The Type I[CLC]a[/CLC] Supernova 1997[CLC]br[/CLC] in ESO 576-G40

Li, W. D.; Qiu, Y.; Qiao, Q. Y.; Zhu, Xizhou; Hu, Jingyao; Richmond, M.; Filippenko, A. V.; Treffers, R. R.; Peng, Chien Y.; Leonard, D. C.

doi:10.1086/300895

Cited by 62 publications

(32 citation statements)

References 50 publications

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“…All the spectra are corrected to the rest-frame using the redshifts (z helio ) of the hosts. The SN 1991T spectra is dereddened by E(B − V ) = 0.13 mag (Li et al 1999;Saha et al 2001). Host extinction for SN 1998aq (Reindl et al 2005 12 days after the date of maximum brightness in the Bband as spectroscopically most similar to a SN 1991T spectrum collected 16 days after maximum, while two SN 1991T-like SNe, SN 1997br and SN 1999aa (spectra collected 12 and 15 days after peak, respectively), are identified as the second and third most similar spectra.…”

Section: Spectramentioning

confidence: 98%

“…Figure 8 compares the SN 2009nr spectra with other SNe that are determined to be spectroscopically similar at the relevant phase by SNID (Blondin & Tonry 2007). Important spectral features have been identified using Li et al (1999) (Blondin & Tonry 2007). Important features are labeled along with the telluric lines (6800Å, 7200Å, and 7600Å).The data for SN 1991T, SN 1998aq, and SN 2003du are from Mazzali et al (1995, Branch et al (2003), and Stanishev et al (2007), respectively.…”

Section: Spectramentioning

confidence: 99%

“…Host extinction for SN 1998aq (Reindl et al 2005 12 days after the date of maximum brightness in the Bband as spectroscopically most similar to a SN 1991T spectrum collected 16 days after maximum, while two SN 1991T-like SNe, SN 1997br and SN 1999aa (spectra collected 12 and 15 days after peak, respectively), are identified as the second and third most similar spectra. In Figure 7, we compare the earliest SN 2009nr spectrum and the spectrum of SN 1997br (Li et al 1999) since both were collected 12 days after maximum. We also show a normal SN Ia template for the same postmaximum epoch (Hsiao et al 2007).…”

Section: Spectramentioning

confidence: 99%

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PRE-DISCOVERY AND FOLLOW-UP OBSERVATIONS OF THE NEARBY SN 2009nr: IMPLICATIONS FOR PROMPT TYPE Ia SUPERNOVAE

Khan

Prieto

Pojmański

et al. 2010

ApJ

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We present photometric and spectroscopic observations of the Type Ia supernova SN 2009nr in UGC 8255 (z = 0.0122). Following the discovery announcement at what turned out to be ten days after peak, we detected it at V ≃ 15.7 mag in data collected by the All Sky Automated Survey (ASAS) North telescope 2 weeks prior to the peak, and then followed it up with telescopes ranging in aperture from 10-cm to 6.5-m. Using early photometric data available only from ASAS, we find that the SN is similar to the over-luminous Type Ia SN 1991T, with a peak at M V ≃ −19.6 mag, and a slow decline rate of ∆m 15 (B) ≃ 0.95 mag. The early post-maximum spectra closely resemble those of SN 1991T, while the late time spectra are more similar to those of normal Type Ia SNe. Interestingly, SN 2009nr has a projected distance of 13.0 kpc (∼ 4.3 disk scale lengths) from the nucleus of the small star-forming host galaxy UGC 8255. This indicates that the progenitor of SN 2009nr is not associated with a young stellar population, calling into question the conventional association of luminous SNe Ia with the "prompt" component directly correlated with current star formation. The pre-discovery observation of SN 2009nr using ASAS demonstrates the science utility of high cadence all sky surveys conducted using small telescopes for the discovery of nearby (d 50 Mpc) supernovae. Subject headings: supernovae: general, individual (SN 2009nr) -galaxies (UGC 8255) 1 Based on observations obtained using the 10-cm ASAS North telescope in Hawaii, the 50-cm Dedicated Monitor of Exotransit (DEMONEX) telescope at the Winer Observatory, the 2.4-m Hiltner telescope at the MDM Observatory, the 2.5-m du Pont telescope at the Las Campanas Observatory, the 3.5-m Astrophysical Research Consortium (ARC) telescope at the Apache Point Observatory, and the 6.5-m Magellan I (Baade) Telescope at the Las Campanas Observatory.

