The Structure of Molecular Clouds: I - All Sky Near Infrared Extinction Maps

Details The Structure of Molecular Clouds: I - All Sky Near Infrared Extinction Maps The Structure of Molecular Clouds: I - All Sky Near Infrared Extinction Maps

2009-02-19

arxiv.org/abs/0902.3403v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

39 pages, 3 tables, 54 figures, accepted for publication by MNRAS, a version with higher resolution figures can be found at

Scientific paper

10.1111/j.1365-2966.2009.14655.x

We are studying the column density distribution of all nearby giant molecular clouds. As part of this project we generated several all sky extinction maps. They are calculated using the median near infrared colour excess technique applied to data from the Two Micron All-Sky Survey (2MASS). Our large scale approach allows us to fit spline functions to extinction free regions in order to accurately determine the colour excess values. Two types of maps are presented: i) Maps with a constant noise and variable spatial resolution; ii) Maps with a constant spatial resolution and variable noise. Our standard Av map uses the nearest 49 stars to the centre of each pixel for the determination of the extinction. The one sigma variance is constant at 0.28mag Av in the entire map. The distance to the 49th nearest star varies from below 1arcmin near the Galactic Plane to about 10arcmin at the poles, but is below 5arcmin for all giant molecular clouds (|b|< 30degr). A comparison with existing large scale maps shows that our extinction values are systematically larger by 20% compared to Dobashi et al. and 40% smaller compared to Schlegel et al.. This is most likely caused by the applied star counting technique in Dobashi et al. and systematic uncertainties in the dust temperature and emissivity in Schlegel et al.. Our superior resolution allows us to detect more small scale high extinction cores compared to the other two maps.

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