Fragmented atomic shell around S187 H ii region and its interaction with molecular and ionized gas

Author:

Zemlyanukha Petr1ORCID,Zinchenko Igor I1ORCID,Dombek Evgeny12ORCID,Pirogov Lev E1,Topchieva Anastasiia3,Joncas Gilles4,Dewangan Lokesh K5ORCID,Ojha Devendra K6,Ghosh Swarna K6

Affiliation:

1. Institute of Applied Physics of the Russian Academy of Sciences , 46 Ul’yanov str., Nizhny Novgorod 603950, Russia

2. Lobachevsky State University of Nizhny Novgorod , 23 Gagarin Ave, Nizhny Novgorod 603950, Russia

3. Institute of Astronomy, Russian Academy of Sciences , Pyatnitskaya str., 48 Moscow, Russia

4. Centre de Recherche en Astrophysique du Québec , Département de Physique, de génie physique et d’optique, Université Laval, Québec, QC, G1V OA6, Canada

5. Physical Research Laboratory , Navrangpura, Ahmedabad 380009, India

6. Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research , Homi Bhabha Road, Mumbai 400 005, India

Abstract

ABSTRACT The environment of S187, a nearby H ii region (1.4 ± 0.3 kpc), is analyzed. A surrounding shell has been studied in the H i line, molecular lines, and also in infrared and radio continua. We report the first evidence of a clumpy H i environment in its photodissociation region. A background radio galaxy enables the estimation of the properties of cold atomic gas. The estimated atomic mass fraction of the shell is ∼260 M⊙, the median spin temperature is ∼50 K, the shell size is ∼4 pc with typical wall width around 0.2 pc. The atomic shell consists of ∼100 fragments. The fragment sizes correlate with mass with a power-law index of 2.39–2.50. The S187 shell has a complex kinematical structure, including the expanding quasi-spherical layer, molecular envelope, an atomic sub-bubble inside the shell and two dense cores (S187 SE and S187 NE) at different stages of evolution. The atomic sub-bubble inside the shell is young, contains a Class II young stellar object and OH maser in the centre and the associated YSOs in the walls of the bubble. S187 SE and S187 NE have similar masses (∼1200 and ∼900 M⊙, respectively). S187 SE is embedded into the atomic shell and has a number of associated objects, including high-mass protostars, outflows, maser sources, and other indicators of ongoing star formation. No YSOs inside S187 NE were detected, but indications of compression and heating by the H ii region exist.

Funder

Russian Science Foundation

National Research Council Canada

NSF

Natural Sciences and Engineering Research Council of Canada

Swedish Research Council

Department of Atomic Energy, Government of India

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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