Physical processes in the ISM

Session

Poster Session: Molecular cloud properties (Poster 8-11)

21 Oct 2013, 09:00

MPE

111. A Multi-Scale Continuum and Line Exploration of the Most Luminous Star Formation Region in the Milky Way. The Mass Structure of the Giant Molecular Cloud.

Roberto Galvan-Madrid (ESO-Garching)

21/10/2013, 09:00

Poster

The Multi-Scale Continuum and Line Exploration of W49 (MUSCLE W49) is a comprehensive gas and dust survey of the parental giant molecular cloud (GMC) of W49A, the most luminous ($L \sim 10^{7.3} L_{sun}$) star-formation region in the Milky Way. The project has multiple components that cover the entire GMC at different scales and angular resolutions. We present results from observations with...

20. Analysis of structural scaling of molecular clouds with wavlet cross-correlation.

Tigran Arshakian (Universität zu Köln)

21/10/2013, 09:00

Poster

We develop a wavelet-based cross-correlation (WCC) method to study the correlation between characteristic structures in molecular clouds as a function of scale. The method compares a pair of maps observed in different tracers, at different wavelenghts or in different velocity ranges. Advantages of the WCC: (i) it allows to measure the correlation coefficient and structural offset between two...

101. CO isotope chemistry in GMC simulations: impact of the $^{12}$CO/$^{13}$CO ratio on column density estimates

László Szücs (Universität Heidelberg, ZAH, ITA)

21/10/2013, 09:00

Poster

Carbon monoxide molecule (CO) and its isotopes are frequently used as tracers of column density in studies of the dense interstellar medium. The most abundant CO isotope, $^{12}$CO, is usually optically thick in intermediate and high density regions and so provides only a lower limit for the column density. In these regions, less abundant isotopes are used, such as $^{13}$CO. To relate...

142. Turbulent assembly of molecular clouds

Juan Camilo Ibañez (ZAH/ITA)

21/10/2013, 09:00

Poster

Studying how self-gravitating turbulence in the interstellar medium determines the morphology, density profile and velocity dispersion of dense molecular clouds is key to understand the initial conditions of star formation. We use the Flash adaptive mesh refinement magnetohydrodynamics code to perform three-dimensional numerical simulations of a vertical column of the interstellar medium...