Molecular Gas toward the Gemini OB1 Molecular Cloud Complex. I. Observation Data

Wang, Chen; Yang, Ji; Xu, Ye; Li, Facheng; Su, Yang; Zhang, Shaobo

doi:10.3847/1538-4365/aa6c6b

Cited by 10 publications

(9 citation statements)

References 39 publications

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“…CO emission of these coherent structures frequently shows asymmetric line profiles or multi-velocity components rather than a single Gaussian profile (e.g., see PV diagrams in Figure 21), possibly indicating the assembling gas in certain regions. Similar features were also revealed by some authors in simulations (e.g., Heitsch et al 2009;Smith et al 2014) and observations (e.g., Wang et al 2017;Dhabal et al 2018). For the particular case of LDN 673, the gas seems to converge toward the hub-like region (see the upper box region in Figure 20 and Figure 22), in which the 13 CO emission is embedded in the enhanced 12 CO emission with broader linewidths (the red circle in Figure 23).…”

Section: Formation By Large-scale Converging Flows?supporting

confidence: 88%

Local Molecular Gas toward the Aquila Rift Region

Su¹,

Yang

Yan³

et al. 2020

ApJ

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We present the results of a ∼250 square degrees CO mapping (+26 • < ∼ l < ∼ + 50 • and −5 • < ∼ b < ∼ + 5 • ) toward the Aquila Rift region at a spatial resolution of ∼ 50 and a grid spacing of 30 . The high dynamic range CO maps with a spectral resolution of ∼ 0.2 km s −1 display highly structured molecular cloud (MC) morphologies with valuable velocity information, revealing complex spatial and dynamical features of the local molecular gas. In combination with the MWISP CO data and the Gaia DR2, distances of the main MC structures in the local ISM are well determined toward the Aquila Rift region. We find that the total MC mass within 1 kpc is about > ∼ 4.1×10 5 M in the whole region. In fact, the mass of the molecular gas is dominated by the W40 giant molecular cloud (GMC) at ∼ 474 pc (∼ 1.4×10 5 M ) and the GMC complex G036.0+01.0 at ∼ 560-670 pc (∼ 2.0 × 10 5 M ), while the MCs at ∼ 220-260 pc have gas mass of ∼ 10 2 −10 3 M . Interestingly, a ∼ 80 pc long filamentary MC G044.0−02.5 at a distance of ∼ 404 pc shows a systematic velocity gradient along and perpendicular to the major axis of the filament. The HI gas with the enhanced emission has the similar spatial morphologies and velocity features compared to the corresponding CO structure, indicating that the large-scale converging HI flows is probably responsible for the formation of the MC. Meanwhile, the long filamentary MC consists of many sub-filaments with the lengths ranging from ∼ 0.5 pc to several pc, as well as prevalent networks of filaments in other large-scale local MCs.

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Section: Formation By Large-scale Converging Flows?supporting

confidence: 88%

Local Molecular Gas toward the Aquila Rift Region

Su¹,

Yang

Yan³

et al. 2020

ApJ

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“…In summary, the MWISP CO survey gives us a good opportunity to study the Galactic structures, the MC properties and the star formation, and the associations between the molecular gas and the extended radio sources such as, for example, H ii regions and supernova remnants (SNRs). Much work has been done based on the MWISP data, such as Galactic arms traced by the CO emission (Sun et al 2015(Sun et al , 2017Du et al 2016Du et al , 2017Su et al 2016), MCs and star formation (Li et al 2013;Zhang et al 2014b;Su et al 2015;Zhan et al 2016;Gong et al 2016Gong et al , 2017Chen et al 2016Chen et al , 2017bXiong et al 2017;Wang et al 2017;Li et al 2018b,a;Sun et al 2018b), and interactions between SNRs and MCs (Su et al 2014b(Su et al ,c, 2017a(Su et al ,b, 2018Zhou et al 2014Zhou et al , 2016Chen et al 2017a). The MWISP project also provides us an invaluable dataset for studying the distribution and kinematics of the MCs in the Milky Way (Section 3).…”

Section: Characteristics and Advantages Of The Mwispmentioning

confidence: 99%

The Milky Way Imaging Scroll Painting (MWISP): Project Details and Initial Results from the Galactic Longitudes of 25.°8–49.°7

Su¹,

Yang²,

Zhang³

et al. 2019

ApJS

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138

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The Milky Way Imaging Scroll Painting (MWISP) project is an unbiased Galactic plane CO survey for mapping regions of l = −10 • to +250 • and |b| < ∼ 5. • 2 with the 13.7 m telescope of the Purple Mountain Observatory. The legacy survey aims to observe the 12 CO, 13 CO, and C 18 O (J=1-0) lines simultaneously with full-sampling using the nine-beam Superconducting SpectroScopic Array Receiver (SSAR) system with an instantaneous bandwidth of 1 GHz. In this paper, the completed 250 deg 2 data from l = +25. • 8 to +49. • 7 are presented with a grid spacing of 30 ′′ and a typical rms noise level of ∼ 0.5 K for 12 CO at the channel width of 0.16 km s −1 and ∼ 0.3 K for 13 CO and C 18 O at 0.17 km s −1 . The high-quality data with moderate resolution (∼50 ′′ ), uniform sensitivity, and high spatial dynamic range, allow us to investigate the details of molecular clouds (MCs) traced by the three CO isotope lines. Three interesting examples are briefly investigated, including distant Galactic spiral arms traced by CO emission with V LSR <0 km s −1 , the bubble-like dense gas structure near the H ii region W40, and the MCs distribution perpendicular to the Galactic plane.

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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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Molecular Gas toward the Gemini OB1 Molecular Cloud Complex. I. Observation Data

Abstract: We present a large-scale mapping toward the GEM OB1 association in the galactic anti-center direction. The 9• ×6

Cited by 10 publications

References 39 publications

Local Molecular Gas toward the Aquila Rift Region

Local Molecular Gas toward the Aquila Rift Region

The Milky Way Imaging Scroll Painting (MWISP): Project Details and Initial Results from the Galactic Longitudes of 25.°8–49.°7

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

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