Erratum: “Astro‐2 Observations of Interstellar Dust and Gas in the Large Magellanic Cloud” (ApJ, 460, 313 [1996])

Clayton, Geoffrey C.; Green, J.; Wolff, Michael; Zellner, N. E. B.; Code, A. D.; Davidsen, A. F.

doi:10.1086/304473

Cited by 21 publications

(24 citation statements)

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“…The total dust mass in the ISM is approximately 1.6 × 10 6 M ⊙ . For this estimate, we use the total ISM gas mass in the LMC of 8 × 10 8 M ⊙ , and assume that the dust to gas extinction ratio in the LMC is about a factor of 2–2.5 lower than the Milky Way (Fitzpatrick 1985; Clayton et al 1996; Gordon et al 2003; Cox et al 2006), the adopted gas‐to‐dust ratio, of 500 in the LMC, is higher than the Galactic value (Zubko, Dwek & Arendt 2004).…”

Section: Discussionmentioning

confidence: 99%

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

Matsuura

Barlow

Zijlstra

et al. 2009

Monthly Notices of the Royal Astronomical Society

202

265

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We report on an analysis of the gas and dust budget in the interstellar medium (ISM) of the Large Magellanic Cloud (LMC). Recent observations from the Spitzer Space Telescope enable us to study the mid‐infrared dust excess of asymptotic giant branch (AGB) stars in the LMC. This is the first time we can quantitatively assess the gas and dust input from AGB stars over a complete galaxy, fully based on observations. The integrated mass‐loss rate over all intermediate and high mass‐loss rate carbon‐rich AGB candidates in the LMC is 8.5 × 10−3 M⊙ yr−1, up to 2.1 × 10−2 M⊙ yr−1. This number could be increased up to 2.7 × 10−2 M⊙ yr−1 if oxygen‐rich stars are included. This is overall consistent with theoretical expectations, considering the star formation rate (SFR) when these low‐ and intermediate‐mass stars where formed, and the initial mass functions. AGB stars are one of the most important gas sources in the LMC, with supernovae (SNe), which produces about 2–4 × 10−2 M⊙ yr−1. At the moment, the SFR exceeds the gas feedback from AGB stars and SNe in the LMC, and the current star formation depends on gas already present in the ISM. This suggests that as the gas in the ISM is exhausted, the SFR will eventually decline in the LMC, unless gas is supplied externally. Our estimates suggest ‘a missing dust‐mass problem’ in the LMC, which is similarly found in high‐z galaxies: the accumulated dust mass from AGB stars and possibly SNe over the dust lifetime (400–800 Myr) is significant less than the dust mass in the ISM. Another dust source is required, possibly related to star‐forming regions.

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Section: Discussionmentioning

confidence: 99%

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

Matsuura

Barlow

Zijlstra

et al. 2009

Monthly Notices of the Royal Astronomical Society

202

265

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“…Based on the previously studied sight lines toward Sk À66 19 and Sk À69 270, it was found that while the gas-to-dust ratio N (H i)/E 0 (B À V ) is much larger in the Clouds than typically seen in the Milky Way, the quantity N (H 2 )/E 0 (B À V ) has a similar value in each galaxy (Clayton et al 1996;Gunderson et al 1998). This suggests a close relationship between dust and H 2 .…”

Section: H 2 In the Magellanic Cloudsmentioning

confidence: 99%

“…However, this result is at odds with Welty et al (2001), whose data suggested negligible silicon depletion in several gas cloud components along a sight line probing the SMC ISM. In order to address issues such as dust composition, particularly for small grains enhancing FUV extinction in the Clouds, it would be helpful to explore LMC and SMC extinction curves shortward of the UV range that Clayton et al (2003) were confined to by their International Ultraviolet Explorer (IUE ) data; unfortunately, FUV extinction curves have been published to date for only very few red-dened Magellanic Cloud stars (Clayton et al 1996;Hutchings & Giasson 2001).…”

Section: Introductionmentioning

confidence: 99%

FUSEMeasurements of Far‐Ultraviolet Extinction. II. Magellanic Cloud Sight Lines

Cartledge

Clayton

Rachford

et al. 2005

ApJ

Self Cite

112

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We present an extinction analysis of nine reddened/comparison star pairs in the Large and Small Magellanic Clouds (LMC and SMC) based on Far-Ultraviolet Spectroscopic Explorer (FUSE ) FUVobservations. To date, just two LMC sight lines have probed dust grain composition and size distributions in the Magellanic Clouds using spectral data for wavelengths as short as 950 8. We supplement these two with data from four regions distinguished by their IR through UV extinction curves and grouped as LMCAvg, LMC2, SMC bar, and SMC wing. Despite the distinct characters of extinction in the Clouds and Milky Way, our results are generally analogous to those found for Galactic curves-namely, that the FUSE portions of each extinction curve are described reasonably well by Fitzpatrick & Massa curves fitted only to longer wavelength data and lack any dramatic new extinction features, and any deviations from the Cardelli, Clayton, & Mathis (CCM) formalism continue into FUV wavelengths. A maximum entropy method analysis of all of these curves suggests that LMCAvg and SMC wing sight lines, whose extinction parameters more closely resemble those for Galactic paths, require more silicon and/or carbon in dust than current abundance measurements would indicate are available. The requirements for LMC2 and SMC bar sight lines do not fully tax the available reservoirs, in part because large grains contribute less to the extinction in these directions. An intermediate product of this extinction analysis is the measurement of new H 2 abundances in the Magellanic Clouds. Collectively considering Cloud sight lines that possess significant H 2 column densities, E(B À V )/N (H i) ratios are reduced by significant factors relative to the Galactic mean, whereas the corresponding E(B À V )/N (H 2 ) values more closely resemble their Galactic counterpart. These trends reflect the fact that among these sight lines f (H 2 ) values are lower than those common in the Milky Way for paths with similar degrees of reddening.

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“…23 A very compact paper giving important results from EUV spectroscopy is that by Clayton et al (1996). With the HUT they observed stars in the LMC to study their UV extinction.…”

Section: Notable Studies Since 1990mentioning

confidence: 99%

“…Using WUPPE the UV-polarization was measured and was found to lie above the Serkowsi law. Although the spectra were only of modest spectral resolution, Clayton et al (1996) could fit the broader spectral depressions with absorption in the Lyman and Werner H 2 absorption bands. Toward 2 stars they find N(H 2 ) of 1-2 .10 20 cm-2 • Of particular relevance for the physics of cool clouds are the 21 em H I absorption line studies carried out by Mebold et al (1991) in the Magellanic Stream and by Dickey et al (1994) and Marx-Zimmer et al (1999) in the LMC itself.…”

Section: Notable Studies Since 1990mentioning

confidence: 99%

New Magellanic Cloud Interstellar Matters

Boer

1999

Symp. - Int. Astron. Union

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Novel instrumentation has always led to new insights in the nature of the universe. Novel astronomical instrumentation is no exception. In numerous areas new instruments led to the detection of hitherto unknown phenomena. I will review some notable studies of the recent past with some emphasis on those dicoveries not extensively covered by others at this conference. Finally, very recent work based on ORFEUS echelle spectra is presented.

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Erratum: “Astro‐2 Observations of Interstellar Dust and Gas in the Large Magellanic Cloud” (ApJ, 460, 313 [1996])

Cited by 21 publications

References 0 publications

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution

FUSEMeasurements of Far‐Ultraviolet Extinction. II. Magellanic Cloud Sight Lines

New Magellanic Cloud Interstellar Matters

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