Comparing Star Formation on Large Scales in the c2d Legacy Clouds: Bolocam 1.1 mm Dust Continuum Surveys of Serpens, Perseus, and Ophiuchus

By M. Enoch, J. Glenn, N. Evans II, A. Sargent, K. Young, T. Huard. 2007

151 citations recorded by the source corpus.

We have undertaken an unprecedentedly large 1.1 mm continuum survey of three nearby star-forming clouds using Bolocam at the Caltech Submillimeter Observatory. We mapped the largest areas in each cloud at millimeter or submillimeter wavelengths to date: 7.5 deg2 in Perseus (Enoch and coworkers), 10.8 deg2 in Ophiuchus (Young and coworkers), and 1.5 deg2 in Serpens with a resolution of 31'', detecting 122, 44, and 35 cores, respectively. Here we report on results of the Serpens survey and compare the three clouds. Average measured angular core sizes and their dependence on resolution suggest that many of the observed sources are consistent with power-law density profiles. Tests of the effects of cloud distance reveal that linear resolution strongly affects measured source sizes and densities, but not the shape of the mass distribution. Core mass distribution slopes in Perseus and Ophiuchus (α = 2.1 ± 0.1 and 2.1 ± 0.3) are consistent with recent measurements of the stellar IMF, whereas the Serpens distribution is flatter (α = 1.6 ± 0.2). We also compare the relative mass distribution shapes to predictions from turbulent fragmentation simulations. Dense cores constitute less than 10% of the total cloud mass in all three clouds, consistent with other measurements of low star formation efficiencies. Furthermore, most cores are found at high column densities; more than 75% of 1.1 mm cores are associated with AV ≳ 8 mag in Perseus, 15 mag in Serpens, and 20-23 mag in Ophiuchus.

