THE BOLOCAM GALACTIC PLANE SURVEY: λ = 1.1 AND 0.35 mm DUST CONTINUUM EMISSION IN THE GALACTIC CENTER REGION

Bally, John; Aguirre, James E.; Battersby, Cara; Bradley, E. T.; Cyganowski, C. J.; Dowell, Darren; Drosback, Meredith M.; Dunham, Miranda K.; Evans, Neal J.; Ginsburg, Adam; Glenn, J.; Harvey, P. M.; Mills, Elisabeth A. C.; Merello, Manuel; Rosolowsky, Erik; Schlingman, W. M.; Shirley, Yancy L.; Stringfellow, Guy S.; Walawender, Josh; Williams, Jonathan P.

doi:10.1088/0004-637x/721/1/137

Cited by 108 publications

(103 citation statements)

References 105 publications

(187 reference statements)

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“…Compared to the objects found in recent surveys of dense cluster-forming molecular clumps, one object, G0.253 + 0.016, stands out as extreme (e.g., Sridharan et al 2002;Hill et al 2005;Beuther et al 2002;Schuller et al 2009;Bally et al 2010;Aguirre et al 2011;Molinari et al 2010a;Rathborne et al 2006;Simon et al 2006aSimon et al , 2006bPillai et al 2006;Peretto & Fuller 2009;Jackson et al 2006;Rathborne et al 2009;Longmore et al 2007;Purcell et al 2006Purcell et al , 2009Walsh et al 2008Walsh et al , 2011Jackson et al 2011). Identified as an infrared dark cloud (IRDC), it is clearly seen as a prominent extinction feature in mid-IR images (see Figure 1).…”

Section: Introductionmentioning

confidence: 82%

G0.253 + 0.016: A Molecular Cloud Progenitor of an Arches-Like Cluster

Longmore¹,

Rathborne²,

Bastian³

et al. 2012

ApJ

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162

258

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Young massive clusters (YMCs) with stellar masses of 10 4 -10 5 M and core stellar densities of 10 4 -10 5 stars per cubic pc are thought to be the "missing link" between open clusters and extreme extragalactic super star clusters and globular clusters. As such, studying the initial conditions of YMCs offers an opportunity to test cluster formation models across the full cluster mass range. G0.253 + 0.016 is an excellent candidate YMC progenitor. We make use of existing multi-wavelength data including recently available far-IR continuum (Herschel/Herschel Infrared Galactic Plane Survey) and mm spectral line (H 2 O Southern Galactic Plane Survey and Millimetre Astronomy Legacy Team 90 GHz Survey) data and present new, deep, multiple-filter, near-IR (Very Large Telescope/NACO) observations to study G0.253 + 0.016. These data show that G0.253 + 0.016 is a high-mass (1.3 × 10 5 M ), low-temperature (T dust ∼ 20 K), high-volume, and column density (n ∼ 8 × 10 4 cm −3 ; N H 2 ∼ 4 × 10 23 cm −2 ) molecular clump which is close to virial equilibrium (M dust ∼ M virial ) so is likely to be gravitationally bound. It is almost devoid of star formation and, thus, has exactly the properties expected for the initial conditions of a clump that may form an Arches-like massive cluster. We compare the properties of G0.253 + 0.016 to typical Galactic cluster-forming molecular clumps and find it is extreme, and possibly unique in the Galaxy. This uniqueness makes detailed studies of G0.253 + 0.016 extremely important for testing massive cluster formation models.

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Section: Introductionmentioning

confidence: 82%

G0.253 + 0.016: A Molecular Cloud Progenitor of an Arches-Like Cluster

Longmore¹,

Rathborne²,

Bastian³

et al. 2012

ApJ

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162

258

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“…No archival SCUBA data were available for the rest of our sources. Thus, for the sources G015.05 MM1, G015.31 MM3, and I18223 MM3 we extracted Bolocam 1.1-mm maps from images produced by the Bolocam Galactic Plane Survey (BGPS; see, e.g., Bally et al 2010, and references therein) 6 . For I18151 MM2, no archival (sub)mm data were found and thus we used the MAMBO 1.2-mm map of this source published in the paper by Beuther et al (2002a;kindly provided by H. Beuther).…”

Section: Archival Dust Continuum Datamentioning

confidence: 99%

Deuterium fractionation and the degree of ionisation in massive clumps within infrared dark clouds

