A survey of interstellar H I from L-alpha absorption measurements. II

Bohlin, R. C.; Savage, Blair D.; Drake, J. F.

doi:10.1086/156357

Cited by 2,333 publications

(2,475 citation statements)

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“…Following this, the E(B-V) is calculated from the HI column density using the relation from Bohlin, Savage & Drake (1978)and Diplas & Savage (1994):…”

Section: Extinction Analysismentioning

confidence: 99%

The Properties of the Magellanic Bridge Based on OGLE IV RR Lyrae Variables

Wagner-Kaiser¹,

Sarajedini²

2016

Mon. Not. R. Astron. Soc.

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We examine the properties of the Magellanic Bridge connecting the Large and Small Magellanic Clouds using ab-type RR Lyrae variables from the extensive dataset of the Optical Gravitational Lensing Experiment (OGLE), Phase IV data release. The metallicities of the RR Lyraes are determined from the characteristics of their light curves, with an average abundance of [Fe/H] = -1.790 ± 0.011 (sem) in the Magellanic Bridge. From the individual reddenings of these stars, derived via their minimum light curve colors, we determined a median color excess of E(V-I) = 0.101 ± 0.007 (sem) (implying E(B-V) ≈ 0.077). The peak distance modulus of 18.57 ± 0.048 (sem) places the Bridge stars at distances between the two systems. The metallicity and distance distributions probe the structure of the Magellanic system as a whole, revealing a smooth transition that connects the galaxies. An examination of the HI content does not find a clear correlation between HI emission strength and RR Lyrae spatial distribution, suggesting that the old stellar populations may trace the overlapping halo distributions of the two Magellanic Clouds.

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“…Following this, the E(B-V) is calculated from the HI column density using the relation from Bohlin, Savage & Drake (1978)and Diplas & Savage (1994):…”

Section: Extinction Analysismentioning

confidence: 99%

The Properties of the Magellanic Bridge Based on OGLE IV RR Lyrae Variables

Wagner-Kaiser¹,

Sarajedini²

2016

Mon. Not. R. Astron. Soc.

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“…Observers measure column densities in cm −2 , i.e., the number density n in cm −3 of a species integrated along a path, N = n dz. An empirical relation between extinction and the column density of hydrogen nuclei has been found 143,144 …”

Section: -39 | 17mentioning

confidence: 99%

Astrochemistry of dust, ice and gas: introduction and overview

Dishoeck

Ewine²

2014

Faraday Discuss.

136

102

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A brief introduction and overview of the astrochemistry of dust, ice and gas and their interplay is presented, aimed at non-specialists. The importance of basic chemical physics studies of critical reactions is illustrated through a number of recent examples. Such studies have also triggered new insight into chemistry, illustrating how astronomy and chemistry can enhance each other. Much of the chemistry in star- and planet-forming regions is now thought to be driven by gas-grain chemistry rather than pure gas-phase chemistry, and a critical discussion of the state of such models is given. Recent developments in studies of diffuse clouds and PDRs, cold dense clouds, hot cores, protoplanetary disks and exoplanetary atmospheres are summarized, both for simple and more complex molecules, with links to papers presented in this volume. In spite of many lingering uncertainties, the future of astrochemistry is bright: new observational facilities promise major advances in our understanding of the journey of gas, ice and dust from clouds to planets.Comment: Introductory paper for Faraday Discussions 168 conference, April 201

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“…This value is a lower limit for the core maximum extinction as no stars are seen through the very centre of the core. Using the relation between the hydrogen column density and extinction in Bohlin et al (1978), the estimated H 2 column density corresponding to this extinction is approximately 2.0 ± 0.4 × 10 22 cm −2 (Av/E(B − V) is assumed to be 3.2). This is slightly lower than that derived in the centre of the core from the C 18 O data.…”

Section: The Mass Of Bhr 160mentioning

confidence: 99%

The Bok globule BHR 160: structure and star formation

Haikala¹,

Reipurth²

2017

A&A

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Context. BHR 160 is a virtually unstudied cometary globule within the Sco OB4 association in Scorpius at a distance of 1600 pc. It is part of a system of cometary clouds which face the luminous O star HD 155806. BHR 160 is special because it has an intense bright rim. Aims. We attempt to derive physical parameters for BHR 160 and to understand its structure and the origin of its peculiar bright rim. Methods. BHR 160 was mapped in the 12 CO, 13 CO and C 18 O (2−1) and (1−0) and CS (3−2) and (2−1) lines. These data, augmented with stellar photometry derived from the ESO VVV survey, were used to derive the mass and distribution of molecular material in BHR 160 and its surroundings. Archival mid-infrared data from the WISE satellite was used to find IR excess stars in the globule and its neighbourhood.Results. An elongated 1 by 0 .6 core lies adjacent to the globule bright rim. 12 CO emission covers the whole globule, but the 13 CO, C 18 O and CS emission is more concentrated to the core. The 12 CO line profiles indicate the presence of outflowing material near the core, but the spatial resolution of the mm data is not sufficient for a detailed spatial analysis. The BHR 160 mass estimated from the C 18 O mapping is 100 ± 50 M (d/1.6 kpc) 2 where d is the distance to the globule. Approximately 70% of the mass lies in the dense core. The total mass of molecular gas in the direction of BHR 160 is 210 ± 80 (d/1.6 kpc) 2 M when estimated from the more extended VVV near-infrared photometry. We argue that the bright rim of BHR 160 is produced by a close-by early B-type star, HD 319648, that was likely recently born in the globule. This star is likely to have triggered the formation of a source, IRS 1, that is embedded within the core of the globule and detected only in Ks and by WISE and IRAS.

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A survey of interstellar H I from L-alpha absorption measurements. II

Cited by 2,333 publications

References 0 publications

The Properties of the Magellanic Bridge Based on OGLE IV RR Lyrae Variables

The Properties of the Magellanic Bridge Based on OGLE IV RR Lyrae Variables

Astrochemistry of dust, ice and gas: introduction and overview

The Bok globule BHR 160: structure and star formation

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