Subfields: Astronomy and Astrophysics, Fluid Flow and Transfer Processes

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Citations in the corpus

TADPOL: A 1.3 mm SURVEY OF DUST POLARIZATION IN STAR-FORMING CORES AND REGIONS (2013, methodology): “To show the B-field morphologies as clearly as possible, we have chosen to plot the lengths of the line segments on a square-root scale. at the CSO, the segment lengths are proportional to the square root of the polarized intensity.”
YOUNG STELLAR OBJECTS IN THE GOULD BELT (2015, background): “Other submillimeter and millimeter photometry from the literature, where available from large surveys of nearby molecular clouds (Young et al. 2005, 2006; Enoch et al. 2006, 2007; Belloche et al. 2011b,a; Maury et al. 2011).”
ANALYTICAL STAR FORMATION RATE FROM GRAVOTURBULENT FRAGMENTATION (2011, background): “A similar density-threshold for significant dense core population has been identified in several surveys (Onishi et al. 1998, Johnstone et al. 2000, Kirk et al. 2006, Enoch et al. 2007, Lada et al. 2010, André et al. 2010).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Other studies have found similar thresholds for efficient star formation or the presence of dense cores (Onishi et al. 1998; Enoch et al. 2007; Johnstone et al. 2004; André et al. 2010; Li et al. 1997; Lada 1992).”
Planck 2015 results - XXVIII. The Planck Catalogue of Galactic cold clumps (2015, unknown): “We have obtained an average θ i /θ PSF ratio of 1.4, which is consistent with other similar observations, e.g., by BLAST (1.1, Netterﬁeld et al. 2009) and Bolocam (1.5, Enoch et al. 2007).”
PROSAC: a submillimeter array survey of low-mass protostars - II. The mass evolution of envelopes, disks, and stars from the class 0 through I stages (2009, background): “One of the main goals of those surveys are naturally to determine core masses and this is often done using single isothermal cores with two temperatures: one for cores with and one without embedded protostellar sources (e.g., Enoch et al.,2007; Hatchell & Fuller, 2008).”
Clustered and Triggered Star Formation in W5: Observations with Spitzer (2008, background): “In recent surveys of low mass star forming regions (Enoch et al. 2007) and the high mass star forming regions in Cygnus (Motte et al. 2007), typical star-forming dense cores are ∼0.1 pc in size.”
Cores, filaments, and bundles: hierarchical core formation in the L1495/B213 Taurus region (2013, background): “At any given time, only a small fraction of the material in a cloud is in the form of dense cores (< 10 %, i.e., Enoch et al. 2007), and this apparent difficulty making dense cores is likely connected to the low efficiency of the star-formation process (Evans 2008).”
The Mass Distribution and Lifetime of Prestellar Cores in Perseus, Serpens, and Ophiuchus (2008, methodology): “Utilizing large-scale 1.1 mm surveys (Enoch et al. 2006; Young et al. 2006; Enoch et al. 2007) together with Spitzer IRAC and MIPS maps from the c2d Legacy program (Evans et al. 2003), we have carried out an unbiased census of prestellar and protostellar cores in the Perseus, Serpens, and Ophiuchus…”
STAR FORMATION RELATIONS IN NEARBY MOLECULAR CLOUDS (2014, result): “This relation was consistent with many studies of star formation in the Galaxy showing that star formation was highly correlated with relatively dense gas within the molecular cloud (Onishi et al. 1998; Enoch et al. 2007; Johnstone et al. 2004; André et al. 2010; Li et al. 1997; Lada 1992).”
FILAMENTARY STRUCTURE OF STAR-FORMING COMPLEXES (2009, background): “Figure 5 shows 1.1 mm emission from Serpens Cluster A (Enoch et al 2007).”
THE SPITZER c2d LEGACY RESULTS: STAR-FORMATION RATES AND EFFICIENCIES; EVOLUTION AND LIFETIMES (2008, methodology): “The data are taken from Alcalá et al. (2008), Brede et al. (2008), Davis et al. (1999), Djupvik et al. (2006), Enoch et al. (2006), Enoch et al. (2007), Hatchell et al. (2005), Hatchell et al. (2007), Henning et al. (1993), Johnstone et al. (2000), Kirk et al. (2006), Meŕın et al. (2008a), Stanke…”
MAMBO Mapping Of Spitzer c2d Small Clouds And Cores (2008, background): “…studied dense cores in large (up to several 10 pc) and massive (up to several 103 M ) complexes of molecular clouds (Motte et al. 1998; Johnstone et al. 2000, 2001, 2004, 2006; Johnstone & Bally 2006; Hatchell et al. 2005; Enoch et al. 2006, 2007; Young K. E. et al. 2006; Stanke et al. 2006).”
THE BOLOCAM GALACTIC PLANE SURVEY: SURVEY DESCRIPTION AND DATA REDUCTION (2010, methodology): “Studies of nearby clouds have demonstrated that star formation is far from uniform over molecular clouds, but is concentrated in unusually dense regions called clumps or cores, which fill a small fraction of the area of most clouds (Lada et al. 1991; Enoch et al. 2007; Evans et al. 2009).”
FILAMENTARY ACCRETION FLOWS IN THE EMBEDDED SERPENS SOUTH PROTOCLUSTER (2013, background): “…centroid velocities, fewer of the spectra have a signal to noise level 11 We assume a temperature of 15 K and a dust opacity of 0.0114 cm2g−1 (e.g. Enoch et al 2007); recent ammonia measurements suggest a dense gas temperature around 10-15 K in Serpens South, with the southern filament at ∼11-12…”
The ATLASGAL survey: a catalog of dust condensations in the Galactic plane (2013, background): “…(e.g. Motte et al. 2007; Russeil et al. 2010; Motte et al. 2010; Tackenberg et al. 2012) and is one order of magnitude lower than that of low-mass cores (e.g. Enoch et al. 2007; Hatchell & Fuller 2008), suggestingthat massive cores, (precursors of high-mass stars) form in a fast, dynamic process.”
THE STAR FORMATION RATE AND GAS SURFACE DENSITY RELATION IN THE MILKY WAY: IMPLICATIONS FOR EXTRAGALACTIC STUDIES (2010, background): “Enoch et al. (2007) also found extinction thresholds for dense cores found in Bolocam 1.1mm maps in the Perseus, Serpens, and Ophiuchus clouds of AV ∼8, 15, and 23, respectively (∼120, 225, and 350 M⊙ pc 2), with a low probability of finding cores below these thresholds.”
PROPERTIES OF THE YOUNGEST PROTOSTARS IN PERSEUS, SERPENS, AND OPHIUCHUS (2008, methodology): “CONCLUSIONS Utilizing large-scale 1.1 mm surveys (Enoch et al. 2006; Young et al. 2006; Enoch et al. 2007) together with Spitzer IRAC and MIPS maps from the c2d Legacy program (Evans et al. 2003), we have constructed an unbiased census of deeply embedded protostars in the Perseus, Serpens, and…”
Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores (2007, methodology): “The surveys used for Perseus are a 1.1 mm dust continuum survey of 7.5 deg2 with Bolocam at the CSO (Enoch et al. 2006), an 850 µm dust continuum survey of 3.5 deg2 with SCUBA at the JCMT (Kirk et al. 2006), a 450 and 850 µm dust continuum survey of 3.0 deg2 with SCUBA at the JCMT (Hatchell et al. 2”