THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. IV. THE NGC 1333 CLOUD IN PERSEUS IN CO
 J
 = 2-1 AND
 13
 CO
 J
 = 2-1

Bieging, John H.; Revelle, Melissa; Peters, William L.

doi:10.1088/0067-0049/214/1/7

Cited by 10 publications

(15 citation statements)

References 33 publications

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“…The diffuse gas shown in Figure 5 certainly displays some large-scale structure, but does not appear to exhibit a single consistent gradient. This is confirmed with higher-excitation CO lines; Bieging et al (2014) present CO (2-1) and 13 CO (2-1) maps of NGC 1333 and speculate that the patchy variations in centroid velocity seen in these tracers could be ascribed to a cloud-cloud collision.…”

Section: Enclosed Stellar Masssupporting

confidence: 68%

In-Sync. Ii. Virial Stars From Subvirial Cores—the Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333

Foster

Cottaar

Covey

et al. 2015

ApJ

112

127

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The initial velocity dispersion of newborn stars is a major unconstrained aspect of star formation theory. Using near-infrared spectra obtained with the APOGEE spectrograph, we show that the velocity dispersion of young (1-2 Myr) stars in NGC 1333 is 0.92±0.12 km s −1 after correcting for measurement uncertainties and the effect of binaries. This velocity dispersion is consistent with the virial velocity of the region and the diffuse gas velocity dispersion, but significantly larger than the velocity dispersion of the dense, star-forming cores, which have a sub-virial velocity dispersion of 0.5 km −1 . Since the NGC 1333 cluster is dynamically young and deeply embedded, this measurement provides a strong constraint on the initial velocity dispersion of newly-formed stars. We propose that the difference in velocity dispersion between stars and dense cores may be due to the influence of a 70µG magnetic field acting on the dense cores, or be the signature of a cluster with initial sub-structure undergoing global collapse.

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Section: Enclosed Stellar Masssupporting

confidence: 68%

In-Sync. Ii. Virial Stars From Subvirial Cores—the Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333

Foster

Cottaar

Covey

et al. 2015

ApJ

112

127

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“…Procedures for the J=2−1 line observations were identical to those described in Bieging et al (2014). The receiver was the dual-polarization ALMA Band 6 prototype sideband-separating mixer system (Lauria et al 2006).…”

Section: Co and 13 Coj=2−1 Linesmentioning

confidence: 99%

“…The field to be mapped was divided into contiguous 10′×10′ "tiles," each of which was observed in the standard On-The-Fly (OTF) scanning mode. The data were calibrated and processed as described in Bieging et al (2014). The line intensity calibrator was the compact molecular source W3(OH), with main-beam brightness temperatures and integrated line intensities as given in Bieging & Peters (2011).…”

Section: Co and 13 Coj=2−1 Linesmentioning

confidence: 99%

“…Previous papers reported on the giant molecular clouds (GMCs) associated with H II regions W51 (Bieging et al 2010) and W3 (Bieging & Peters 2011); and on the lower-mass clouds in Serpens (Burleigh et al 2013) and the NGC1333 region in Perseus (Bieging et al 2014). In addition, summary results have been given for molecular clouds associated with the H II regions Sh2-254-258 ) and M17 (Povich et al 2009), and for a selection of Bok Globules (Stutz et al 2009;Lippok et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

Bieging

Patel

Peters

et al. 2016

ApJS

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We present the results of a program to map the Sh2-235 molecular cloud complex in the CO and 13 COJ=2−1 transitions using the Heinrich Hertz Submillimeter Telescope. The map resolution is 38″ (FWHM), with an rms noise of 0.12 K brightness temperature, for a velocity resolution of 0.34 km s −1. With the same telescope, we also mapped the CO J=3−2 line at a frequency of 345 GHz, using a 64 beam focal plane array of heterodyne mixers, achieving a typical rms noise of 0.5 K brightness temperature with a velocity resolution of 0.23 km s −1. The three spectral line data cubes are available for download. Much of the cloud appears to be slightly sub-thermally excited in the J=3 level, except for in the vicinity of the warmest and highest column density areas, which are currently forming stars. Using the CO and 13 COJ=2−1 lines, we employ an LTE model to derive the gas column density over the entire mapped region. Examining a 125 pc 2 region centered on the most active star formation in the vicinity of Sh2-235, we find that the young stellar object surface density scales as approximately the 1.6-power of the gas column density. The area distribution function of the gas is a steeply declining exponential function of gas column density.Comparison of the morphology of ionized and molecular gas suggests that the cloud is being substantially disrupted by expansion of the H II regions, which may be triggering current star formation.

