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A new method of determining distances to dark globules.: The distance to B 335
Stockholm University, Faculty of Science, Department of Astronomy.
Stockholm University, Faculty of Science, Department of Astronomy.
2009 (English)In: Astronomy & Astrophysics, Vol. 498, no 2, 455-461 p.Article in journal (Refereed) Published
Abstract [en]

Context. The distance to an isolated dark globule is often unknown and yet crucial for understanding its properties, in particular its mass. A new approach to this problem is discussedAims. The purpose of the present paper is to investigate how well the distances of more or less reddened field stars can be determined by using multi-colour imaging.Methods. We observed a test globule, B 335 in UBgr, and I, and together with the 2MASS survey, this data set gives a well-defined spectral energy distribution (SED) of a large number of stars. The SED of each star depends on the interstellar extinction, the distance to the star, and its intrinsic SED. As we had good reasons to suspect that the wavelength dependence of the extinction (the reddening) changes from the outskirts of the globule to the central parts, we did not assume any specific reddening law. Instead, we use a scheme that allows independent determination of the extinction in each line of sight as determined by groups of adjacent stars. The method is based on the use of stellar atmospheric models to represent the intrinsic SEDs of the stars. Formally, it is then possible to determine the spectral class of each star and thereby its distance. For some of the stars we have optical spectra, allowing us to compare the photometric classification to the spectrometric. Results. As expected, the main problem is that there are few stars found within each distance bin for the small field size defining a typical dark globule. However, the characterisation of the extinction and photometric classification give consistent results and we can identify one star at the front side of the globule. It has a photometric distance of 90 pc. The closest star behind the B 335 globule has a distance of only 120 pc and we therefore determine the distance to B 335 as 90-120 pc. Our deep U image shows a relatively bright south-western rim of the globule, and we investigate whether it might be due to a local enhancement of the radiation field. A candidate source, located 1.5 arcmin outside our field, would be the field star, HD 184982. This star has an entry in the Hipparcos Catalogue and its distance is 140-200 pc. However, we come to the conclusion that the bright SW rim is more likely due to the wing of the point-spread-function (PSF) of this star.

Place, publisher, year, edition, pages
2009. Vol. 498, no 2, 455-461 p.
Keyword [en]
ISM: clouds -- ISM: individual objects: B 335 -- ISM: dust, extinction
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy
Identifiers
URN: urn:nbn:se:su:diva-34487DOI: 10.1051/0004-6361/200811574ISI: 000265868600020OAI: oai:DiVA.org:su-34487DiVA: diva2:284896
Available from: 2010-01-08 Created: 2010-01-08 Last updated: 2012-02-14Bibliographically approved
In thesis
1. Extinction in Molecular Clouds: Case of Barnard 335
Open this publication in new window or tab >>Extinction in Molecular Clouds: Case of Barnard 335
2012 (English)Doctoral thesis, comprehensive summary (Other academic)
Abstract [en]

The Bok globule B335 is a small molecular cloud in the solar neighbourhood near the galactic plane. The aim for this three-paper-study is to construct and analyze the extinction for this globule.

The method we apply is to use the light from field stars behind the cloud in broadband filters ranging from UV to the mid-infrared. We have observations performed at the ESO telescopes at La Silla and Paranal as well as at the Nordic 2.5 m telescope at La Palma. Together with images and spectra from 2MASS-, ISO- and Spitzer-archives we are able to cover the wavelength range from 0.35 to 24 μm. An important tool to analyze these observations results in order to get the extinction is the grid of synthetic stellar atmospheric spectra provided by Hauschildt (2005).

The extinction so received is a result in itself. From the analysis of the extinction wavelength dependence we derive properties of the dust, especially its composition and grain size distribution. By modeling the grain size distribution we are able to find the extinction from the reddening of the stars.

We find that the extinction in the optical wavelength 0.35 to 2 μm range nicely follows the functional form described by Cardelli et al. (1989). Our result from the wavelength range redward of 2 μm show an extinction dependent on the part of the cloud examined. For the rim of the cloud we get an extinction similar to that reported earlier for the diffuse interstellar medium. From the central parts of the cloud, however, a higher extinction was found. Our grain size model contains a carbonaceous particle distribution and a silicate one. The result can be explained by depletion of carbon onto carbonaceous grains and also by carbon onto all grains including the silicates.

Our modeling of the extinction and our classification of the background stars allow us to

- determine the distance to the globule

- estimate the gas column density ratio

- estimate the mass of globule

- get a handle on the dust conversion processes through the grain size distribution

 

From the water- and CO-ice spectra we are able to estimate the ice column densities. We find similar ice column densities for the two ices. The estimates differ, when calculated from band strengths or from Lorenz-Mie calculations of ice mantles on the grain size distribution, by a factor of two.

Place, publisher, year, edition, pages
Stockholm: Department of Astronomy, Stockholm University, 2012. 78 p.
Keyword
ISM, interstellar medium, extinction, molecular cloud
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy; Astronomy
Identifiers
urn:nbn:se:su:diva-72523 (URN)978-91-7447-430-5 (ISBN)
Public defence
2012-03-16, sal FB52, AlbaNova universitetscentrum, Roslagstullsbacken 21, Stockholm, 13:00 (English)
Opponent
Supervisors
Available from: 2012-02-23 Created: 2012-02-14 Last updated: 2012-02-21Bibliographically approved

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