The Bolocam Galactic Plane Survey. Ix. Data Release 2 and Outer Galaxy Extension

Ginsburg, Adam; Glenn, J.; Rosolowsky, Erik; Ellsworth-Bowers, T. P.; Battersby, Cara; Dunham, Miranda K.; Merello, Manuel; Shirley, Yancy L.; Bally, John; Evans, Neal J.; Stringfellow, Guy S.; Aguirre, James E.

doi:10.1088/0067-0049/208/2/14

Cited by 152 publications

(212 citation statements)

References 41 publications

Supporting

Mentioning

208

Contrasting

Order By: Relevance

“…The BGPS observed part of the Galactic Plane at the effective resolution of 33 ′′ and 1σ sensitivity ranging from 30 to 100 mJy per beam (Aguirre et al 2011;Ginsburg et al 2013). The BGPS provides contiguous observational data over the ranges of |b| < 0.5…”

Section: Millimeter Dust Continuum Emissionmentioning

confidence: 99%

Star Formation Relations in the Milky Way

Vutisalchavakul¹,

Evans²

2016

ApJ

Self Cite

111

141

View full text Add to dashboard Cite

The relations between star formation and properties of molecular clouds are studied based on a sample of star forming regions in the Galactic Plane. Sources were selected by having radio recombination lines to provide identification of associated molecular clouds and dense clumps. Radio continuum and mid-infrared emission were used to determine star formation rates, while 13 CO and submillimeter dust continuum emission were used to obtain masses of molecular and dense gas, respectively. We test whether total molecular gas or dense gas provides the best predictor of star formation rate. We also test two specific theoretical models, one relying on the molecular mass divided by the free-fall time, the other using the free-fall time divided by the crossing time. Neither is supported by the data. The data are also compared to those from nearby star forming regions and extragalactic data. The star formation "efficiency," defined as star formation rate divided by mass, spreads over a large range when the mass refers to molecular gas; the standard deviation of the log of the efficiency decreases by a factor of three when the mass of relatively dense molecular gas is used rather than the mass of all the molecular gas.

show abstract

Section: Millimeter Dust Continuum Emissionmentioning

confidence: 99%

Star Formation Relations in the Milky Way

Vutisalchavakul¹,

Evans²

2016

ApJ

Self Cite

111

141

View full text Add to dashboard Cite

show abstract

“…We decided not to consider the MIPSGAL 24 μm fluxes because in most of our objects these happen to be heavily saturated. For the sake of completeness, we also included the ATLASGAL 1 (Schuller et al 2009;Contreras et al 2013) 870 μm and BGPS v2 (Ginsburg et al 2013) 1.1 mm fluxes. The resulting SEDs from 21 μm to 1.1 mm are shown in Fig.…”

Section: Ir and (Sub)mm Counterparts Of The Hii Regionsmentioning

confidence: 99%

Infrared emission of young HII regions: aHerschel/Hi-GAL study

Cesaroni

Pestalozzi

Beltrán

et al. 2015

A&A

View full text Add to dashboard Cite

Context. Investigating the relationship between radio and infrared emission of Hii regions may help shed light on the nature of the ionizing stars and the formation mechanism of early-type stars in general. Aims. We have taken advantage of recent unbiased surveys of the Galactic plane such as Herschel/Hi-GAL and VLA/CORNISH to study a bona fide sample of young Hii regions located in the Galactic longitude range 10 • -65 • by comparing the mid-and far-IR continuum emission to the radio free-free emission at 5 GHz. Methods. We have identified the Hi-GAL counterparts of 230 CORNISH Hii regions and reconstructed the spectral energy distributions of 204 of these by complementing the Hi-GAL fluxes with ancillary data at longer and shorter wavelengths. Using literature data, we obtained a kinematical distance estimate for 200 Hii regions with Hi-GAL counterparts and determined their luminosities by integrating the emission of the corresponding spectral energy distributions. We have also estimated the mass of the associated molecular clumps from the (sub)millimeter flux densities. Results. Our main finding is that for ∼1/3 of the Hii regions the Lyman continuum luminosity appears to be greater than the value expected for a zero-age main-sequence star with the same bolometric luminosity. This result indicates that a considerable fraction of young, embedded early-type stars presents a "Lyman excess" possibly due to UV photons emitted from shocked material infalling onto the star itself and/or a circumstellar disk. Finally, by comparing the bolometric and Lyman continuum luminosities with the mass of the associated clump, we derive a star formation efficiency of 5%. Conclusions. The results obtained suggest that accretion may still be present during the early stages of the evolution of Hii regions, with important effects on the production of ionizing photons and thus on the circumstellar environment. More reliable numerical models describing the accretion process onto massive stars are required to shed light on the origin of the observed Lyman excess.

