Submillimeter Observations of Midcourse Space Experiment Galactic Infrared-Dark Clouds

By S. Carey, P. Feldman, R. O. Redman, M. P. Egan, J. Macleod, Stephan D. Price. 2000

147 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/17dff54d2b02b7b2ee9f1a3dc31cd5a92128d62e

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Citations in the corpus

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…”
FRAGMENTATION AT THE EARLIEST PHASE OF MASSIVE STAR FORMATION (2009, methodology): “As shown in Figure 2, the two dust clumps P1 and P2 detected with the IRAM 30 m telescope and JCMT at resolutions from 11′′ to 15′′ (Rathborne et al. 2006; Carey et al. 1998) are resolved by the SMA into multiple structures at 1.”
The 6-GHz multibeam maser survey-I. Techniques (2008, methodology): “Furthermore, Infrared Dark Clouds (IRDCs) detected by the Midcourse Space Experiment (MSX), and recognised as potential star formation regions in their early stages (Carey et al. 2000), have up to 50 per cent of their population outside | b |6 0.5◦.”
CHEMISTRY IN INFRARED DARK CLOUD CLUMPS: A MOLECULAR LINE SURVEY AT 3 mm (2011, background): “The first studies characterizing them suggested that they were cold (<25 K), massive (∼102–104 M⊙), and dense (&10 5 cm−3) molecular clouds with high column densities (&1023 cm−2) (Carey et al. 1998, 2000).”
Methanol Masers: Reliable Tracers of the Early Stages of High-Mass Star Formation (2005, methodology): “These cold clouds are sufficiently dense to be detected in sub-millimeter emission with instruments such as the JCMT, and show similar overall morphology in sub-millimeter emission to that seen in infrared absorption (Carey et al. 2000).”
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).”
Infrared Dark Clouds: Precursors to Star Clusters (2004, methodology): “…of 15 K, which is consistent with temperature estimates from molecular line emission (Teyssier et al. 2002), previous observations of a few IRDCs at submillimeter wavelengths (Carey et al. 2000), and the fact that some IRDCs are seen as extinction features up to 100 µm (Egan et al. 1998).”
THE LEGACY OF SCUPOL: 850 μm IMAGING POLARIMETRY FROM 1997 TO 2005 (2009, unknown): “34+0.06 SFR 58 ∼4.8 Carey et al. (2000) Y IRAS 18437-0216 SFR 59 6.6 Sridharan et al. (2005) Y W48 SFR 60 3.4 Vallée & MacLeod (1990) N Curran et al. (2004, 2005) R Cr A SFR 61 0.130 Marraco & Rydgren (1981) N Curran & Chrysostomou (2007) Clark et al. (2000) W49 SFR 62 11.4 Gwinn et al. (1992) N…”
Ammonia in infrared dark clouds (2006, background): “SCUBA 850 µm image (Carey et al. 2000) of the cloud G11.”
STAR FORMATION ACTIVITY OF CORES WITHIN INFRARED DARK CLOUDS (2009, background): “The detection of strong mm (Beuther et al. 2005; Rathborne et al. 2005, 2006) and (sub)mm (Lis & Carlstrom 1994; Carey et al. 2000; Redman et al. 2003; Rathborne et al. 2005) dust emission from cores within IRDCs, combined with their cold temperatures and high densities, make IRDCs ideal candidates…”
Hierarchical fragmentation and differential star formation in the Galactic ‘Snake’: infrared dark cloud G11.11−0.12 (2014, methodology): “On clump scale, Gaussian fitting o the JCMT 850µm image (Carey et al. 2000; Johnstone et al. 2003) yields an integrated flux of 8.7 Jy in a FWHM size of40′′ × 25′′ (0.7 × 0.4 pc) for P1.”
THE “NESSIE” NEBULA: CLUSTER FORMATION IN A FILAMENTARY INFRARED DARK CLOUD (2009, background): “…clouds (IRDCs) were originally identified as dark extinction features against the Galactic background at mid-IR wavelengths (Perault et al. 1996; Egan et al. 1998; Carey et al. 1998, 2000; Hennebelle et al. 2001), it was not clear what role, if any, they might play in the process of star formation.”
The earliest phases of high-mass star formation: a 3 square degree millimeter continuum mapping of Cygnus X (2007, background): “…have been made in submillimeter continuum maps (e.g. Molinari et al. 1998; Motte et al. 2003; Sandell & Sievers 2004; Hill et al. 2005) and as absorption regions in mid-infrared images (often called “infrared dark clouds”, e.g. Carey et al. 2000; Thompson et al. 2005; Rathborne et al. 2006).”
A Catalog of Midcourse Space Experiment Infrared Dark Cloud Candidates (2006, methodology): “Source Validation To validate a subsample of our IRDCs, we correlated our catalog with the source lists obtained from MSX (Egan et al. 1998; Carey et al. 1998, 2000) and ISO data (Hennebelle et al. 2001; Teyssier et al. 2002).”
HOW MANY INFRARED DARK CLOUDS CAN FORM MASSIVE STARS AND CLUSTERS? (2010, background): “Embedded in IRDCs are “cores” of a few dozen solar masses (Carey et al. 2000).”
The evolution of the spectral energy distribution in massive young stellar objects (2008, background): “…and submm surveys are needed to extend the source coverage to equally massive but lower luminosity objects; the InfraRed Dark Clouds revealed by MSX (Egan et al. 1998; Carey et al. 2000; Simon et al. 2006) are very promising objects to investigate for the earlier stages of massive star formation.”
Slow Star Formation in Dense Gas: Evidence and Implications (2006, background): “Infrared dark clouds (IRDCs) are regions of high extinction seen in absorption against the Galactic infrared background (Egan et al. 1998; Carey et al. 2000; Simon et al. 2006).”
Ammonia from cold high-mass clumps discovered in the inner Galactic disk by the ATLASGAL survey (2012, background): “But to date, only a small fraction of them has been investigated in detail (Carey et al. 1998, 2000; Pillai et al. 2006; Rathborne et al. 2006).”