A Large-scale Survey of CO and Its Isotopologues toward the Rosette Molecular Cloud

Li, Chong; Wang, Hongchi; Zhang, Miaomiao; Ma, Yuehui; Fang, Min; Yang, Ji

doi:10.3847/1538-4365/aad963

Cited by 26 publications

(30 citation statements)

References 66 publications

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“…Observations of the MWISP 1 survey contain three CO isotopologue lines, 12 CO (J = 1 → 0), 13 CO (J = 1 → 0), and C 18 O (J = 1 → 0). The MWISP project is a new uniform and large-scale CO survey of the Galactic plane (−10 • ≤ l ≤ 250 • and |b| ≤ 5 • ), which has refined and newly detected many molecular clouds (Sun et al 2015Wang et al 2017;Du et al 2017;Li et al 2018). We refer the reader to Su et al (2019) for a more detailed description of the MWISP survey and here briefly review the observation and data reduction processes.…”

Section: The Mwisp Surveymentioning

confidence: 99%

Molecular Cloud Distances Based on the MWISP CO Survey and Gaia DR2

Yan

Yang

Sun

et al. 2019

ApJ

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We present a new method of calculating distances of molecular clouds in the Galactic plane, using CO observations and the Gaia DR2 parallax and G-band extinction (A G ) measurements. Due to the complexity of dust environments in the Galactic plane, A G contains irregular variations, which is difficult to model. To overcome this difficulty, we propose that the A G of off-cloud stars (Gaia stars around molecular clouds) can be used as a baseline to calibrate the A G of on-cloud stars (Gaia stars toward molecular clouds), which removes the A G components that are unrelated to molecular clouds. The distance is subsequently inferred from the jump point in on-cloud A G with Bayesian analysis and Markov chain Monte Carlo (MCMC) sampling. We applied this baseline subtraction method to a 100 deg 2 region (209.75 • ≤ l ≤ 219.75 • and |b| ≤ 5 • ) in the third Galactic quadrant, which was mapped as part of the Milky Way Imaging Scroll Painting (MWISP) project, covering three CO isotopologue lines, and derived distances and masses for 11 molecular clouds, including the Maddalena molecular cloud and Sh 2-287. The results indicate that the distance of the Perseus Arm in this region is about 2.4 kpc and molecular clouds are present in the interarm regions.

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Section: The Mwisp Surveymentioning

confidence: 99%

Molecular Cloud Distances Based on the MWISP CO Survey and Gaia DR2

Yan

Yang

Sun

et al. 2019

ApJ

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“…Firstly, we assume that the 12 CO and 13 CO molecules are under local thermodynamic equilibrium (LTE) conditions and the 12 CO emission is optically thick. Then the excitation temperature can be obtained from the peak intensity of the 12 CO line (Li et al 2018;Ma et al 2020),…”

Section: Physical Propertiesmentioning

confidence: 99%

“…where T peak ( 12 CO) is the peak brightness temperature of the 12 CO line. The optical depth and the column density of the 13 CO molecule are derived according to the following formula (Pineda et al 2010;Li et al 2018;Ma et al 2020),…”

Section: Physical Propertiesmentioning

confidence: 99%

Molecular Clouds Associated with {H \small{II}} regions and Candidates within l = 106.65$^\circ$ to 109.50$^\circ$ and b = ${-}$1.85$^\circ$ to 0.95$^\circ$