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“…The J=2-1 rotational transitions of the two most abundant isotopologues, 12 C 16 O (hereafter CO) and 13 C 16 O (hereafter CO 13 ), were observed with the sideband-separating mixer receiver (ALMA band 6) described by Lauria et al (2006). The observing procedures were identical to those described in Bieging et al (2014). The cloud to be mapped was divided into 10′×10′"tiles," which were observed with the on-the-fly (OTF) method, and the resulting images were combined to make data cubes of brightness temperature on the sky in a series of spectral channels for each CO isotopologue.…”

Section: Introductionmentioning

confidence: 99%

The Arizona Radio Observatory CO Mapping Survey of Galactic Molecular Clouds. VI. The Cep OB3 Cloud (Cepheus B and C) in CO J = 2–1, ¹³CO J = 2–1, and CO J = 3–2

Bieging

Patel

Hofmann

et al. 2018

ApJS

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We present (1) new fully sampled maps of CO and CO 13 J=2-1 emission and CO J=3-2 emission toward the molecular clouds Cep B and C, associated with the Cep OB3 association; (2) a map of extinction, A V , derived from IR colors of background stars; and (3) the distribution of young stellar objects (YSOs) over the same field as the molecular maps. An LTE analysis of the CO and CO 13 maps yields the distribution of molecular column densities and temperatures. Substantial variations are evident across the clouds; smaller subregions show correlations between molecular properties and dust extinction, consistent with a picture of outer photodissociation regions with a layer of CO-dark molecular gas, a CO self-shielded interior, and an inner cold dense region where CO is largely depleted onto grains. Comparing the distribution of YSOs with molecular gas surface density shows a power-law relation very similar in slope to that for the giant molecular cloud associated with the H II region Sh2-235 from a previous paper in this series that employed the same methodology. We note the presence of several compact, isolated CO emission sources in the J=3-2 maps. The gas temperature and CO 13 velocity dispersion yield a map of the sonic Mach number, which varies across the cloud but always exceeds unity, confirming the pervasiveness of supersonic turbulence over length scales 0.1 pc (the map resolution). We also compute a J=2-1 CO X-factor that varies with position but is, on average, within20% of the Galactic average derived from CO J=1-0 observations.

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THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. IV. THE NGC 1333 CLOUD IN PERSEUS IN CO J = 2-1 AND ¹³ CO J = 2-1

Cited by 10 publications

References 33 publications

In-Sync. Ii. Virial Stars From Subvirial Cores—the Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333

In-Sync. Ii. Virial Stars From Subvirial Cores—the Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

The Arizona Radio Observatory CO Mapping Survey of Galactic Molecular Clouds. VI. The Cep OB3 Cloud (Cepheus B and C) in CO J = 2–1, ¹³CO J = 2–1, and CO J = 3–2

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THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. IV. THE NGC 1333 CLOUD IN PERSEUS IN CO J = 2-1 AND 13 CO J = 2-1

Cited by 10 publications

References 33 publications

In-Sync. Ii. Virial Stars From Subvirial Cores—the Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333

In-Sync. Ii. Virial Stars From Subvirial Cores—the Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, 13CO J = 2 − 1, AND CO J = 3 − 2

The Arizona Radio Observatory CO Mapping Survey of Galactic Molecular Clouds. VI. The Cep OB3 Cloud (Cepheus B and C) in CO J = 2–1, 13CO J = 2–1, and CO J = 3–2

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Resources

About

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. IV. THE NGC 1333 CLOUD IN PERSEUS IN CO J = 2-1 AND ¹³ CO J = 2-1

THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, ¹³CO J = 2 − 1, AND CO J = 3 − 2

The Arizona Radio Observatory CO Mapping Survey of Galactic Molecular Clouds. VI. The Cep OB3 Cloud (Cepheus B and C) in CO J = 2–1, ¹³CO J = 2–1, and CO J = 3–2