The Characterization and Galactic Distribution of Infrared Dark Clouds

By R. Simon, J. Rathborne, R. Shah, J. Jackson, E. Chambers. 2006

175 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/fe24aabaf514e075734a8e85c60e247d366620ae

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

A CATALOG OF EXTENDED GREEN OBJECTS IN THE GLIMPSE SURVEY: A NEW SAMPLE OF MASSIVE YOUNG STELLAR OBJECT OUTFLOW CANDIDATES (2008, methodology): “The range of distances–from 2.6 to 5.3 kpc–is typical of distances to MSFR in the Galactic Plane and to IRDCs as determined by Simon et al. (2006b) from 13CO emission.”
Planck 2015 results - XXVIII. The Planck Catalogue of Galactic cold clumps (2015, unknown): “The locus of the Simon et al. (2006b) IRDCs properties is shown as red points, including local thermodynamic equilibrium (LTE) mass estimates.”
HOW MANY INFRARED DARK CLOUDS CAN FORM MASSIVE STARS AND CLUSTERS? (2010, background): “Analysis by Simon et al. (2006) and Jackson et al. (2008) suggests that most IRDCs have distances of 2–8 kpc. Figure 4 illustrates the derived masses and sizes, and Table 1 characterizes the IRDCs found to be compact (i.e., m[r]/mlim[r] > 1).”
Hierarchical fragmentation and differential star formation in the Galactic ‘Snake’: infrared dark cloud G11.11−0.12 (2014, background): “This is what led to the cloud complexes containing such regions tobe ⋆ E-mail: kwang@eso.org coined “infrared-dark clouds” (IRDCs; Perault et al. 1996;Egan et al. 1998; Hennebelle et al. 2001; Simon et al. 2006a,b; Peretto & Fuller 2009).”
Infrared Dark Clouds: Precursors to Star Clusters (2004, methodology): “The total number of IRDCs in the Galaxy is not yet known.”
FRAGMENTATION AT THE EARLIEST PHASE OF MASSIVE STAR FORMATION (2009, background): “Systematic studies found that many IRDCs contain over 103M of dense molecular gas (Simon et al. 2006a; Rathborne et al. 2006; Pillai et al. 2006).”
CHEMISTRY IN INFRARED DARK CLOUD CLUMPS: A MOLECULAR LINE SURVEY AT 3 mm (2011, methodology): “They also correspond to the densest clouds embedded within giant molecular clouds (Simon et al. 2006b).”
The ATLASGAL survey: a catalog of dust condensations in the Galactic plane (2013, methodology): “These clouds have been cataloged using MSX (Simon et al. 2006; Rathborne et al. 2006) and the more sensitive Spitzer Space Telescope (Peretto & Fuller 2009; Butler & Tan 2009; Peretto & Fuller 2010; Rygl et al. 2010).”
The simultaneous formation of massive stars and stellar clusters (2009, background): “Recent observations of infrared dark clouds (IRDCs) (Carey et al. 1998; Egan et al. 1998; Carey et al. 2000; Rathborne, Jackson & Simon 2006; Simon et al. 2006) and high-mass protostellar objects (HMPOs) (Beuther et al. 2002; Sridharan et al. 2002; Faúndez et al. 2004; Williams, Fuller & Sridharan…”
Ammonia from cold high-mass clumps discovered in the inner Galactic disk by the ATLASGAL survey (2012, background): “Previous studies revealed that IRDCs are cold (<25 K), dense (>105 cm−3) and have high column densities (∼1023–1025 cm−2, Rathborne et al. 2006; Simon et al. 2006a).”
THE GREEN BANK TELESCOPE H ii REGION DISCOVERY SURVEY. II. THE SOURCE CATALOG (2011, methodology): “The 86.2 km s−1 velocity is similar to that of the IRDC, which is 75.8 km s−1 (Simon et al. 2006).”
The initial conditions of stellar protocluster formation - I. A catalogue of Spitzer dark clouds (2009, methodology): “Indeed, the large infrared surveys these satellites carried out identified infrared dark structures, seen in absorption from 7 to 25µm against the background emission (Perault et al. 1996; Hennebelle et al. 2001; Egan et al. 1998; Simon et al. 2006a) .”
STAR FORMATION ACTIVITY OF CORES WITHIN INFRARED DARK CLOUDS (2009, methodology): “In this paper, we use the mm continuum to identify IRDCs, but for future work we can also use the Catalog of IRDC candidates of Simon et al. (2006a) for this purpose.”
A CLASS I AND CLASS II CH3OH MASER SURVEY OF EGOs FROM THE GLIMPSE SURVEY (2009, background): “…against MIR Galactic background emission, particularly at 8 µm (Churchwell et al. 2009) surveys of the Galactic Plane, IRDCs are cold (T<20 K), dense (n(H 2 )>10 5 cm −3 ) clouds of molecular gas and dust (e.g. Carey et al. 1998; Egan et al. 1998; Hennebelle et al. 2001; Simon et al. 2006a,b).”
STAR FORMATION IN THE CENTRAL 400 PC OF THE MILKY WAY: EVIDENCE FOR A POPULATION OF MASSIVE YOUNG STELLAR OBJECTS (2009, background): “IRDCs are dense (> 105 cm−3), cold (< 25K) and attain high column densities (1023 cm−2) in the Galactic disk (Egan et al. 1998; Carey et al. 2000; Simon et al. 2006).”
Theory of Star Formation (2007, background): “Final Stars The earliest stages of high-mass star formation may occur in the Infrared Dark Clouds (IRDCs–Egan et al., 1998), which have properties consistent with being the dense clumps out of which clusters eventually form (Simon et al., 2006).”
THE BOLOCAM GALACTIC PLANE SURVEY: SURVEY DESCRIPTION AND DATA REDUCTION (2010, methodology): “IRDCs have now been extensively cataloged with MSX (Simon et al. 2006a) and GLIMPSE 8 μm data (Peretto & Fuller 2009).”
Initial highlights of the HOBYS key program, the Herschel imaging survey of OB young stellar objects (2010, background): “Controversy remains about the existence and the lifetime of high-mass analogs of prestellar cores, since infrared dark clouds are numerous (Simon et al. 2006) but only a few harbor starless, massive, and dense enough cores (e.g. Motte et al. 2007).”