Li,

Wang,

et al. 2022

Preprint

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We present a large-scale simultaneous survey of the CO isotopologues ( 12 CO, 13 CO, and C 18 O) J = 1 − 0 line emission toward the Galactic plane region of l = 106.65 • to 109.50 • and b = −1.85 • to 0.95 • using the Purple Mountain Observatory 13.7 m millimeter-wavelength telescope. Except for the molecular gas in the solar neighborhood, the emission from the molecular gas in this region is concentrated in the velocity range of [−60, −35] km s −1 . The gas in the region can be divided into four clouds, with mass in the range of ∼10 3 to 10 4 M . We have identified 25 filaments based on the 13 CO data. The median excitation temperature, length, line mass, line width, and virial parameter of the filaments are 10.89 K, 8.49 pc, 146.11 M pc −1 , 1.01 km s −1 , and 3.14, respectively. Among these filaments, eight have virial parameters of less than 2, suggesting that they are gravitationally bound and can lead to star formation. Nineteen H II regions or candidates have previously been found in the region and we investigate the relationships between these H II regions/candidates and surrounding molecular clouds in detail. Using morphology similarity and radial velocity consistency between H II regions/candidates and molecular clouds as evidence for association, and raised temperature and velocity broadening as signatures of interaction, we propose that 12 H II regions/candidates are associated with their surrounding molecular clouds. In the case of the H II region of S142, the energy of the H II region is sufficient to maintain the turbulence in the surrounding molecular gas.

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“…Using the PMO-13.7m millimeter telescope at Delingha in China, Li et al (2018) have conducted a large-scale simultaneous survey of 12 CO, 13 CO, and C 18 O J=1-0 emission toward the Rosette molecular cloud (RMC) region with a sky coverage of 3.5 × 2.5 square degrees ( Figure 11). The spatial pixel of the FITS data cube has a size of 30 ′′ × 30 ′′ and the effective spectral resolution is 61.0 kHz, corresponding to a velocity resolution of 0.16 km s −1 at the 115 GHz frequency of the 12 CO J = 1 − 0 line.…”

Section: The Performance Of the Algorithms In Identifying Clumps In Tmentioning

confidence: 99%

“…Maps of 12 CO emission intensity integrated from -2 km s −1 to 30 km s −1 (a), 13 CO emission intensity integrated from 3 km s −1 to 26 km s −1 (b), and C 18 O emission intensity integrated from 3 km s −1 to 19 km s −1 (c). For details, seeLi et al (2018). Left: the output number for each algorithm in identifying clumps of 12 CO, 13 CO, and C 18 O emission.…”

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confidence: 99%

Assessing the performance of molecular gas clump identification algorithms

Wang

et al. 2020

Res. Astron. Astrophys.

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The detection of clumps(cores) in molecular clouds is an important issue in submillimetre astronomy. However, the completeness of the identification and the accuracy of the returned parameters of the automated clump identification algorithms are still not clear by now. In this work, we test the performance and bias of the GaussClumps, ClumpFind, Fellwalker, Reinhold, and Dendrograms algorithms in identifying simulated clumps. By designing the simulated clumps with various sizes, peak brightness, and crowdedness, we investigate the characteristics of the algorithms and their performance. In the aspect of detection completeness, Fellwalker, Dendrograms, and Gaussclumps are the first, second, and third best algorithms, respectively. The numbers of correct identifications of the six algorithms gradually increase as the size and SNR of the simulated clumps increase and they decrease as the crowdedness increases. In the aspect of the accuracy of retrieved parameters, Fellwalker and Dendrograms exhibit better performance than the other algorithms. The average deviations in clump parameters for all algorithms gradually increase as the size and SNR of clumps increase. Most of the algorithms except Fellwalker exhibit significant deviation in extracting the total flux of clumps. Taken altogether, Fellwalker, Gaussclumps, and Dendrograms exhibit the best performance in detection completeness and extracting parameters. The deviation in virial parameter for the six algorithms is relatively low. When applying the six algorithms to the clump identification for the Rosette molecular cloud, ClumpFind1994, ClumpFind2006, Gaussclumps, Fellwalker, and Reinhold exhibit performance that is consistent with the results from the simulated test.

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A Large-scale Survey of CO and Its Isotopologues toward the Rosette Molecular Cloud

Cited by 26 publications

References 66 publications

Molecular Cloud Distances Based on the MWISP CO Survey and Gaia DR2

Molecular Cloud Distances Based on the MWISP CO Survey and Gaia DR2

Molecular Clouds Associated with {H \small{II}} regions and Candidates within l = 106.65$^\circ$ to 109.50$^\circ$ and b = ${-}$1.85$^\circ$ to 0.95$^\circ$

Assessing the performance of molecular gas clump identification algorithms

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