Interstellar and Circumstellar Optical and Ultraviolet Lines toward SN 1998S

Bowen, David V.; Roth, Katherine C.; Meyer, David M.; Blades, J. C.

doi:10.1086/308913

Cited by 39 publications

(65 citation statements)

References 35 publications

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“…A comparison with the SN 1998S spectrum from Bowen et al (2000) reveals that several sets of absorption lines match the SN 2011ht lines, namely, Mg ii (∼λ2800) and Fe ii (∼λ2400, λ2586, and λ2612; Figure 10). An 11 Å shift of the UVOT spectrum (which is within the wavelength accuracy of the instrument) was applied based on the line identifications, so it is possible that the overall blueshift seen in the optical is masked.…”

Section: The Spectra Of Sn 2011htmentioning

confidence: 96%

THE UNUSUAL TEMPORAL AND SPECTRAL EVOLUTION OF THE TYPE IIn SUPERNOVA 2011ht

Roming¹,

Pritchard²,

Prieto³

et al. 2012

ApJ

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We present very early UV to optical photometric and spectroscopic observations of the peculiar Type IIn supernova (SN) 2011ht in UGC 5460. The UV observations of the rise to peak are only the second ever recorded for a Type IIn SN and are by far the most complete. The SN, first classified as an SN impostor, slowly rose to a peak of M V ∼ −17 in ∼55 days. In contrast to the ∼2 mag increase in the v-band light curve from the first observation until peak, the UV flux increased by >7 mag. The optical spectra are dominated by strong, Balmer emission with narrow peaks (FWHM ∼ 600 km s −1 ), very broad asymmetric wings (FWHM ∼ 4200 km s −1 ), and blueshifted absorption (∼300 km s −1 ) superposed on a strong blue continuum. The UV spectra are dominated by Fe ii, Mg ii, Si ii, and Si iii absorption lines broadened by ∼1500 km s −1 . Merged X-ray observations reveal a L 0.2-10 = (1.0 ± 0.2) × 10 39 erg s −1 . Some properties of SN 2011ht are similar to SN impostors, while others are comparable to Type IIn SNe. Early spectra showed features typical of luminous blue variables at maximum and during giant eruptions. However, the broad emission profiles coupled with the strong UV flux have not been observed in previous SN impostors. The absolute magnitude and energetics (∼2.5 × 10 49 erg in the first 112 days) are reminiscent of normal Type IIn SN, but the spectra are of a dense wind. We suggest that the mechanism for creating this unusual profile could be a shock interacting with a shell of material that was ejected a year before the discovery of the SN.

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Section: The Spectra Of Sn 2011htmentioning

confidence: 96%

THE UNUSUAL TEMPORAL AND SPECTRAL EVOLUTION OF THE TYPE IIn SUPERNOVA 2011ht

Roming¹,

Pritchard²,

Prieto³

et al. 2012

ApJ

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“…Bowen et al (2000) concluded that the narrow and variable absorption is a signature of the outflows from the super-giant progenitor of SN 1998S, arising in a dense shell, expanding at about 50 km s −1 (see also Fassia et al 2001).…”

Section: Discussionmentioning

confidence: 99%

“…See also Patat et al 2010). To the best of our knowledge, short timescale variations of narrow absorptions are known to this level of detail only for one other object, i.e., the core-collapse, type IIn SN 1998S (Bowen et al 2000). High-resolution spectroscopy of this object has revealed a number of Na i D components within the host galaxy, the bluest of which deepened significantly during the 19 days spanned by the two epochs available, implying a Na i column density increase of 1 dex.…”

Section: Discussionmentioning

confidence: 99%

Connecting RS Ophiuchi to [some] type Ia supernovae

Patat

Чугай

Podsiadlowski

et al. 2011

A&A

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Aims. Recurrent nova systems like RS Oph have been proposed as a possible channel for type Ia supernova (SN) explosions based on the high mass of the accreting white dwarf. Additional support for this hypothesis has recently been provided by the detection of circumstellar material around SN 2006X and SN 2007le, showing a structure compatible with that expected for recurrent nova outbursts. We investigate the circumstellar environment of RS Oph and its structure with the aim of establishing a firmer and independent link between this class of objects and type Ia SN progenitors. Methods. We study the time evolution of Ca ii, Na i, and K i absorption features in RS Oph before, during, and after the last outburst, using multi-epoch, high-resolution spectroscopy and applying the same method as was adopted for SN 2006X and SN 2007le. Results. A number of components are detected , that are blue-shifted with respect to the systemic velocity of RS Oph. In particular, one feature strongly weakens in the first two weeks after the outburst, at the same time that the very narrow P-Cyg profiles disappear, which are overimposed on the much wider nova emission lines of H, He, Fe ii, and other elements. Conclusions. We interpret this as the signature of density enhancements in the circumstellar material, suggesting that the recurrent eruptions might indeed create complex structures within the material lost by the donor star. This establishes a strong link between RS Oph and the progenitor system of the type Ia SN 2006X, for which similar features have been detected.

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“…Previous observations of Ca ii absorption in HVCs with bright 21 cm emission have yielded six detections, giving Ca ii/H i ratios of (17 AE 6) ; 10 À9 for Complex A (Schwarz et al 1995), (22 AE 1) ; 10 À9 for Complex C (Wakker et al 1996), (3:3 AE 0:9) ; 10 À9 for Complex M (Bowen et al 2000), (33 AE 4) ; 10 À9 for the Magellanic Stream (Songaila & York 1980), (66 AE 8) ; 10 À9 for the Leading Arm of the Magellanic Stream (West et al 1985), and (270 AE 120) ; 10 À9 for Complex WB (Robertson et al 1991). There are also several Ca ii detections toward extragalactic supernovae in directions with very faint or no 21 cm (d 'Odorico et al 1985'Odorico et al , 1989Meyer & Roth 1991;Vladilo et al 1994;Ho & Filippenko 1995, 1996, which yield very high Ca ii/H i ratios.…”

Section: Methodsmentioning

confidence: 98%

Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

Wakker

York

Wilhelm

et al. 2008

ApJ

183

198

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The high-and intermediate-velocity interstellar clouds (HVCs/IVCs) are tracers of energetic processes in and around the Milky Way. Clouds with near-solar metallicity about 1 kpc above the disk trace the circulation of material between disk and halo (the Galactic fountain). The Magellanic Stream consists of gas tidally extracted from the SMC, tracing the dark matter potential of the Milky Way. Several other HVCs have low metallicity and appear to trace the continuing accretion of infalling intergalactic gas. These assertions are supported by the metallicities (0

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Interstellar and Circumstellar Optical and Ultraviolet Lines toward SN 1998S

Cited by 39 publications

References 35 publications

THE UNUSUAL TEMPORAL AND SPECTRAL EVOLUTION OF THE TYPE IIn SUPERNOVA 2011ht

THE UNUSUAL TEMPORAL AND SPECTRAL EVOLUTION OF THE TYPE IIn SUPERNOVA 2011ht

Connecting RS Ophiuchi to [some] type Ia supernovae

Distances to Galactic High‐Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1

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