show abstract

“…There are three primary surveys that have mapped far-infrared through millimeter wavelength emission in the Milky Way. The BGPS 10 Aguirre et al 2011;Ginsburg et al 2013) at λ=1.1 mm surveyed in the range−10°<ℓ<90°and targeted regions in the second and third quadrants with <  b 0.5 | | (expands to < b 1.5 | | at selected ℓ) at 33″ resolution. ATLASGAL (Schuller et al 2009;Contreras et al 2013;Csengeri et al 2014) surveyed at λ=870 μm in the range−60°<ℓ<60°and <  b 1 .…”

Section: Introductionmentioning

confidence: 99%

“…The second data release (v2.0) of the Bolocam images and source catalog (Ginsburg et al 2013) used improved analysis of the time-stream data to improve angular flux recovery with full recovery out to ∼80″ and partial recovery out to ∼300″. The v2.0 data also resolvesystematic flux and pointing calibration offsets and includenew fields in the second quadrant.…”

Section: Introductionmentioning

confidence: 99%

The Bolocam Galactic Plane Survey. Xiv. Physical Properties of Massive Starless and Star-Forming Clumps

Svoboda

Shirley

Battersby

et al. 2016

ApJ

Self Cite

106

200

View full text Add to dashboard Cite

We sort 4683 molecular clouds between 10°<ℓ<65°from the Bolocam Galactic Plane Survey based on observational diagnostics of star formation activity: compact 70 μm sources, mid-IR color-selected YSOs, H 2 O and CH 3 OH masers, and UCH IIregions. We also present a combined NH 3 -derived gas kinetic temperature and H 2 O maser catalog for 1788 clumps from our own GBT 100 m observations and from the literature. We identify a subsample of 2223 (47.5%) starless clump candidates (SCCs), the largest and most robust sample identified from a blind survey to date. Distributions of flux density, flux concentration, solid angle, kinetic temperature, column density, radius, and mass show strong (>1 dex) progressions when sorted by star formation indicator. The median SCC is marginally subvirial (α∼0.7) with >75% of clumps with known distance being gravitationally bound (α<2). These samples show a statistically significant increase in the median clump mass of ΔM∼170-370 M e from the starless candidates to clumps associated with protostars. This trend could be due to (i) mass growth of the clumps atM 200 440 -M e Myr −1 for an average freefall 0.8 Myr timescale, (ii) a systematic factor of two increase in dust opacity from starless to protostellar phases, and/or (iii)a variation in the ratio of starless to protostellar clump lifetime that scales as ∼M −0.4 . By comparing to the observed number of CH 3 OH maser containing clumps, we estimate the phaselifetime of massive (M>10 3 M e ) starless clumps to be 0.37±0.08 Myr (M/103 M e ) −1; the majority (M<450 M e ) have phaselifetimes longer than their average freefall time.

show abstract

The Bolocam Galactic Plane Survey. Ix. Data Release 2 and Outer Galaxy Extension

Cited by 152 publications

References 41 publications

Star Formation Relations in the Milky Way

Star Formation Relations in the Milky Way

Infrared emission of young HII regions: aHerschel/Hi-GAL study

The Bolocam Galactic Plane Survey. Xiv. Physical Properties of Massive Starless and Star-Forming Clumps

Contact Info

Product

Resources

About