Ammonia survey of the BGPS sources with the Nanshan 26-m telescope
Sailanbek S. Esimbek J. Henkel C. Sobolev A.M. Ladeyschikov D.A. Berdikhan D. Wu G. Zhou J. Tang X. He Y. Li D. Tursun K. Zhou D. Ma Y. Komesh T. Ibraimov M. Adilzhan K.
1 June 2025Oxford University Press
Monthly Notices of the Royal Astronomical Society
2025#539Issue 42987 - 3012 pp.
We conducted an ammonia surv e y targeting 217 sources from the Bolocam Galactic Plane Surv e y v1.0 using the Nanshan 26-m radio telescope, focusing on the NH 3 (1,1) and (2,2) lines, selecting sources based on the criteria that their 1.1 mm fluxes are greater than 5 Jy and that they are observable with the Nanshan 26-m radio telescope at the Xinjiang Astronomical Observatory. We successfully detected 188 (86.6 per cent) of our sources. These sources span a galactic longitude range of 1.2 °-192.6 °and reside in the local, Perseus, Saggitarius-Carina, Scutum-Centaurus, and Norma spiral arms and between them. Among them, 185 sources exhibit NH 3 (1,1) and (2,2) inversion lines, all showing well-defined structural characteristics. Total NH 3 column densities vary from 0.12 ×10 15 to 15 ×10 15 cm -2 , with para-NH 3 fractional abundances averaging 1.8 ×10 -7 . This study concludes that 82 per cent of our observed sources exhibit star formation acti vity, e videnced by 22 GHz water maser emission, and 52 per cent are identified as high-mass star formation regions through 6.7 GHz Class II methanol maser detections. Turbulence, reflected in non-thermal velocity dispersion, correlates positively with kinetic temperature, influencing cloud evolution and star formation. These results emphasize the role of turbulence in star formation processes and maser emission as their indicator. We also find a weak ne gativ e trend between ammonia column density and galactocentric distance with the 2 σsignificance, potentially linked to Galactic isotope ratio and gas density gradients.
dust, extinction , H ii regions , ISM: abundances , ISM: clouds , ISM: molecules
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Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, 830011, China
University of the Chinese Academy of Sciences, Beijing, 100080, China
Department of Electronics and Astrophysics, Faculty of Physics and Technology, Al-Farabi Kazakh National University, Almaty, 050040, Kazakhstan
Key Laboratory of Radio Astronomy, Chinese Academy of Science, Urumqi, 830011, China
Xinjiang Key Laboratory of Radio Astrophysics, Urumqi, 830011, China
Max-Plank-Institute fur Radioastronomie, Auf dem Hugel 69, Bonn, D-53121, Germany
Astronomical Observatory, Institute for Natural Sciences and Mathematics, Ural Federal University, 19 Mira street, Ekaterinburg, 620002, Russian Federation
Energetic Cosmos Laboratory, Nazarbayev University, Astana, 010000, Kazakhstan
Department of Plasma Physics Nonotechnology and Computer Physics, Faculty of Physics and Technology, Al - Farabi Kazakh National University, Almaty, 050040, Kazakhstan
Xinjiang Astronomical Observatory
University of the Chinese Academy of Sciences
Department of Electronics and Astrophysics
Key Laboratory of Radio Astronomy
Xinjiang Key Laboratory of Radio Astrophysics
Max-Plank-Institute fur Radioastronomie
Astronomical Observatory
Energetic Cosmos Laboratory
Department of Plasma Physics Nonotechnology and Computer Physics
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