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Section: Spectramentioning

confidence: 98%

Section: Spectramentioning

confidence: 99%

Section: Spectramentioning

confidence: 99%

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PRE-DISCOVERY AND FOLLOW-UP OBSERVATIONS OF THE NEARBY SN 2009nr: IMPLICATIONS FOR PROMPT TYPE Ia SUPERNOVAE

Khan

Prieto

Pojmański

et al. 2010

ApJ

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“…These are more evident before maximum and in the nebular phase, but they disappear in the 2–3 months following maximum (cf. Li et al 1999). In any case, differences among the spectra of ‘normal’ SNe Ia are small and can be appreciated only when observations of high signal‐to‐noise ratio are compared.…”

Section: The Spectral Evolutionmentioning

confidence: 99%

The template type Ia supernova 1996X

Salvo

Cappellaro

Mazzali

et al. 2001

Monthly Notices of the Royal Astronomical Society

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UBVRIJ photometry and optical spectra of the Type Ia SN 1996X obtained at ESO during a one-year-long observational campaign are presented, and supplemented by late time HST photometry. Spectroscopically, SN 1996X appears to be a `normal' SN Ia. The apparent magnitude at maximum was B=13.24 +/- 0.02, and the colour B-V=0.00 +/- 0.03. The luminosity decline rate, Delta m_B(15) = 1.31 +/- 0.08, is close to average for a SN Ia. The best estimate of the galactic extinction is A_B=0.30 +/- 0.05, and there is evidence that reddening within the parent galaxy is negligible. Detailed comparison of the light and colour curves of various `normal' SNe Ia shows that the assumption that multicolour light curves can be described simply as a one-parameter family is not perfect. Together with problems in the calibration of the templates, this may explain the discrepancies in the distance modulus derived adopting different calibrations of the absolute magnitude vs. light curve shape relations. Indeed we found that M_B ranges from -19.08 to -19.48 and M-m range from 32.02 to 32.48 depending on the method used (Hamuy et al. 1996a,Phillips et al. 1999, Riess et al. 1998a). Computations of model light curve and synthetic spectra for both early- and late-times, confirm that 1996X is a normal Type Ia SN and that a satisfactory fit can be obtained using a W7 progenitor structure only if we adopt the short distance. A larger distance would imply a too large Ni mass for this fainter than average SNIa.Comment: 17 pages, 17 figures. Accepted for publication in MNRA

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“…We compiled a set of publicly available SN Ia spectra from a variety of sources: the Berkeley Supernova Program (Silverman et al 2012), the CfA spectroscopic release (Blondin et al 2012) and the Carnegie Supernova Project (CSP) (Folatelli et al 2013). Spectra have been collected from the SUSPECT 2 (Barbon et al 1990;Mazzali et al 1995;Patat et al 1996;Turatto et al 1996;Gómez & López 1998;Turatto et al 1998;Jha et al 1999;Li et al 1999;Cappellaro et al 2001;Li et al 2001a;Salvo et al 2001;Hamuy et al 2002;Branch et al 2003a;Valentini et al 2003;Benetti et al 2004;Garavini et al 2004;Anupama et al 2005;Gerardy 2005;Kotak et al 2005;Chornock et al 2006;Elias-Rosa et al 2006;Altavilla et al 2007;Garavini et al 2007;Gerardy et al 2007;Hicken et al 2007;Krisciunas et al 2007;Leonard 2007;Pastorello et al 2007;Phillips et al 2007;Stanishev et al 2007;Matheson et al 2008;Pignata et al 2008;Taubenberger et al 2008;Wang et al 2008;Bufano et al 2009;…”

Section: Datamentioning

confidence: 99%

Exploring the spectroscopic diversity of Type Ia supernovae with dracula: a machine learning approach

Sasdelli

Ishida

Vilalta

et al. 2016

Mon. Not. R. Astron. Soc.

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The existence of multiple subclasses of type Ia supernovae (SNeIa) has been the subject of great debate in the last decade. One major challenge inevitably met when trying to infer the existence of one or more subclasses is the time consuming, and subjective, process of subclass definition. In this work, we show how machine learning tools facilitate identification of subtypes of SNe Ia through the establishment of a hierarchical group structure in the continuous space of spectral diversity formed by these objects. Using Deep Learning, we were capable of performing such identification in a 4 dimensional feature space (+1 for time evolution), while the standard Principal Component Analysis barely achieves similar results using 15 principal components. This is evidence that the progenitor system and the explosion mechanism can be described by a small number of initial physical parameters. As a proof of concept, we show that our results are in close agreement with a previously suggested classification scheme and that our proposed method can grasp the main spectral features behind the definition of such subtypes. This allows the confirmation of the velocity of lines as a first order effect in the determination of SN Ia subtypes, followed by 91bg-like events. Given the expected data deluge in the forthcoming years, our proposed approach is essential to allow a quick and statistically coherent identification of SNeIa subtypes (and outliers). All tools used in this work were made publicly available in the Python package DRACULA (Dimensionality Reduction And Clustering for Unsupervised Learning in Astronomy) and can be found within COINtoolbox (https://github.com/COINtoolbox/DRACULA).

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The Type I[CLC]a[/CLC] Supernova 1997[CLC]br[/CLC] in ESO 576-G40

Cited by 62 publications

References 50 publications

PRE-DISCOVERY AND FOLLOW-UP OBSERVATIONS OF THE NEARBY SN 2009nr: IMPLICATIONS FOR PROMPT TYPE Ia SUPERNOVAE

PRE-DISCOVERY AND FOLLOW-UP OBSERVATIONS OF THE NEARBY SN 2009nr: IMPLICATIONS FOR PROMPT TYPE Ia SUPERNOVAE

The template type Ia supernova 1996X

Exploring the spectroscopic diversity of Type Ia supernovae with dracula: a machine learning approach

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