The Bolocam Galactic Plane Survey. Ii. Catalog of the Image Data

Rosolowsky, Erik; Dunham, Miranda K.; Ginsburg, Adam; Bradley, E. T.; Aguirre, James E.; Bally, John; Battersby, Cara; Cyganowski, C. J.; Dowell, Darren; Drosback, Meredith M.; Evans, Neal J.; Glenn, J.; Harvey, P. M.; Stringfellow, Guy S.; Walawender, Josh; Williams, Jonathan P.

doi:10.1088/0067-0049/188/1/123

Cited by 228 publications

(356 citation statements)

References 23 publications

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“…size of the beam (i.e., σ bm = θ FWHM / √ 8 ln 2 ≃ 8 ′′ ). Following Rosolowsky et al (2010) to be consistent with the analysis presented in Paper I we adopt a value for η of 2.4; this is roughly equivalent to the usual source effective radius R eff = √ (A/π) (where A is the surface area of the source; Dunham et al 2011). Combining this angular size with the kinematic distances we calculate the physical size of the host dust clump.…”

Section: Effective Radiusmentioning

confidence: 95%

The almost ubiquitous association of 6.7-GHz methanol masers with dust★

Urquhart

Moore

Menten

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We report the results of 870-µmcontinuum observations, using the Large APEX Bolometer Camera (LABOCA), towards 77 class-II, 6.7-GHz methanol masers identified by the Methanol Multibeam (MMB) survey to map the thermal emission from cool dust towards these objects. These data complement a study of 630 methanol masers associated with compact dense clumps identified from the ATLASGAL survey. Compact dust emission is detected towards 70 sources, which implies a dust-association rate of 99 per cent for the full MMB catalogue. Evaluation of the derived dust and maser properties leads us to conclude that the combined sample represents a single population tracing the same phenomenon. We find median clump masses of a few 10 3 M ⊙ and that all but a handful of sources satisfy the mass-size criterion required for massive star formation. This study provides the strongest evidence of the almost ubiquitous association of methanol masers with massive, star-forming clumps. The fraction of methanol-maser associated clumps is a factor of ∼2 lower in the outer Galaxy than the inner Galaxy, possibly a result of the lower metallicity environment of the former. We find no difference in the clump-mass and maser-luminosity distributions of the inner and outer Galaxy. The maser-pumping and clump-formation mechanisms are therefore likely to be relatively invariant to Galactic location. Finally, we use the ratio of maser luminosity and clump mass to investigate the hypothesis that the maser luminosity is a good indicator of the evolutionary stage of the embedded source, however, we find no evidence to support this.

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Section: Effective Radiusmentioning

confidence: 95%

The almost ubiquitous association of 6.7-GHz methanol masers with dust★

Urquhart

Moore

Menten

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…We used the ATLASGAL-MMB associations identified in Urquhart et al (2013) to compare the dust emission of the 6.7-GHz methanol masers with and without associated water masers and also to compare the 870-µm emission with the results from Titmarsh et al (2014) using the 1.1 mm emission from the Galactic Plane is the Bolocam Galactic Plane Survey (BGPS; Rosolowsky et al 2010). The BGPS is another unbiased submillimeter survey of the Galactic Plane which used the Bolocam instrument on the Caltech Submillimeter Observatory to make a continuum survey of the Galactic Plane at 1.1 mm with an effective resolution of 33 arcseconds.…”

Section: Associations With 870-µm Emission From Dust Clumpsmentioning

confidence: 99%

“…Recently, there have been two large, unbiased surveys of the Galactic Plane in the submillimetre regime. The Bolocam Galactic Plane Survey (BGPS; Rosolowsky et al 2010) at 1.1 mm and the APEX Telescope Large Area Survey of the GALaxy (ATLASGAL; Schuller et al 2009;Contreras et al 2013;Csengeri et al 2014) at 870 µm.…”

Section: Introductionmentioning

confidence: 99%

A search for water masers associated with class II methanol masers – II. Longitude range 341° to 6°

Titmarsh

Ellingsen

Breen

et al. 2016

Mon. Not. R. Astron. Soc.

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This is the second paper in a series of catalogues of 22-GHz water maser observations towards the 6.7-GHz methanol masers from the Methanol Multibeam (MMB) Survey. In this paper we present our water maser observations made with the Australia Telescope Compact Array towards the masers from the MMB survey between l = 341 • through the Galactic centre to l = 6 • . Of the 204 6.7-GHz methanol masers in this longitude range we found 101 to have associated water maser emission (∼ 50 per cent). We found no difference in the 6.7-GHz methanol maser luminosities of those with and without water masers. In sources where both maser species are observed, the luminosities of the methanol and water masers are weakly correlated. Studying the mid-infrared colours from GLIMPSE we found no differences between the colours of those sources associated with both methanol and water masers and those associated with just methanol. Comparing the column density and dust mass calculated from the 870-µm thermal dust emission observed by ATLASGAL, we found no differences between those sources associated with both water and methanol masers and those with methanol only. Since water masers are collisionally pumped and often show emission further away from their accompanying YSO than the radiatively pumped 6.7-GHz methanol masers, it is likely water masers are not as tightly correlated to the evolution of the parent YSO and so do not trace such a well defined evolutionary state as 6.7-GHz methanol masers.

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“…BGPS is a 1.1 mm continuum survey of the Galactic Plane made using Bolocam on the Caltech submillimeter Observatory, the survey coverage totals 170 square degrees (with 33. ′′ FWHM effective resolution) and detected about 8400 point sources (Rosolowsky et al (2010)). …”

Section: Datamentioning

confidence: 99%

A detailed study of the high-mass clump interacting with the bubble N10

Zhou

Esimbek

et al. 2013

Astrophys Space Sci

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We performed a detailed study of the highmass clump interacting with bubble N10 based on the spectral lines 12 CO(3 − 2), HCO + (4 − 3), N 2 H + (4 − 3) and CH 3 OH(7(0, 7) − 6(0, 6)) and continuum emission data at 450 µm and 850 µm released on CADC and Spitzer data. Blue-shifted optically thick line 12 CO(3− 2) seems to indicate that the outer envelope of the highmass clump is still falling toward the center. Detection of CH 3 OH(7(0, 7) − 6(0, 6)) suggests that a hot core has formed around YSO N10-7. And position-velocity diagram of N 2 H + (4−3) indicates the cold dense core of the clump has not been destroyed by the star formation activities. The mass of N10-7 is about 27.44 M ⊙ . The ratio HCO + (4 − 3)/N 2 H + (4 − 3) in the outer part of the clump is larger than that in the inner part of it. The reason may be that the CO abundance relative to N 2 H + (4 − 3) increased in the outer part of the highmass clump, more N 2 H + (4 − 3) were converted into HCO + (4 − 3).

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The Bolocam Galactic Plane Survey. Ii. Catalog of the Image Data

Cited by 228 publications

References 23 publications

The almost ubiquitous association of 6.7-GHz methanol masers with dust★

The almost ubiquitous association of 6.7-GHz methanol masers with dust★

A search for water masers associated with class II methanol masers – II. Longitude range 341° to 6°

A detailed study of the high-mass clump interacting with the bubble N10

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