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The ATLASGAL survey: distribution of cold dust in the Galactic plane. Combination with Planck data | | T. Csengeri
; A. Weiss
; F. Wyrowski
; K. M. Menten
; J. S. Urquhart
; S. Leurini
; F. Schuller
; H. Beuther
; S. Bontemps
; L. Bronfman
; Th. Henning
; N. Schneider
; | | Date: |
23 Nov 2015 | | Abstract: | Sensitive ground-based submillimeter surveys, such as ATLASGAL, provide a
global view on the distribution of cold dense gas in the Galactic plane. Here
we use the 353 GHz maps from the Planck/HFI instrument to complement the
ground-based APEX/LABOCA observations with information on larger angular
scales. The resulting maps reveal the distribution of cold dust in the inner
Galaxy with a larger spatial dynamic range. We find examples of elongated
structures extending over angular scales of 0.5 degree. Corresponding to >30 pc
structures in projection at a distance of 3 kpc, these dust lanes are very
extended and show large aspect ratios. Furthermore, we assess the fraction of
dense gas ($f_{
m DG}$), and estimate 2-5% (above A$_{
m{v}}>$7 mag) on
average in the Galactic plane. PDFs of the column density reveal the typically
observed log-normal distribution for low- and exhibit an excess at high column
densities. As a reference for extragalactic studies, we show the line-of-sight
integrated N-PDF of the inner Galaxy, and derive a contribution of this excess
to the total column density of $sim2.2$%, above $N_{
m H_2} =
2.92 imes10^{22}$ cm$^{-2}$. Taking the total flux density, we provide an
independent estimate of the mass of molecular gas in the inner Galaxy of
$sim1 imes10^9,M_{odot}$, which is consistent with previous estimates using
CO emission. From the mass and $f_{
m DG}$ we estimate a Galactic SFR of $dot
M = 1.3,M_{odot}$ yr$^{-1}$. While the distribution of diffuse gas is
homogenous in the inner Galaxy, the CMZ stands out with a higher dense gas
fraction. The low star formation efficiency of the Milky Way is well explained
by the low $f_{
m DG}$ in the Galactic ISM, while the high $f_{
m DG}$
towards the CMZ, despite its low star formation activity, suggests that, in
that particular region of our Galaxy, high-density gas is not the bottleneck
for star formation. | | Source: | arXiv, 1511.7145 | | Services: | Forum | Review | PDF | Favorites | |
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