A KOSMA 7 deg^2 13CO 2--1 & 12CO 3--2 survey of the Perseus cloud

Details A KOSMA 7 deg^2 13CO 2--1 & 12CO 3--2 survey of the Perseus cloud A KOSMA 7 deg^2 13CO 2--1 & 12CO 3--2 survey of the Perseus cloud

2006-01-27

arxiv.org/abs/astro-ph/0601650v2

Astronomy and Astrophysics

Astrophysics

11 pages, 10 figures, accepted by A&A

Scientific paper

Characterizing the spatial and velocity structure of molecular clouds is a first step towards a better understanding of interstellar turbulence and its link to star formation. We present observations and structure analysis results for a large-scale (~ 7.10 deg^2) 13CO J = 2--1 and 12 CO J = 3--2 survey towards the nearby Perseus molecular cloud observed with the KOSMA 3m telescope. We study the spatial structure of line-integrated and velocity channel maps, measuring the $\Delta$-variance as a function of size scale. We determine the spectral index $\beta$ of the corresponding power spectrum and study its variation across the cloud and across the lines. We find that the spectra of all CO line-integrated maps of the whole complex show the same index, $\beta$ ~ 3.1, for scales between about 0.2 and 3pc, independent of isotopomer and rotational transition. A complementary 2MASS map of optical extinction shows a noticeably smaller index of 2.6. In contrast to the overall region, the CO maps of individual subregions show a significant variation of $\beta$. The 12CO 3--2 data provide e.g. a spread of indices between 2.9 in L1455 and 3.5 in NGC1333. In general, active star forming regions show a larger power-law exponent. We find that the $\Delta$-variance spectra of individual velocity channel maps are very sensitive to optical depth effects clearly indicating self-absorption in the densest regions. When studying the dependence of the channel-map spectra as a function of the velocity channel width, the expected systematic increase of the spectral index with channel width is only detected in the blue line wings.This could be explained by a filamentary, pillar-like structure which is left at low velocities while the overall molecular gas is swept up by a supernova shock wave.

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