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

Su, Yang; Yang, Ji; Zhang, Shaobo; Gong, Y.; Wang, Hongchi; Zhou, Xin; Wang, Min; Chen, Zhiwei; Sun, Yan; Chen, Xuepeng; Xu, Ye; Jiang, Zhibo

doi:10.3847/1538-4365/aaf1c8

Cited by 138 publications

(111 citation statements)

References 73 publications

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“…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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“…The MWISP project is a high-sensitivity survey of the northern Galactic plane observed with the Purple Mountain Observatory 13.7 m telescope (Sun et al 2018;Su et al 2019). In this work we used the published data from the survey in the region within 25.…”

Section: The Milky Way Imaging Scroll Painting (Mwisp)mentioning

confidence: 99%

“…The vertical structures may arise from the combined effect of supernova (SN) feedback and strong magnetic fields (Hennebelle 2018;Smith et al 2020). To test if the trends found in the Hi emission are also present in the molecular gas, we applied the Hessian matrix analysis to the 12 CO, 13 CO, and C 18 O observations from the Milky Way Imaging Scroll Painting (MWISP) survey (Su et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The filamentary structures in the CO emission toward the Milky Way disk

Soler

Beuther

Syed

et al. 2021

A&A

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We present a statistical study of the filamentary structure orientation in the CO emission observations obtained in the Milky Way Imaging Scroll Painting survey in the range 25.°8 < l < 49.°7, |b| ≤ 1.°25, and −100 < vLSR < 135 km s−1. We found that most of the filamentary structures in the 12CO and 13CO emission do not show a global preferential orientation either parallel or perpendicular to the Galactic plane. However, we found ranges in Galactic longitude and radial velocity where the 12CO and 13CO filamentary structures are parallel to the Galactic plane. These preferential orientations are different from those found for the HI emission. We consider this an indication that the molecular structures do not simply inherit these properties from parental atomic clouds. Instead, they are shaped by local physical conditions, such as stellar feedback, magnetic fields, and Galactic spiral shocks.

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“…The large-scale CO map is obtained from the MWISP survey (see details in Su et al 2019). The 12 CO(J=1-0), 13 CO(J=1-0), and C18O (J=1-0) lines were simultaneously observed using the 13.7 m telescope.…”

Section: Co Observationsmentioning

confidence: 99%

SNR G39.2−0.3, an hadronic cosmic rays accelerator

Wilhelmi

Sushch

Brose

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Recent results obtained with gamma-ray satellites have established supernova remnants as accelerators of GeV hadronic cosmic rays. In such processes, CRs accelerated in SNR shocks interact with particles from gas clouds in their surrounding. In particular, the rich medium in which core-collapse SNRs explode provides a large target density to boost hadronic gamma-rays. SNR G39.2–0.3 is one of the brightest SNR in infrared wavelengths, and its broad multi-wavelength coverage allows a detailed modeling of its radiation from radio to high energies. We reanalysed the Fermi-LAT data on this region and compare it with new radio observations from the MWISP survey. The modeling of the spectral energy distribution from radio to GeV energies favours a hadronic origin of the gamma-ray emission and constrains the SNR magnetic field to be at least ∼100 μG. Despite the large magnetic field, the present acceleration of protons seems to be limited to ∼10 GeV, which points to a drastic slow down of the shock velocity due to the dense wall traced by the CO observations, surrounding the remnant. Further investigation of the gamma-ray spectral shape points to a dynamically old remnant subjected to severe escape of CRs and a decrease of acceleration efficiency. The low-energy peak of the gamma-ray spectrum also suggests that that the composition of accelerated particles might be enriched by heavy nuclei which is certainly expected for a core-collapse SNR. Alternatively, the contribution of the compressed pre-existing Galactic cosmic rays is discussed, which is, however, found to not likely be the dominant process for gamma-ray production.

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

Cited by 138 publications

References 73 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

The filamentary structures in the CO emission toward the Milky Way disk

SNR G39.2−0.3, an hadronic cosmic rays accelerator

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