[ITAL]MIDCOURSE SPACE EXPERIMENT[/ITAL][ITAL]Midcourse Space Experiment[/ITAL] Survey of the Galactic Plane

Price, S. D.; Egan, M. P.; Carey, Sean; Mizuno, D. R.; Kuchar, T. A.

doi:10.1086/320404

Cited by 479 publications

(419 citation statements)

References 32 publications

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“…When the distance ambiguity could be solved, the preferred distance and mass are shown in boldface. searched systematically for infrared counterparts to our preliminary catalog of 6000 sources in the IRAS Point Source Catalog (Beichman et al 1988) and in the Midcourse Space Experiment (MSX, Price et al 2001) data, using a search radius of 30 (more details will be given in Contreras et al, in prep.). Only ∼10% of the submm compact sources can be associated with an IRAS point source, and ∼32% have a possible MSX counterpart (Fig.…”

Section: Nature Of the Sourcesmentioning

confidence: 99%

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Schüller¹,

Menten²,

Contreras

et al. 2009

A&A

725

927

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Context. Thanks to its excellent 5100 m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so far. Aims. Our goal is to produce a large-scale, systematic database of massive pre-and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. Only a systematic survey of the Galactic Plane can provide the statistical basis for unbiased studies. A well characterized sample of Galactic star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submillimeter wavelengths also represents a preparatory work for Herschel and ALMA. Methods. The APEX telescope is ideally located to observe the inner Milky Way. The Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer array observing at 870 μm, with a beam size of 19. 2. Taking advantage of its large field of view (11. 4) and excellent sensitivity, we started an unbiased survey of the entire Galactic Plane accessible to APEX, with a typical noise level of 50−70 mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). Results. As a first step, we covered ∼95 deg 2 of the Galactic Plane. These data reveal ∼6000 compact sources brighter than 0.25 Jy, or 63 sources per square degree, as well as extended structures, many of them filamentary. About two thirds of the compact sources have no bright infrared counterpart, and some of them are likely to correspond to the precursors of (high-mass) proto-stars or protoclusters. Other compact sources harbor hot cores, compact H ii regions, or young embedded clusters, thus tracing more evolved stages after massive stars have formed. Assuming a typical distance of 5 kpc, most sources are clumps smaller than 1 pc with masses from a few 10 to a few 100 M . In this first introductory paper, we show preliminary results from these ongoing observations, and discuss the mid-and long-term perspectives of the survey.

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Section: Nature Of the Sourcesmentioning

confidence: 99%

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

Schüller¹,

Menten²,

Contreras

et al. 2009

A&A

725

927

View full text Add to dashboard Cite

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“…(This table is available in its entirety in FITS format.) 10 Bright, massive YSO candidates in M17 SWex detected by The Midcourse Space Experiment (MSX; Price et al 2001) were previously cataloged by PW10; we incorporate three of these sources into our analysis of the M17 SWex stellar population in the ACIS FOV (Section 3). 11 This essentially leaves A V unconstrained when fitting sources with YSO models, necessary because candidate protostars are found deeply embedded in the IRDC lanes, where extinction can be extreme and background stars are obscured even in the IR.…”

Section: A1 Mir Identification Of Ysos Associated With M17 Swexmentioning

confidence: 99%

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Povich

Townsley

Robitaille

et al. 2016

ApJ

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We present a catalog of 840 X-ray sources and first results from a 100 ks Chandra X-ray Observatory imaging study of the filamentary infrared (IR) dark cloud G014.225-00.506, which forms the central regions of a larger cloud complex known as the M17 southwest extension (M17 SWex). In addition to the rich population of protostars and young stellar objects with dusty circumstellar disks revealed by archival data from the Spitzer Space Telescope, we discover a population of X-ray-emitting, intermediate-mass pre-main-sequence stars that lack IR excess emission from circumstellar disks. We model the IR spectral energy distributions of this source population to measure its mass function and place new constraints on the destruction timescales for the inner dust disk for 2-8 M ☉ stars. We also place a lower limit on the star formation rate (SFR) and find that it is quite high (  M 0.007 M ☉ yr −1 ), equivalent to several Orion Nebula Clusters in G14.225-0.506 alone, and likely accelerating. The cloud complex has not produced a population of massive, O-type stars commensurate with its SFR. This absence of very massive (20 M ☉ ) stars suggests that either (1) M17 SWex is an example of a distributed mode of star formation that will produce a large OB association dominated by intermediate-mass stars but relatively few massive clusters, or (2) the massive cores are still in the process of accreting sufficient mass to form massive clusters hosting O stars.

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“…The panel at lower right shows (red) contours of the peak CO brightness over the wider range −26 km s −1 < v < 26 km s −1 overlaid on an image of MSX (Price et al 2001) Band A 8.3μ emission.…”

Section: Disk and Bar Gas Atmentioning

confidence: 99%

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

Liszt

2009

A&A

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Results. Although broad CO lines characteristic of shocked gas were not seen in this kinematically complex region, a bright (14 K), new, marginally-resolved ±9 km s −1 outflow source G5.638+0.233 and a comparably bright rim of CO emission were found at/around the periphery of SNR G5.55+0.12. Most of the periphery of SNR G5.71-0.08 is surrounded by a bright rim of CO emission. CO emission at the 7 km s −1 velocity of a 1720 OH maser spot near SNR G5.70-0.12 is very bright, 19 K, but gas at −21 km s −1 is widespread over the region and CO emission is rather weak toward the OH maser spots at this velocity north of G5.4-1.2. Other very bright CO lines in the region are associated with H II regions, i.e. 27 K toward W28A2 = G5.89-0.39 and 15 K toward an MSX-IR source at l = 5.9 o , b = −0.13 o which is probably the exciting agent of a separate, classical HII region just north of W28A2.

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[ITAL]MIDCOURSE SPACE EXPERIMENT[/ITAL][ITAL]Midcourse Space Experiment[/ITAL] Survey of the Galactic Plane

Cited by 479 publications

References 32 publications

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

ATLASGAL – The APEX telescope large area survey of the galaxy at 870 $\mathsf{\mu}$m

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

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