and show a linear correlation with color, color excess, and extinction in the visual band. Larger dispersion correlations were found with the equivalent width of the Na ID and Ca II H and K lines, and also a noisy relation between P mean and R V , the ratio of total to selective extinction. Redder SNe show stronger continuum polarization, with larger color excesses and extinctions. We also confirm that high continuum polarization is associated with small values of R V . The correlation between extinction and polarization-and polarization angles-suggest that the dominant fraction of dust polarization is imprinted in interstellar regions of the host galaxies. We show that Na ID lines from foreground matter in the SN host are usually associated with non-galactic ISM, challenging the typical assumptions in foreground interstellar polarization models.

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Section: Observations and Ancillary Datamentioning

confidence: 99%

Continuum Foreground Polarization and Na i Absorption in Type Ia SNe*

Zelaya

Clocchiatti

Baade

et al. 2017

ApJ

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“…In particular, SN 2002cx (Filippenko 2003;Li et al 2003) has emerged as the namesake event for an emerging subclass of SNe Ia. SN 2002cx-like events are characterized by high-ionization iron lines in the premaximum spectra, but low expansion velocities and low peak luminosities (Jha et al 2006b;Phillips et al 2007;Valenti et al 2009;Foley et al 2009). Furthermore, the R-and I-band light curves did not feature the normal secondary maxima.…”

Section: Sn Ia Subclassesmentioning

confidence: 99%

NEAR-ULTRAVIOLET PROPERTIES OF A LARGE SAMPLE OF TYPE Ia SUPERNOVAE AS OBSERVED WITH THESwiftUVOT

Milne

Brown

Roming

et al. 2010

ApJ

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We present ultraviolet (UV) and optical photometry of 26 Type Ia supernovae (SNe Ia) observed from 2005 March to 2008 March with the NASA Swift Ultraviolet and Optical Telescope (UVOT). The dataset consists of 2133 individual observations, making it by far the most complete study of the UV emission from SNe Ia to date. Grouping the SNe into three subclasses as derived from optical observations, we investigate the evolution of the colors of these SNe, finding a high degree of homogeneity within the normal subclass, but dramatic differences between that group and the subluminous and SN 2002cx-like groups. For the normal events, the redder UV filters on UVOT (u, uvw1) show more homogeneity than do the bluer UV filters (uvm2, uvw2). Searching for purely UV characteristics to determine existing optically based groupings, we find the peak width to be a poor discriminant, but we do see a variation in the time delay between peak emission and the late, flat phase of the light curves. The UV light curves peak a few days before the B band for most subclasses (as was previously reported by Jha et al.), although the SN 2002cx-like objects peak at a very early epoch in the UV. That group also features the bluest emission observed among SNe Ia. As the observational campaign is ongoing, we discuss the critical times to observe, as determined by this study, in order to maximize the scientific output of future observations.

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“…In the end, there are a handful of objects for which the classification may be ambiguous. (Phillips et al 2007, and this work) compared to those of SN 2002cx (Li et al 2003;Jha et al 2006a). These ectra throughout their evolution, and diverge dramatically from normal SNe Ia at late times, as shown by comparison nd SN 1998bu (Jha et al 1999;Li et al 2001;Silverman et al 2012 We used Syn++ (Thomas et al 2011b) to model the permitted lines in the late-time spectra.…”

Section: Absolute Magnitudes Uvoir Light Cur Modelingmentioning

confidence: 60%

“…To speed tion, as discussed optically thick cells initial three days a thermodynamic equ used the 'big_gf-4' with a total of ⇠ 8 resulting broad-ban are shown in Figs Other peculiar declining light curv quently also in UVO has some shortcomi maximum decline maximum light cur and redder bands, b be a consequence o which is not able to We note, however, are only powered b we neglect any pos a pu↵ed-up stellar from the 56 Ni that f After maximum ligh cally thin, the boun kick in as an addit this intriguing poss However, looki curves, an insu ci and thus too low ej a B-band rise time too fast compared t (Phillips et al 2007 adapted from Kromer et al (2013) Fig. 6 Snapshots of a partial 3-d deflagration of a Chandrasekhar-mass carbon-oxygen white dwarf that leaves a bound remnant.…”

Section: Synthetic Obser V Ablesmentioning

confidence: 92%

“…I discuss analogues of SN 2002cx and well-studied examples like SN 2005hk Phillips et al 2007;Stanishev et al 2007;Sahu et al 2008), SN 2008A (McCully et al 2014b), SN 2012Z (Stritzinger et al 2015;Yamanaka et al 2015), and SN 2014ck (Tomasella et al 2016) as well as more extreme members of the class like SN 2008ha (Foley et al 2009;Valenti et al 2009) and SN 2010ae ). There may be some connection between SN Iax and other classes of peculiar white-dwarf supernovae (like SN 2002es-like objects; Ganeshalingam et al 2012;White et al 2015;Cao et al 2016) but I restrict my focus to SN Iax here; other peculiar objects are explored by Taubenberger (2016).…”

Section: Introductionmentioning

confidence: 98%

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Type Iax Supernovae

Jha

2017

Handbook of Supernovae

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Type Iax supernovae (SN Iax), also called SN 2002cx-like supernovae, are the largest class of "peculiar" white dwarf (thermonuclear) supernovae, with over fifty members known. SN Iax have lower ejecta velocity and lower luminosities, and these parameters span a much wider range, than normal type Ia supernovae (SN Ia). SN Iax are spectroscopically similar to some SN Ia near maximum light, but are unique among all supernovae in their late-time spectra, which never become fully "nebular". SN Iax overwhelmingly occur in late-type host galaxies, implying a relatively young population. The SN Iax 2012Z is the only white dwarf supernova for which a pre-explosion progenitor system has been detected. A variety of models have been proposed, but one leading scenario has emerged: a type Iax supernova may be a pure-deflagration explosion of a carbonoxygen (or hybrid carbon-oxygen-neon) white dwarf, triggered by helium accretion to the Chandrasekhar mass, that does not necessarily fully disrupt the star.

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The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations?

Cited by 206 publications

References 79 publications

Continuum Foreground Polarization and Na i Absorption in Type Ia SNe*

Continuum Foreground Polarization and Na i Absorption in Type Ia SNe*

NEAR-ULTRAVIOLET PROPERTIES OF A LARGE SAMPLE OF TYPE Ia SUPERNOVAE AS OBSERVED WITH THESwiftUVOT

Type Iax Supernovae

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