Bolocam Survey for 1.1 mm Dust Continuum Emission in the c2d Legacy Clouds. I. Perseus

Enoch, Melissa L.; Young, Kaisa E.; Glenn, J.; Evans, Neal J.; Golwala, S. R.; Sargent, Anneila I.; Harvey, P. M.; Aguirre, James E.; Goldin, Alexey; Haig, D.; Huard, Tracy L.; Lange, A. E.; Laurent, G. T.; Maloney, Philip R.; Mauskopf, Philip Daniel; Rossinot, P.; Sayers, Jack

doi:10.1086/498678

Cited by 311 publications

(485 citation statements)

References 68 publications

(96 reference statements)

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“…where S ν is the flux density measurement in the BGPS catalog, B ν is the Planck function and the opacity κ ν is assumed as 0.0114 cm 2 g −1 (Enoch et al 2006). The estimated mass of the BGPS source is about 69 ± 15 M , which is in line with the estimated mass of the envelope (M env ≈ 22 M , see Sect.…”

Section: Physical Parameterssupporting

confidence: 58%

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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Section: Physical Parameterssupporting

confidence: 58%

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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“…Motte et al 1998;Testi & Sargent 1998;Johnstone et al 2000). In these submm surveys, prestellar cores are found only above a visual extinction of 5-7 mag, suggesting the existence of an extinction threshold for star formation to occur (see, e.g., Johnstone et al 2004;Enoch et al 2006;Kirk et al 2006; but also Onishi et al 1998, based on molecular line observations).…”

Section: Introductionmentioning

confidence: 73%

The end of star formation in Chamaeleon I?

Беллоче

Schüller

Parise

et al. 2011

A&A

144

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Context. Chamaeleon I is the most active region in terms of star formation in the Chamaeleon molecular cloud complex. Although it is one of the nearest low-mass star forming regions, its population of prestellar and protostellar cores is not known and a controversy exists concerning its history of star formation. Aims. Our goal is to search for prestellar and protostellar cores and characterize the earliest stages of star formation in this cloud. Methods. We used the bolometer array LABOCA at the APEX telescope to map the cloud in dust continuum emission at 870 μm with a high sensitivity. This deep, unbiased survey was performed based on an extinction map derived from 2MASS data. The 870 μm map is compared with the extinction map and C 18 O observations, and decomposed with a multiresolution algorithm. The extracted sources are analysed by carefully taking into account the spatial filtering inherent in the data reduction process. A search for associations with young stellar objects is performed using Spitzer data and the SIMBAD database. Results. Most of the detected 870 μm emission is distributed in five filaments. We identify 59 starless cores, one candidate first hydrostatic core, and 21 sources associated with more evolved young stellar objects. The estimated 90% completeness limit of our survey is 0.22 M for the starless cores. The latter are only found above a visual extinction threshold of 5 mag. They are less dense than those detected in other nearby molecular clouds by a factor of a few on average, maybe because of the better sensitivity of our survey. The core mass distribution is consistent with the IMF at the high-mass end but is overpopulated at the low-mass end. In addition, at most 17% of the cores have a mass larger than the critical Bonnor-Ebert mass. Both results suggest that a large fraction of the starless cores may not be prestellar in nature. Based on the census of prestellar cores, Class 0 protostars, and more evolved young stellar objects, we conclude that the star formation rate has decreased with time in this cloud. Conclusions. The low fraction of candidate prestellar cores among the population of starless cores, the small number of Class 0 protostars, the high global star formation efficiency, the decrease of the star formation rate with time, and the low mass per unit length of the detected filaments all suggest that we may be witnessing the end of the star formation process in Chamaeleon I.

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“…Using the Submillimetre Common User Bolometer Array (SCUBA) instrument, Johnstone et al (2004) mapped 4 deg 2 of the Ophiuchus star-forming cloud, and Hatchell et al (2005) covered 3 deg 2 of the Perseus molecular cloud. Complementary to the Spitzer "Cores to Disks" legacy project (Evans et al 2003), Enoch et al (2006) mapped 7.5 deg 2 covering the Perseus cloud, and Young et al (2006) mapped nearly 11 deg 2 covering Ophiuchus, both using the BOLOCAM instrument at 1.1 mm.…”

Section: Article Published By Edp Sciencesmentioning

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

712

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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Bolocam Survey for 1.1 mm Dust Continuum Emission in the c2d Legacy Clouds. I. Perseus

Cited by 311 publications

References 68 publications

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

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

The end of star formation in Chamaeleon I?

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

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