Miettinen

Hennemann

Linz

2011

A&A

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Context. Massive clumps associated with infrared dark clouds (IRDCs) are promising targets for studying the earliest stages of highmass star and cluster formation. Aims. We aim to determine the degrees of CO depletion, deuterium fractionation, and ionisation in a sample of seven massive clumps associated with IRDCs. Methods. The APEX telescope was used to observe the C 17 O(2−1), H 13 CO + (3−2), DCO + (3−2), N 2 H + (3−2), and N 2 D + (3−2) transitions towards the clumps. The spectral line data were used in conjunction with the previously published and/or archival (sub)millimetre dust continuum observations of the sources. The data were used to derive the molecular column densities and fractional abundances for the analysis of deuterium fractionation and ionisation. Results. The CO molecules do not appear to be significantly depleted in the observed clumps. The DCO + /HCO + and N 2 D + /N 2 H + column density ratios are about 0.0002-0.014 and 0.002-0.028, respectively. The former ratio is found to decrease as a function of gas kinetic temperature. A simple chemical analysis suggests that the lower limit to the ionisation degree is in the range x(e) ∼ 10 −8 −10 −7 , whereas the estimated upper limits range from a few 10 −6 up to ∼10 −4 . Lower limits to x(e) imply that the cosmic-ray ionisation rate of H 2 lies between ζ H 2 ∼ 10 −17 −10 −15 s −1 . These are the first estimates of x(e) and ζ H 2 towards massive IRDCs reported so far. Some additional molecular transitions, mostly around 216 and 231 GHz, were detected towards all sources. In particular, IRDC 18102-1800 MM1 and IRDC 18151-1208 MM2 show relatively line-rich spectra. Some of these transitions might be assigned to complex organic molecules, although the line blending hampers the identification. The C 18 O(2−1) transition is frequently seen in the image band. Conclusions. The finding that CO is not depleted in the observed sources conforms to the fact that they show evidence of star formation activity, which is believed to release CO from the icy grain mantles back into the gas phase. The observed degree of deuteration is lower than in low-mass starless cores and protostellar envelopes. Decreasing deuteration with increasing temperature is likely to reflect the clump evolution. On the other hand, the association with young high-mass stars could enhance ζ H 2 and x(e) above the levels usually found in low-mass star-forming regions. On the scale probed by our observations, ambipolar diffusion cannot be a main driver of clump evolution unless it occurs on timescales 10 6 yr.

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“…The Bolocam Galactic Plane Survey (BGPS, Bally et al 2010;Rosolowsky et al 2010) is a 1.1 mm continuum survey of the Galactic Plane performed with the Bolocam on the Caltech Submillimeter Observatory, which is operated by Caltech under a contract from the NSF. A cutout image from archived Bolocam 1.1 mm data was employed in this investigation.…”

Section: Date Acquisition and Analysismentioning

confidence: 99%

The discovery based on GLIMPSE data of a protostar driving a bipolar outflow

Yuan¹,

Li²,

Huang³

et al. 2012

A&A

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We report the discovery based on GLIMPSE data of a proto-stellar system driving a bipolar outflow. The bipolar outflow closely resembles the shape of an hourglass in the infrared. The total luminosity of L total = 5507 L , derived from IRAS fluxes, indicates the ongoing formation of a massive star in this region. The spectral energy distribution (SED) of the driving source is fitted with an online SED fitting tool, which results in a spectral index of about 1.2. This, along with the presence of a bipolar outflow, suggests the detection of a Class I protostar. The driving source indicates prominent infrared excesses in color-color diagrams based on archived 2 MASS and GLIMPSE data, which is in line with an early evolutionary stage of the system.

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THE BOLOCAM GALACTIC PLANE SURVEY: λ = 1.1 AND 0.35 mm DUST CONTINUUM EMISSION IN THE GALACTIC CENTER REGION

Abstract: The Bolocam Galactic Plane Survey (BGPS) data for a six square degree region of the Galactic plane containing the Galactic center is analyzed and compared to infrared and radio continuum data. The BGPS 1.

Cited by 108 publications

References 105 publications

G0.253 + 0.016: A Molecular Cloud Progenitor of an Arches-Like Cluster

G0.253 + 0.016: A Molecular Cloud Progenitor of an Arches-Like Cluster

Deuterium fractionation and the degree of ionisation in massive clumps within infrared dark clouds

The discovery based on GLIMPSE data of a protostar driving a bipolar outflow

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