Compact Molecular Outflow From NGC 2264 Cmm3: A Candidate for Very Young High-Mass Protostar

Saruwatari, Osamu; Sakai, Nami; Liu, Sheng-Yuan; Su, Yu‐Nung; Sakai, Takeshi; Yamamoto, Satoshi

doi:10.1088/0004-637x/729/2/147

Cited by 13 publications

(45 citation statements)

References 29 publications

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“…The blue-shifted and redshifted outflows can also be seen in the channel maps of HCN ( Figure 6). This bipolar outflow system corresponds to that found by Saruwatari et al (2011) in the CO(J = 2 − 1) line with SMA. Their B1 and R1 lobes are seen in Figure 5, while B2 and R2 lobes are out of the field of view in the present ALMA observation.…”

Section: Outflowssupporting

confidence: 85%

“…The contours levels are the same as those in Figure 1a. B1 and R1 indicate the positions of CO lobes identified by Saruwatari et al (2011). 8, 13, ..., 33) for CO, CS, SO, and CH 3 OH, respectively.…”

Section: Discussionmentioning

confidence: 99%

“…Moreover, a part of the second outflow is strongly affected by the resolving-out effect at the system velocity (8.2 km s −1 and 6.6 km s −1 in Figure 6). The southwestern lobe of this outflow can be seen in the CH 3 OH (5 0 − 4 0 A + ) line in Figure 4a of Saruwatari et al (2011). This collimated outflow system seems to be launched from CMM3B, since the outflow axis just passes through the peak of CMM3B (Figure 5b).…”

Section: Outflowsmentioning

confidence: 91%

“…In the previous studies, CMM3 has been recognized as a single source because of insufficient angular resolutions (e.g. Peretto et al 2007;Sakai et al 2007;Saruwatari et al 2011;Cunningham et al 2016). It should be noted that the potential binary components, CMM3A and CMM3B, are surrounded by an extended envelope.…”

Section: Detection Of a Potential Binary System In The Cmm3mentioning

confidence: 99%

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Discovery of Striking Difference of Molecular-emission-line Richness in the Potential Proto-binary System NGC 2264 CMM3

Watanabe

Sakai

López-Sepulcre

et al. 2017

ApJ

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We have conducted an interferometric line survey in the 0.8 mm band toward the young high-mass protostar candidate NGC 2264 CMM3 with ALMA. CMM3 is resolved into the two continuum peaks, CMM3A and CMM3B, at an angular separation of 0.9 ′′ . Thus, CMM3 is found to be a binary system candidate. We have detected molecular outflows associated with CMM3A and CMM3B each, indicating active star formation. In addition to the two peaks, six faint continuum peaks are detected around CMM3A and CMM3B, most of which are thought to be evolved low-mass protostars. CMM3A is found to be rich in molecular line emission including complex organic molecules such as HCOOCH

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Section: Outflowssupporting

confidence: 85%

Section: Discussionmentioning

confidence: 99%

Section: Outflowsmentioning

confidence: 91%

Section: Detection Of a Potential Binary System In The Cmm3mentioning

confidence: 99%

See 2 more Smart Citations

Discovery of Striking Difference of Molecular-emission-line Richness in the Potential Proto-binary System NGC 2264 CMM3

Watanabe

Sakai

López-Sepulcre

et al. 2017

ApJ

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“…We pointed at the NGC2264 C-MM3 source, where the peak CH 3 OH intensity is located (Sakai et al 2007;Saruwatari et al 2011), and a rich chemistry was observed by combining extensive Nobeyama 45m dish (4 and 3 mm) and ASTE 10m dish (0.89 mm; Watanabe et al 2015). CH 3 OH, 13 CH 3 OH, CH 3 CCH, HC 5 N, CH 3 CN, CH 3 CHO, H 2 CCO, CH 3 OCH 3 , HCOOCH 3 , and NH 2 CHO lines were detected in this survey.…”

Section: Ngc2264mentioning

confidence: 99%

Deep, Broadband Spectral Line Surveys of Molecule-rich Interstellar Clouds

Weaver

Laas

Zou

et al. 2017

ApJS

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Spectral line surveys are an indispensable tool for exploring the physical and chemical evolution of astrophysical environments due to the vast amount of data that can be obtained in a relatively short amount of time. We present deep, broadband spectral line surveys of 30 interstellar clouds using two broadband λ=1.3 mm receivers at the Caltech Submillimeter Observatory. This information can be used to probe the influence of physical environment on molecular complexity. We observed a wide variety of sources to examine the relative abundances of organic molecules as they relate to the physical properties of the source (i.e., temperature, density, dynamics, etc.). The spectra are highly sensitive, with noise levels 25 mK at a velocity resolution of ∼0.35kms −1 . In the initial analysis presented here, column densities and rotational temperatures have been determined for the molecular species that contribute significantly to the spectral line density in this wavelength regime. We present these results and discuss their implications for complex molecule formation in the interstellar medium.

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On the chemistry of the young massive protostellar core NGC 2264 CMM3

Awad

Shalabeia

2017

Astrophys Space Sci

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We present the first gas-grain astrochemical model of the NGC 2264 CMM3 protostellar core. The chemical evolution of the core is affected by changing its physical parameters such as the total density and the amount of gas-depletion onto grain surfaces as well as the cosmic ray ionisation rate, ζ. We estimated ζ CMM3 = 1.6 × 10 −17 s −1 . This value is 1.3 times higher than the standard CR ionisation rate, ζ ISM = 1.3 × 10 −17 s −1 . Species response differently to changes into the core physical conditions, but they are more sensitive to changes in the depletion percentage and CR ionisation rate than to variations in the core density. Gas-phase models highlighted the importance of surface reactions as factories of large molecules and showed that for sulphur bearing species depletion is important to reproduce observations.Comparing the results of the reference model with the most recent millimeter observations of the NGC 2264 CMM3 core showed that our model is capable of reproducing the observed abundances of most of the species during early stages (≤ 3×10 4 yrs) of their chemical evolution. Models with variations in the core density between 1 -20 × 10 6 cm −3 are also in good agreement with observations during the early time interval 1 × 10 4 < t (yr) < 5 × 10 4 . In addition, models with higher CR ionisation rates (5 -10) ×ζ ISM are often overestimating the fractional abundances of the species. However, models with ζ CMM3 = 5 ζ ISM may best fit observations at times ∼ 2 × 10 4 yrs. Our results suggest that CMM3 is (1 -5) × 10 4 yrs old. Therefore, the core is chemically young and it may host a Class 0 object as suggested by previous studies.

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Compact Molecular Outflow From NGC 2264 Cmm3: A Candidate for Very Young High-Mass Protostar

Cited by 13 publications

References 29 publications

Discovery of Striking Difference of Molecular-emission-line Richness in the Potential Proto-binary System NGC 2264 CMM3

Discovery of Striking Difference of Molecular-emission-line Richness in the Potential Proto-binary System NGC 2264 CMM3

Deep, Broadband Spectral Line Surveys of Molecule-rich Interstellar Clouds

On the chemistry of the young massive protostellar core NGC 2264 CMM3

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