Extended CO(1–0) survey and ammonia measurements towards two bubble regions in W5 Feedback on molecular gas and clumps
Shen H. Esimbek J. Henkel C. Xu Y. Zhou J. Li D. He Y. Tang X. Wu G. Komesh T. Tursun K. Zhou D. Imanaly E. Berdikhan D.
1 September 2024EDP Sciences
Astronomy and Astrophysics
2024#689
The feedback effect of massive stars can either accelerate or inhibit star formation activity within molecular clouds. Studying the morphology of molecular clouds near W5 offers an excellent opportunity to examine this feedback effect. We conducted a comprehensive survey of the W5 complex using the Purple Mountain Observatory 13.7 m millimeter telescope. This survey includes 12CO, 13CO, and C18O (J = 1−0), with a sky coverage of 6.6 deg2 (136.0◦ < l < 138.75◦, 0◦ < b < 2.4◦). Furthermore, we performed simultaneous observations of the NH3 (1,1) and NH3 (2,2) lines in the four densest star-forming regions of W5, using the 26 m radio telescope of the Xinjiang Astronomy Observatory (XAO). Our analysis of the morphological distribution of the molecular clouds, distribution of high-mass young stellar objects (HMYSOs), 13CO/C18O abundance ratio, and the stacked average spectral line distribution at different 8 µm thresholds provide compelling evidence of triggering. Within the mapped region, we identified a total of 212 molecular clumps in the 13CO cube data using the astrodendro algorithm. Remarkably, approximately 26.4% (56) of these clumps demonstrate the potential to form massive stars and 42.9% (91) of them are gravitationally bound. Within clumps that are capable of forming high-mass stars, there is a distribution of class I YSOs, all located in dense regions near the boundaries of the Hii regions. The detection of NH3 near the most prominent cores reveals moderate kinetic temperatures and densities (as CO). Comparing the Tkin and Tex values reveals a reversal in trends for AFGL 4029 (higher Tex and lower Tkin) and W5-W1, indicating the inadequacy of optically thick CO for dense region parameter calculations. Moreover, a comparison of the intensity distributions between NH3 (1,1) and C18O (1–0) in the four densest region reveals a notable depletion effect in AFGL 4029, characterised by a low Tkin (9 K) value and a relatively high NH3 column density, 2.5 × 1014 cm−2. By classifying the 13CO clumps as: “feedback,” “non-feedback,” “outflow,” or “non-outflow” clumps, we observe that the parameters of the “feedback” and “outflow” clumps exhibit variations based on the intensity of the internal 8 µm flux and the outflow energy, respectively. These changes demonstrate a clear linear correlation, which distinctly separate them from the parameter distributions of the “non-feedback” and “non-outflow” clumps, thus providing robust evidence to support a triggering scenario.
ISM: clouds , ISM: kinematics and dynamics , methods: observational , outflows , stars: winds , submillimeter: ISM , techniques: image processing
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Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, 830011, China
University of Chinese Academy of Sciences, Beijing, 100080, China
Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Urumqi, 830011, China
Xinjiang Key Laboratory of Radio Astrophysics, Urumqi, 830011, China
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, Bonn, 53121, Germany
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, China
Energetic Cosmos Laboratory, Nazarbayev University, Astana, 010000, Kazakhstan
Institute of Experimental and Theoretical Physics, Al-Farabi Kazakh National University, Almaty, 050040, Kazakhstan
Xinjiang Astronomical Observatory
University of Chinese Academy of Sciences
Key Laboratory of Radio Astronomy
Xinjiang Key Laboratory of Radio Astrophysics
Max-Planck-Institut für Radioastronomie
Purple Mountain Observatory
Energetic Cosmos Laboratory
Institute of Experimental and Theoretical Physics
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