Spectra of SN 1972e, in NGC 5253

Bolton, C. T.; Garrison, R. F.; Salmon, Derrick; Geffken, N.

doi:10.1086/129627

Cited by 3 publications

(2 citation statements)

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“…Significantly more information is available for SN 1972E, which was the second-brightest SN of the 20th century. Discovered on 1972 May 13 (J2000 coordinates: R. A.=13:39:52.7, decl.=−31:40:09), SN 1972E was identified just prior to maximum light (Leibundgut et al 1991), peaked at a visual of 8.5 mag and was observed for 700 days after initial discovery (Ardeberg & de Groot 1973;Bolton et al 1974;Kirshner & Oke 1975). As with SN 1895B, we adopt the discovery date as the explosion date for the analysis below.…”

Section: Background: Sn 1895b and Sn 1972ementioning

confidence: 99%

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells

Cendes

Drout

Chomiuk

et al. 2020

ApJ

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We have imaged 35 yr of archival Very Large Array observations of the nearby (d L =3.15 Mpc) Type Ia supernovae SN 1972E and SN 1895B between 9 and 121 yr post-explosion. No radio emission is detected, constraining their radio luminosities to be L ν,8.5GHz < 6.0×10 23 erg s −1 Hz −1 45 yr post-explosion and L ν,8.5GHz < 8.9×10 23 erg s −1 Hz −1 121 yr post-explosion, respectively. These limits imply a clean circumstellar medium (CSM), with n < 0.9 cm −3 out to radii of a few×10 18 cm, if the SN blast wave is expanding into uniform density material. We also constrain the presence of CSM shells surrounding the progenitor of SN 1972E. We rule out essentially all medium and thick shells with masses of 0.05-0.3 M e at radii between ∼10 17 and 10 18 cm, and thin shells at specific radii with masses down to 0.01 M e . These constraints rule out swaths of parameter space single and double degenerate progenitor scenarios, including recurrent nova, core-degenerate objects, ultra-prompt explosions, and white dwarf (WD) mergers with delays of a few hundred years between the onset of merger and explosion. Allowed progenitors include WD-WD systems with a significant (>10 4 yr) delay from the last episode of common envelope evolution and single degenerate systems undergoing recurrent nova-provided that the system has been in the nova phase for 10 4 yr, such that a large (>10 18 cm) cavity has been evacuated. Future multi-epoch observations of additional intermediate-aged SNe Ia will provide a comprehensive view of the largescale CSM around these explosions.

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Section: Background: Sn 1895b and Sn 1972ementioning

confidence: 99%

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells

Cendes

Drout

Chomiuk

et al. 2020

ApJ

View full text Add to dashboard Cite

show abstract

“…Significantly more information is available for SN 1972E, which was the second-brightest SN of the 20th century. Discovered on May 13, 1972 (J2000 coordinates: RA = 13:39:52.7, Dec = −31:40:09), SN 1972E was identified just prior to maximum light (Leibundgut et al 1991), peaked at a visual of 8.5 mag and was observed for 700 days after initial discovery (Kirshner & Oke 1975;Ardeberg & de Groot 1973;Bolton et al 1974). As with SN 1895B, we adopt the discovery date as the explosion date for the analysis below 2 .…”

Section: Introductionmentioning

confidence: 99%

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells

Cendes,

Drout,

Chomiuk

et al. 2020

Preprint

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We have imaged over 35 years of archival Very Large Array (VLA) observations of the nearby (d L = 3.15 Mpc) Type Ia supernovae SN 1972E and SN 1895B between 9 and 121 years post-explosion. No radio emission is detected, constraining the 8.5 GHz luminosities of SN 1972E and SN 1895B to be L ν,8.5GHz < 6.0 × 10 23 erg s −1 Hz −1 45 years post-explosion and L ν,8.5GHz < 8.9 × 10 23 erg s −1 Hz −1 121 years post-explosion, respectively. These limits imply a clean circumstellar medium (CSM), with n < 0.9 cm −3 out to radii of a few × 10 18 cm, if the SN blastwave is expanding into uniform density material. Due to the extensive time coverage of our observations, we also constrain the presence of CSM shells surrounding the progenitor of SN 1972E. We rule out essentially all medium and thick shells with masses of 0.05−0.3 M at radii between ∼10 17 and 10 18 cm, and thin shells at specific radii with masses down to 0.01 M . These constraints rule out swaths of parameter space for a range of single and double degenerate progenitor scenarios, including recurrent nova, core-degenerate objects, ultraprompt explosions and white dwarf (WD) mergers with delays of a few hundred years between the onset of merger and explosion. Allowed progenitors include WD-WD systems with a significant (> 10 4 years) delay from the last episode of common envelope evolution and single degenerate systems undergoing recurrent nova-provided that the recurrence timescale is relatively short and the system has been in the nova phase for 10 4 years, such that a large (> 10 18 cm) cavity has been evacuated. Future multi-epoch observations of additional intermediate-aged Type Ia SNe will provide a comprehensive view of the large-scale CSM environments around these explosions.

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Spectra of Supernovae

Branch¹

1990

Astronomy and Astrophysics Library

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Ever since the spectrum of a supernova was first observed in 1885, astronomers have known that a correct reading of the spectrum would reveal otherwise unattainable information about the physical conditions and composition of the radiation source. But the spectra of supernovae resisted interpretation for a very long time. The outstanding obstacle was the great characteristic width of the spectral features-150-300 A-corresponding to Doppler broadening velocities of 5000-10,000 km S-l. Because only a dozen or so overlapping spectral features occupy the whole optical spectrum at anyone time, line identifications proved to be so difficult that very little was known about Type II spectra, and even less about Type I, until around 1970. In the hope that a brief history of the subject will be interesting (if not of great utility), I attempt in Section 2.2 to outline the development of supernova spectrum interpretations, and to cite in one place most of the significant papers. Section 2.3 then presents a list of classifications of all supernovae whose spectra I have seen, and a (nearly) complete spectrum bibliography.We now know that during the first months after an explosion the ejected matter remains optically thick; "P Cygni" profiles of spectral lines formed in the outer layers are superimposed on a thermal continuum emitted from a photosphere, and spectrum formation is analagous to that which occurs in an expanding stellar atmosphere. As the ejected matter becomes optically thin to continuum photons via expansion and cooling, the supernova gradually becomes a self-excited nebula, with emission lines dominating the spectrum. In Section 2.4, the basic theory of spectrum formation during the photospheric and nebular phases, and methods for calculating synthetic spectra that were developed before the time ofSN 1987A, are reviewed in qualitative terms. As summarized in Section 2.5, it was only during the early 1980s that the classical mysteries of supernova spectra were fully resolved-definite line identifications were established and a good semiquantitative picture of spectrum formation was achieved. Now the spectra of supernova 1987 A are stimulating the development of more detailed, quantitative analyses. The techniques now being tested on SN 1987 A are likely to lead in a few years to reliable information on the composition of the matter ejected by supernovae of all types-information which will have a strong impact on attempts to relate the various kinds of supernovae to their stellar progenitors and explosion mechanisms. The first applications of the new quantitative spectroscopy, and the prospects for further work, are discussed briefly in Section 2.6.A. G. Petschek (ed.), Supernovae

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Spectra of SN 1972e, in NGC 5253

Abstract: Wavelengths of features in the spectrum of SN 1972# in NGC 5253 derived from 14 blue spectra taken between 19 and 260 days after maximum light are given and the evolution of the spectrum is discussed.

Cited by 3 publications

References 8 publications

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells

Spectra of Supernovae

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