Asiago Supernova classification program: Blowing out the first two hundred candles

Tomasella, L.; Benetti, S.; Pastorello, A.; Turatto, M.; Barbon, R.; Elias‐Rosa, N.; Harutyunyan, A.; Ochner, P.; Tartaglia, L.; Valenti, S.

doi:10.1002/asna.201412068

Cited by 34 publications

(40 citation statements)

References 56 publications

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“…Similarly, Johnson et al (2017) only assumed Galactic reddening of E(B − V) = 0.03 mags, in their analysis of pre-explosion observations of SN 2012fh. From a spectrum of SN 2012fh, from the Asiago Supernova classification program (Tomasella et al 2014), we find a strong Na I D absorption feature, at the recessional velocity of the host galaxy, for which we measure an equivalent width of 3.8 Å. As with SN 2000ew, this is beyond the range established for the Poznanski et al relation, but supports high levels of extinction arising in the host galaxy.…”

Section: Extinctionsupporting

confidence: 49%

The very young resolved stellar populations around stripped-envelope supernovae

Maund

2018

Monthly Notices of the Royal Astronomical Society

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The massive star origins for Type IIP supernovae (SNe) have been established through direct detection of their red supergiants progenitors in pre-explosion observations; however, there has been limited success in the detection of the progenitors of H-deficient SNe. The final fate of more massive stars, capable of undergoing a Wolf-Rayet phase, and the origins of Type Ibc SNe remains debated, including the relative importance of single massive star progenitors or lower mass stars stripped in binaries. We present an analysis of the ages and spatial distributions of massive stars around the sites of 23 stripped-envelope SNe, as observed with the Hubble Space Telescope, to probe the possible origins of the progenitors of these events. Using a Bayesian stellar populations analysis scheme, we find characteristic ages for the populations observed within 150 pc of the target Type IIb, Ib and Ic SNe to be log(t) = 7.20, 7.05 and 6.57, respectively. The Type Ic SNe in the sample are nearly all observed within 100 pc of young, dense stellar populations. The environment around SN 2002ap is an important exception both in terms of age and spatial properties. These findings may support the hypothesis that stars with M init > 30M produce a relatively large proportion of Type Ibc SNe, and that these SN subtypes arise from progressively more massive progenitors. Significantly higher extinctions are derived towards the populations hosting these SNe than previously used in analysis of constraints from pre-explosion observations. The large initial masses inferred for the progenitors are in stark contrast with the low ejecta masses estimated from SN light curves.

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Section: Extinctionsupporting

confidence: 49%

The very young resolved stellar populations around stripped-envelope supernovae

Maund

2018

Monthly Notices of the Royal Astronomical Society

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“…ASASSN-15uh was reported as a 98es-like SN Ia by the Asiago Transient Classification Program (Tomasella et al 2014;Turatto et al 2015). Due to the limited photometric and spectroscopic information of both the SN and its host galaxy, we took a low-resolution spectrum of the host galaxy with the Line Imager and Slit Spectrograph (LISS; Hashiba et al 2014) mounted on the Nayuta 2-m telescope in December 2017.…”

Section: Luminous Eexsne Iamentioning

confidence: 99%

Surface Radioactivity or Interactions? Multiple Origins of Early-excess Type Ia Supernovae and Associated Subclasses

Jiang

Doi

Maeda

et al. 2018

ApJ

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Early-phase Type Ia supernovae (SNe Ia), especially those with luminosity enhancement within the first few days of explosions ("early-excess SNe Ia"), play an irreplaceable role in addressing the long-standing progenitor and explosion issue of SNe Ia. In this paper, we systematically investigate 11 early-excess SNe Ia from subluminous to luminous subclasses. Eight of them are selected from 23 SNe Ia with extremely early-phase optical light curves ("golden" early-phase SNe Ia), and three of them are selected from 40 SNe Ia (including 14 golden samples) with early-phase UV/NUV light curves. We found that previously discovered early-excess SNe Ia show a clear preference for specific SN Ia subclasses. In particular, the early-excess feature shown in all six luminous (91T-and 99aa-like) SNe Ia is in conflict with the viewing angle dependence predicted by the companion-ejecta interaction scenario. Instead, such a high early-excess fraction is likely related to the explosion physics of luminous SNe Ia; i.e. a more efficient detonation happening in the progenitor of luminous SNe Ia may consequently account for the early-excess feature powered by the radiation from a 56 Ni-abundant outer layer. The diversity of early-excess features shown in different SN Ia subclasses suggests multiple origins of the discovered early-excess SNe Ia, challenging their applicability as a robust progenitor indicator. Further understanding of the early-excess diversity relies not only on multiband photometry and promptresponse spectroscopy of individual early-excess SNe Ia but also on investigations of the general early-phase light-curve behavior of each SN Ia subclass, which can be realized through ongoing/forthcoming transient survey projects in the near future.

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“…The archive provides also the important references to the original publications, which we considered along with the Astronomer's Telegram 4 (ATEL), website of the Central Bureau for Astronomical Telegrams 5 (CBAT) and other supporting publications (e.g. Branch et al 1993;Silverman et al 2012;Tomasella et al 2014). In total, we managed to collect the subclasses for 109 SNe in 104 host galaxies: 66 SNe are normal, 41 SNe are 91bg-like, and two SNe are 06gz-like (super-Chandrasekhar) events.…”

Section: Sample Selection and Reductionmentioning

confidence: 99%

Supernovae and their host galaxies – VI. Normal Type Ia and 91bg-like supernovae in ellipticals

Barkhudaryan

Hakobyan

Karapetyan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the galactocentric distributions of the "normal" and peculiar "91bglike" subclasses of 109 supernovae (SNe) Ia, and study the global parameters of their elliptical hosts. The galactocentric distributions of the SN subclasses are consistent with each other, and with the radial light distribution of host stellar populations, when excluding bias against central SNe. Among the global parameters, only the distributions of u−r colours and ages are inconsistent significantly between the ellipticals of different SN Ia subclasses: the normal SN hosts are on average bluer/younger than those of 91bg-like SNe. In the colour-mass diagram, the tail of colour distribution of normal SN hosts stretches into the Green Valley -transitional state of galaxy evolution, while the same tail of 91bg-like SN hosts barely reaches that region. Therefore, the bluer/younger ellipticals might have more residual star formation that gives rise to younger "prompt" progenitors, resulting in normal SNe Ia with shorter delay times. The redder and older ellipticals that already exhausted their gas for star formation may produce significantly less normal SNe with shorter delay times, outnumbered by "delayed" 91bg-like events. The host ages (lower age limit of the delay times) of 91bg-like SNe does not extend down to the stellar ages that produce significant u-band fluxes -the 91bg-like events have no prompt progenitors. Our results favor SN Ia progenitor models such as He-ignited violent mergers that have the potential to explain the observed SN/host properties.

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Asiago Supernova classification program: Blowing out the first two hundred candles

Cited by 34 publications

References 56 publications

The very young resolved stellar populations around stripped-envelope supernovae

The very young resolved stellar populations around stripped-envelope supernovae

Surface Radioactivity or Interactions? Multiple Origins of Early-excess Type Ia Supernovae and Associated Subclasses

Supernovae and their host galaxies – VI. Normal Type Ia and 91bg-like supernovae in ellipticals

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