Optical Spectroscopy of Supernova 1993J During Its First 2500 Days

Matheson, T.; Filippenko, A. V.; Barth, Aaron J.; Ho, Luis C.; Leonard, Douglas C.; Bershady, Matthew A.; Davis, Marc; Finley, David S.; Fisher, David; Gonzalez, Ruben L.; Hawley, Suzanne L.; Koo, David C.; Li, Weidong; Lonsdale, C. J.; Schlegel, David J.; Smith, H. E.; Spinrad, Hyron; Wirth, Gregory D.

doi:10.1086/301518

Cited by 124 publications

(91 citation statements)

References 78 publications

(75 reference statements)

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“…Comparison of (B − V ) colors of SN derived from spectroscopy using the same telescopes and instruments yields consistency with SN photometry at the 5% level (Matheson et al 2007); thus, we are confident that our relative flux calibration is accurate to ∼5% across 4000-6500 Å and most likely across the rest of the covered wavelength range. Telluric lines were removed following a procedure similar to that of Wade & Horne (1988) and Matheson et al (2000). The final flux calibrations were derived from observations of spectrophotometric standard stars.…”

Section: Cfa Datamentioning

confidence: 99%

MEASURED METALLICITIES AT THE SITES OF NEARBY BROAD-LINED TYPE Ic SUPERNOVAE AND IMPLICATIONS FOR THE SUPERNOVAE GAMMA-RAY BURST CONNECTION

Modjaz

Kewley

Kirshner

et al. 2008

The Astronomical Journal

342

441

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We compare the chemical abundances at the sites of 12 nearby (z < 0.14) Type Ic supernovae (SN Ic) that showed broad lines, but had no observed gamma-ray burst (GRB), with the chemical abundances in five nearby (z < 0.25) galaxies at the sites of GRBs where broad-lined SN Ic were seen after the fireball had faded. It has previously been noted that GRB hosts are low in luminosity and low in their metal abundances. If low metallicity is sufficient to force the evolution of massive stars to end their lives as GRBs with an accompanying broad-lined SN Ic, then we would expect higher metal abundances for the broad-lined SN Ic that have no detected GRBs. This is what we observe, and this trend is independent of the choice of metallicity calibration we adopt and the mode of SN survey that found the broad-lined SN Ic. A unique feature of this analysis is that we present new spectra of the host galaxies and analyze all measurements of both samples in the same set of methods, using the galaxy emission-line measurements corrected for extinction and stellar absorption, via independent metallicity diagnostics of Kewley & Dopita, McGaugh, and Pettini & Pagel. In our small sample, the boundary between galaxies that have GRBs accompanying their broad-lined SN Ic and those that have broad-lined SN Ic without GRBs lies at an oxygen abundance of 12 + log(O/H) KD02 ∼ 8.5, which corresponds to 0.2-0.6 Z depending on the adopted metallicity scale and solar abundance value. Even when we limit the comparison to SN Ic that were found in untargeted supernova surveys, the environment of every broad-lined SN Ic that had no GRB is more metal rich than the site of any broad-lined SN Ic where a GRB was detected.

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Section: Cfa Datamentioning

confidence: 99%

MEASURED METALLICITIES AT THE SITES OF NEARBY BROAD-LINED TYPE Ic SUPERNOVAE AND IMPLICATIONS FOR THE SUPERNOVAE GAMMA-RAY BURST CONNECTION

Modjaz

Kewley

Kirshner

et al. 2008

The Astronomical Journal

342

441

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“…For example, the best-studied SN IIb and SN Ic are SN 1993J (Filippenko et al 1993;Matheson et al 2000aMatheson et al , 2000b and SN 1994I (Filippenko et al 1995;Richmond et al 1996), respectively. However, statistical analyses of large SN samples are needed to characterize spectra of different SN subtypes.…”

Section: Introductionmentioning

confidence: 99%

Analyzing the Largest Spectroscopic Data Set of Stripped Supernovae to Improve Their Identifications and Constrain Their Progenitors

