Detailed Analysis of Early to Late-Time Spectra of Supernova 1993J

By Thomas Matheson, A. Filippenko, Luis C. Ho, A. Barth, D. Leonard. 2000

201 citations recorded by the source corpus.

We present a detailed study of line structure in early to late-time spectra of supernova (SN) 1993J. Spectra during the nebular phase, but within the first two years after explosion, exhibit small-scale structure in the emission lines of some species, notably oxygen and magnesium, showing that the ejecta of SN 1993J are clumpy. On the other hand, a lack of structure in emission lines of calcium implies that the source of calcium emission is uniformly distributed throughout the ejecta. These results are interpreted as evidence that oxygen emission originates in clumpy, newly synthesized material, while calcium emission arises from material preexisting in the atmosphere of the progenitor. Spectra spanning the range 433–2454 days after the explosion show boxlike profiles for the emission lines, clearly indicating circumstellar interaction in a roughly spherical shell. This is interpreted within the Chevalier & Fransson model for SNe interacting with mass lost during prior stellar winds. At very late times, the emission lines have a two-horned profile, implying the formation of a somewhat flattened or disklike structure that is a significant source of emission. The very high signal-to-noise ratio spectra are used to demonstrate the potential significance of misinterpretation of telluric absorption lines in the spectra of bright SNe.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bf10fc883a186b8f882ecd0f82af9805277d3a18

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In Astronomy and Astrophysics

1. N. Smith
2. A. Filippenko
3. E. Berger
4. S. Smartt
5. Ryan Chornock
6. Weidong Li
7. J. Silverman
8. P. Hopkins

In Instrumentation

1. N. Smith
2. A. Filippenko
3. Jenny E. Greene
4. L. Hernquist
5. P. Hopkins
6. Luis C. Ho
7. S. Smartt
8. Weidong Li

Citations in the corpus

• OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, methodology): “Spectrophotometric standard stars (e.g., Massey et al. 1988; Hamuy et al. 1992) were observed on the same nights for flux calibration (see Table 1) and are also used to remove telluric absorption features from the spectra (see, e.g., Wade & Horne 1988; Matheson et al. 2000a).”
• THE SPECTROSCOPIC DIVERSITY OF TYPE Ia SUPERNOVAE (2000, methodology): “The spectrophotometric standard stars observed on the same night (see Table A1) are also used to remove telluric absorption features from the spectra (see, e.g., Wade & Horne 1988; Matheson et al. 2000).”
• A Study of the Type II-Plateau Supernova 1999gi and the Distance to its Host Galaxy, NGC 3184 (2002, background): “…SN 1993J, a ‘‘ Type IIb ’’ event (Filippenko 1988) thought to arise from a progenitor that exploded with just a low-mass outer layer of hydrogen remaining, since the spectrum showed hydrogen at early times but subsequently became helium dominated (see Matheson et al. 2000 and references therein).”
• Constraining the Type Ia Supernova Progenitor: The Search for Hydrogen in Nebular Spectra (2006, methodology): “…one-dimensional sky-subtracted spectra optimally (Horne 1986) in the usual manner using the apall task within IRAF.3 Each spectrum was then wavelength and flux calibrated, and corrected for continuum atmospheric extinction and telluric absorption bands (Matheson et al. 2000 and references therein).”
• The Distance to SN 1999em in NGC 1637 from the Expanding Photosphere Method (2001, unknown): “Each spectrum was then wavelength and flux calibrated, as well as corrected for continuum atmospheric extinction and telluric absorption bands (Wade & Horne 1988; Bessell 1999; Matheson et al. 2000).”
• VARIABLE SODIUM ABSORPTION IN A LOW-EXTINCTION TYPE Ia SUPERNOVA, (2009, methodology): “These data were reduced in IRAF and IDL following normal procedures (for details, see Foley et al. 2003; Matheson et al. 2000; Horne 1986).”
• Berkeley Supernova Ia Program – I. Observations, data reduction and spectroscopic sample of 582 low-redshift Type Ia supernovae (2012, methodology): “Namely, Type IIb SNe (whose spectra evolve from a Type II SN to a Type Ib SN, as in SNe 1987K and 1993J; see Filippenko 1988; Filippenko et al. 1993; Matheson et al. 2000) are included only in the “Ib” SNID type (as opposed to being included in the “II” SNID type as well).”
• Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars (2015, background): “The IIb SNe are those which begin by resembling type II SNe with unmistakable H i Balmer lines and evolve to have H-weak and He-strong spectra (Filippenko 1997), the prototype of which is SN1993J (Filippenko, Matheson, & Ho 1993; Matheson et al. 2000).”
• SPECTRAL EVOLUTION OF THE EXTRAORDINARY TYPE IIn SUPERNOVA 2006gy (2009, methodology): “The spectra were corrected for atmospheric extinction (Bessell 1999; Matheson et al. 2000) using standard stars observed at an airmass similar to that of the SN and then flux calibrated using our photometry of SN 2006gy.”
• The Type IIn supernova 1994W: evidence for the explosive ejection of a circumstellar envelope (2004, methodology): “…the Lick data, all one-dimensional sky-subtracted spectra were extracted in the usual manner, and each spectrum was then wavelength and flux calibrated, as well as corrected for continuum atmospheric extinction and telluric absorption bands (Wade & Horne 1988; Bessell 1999; Matheson et al. 2000).”
• The ESSENCE Supernova Survey: Survey Optimization, Observations, and Supernova Photometry (2007, methodology): “Note that SNe IIb (whose spectra evolve from a Type II to a Type Ib, as, for example, in SN 1993J; see Filippenko et al. 1993; Matheson et al. 2000b) are included in both the ‘‘Ib’’ and ‘‘II’’ types.”
• THE LICK AGN MONITORING PROJECT 2011: SPECTROSCOPIC CAMPAIGN AND EMISSION-LINE LIGHT CURVES (2015, methodology): “Flux calibration and removal of telluric absorption features (following the procedure of Wade & Horne 1988) were carried out using IDL routines as described by Matheson et al. (2000).”
• On the Progenitor of SN 2005gl and the Nature of Type IIn Supernovae (2006, methodology): “The spectra were then wavelength and flux calibrated, corrected for continuumatmospheric extinction and telluric absorption bands (Wade & Horne 1988; Bessell 1999; Matheson et al. 2000), and combined.”
• Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329 (2003, methodology): “We attempted to remove telluric lines using the well-exposed continua of the spectrophotometric standards (Wade & Horne 1988; Matheson et al. 2000).”
• Fourteen months of observations of the possible super-Chandrasekhar mass Type Ia Supernova 2009dc (2010, methodology): “Journal compilation C© 2010 RAS, MNRAS 410, 585–611 Downloaded from https://academic.oup.com/mnras/article-abstract/410/1/585/1036265 by guest on 27 July 2018 spectra to the data in order to flux calibrate our spectra and to remove telluric lines (Wade & Horne 1988; Matheson et al. 2000).”
• SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by the Death of an Extremely Massive Star like η Carinae (2006, methodology): “The spectra were corrected for atmospheric extinction (Bessell 1999; Matheson et al. 2000) and then flux calibrated using standard stars observed at an air mass similar to that of the SN.”