Comparative Direct Analysis of Type Ia Supernova Spectra. I. SN 1994D

By D. Branch, M. Troxel, D. Jeffery, K. Hatano, Miriam Musco, J. Parrent, Eddie Baron, L. Dang, D. Casebeer, N. Hall and 1 more. 2005

232 citations recorded by the source corpus.

As the first step in a comprehensive, comparative, direct analysis of the spectra of Type Ia supernovae (SNe Ia), we use the parameterized supernova synthetic‐spectrum code SYNOW to interpret 26 spectra of the well‐observed SN 1994D. Our results are consistent with the traditional view that the composition structure (element abundance fractions versus ejection velocity) is radially stratified. We find that resonance‐scattering features due to permitted lines of Ca ii, Na i, and Fe ii persist to more than 100 days after explosion. The fitting parameters for SN 1994D, together with those to be determined for other SNe Ia, will provide an internally consistent quantification of the spectroscopic diversity among SNe Ia and shed light on how the various manifestations of observational diversity are related to their physical causes.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/aaa0e1b749941cade9623f6e1dff5e621bf0837c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Filippenko
2. A. Riess
3. N. Smith
4. F. Mannucci
5. S. Jha
6. Ryan Chornock
7. R. Kirshner
8. Weidong Li

Citations in the corpus

• Time-dependent Monte Carlo Radiative Transfer Calculations for Three-dimensional Supernova Spectra, Light Curves, and Polarization (2006, background): “However, note that Branch et al. (2005) has shown, surprisingly, that resonance line scattering by permitted transitions actually does a good job of characterizing the spectrum out past texp= 200 days.”
• THE SPECTROSCOPIC DIVERSITY OF TYPE Ia SUPERNOVAE (2000, methodology): “We do not attempt to confirm these detections with parameterized spectrum synthesis codes as done by Parrent et al. (2011) using SYNOW (e.g., Branch et al. 2005) or by Thomas et al. (2011a) using SYNAPPS (Thomas et al. 2011b), but most of the tentative C ii identifications (17 out of 24) correspond…”
• Optical and Near-Infrared Observations of the Highly Reddened, Rapidly Expanding Type Ia Supernova SN 2006X in M100 (2007, methodology): “The line identifications adopted here are taken from Branch et al. (2005, 2006).”
• High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios (2010, methodology): “Spectroscopically fairly similar to ordinary SNe Ia (of the core-normal or shallow-silicon variety; Branch et al. 2006), these objects will be identified as SNe Ia in surveys, especially at high z where the S/N of spectra is usually poor.”
• Constraints on the Physics of Type Ia Supernovae from the X-Ray Spectrum of the Tycho Supernova Remnant (2005, background): “…theoreticalmodels,mostly through the optical/IR spectra (e.g., Höflich& Khokhlov 1996; Fisher et al. 1997; Höflich et al.1998;Wheeler et al. 1998; Branch et al. 2005; Kozma et al. 2005) and light curves (e.g., Höflich et al. 1998; Stritzinger et al. 2005) of Type Ia SNe and also through the…”
• An Open Catalog for Supernova Data (2016, background): “…commonalities between seemingly different supernova types, to generating mean spectra and exploring spectroscopic diversity (Benetti et al. 2005; Branch et al. 2005, 2006, 2007, 2008, 2009; Wang et al. 2009; Blondin et al. 2012; Folatelli et al. 2013; Maguire et al. 2014; Sasdelli et al. 2015,…”
• Theoretical light curves for deflagration models of Type Ia supernova (2006, methodology): “Similar values are found by Branch et al. (2005), see Fig.”
• Spectrophotometric time series of SN 2011fe from the Nearby Supernova Factory (2013, unknown): “…(Nugent et al. 1995; Bongard et al. 2006); the R642/443 flux ratio (Bailey et al. 2009); the Ca H&K (Walker et al. 2010), Si λ4131 (Bronder et al. 2008; Arsenijevic et al. 2008; Chotard et al. 2011), Si λ5972 & λ6355 (Hachinger et al. 2006; Branch et al. 2006, 2009) and C λ6580 (cf. Sect.”
• The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations? (2006, background): “As Branch et al. (2006) have speculated, it may be that these two subclasses of SNe Ia have little in common except a high initial temperature.”
• VARIABLE SODIUM ABSORPTION IN A LOW-EXTINCTION TYPE Ia SUPERNOVA, (2009, methodology): “…displaying variable absorption share common features in their early-time and maximum-light spectra, classifying them in the broad line group according to Branch et al. (2009) and the high velocity gradient group of Benetti et al. (2005, although the HVG classification of SN 2007le is less firm).”
• The Progenitors of Type Ia Supernovae (2012, background): “…Ia explosion dominates its maximum luminosity (Arnett, 1982), but the origin of the variation of the amount of56Ni for 8There is increasing evidence showing that even the normal SNe Ia exhibit diversity in their spectral features (e.g. Branch et al., 2009; Wang et al., 2009c; Blondin et al., 2012).”
• The Carnegie Supernova Project. I. Third Photometry Data Release of Low-redshift Type Ia Supernovae and Other White Dwarf Explosions (2017, methodology): “Also given are classifications in the Branch et al. (2006) and Wang et al. (2009) schemes using the same criteria as Folatelli et al. (2013).”
• Spectropolarimetry of Supernovae (2008, background): “J., 623, 1011 Blondin & Mezzacappa(2007)Blondin, J. M., & Mezzacappa, A. 2007, Nature, 445, 58 Boisseau, Wheeler, Oran, & Khokhlov(1996)Boisseau, J. R., Wheeler, J. C., Oran, E. S., & Khokhlov, A. M. 1996, ApJl, 471, L99 Branch et al.(2006)Branch, D., et al. 2006, Pub.”
• Two populations of progenitors for type ia supernovae (2005, result): “• Finally we notice that the existence of a continuous sequence in the spectroscopic properties of maximum light spectra of SNe Ia (Branch et al. 2006) is not at variance with the existence of two different evolutionary paths to rise SNe Ia, as our results may suggest.”
• IMPROVED DISTANCES TO TYPE Ia SUPERNOVAE WITH TWO SPECTROSCOPIC SUBCLASSES (2009, methodology): “Based on the EW of the absorption near Si IIλ5972 and Si IIλ6355, Branch et al. (2006, 2009) suggest dividing the SN Ia sample into four groups: cool (CL), shallow silicon (SS), core normal (CN), and broad line (BL); their CL and SS groups consist mainly of peculiar events such as SN 1991bg and SN…”