Distances to Nearby Molecular Clouds Traced by Young Stars

Zhang, M.

doi:10.3847/1538-4365/acc1e8

Cited by 10 publications

(4 citation statements)

References 132 publications

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“…Therefore, we propose that these 13 CO structures constitute a large GMC complex at a distance of 680-770 pc. This result is in good agreement with previous studies toward the Mon OB1 region (Kamezaki et al 2014;Yan et al 2019;Chen et al 2020;Zucker et al 2020;Lim et al 2022;Flaccomio et al 2023;Zhang 2023).…”

Section: Distance Measurementssupporting

confidence: 93%

“…Circles indicate distances obtained by extinction measurements of clouds (Yan et al 2019;Chen et al 2020;Zucker et al 2020). Triangles indicate distances obtained using star parallax (Lim et al 2022;Flaccomio et al 2023;Zhang 2023). The diamond indicates the distance obtained from maser measurements (Kamezaki et al 2014).…”

Section: Physical Properties Based On Identified 13 Co Structuresmentioning

confidence: 99%

“…NGC 2264 is an active star-forming region based on the detection of many outflows, Herbig-Haro (HH) objects, and shock H 2 jets (Margulis et al 1988;Schreyer et al 1997;Wolf-Chase et al 2003;Reipurth et al 2004b;Peretto et al 2006;Buckle et al 2012), including the famous NGC 2264G (Lada & Fich 1996). The distribution of many young stellar object candidates is tightly associated with the surrounding dense gas in NGC 2264 (Rapson et al 2014;Zhang 2023). In addition, some studies also have been done to investigate the kinematic connection between stellar populations/activities and associated molecular gas (e.g., Tobin et al 2015;Montillaud et al 2019;Flaccomio et al 2023).…”

Section: Introductionmentioning

confidence: 99%

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Distribution and Properties of Molecular Gas toward the Monoceros OB1 Region

Zhuang,

Su,

Zhang

et al. 2024

ApJ

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We perform a comprehensive CO study toward the Monoceros OB1 (Mon OB1) region based on the Milky Way Imaging Scroll Painting survey at an angular resolution of about 50″. The high-sensitivity data, together with the high dynamic range, show that molecular gas in the 8° × 4° region displays complicated hierarchical structures and various morphology (e.g., filamentary, cavity-like, shell-like, and other irregular structures). Based on Gaussian decomposition and clustering for 13CO data, a total of 263 13CO structures are identified in the whole region, and 88% of raw data flux is recovered. The dense gas with relatively high column density from the integrated CO emission is mainly concentrated in the region where multiple 13CO structures are overlapped. Combining the results of 32 large 13CO structures with distances from Gaia DR3, we estimate an average distance of 729 − 45 + 45 pc for the giant molecular cloud (GMC) complex. The total mass of the GMC complex traced by 12CO, 13CO, and C18O is 1.1 × 105 M ⊙, 4.3 × 104 M ⊙, and 8.4 × 103 M ⊙, respectively. The dense gas fraction shows a clear difference between Mon OB1 GMC East (12.4%) and Mon OB1 GMC West (3.3%). Our results show that the dense gas environment is closely linked to the nearby star-forming regions. On the other hand, star-forming activities have a great influence on the physical properties of the surrounding molecular gas (larger velocity dispersion, higher temperatures, more complex velocity structures, etc.). We also discuss the distribution/kinematics of molecular gas associated with nearby star-forming activities.

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Section: Distance Measurementssupporting

confidence: 93%

Section: Physical Properties Based On Identified 13 Co Structuresmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Distribution and Properties of Molecular Gas toward the Monoceros OB1 Region

Zhuang,

Su,

Zhang

et al. 2024

ApJ

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“…Young stellar objects (YSOs) that only recently formed in starforming molecular clouds are still close to their birth sites; hence, they still, on average, share the distance and kinematic properties of their parent clouds (e.g., Fűrész et al 2008;Tobin et al 2009;Hacar et al 2016;Großschedl et al 2021). On this basis, cloud distances can be estimated by using the distances of YSOs located within the clouds as proxies (e.g., Großschedl et al 2018Großschedl et al , 2021Zhang 2023). The recent release of astrometric data from Gaia Data Release 3 (DR3; Gaia Collaboration et al 2023) allows one to obtain a large number of high-quality parallaxes and proper motions of nearby YSOs, which also makes it possible to explore further the 3D kinematics of molecular clouds that harbor these YSOs (e.g., Großschedl et al 2021;Flaccomio et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Molecular Bubble and Outflow in S Mon Revealed by Multiband Data Sets

Liu,

Xu,

et al. 2024

ApJ

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We identify a molecular bubble, and study the star formation and its feedback in the S Mon region, using multiple molecular lines, young stellar objects (YSOs), and infrared data. We revisit the distance to S Mon, ∼722 ± 9 pc, using Gaia Data Release 3 parallaxes of the associated Class II YSOs. The bubble may be mainly driven by a massive binary system (namely 15 Mon), the primary of which is an O7V-type star. An outflow is detected in the shell of the bubble, suggesting ongoing star formation activities in the vicinity of the bubble. The total wind energy of the massive binary star is 3 orders of magnitude higher than the sum of the observed turbulent energy in the molecular gas and the kinetic energy of the bubble, indicating that stellar winds help to maintain the turbulence in the S Mon region and drive the bubble. We conclude that the stellar winds of massive stars have an impact on their surrounding environment.

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New method for estimating molecular cloud distances based on Gaia, 2MASS, and the TRILEGAL galaxy model

Mei,

Chen,

Jiang

et al. 2024

A&A

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We propose a new method for estimating the distances of molecular clouds traced by CO line emission. Stars from 2MASS and Gaia EDR3 are selected as on-cloud stars when they are projected on a cloud. The background on-cloud stars have redder colors on average than the foreground stars. Instead of searching for stars projected away from the cloud, we employed the TRILEGA galaxy model to mimic the stellar population without cloud extinction along the sightline toward the cloud. Our method does not require an exact boundary of a cloud. The boundaries are highly variable and depend on the sensitivity of the molecular line data. For each cloud, we compared the distributions of on-cloud stars to the TRILEGAL stellar populations in the diagram of $J-K_s$ color versus distance. The intrinsic $J-K_s$ colors of main-sequence and evolved stars from TRILEGAL were considered separately, and they were used as the baseline for subtracting the observed $J-K_s$ colors. The baseline-corrected $J-K_s$ color was deployed with the Bayesian analysis and Markov chain Monte Carlo sampling to determine the distance at which the $J-K_s$ color jump is largest. This method was successfully applied to measure the distances of 27 molecular clouds, which were selected from previously published cloud samples. By replacing TRILEGAL with the GALAXIA galaxy model, we were able to measure the distances for 21 of the 27 clouds. The distances of the 21 clouds based on the GALAXIA model agree well with those based on the TRILEGAL model. The distances of the 27 clouds estimated by this method are consistent with previous estimates. We will apply this new method to a larger region of the gaseous galactic plane, in particular, for the inner galactic region, where a region free of CO emission is hard to separate from the crowded field of clouds.

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Distances to Nearby Molecular Clouds Traced by Young Stars

Cited by 10 publications

References 132 publications

Distribution and Properties of Molecular Gas toward the Monoceros OB1 Region

Distribution and Properties of Molecular Gas toward the Monoceros OB1 Region

Molecular Bubble and Outflow in S Mon Revealed by Multiband Data Sets

New method for estimating molecular cloud distances based on Gaia, 2MASS, and the TRILEGAL galaxy model

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