Liu

Modjaz

Bianco

et al. 2016

ApJ

128

220

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Using the largest spectroscopic data set of stripped-envelope core-collapse supernovae (stripped SNe), we present a systematic investigation of spectral properties of Type IIb SNe (SNe IIb), Type Ib SNe (SNe Ib), and Type Ic SNe (SNe Ic). Prior studies have been based on individual objects or small samples. Here, we analyze 242 spectra of 14 SNe IIb, 262 spectra of 21 SNe Ib, and 207 spectra of 17 SNe Ic based on the stripped SN data set of Modjaz et al. and other published spectra of individual SNe. Each SN in our sample has a secure spectroscopic ID, a date of V-band maximum light, and most have multiple spectra at different phases. We analyze these spectra as a function of subtype and phase in order to improve the SN identification scheme and constrain the progenitors of different kinds of stripped SNe. By comparing spectra of SNe IIb with those of SNe Ib, we find that the strength of Hα can be used to quantitatively differentiate between these two subtypes at all epochs. Moreover, we find a continuum in observational properties between SNe IIb and Ib. We address the question of hidden He in SNe Ic by comparing our observations with predictions from various models that either include hidden He or in which He has been burnt. Our results favor the He-free progenitor models for SNe Ic. Finally, we construct continuum-divided average spectra as a function of subtype and phase to quantify the spectral diversity of the different types of stripped SNe.

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“…SNe IIb are intrinsically rare (∼10%-11% of all core-collapse SNe; Smith et al 2011;Li et al 2011). The first identified case was SN 1987K (Filippenko 1988); wellstudied examples are the nearby SN 1993J in Messier 81 (e.g., Richmond et al 1996;Matheson et al 2000) and SN 2011dh in Messier 51 (e.g., Arcavi et al 2011;Ergon et al 2013). The progenitor channel for SN 1993J that has garnered most favor 10 Hubble fellow.…”

Section: Introductionmentioning

confidence: 99%

“…Spectroscopically, SNe IIb exhibit at early times emission and absorption features due to H, resembling SNe II, which subsequently give way to the emergence of the He i absorption lines typical of SNe Ib (e.g., Filippenko et al 1993;Chornock et al 2011), with broad H emission reappearing in the nebular phase (e.g., Filippenko et al 1994;Matheson et al 2000;Taubenberger et al 2011;Shivvers et al 2013). Although rarely seen owing to its very short duration early in the evolution of an SN, a rapid decline after an initial peak has been observed among SNe IIb (e.g., Richmond et al 1994Richmond et al , 1996Roming et al 2009;Arcavi et al 2011).…”

Section: Introductionmentioning

confidence: 99%

THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR

Dyk

Zheng

Fox

et al. 2014

Self Cite

124

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We have obtained early-time photometry and spectroscopy of supernova (SN) 2013df in NGC 4414. The SN is clearly of Type IIb, with notable similarities to SN 1993J. From its luminosity at secondary maximum light, it appears that less 56 Ni ( 0.06 M ) was synthesized in the SN 2013df explosion than was the case for the SNe IIb 1993J, 2008ax, and 2011dh. Based on a comparison of the light curves, the SN 2013df progenitor must have been more extended in radius prior to explosion than the progenitor of SN 1993J. The total extinction for SN 2013df is estimated to be A V = 0.30 mag. The metallicity at the SN location is likely to be solar. We have conducted Hubble Space Telescope (HST) Target of Opportunity observations of the SN with the Wide Field Camera 3, and from a precise comparison of these new observations to archival HST observations of the host galaxy obtained 14 yr prior to explosion, we have identified the progenitor of SN 2013df to be a yellow supergiant, somewhat hotter than a red supergiant progenitor for a normal Type II-Plateau SN. From its observed spectral energy distribution, assuming that the light is dominated by one star, the progenitor had effective temperature T eff = 4250 ± 100 K and a bolometric luminosity L bol = 10 4.94±0.06 L . This leads to an effective radius R eff = 545 ± 65 R . The star likely had an initial mass in the range of 13-17 M ; however, if it was a member of an interacting binary system, detailed modeling of the system is required to estimate this mass more accurately. The progenitor star of SN 2013df appears to have been relatively similar to the progenitor of SN 1993J.

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Optical Spectroscopy of Supernova 1993J During Its First 2500 Days

Cited by 124 publications

References 78 publications

MEASURED METALLICITIES AT THE SITES OF NEARBY BROAD-LINED TYPE Ic SUPERNOVAE AND IMPLICATIONS FOR THE SUPERNOVAE GAMMA-RAY BURST CONNECTION

MEASURED METALLICITIES AT THE SITES OF NEARBY BROAD-LINED TYPE Ic SUPERNOVAE AND IMPLICATIONS FOR THE SUPERNOVAE GAMMA-RAY BURST CONNECTION

Analyzing the Largest Spectroscopic Data Set of Stripped Supernovae to Improve Their Identifications and Constrain Their Progenitors

THE TYPE IIb SUPERNOVA 2013df AND ITS COOL SUPERGIANT PROGENITOR

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