A study of the interstellar medium in line to M83 from high-resolution observations of the nucleus and supernova 1983n

D’Odorico, S.; Ponz, D.

doi:10.1086/163752

Cited by 13 publications

(8 citation statements)

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“…With the use of space observatories including the International Ultraviolet Explorer (IUE), the Far Ultraviolet Spectroscopic Explorer (FUSE) and Hubble Space Telescope (HST), since 1980s, a large number of DIBs have been detected in LMC and SMC (Morgan [17] , Ehrenfreund et al [18] , Cox et al [19] ), in Starburst Galaxies (Heckman et al [20] ), in NGC 1448 (Sollerman et al [21] ), in NGC 5128 (Rich [22] , D'Odorico et al [23] ) and in Damped Lyα Systems (Junkkarinen et al [24] , York et al [25] , Prochaska et al [26] ).…”

Section: Dibs In the External Galaxiesmentioning

confidence: 99%

Diffuse interstellar absorption bands

Xiang

Liang

2009

Sci. China Ser. G-Phys. Mech. Astron.

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The diffuse interstellar bands (DIBs) are a large number of absorption bands that are superposed on the interstellar extinction curve and are of interstellar origin. Since the discovery of the first two DIBs in the 1920s, the exact nature of DIBs still remains unclear. This article reviews the history of the detections of DIBs in the Milky Way and external galaxies, the major observational characteristics of DIBs, the correlations or anti-correlations among DIBs or between DIBs and other interstellar features (e.g. the prominent 2175 Angstrom extinction bump and the far-ultraviolet extinction rise), and the proposed candidate carriers. Whether they are also present in circumstellar environments is also discussed.astrophysics, interstellar matter, interstellar extinction, diffuse interstellar band, circumstellar environment

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Section: Dibs In the External Galaxiesmentioning

confidence: 99%

Diffuse interstellar absorption bands

Xiang

Liang

2009

Sci. China Ser. G-Phys. Mech. Astron.

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“…1). Detailed observations at radio (Condon et al 1982;Cowan & Branch 1985;Eck et al 2002), infrared ( Telesco & Harper 1980;Thornley et al 2000;Roussel et al 2001), ultraviolet ( Bohlin et al 1983( Bohlin et al , 1990; and now GALEX 2 ), X-ray ( Trinchieri et al 1985;Ehle et al 1998;Immler et al 1999;Soria & Wu 2002, 2003, and optical wavelengths ( D'Odorico et al 1985;Rumstay & Kaufman 1983) indicate that the nucleus and spiral arms of M83 are regions of intense star formation. D 'Odorico et al (1985) found absorption features in the nucleus consistent with a population dominated by massive OB stars, which are believed to be the precursors of Type Ib,c/II SNe ( Huang 1987).…”

Section: Introductionmentioning

confidence: 99%

An Optical Survey of Supernova Remnants in M83

Blair

Long

2004

ASTROPHYS J SUPPL S

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Observations of the face-on spiral galaxy M83 ( NGC 5236) performed at the Cerro Tololo Inter-American Observatory in Chile have yielded a catalog of optical supernova remnant (SNR) candidates. These observations were performed with the 4 m Blanco telescope and a prime focus CCD imaging system using narrowband interference filters centered on the light of [S ii], H, [O iii], and red and blue continuum bands. Based on strong relative [S ii]:H emission, 71 emission nebulae have been identified as SNR candidates. Positions and H fluxes of the candidates are presented. Follow-up spectra of 25 of the SNR candidates, also performed at CTIO, have confirmed many of the SNR identifications, although the spectra of a few objects are discrepant, perhaps because of inaccurate aperture placement. In addition, the low mean excitation of M83 H ii regions has allowed a separate search for young oxygen-dominated (core collapse) SNRs similar to Cas A in our Galaxy, using [O iii]:H. This search found a number of the same objects as the [S ii]:H search, indicating that many of these SNRs have shock velocities in excess of 100 km s À1 . However, no bona fide young core-collapse SNRs were detected with this technique, with the possible exception of the independent recovery of SN 1957D, which had been seen previously. We have also attempted to identify optical counterparts for the six historical supernovae that have occurred in M83. Except for SN 1957D, none of the historical supernovae have been detected by this survey. We compare our SNR candidate list against the Chandra X-ray source list of Soria and Wu and identify 15 X-ray sources as likely SNRs, based on positional coincidence within 1 00 . The sources identified have hardness ratios that are soft compared to the general X-ray source population in M83.

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“…Supernovae have been used successfully to probe galaxy ISMs both from the ground (e.g. Wallerstein et al 1972;Jenkins et al 1984;D'Odorico et al 1985;Vidal-Madjar et al 1987;Steidel et al 1990;Meyer & Roth 1991) using Ca II and Na I absorption lines, and more recently, from space with IUE (Pettini et al 1982;Blades et al 1988). Since the launch of HST , we have been using the high resolution spectrographs to study the ISMs of nearby galaxies in more detail.…”

Section: Introductionmentioning

confidence: 99%

Interstellar and Circumstellar Optical and Ultraviolet Lines toward SN 1998S

Bowen¹,

Roth²,

Meyer³

et al. 2000

ApJ

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We have observed SN 1998S which exploded in NGC 3877, with the Utrecht Echelle Spectrograph (6 − 7 km s −1 FWHM) at the William Herschel Telescope and with the E230M echelle of the Space Telescope Imaging Spectrograph (8 km s −1 FWHM) aboard the Hubble Space Telescope. Both data sets were obtained at two epochs, separated by 19 (optical) and seven days (UV data).From our own Galaxy we detect interstellar absorption lines of Ca II K, Fe II λλ2600, 2586, 2374, 2344, Mg I λ2852, and probably Mn II λ2576, at v LSR = −95 km s −1 arising from the outer edge of the High Velocity Cloud Complex M. We derive gas-phase abundances of [Fe/H] = −1.4 and [Mn/H] = −1.0, values which are very similar to warm disk clouds found in the local ISM. This is the first detection of manganese from a Galactic HVC, and we believe that the derived gas-phase abundances argue against the HVC material having an extragalactic origin.At the velocity of NGC 3877 we detect interstellar Mg I λ2852, Mn II λλ2576, 2594, 2606, Ca II K and Na I D 2 ,D 1 absorption lines, spanning a velocity range of −102 to +9 km s −1 from the systemic velocity of the galaxy (910 km s −1 ).

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A study of the interstellar medium in line to M83 from high-resolution observations of the nucleus and supernova 1983n

Cited by 13 publications

References 0 publications

Diffuse interstellar absorption bands

Diffuse interstellar absorption bands

An Optical Survey of Supernova Remnants in M83

Interstellar and Circumstellar Optical and Ultraviolet Lines toward SN 1998S

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