3D structure of H ii regions in the star-forming complex S254-S258

Author:

Kirsanova Maria S1ORCID,Moiseev Alexei V12ORCID,Boley Paul A13

Affiliation:

1. Institute of Astronomy, Russian Academy of Sciences , 48 Pyatnitskaya Str, Moscow 119017 , Russia

2. Special Astrophysical Observatory, Russian Academy of Sciences , Nizhny Arkhyz 369167 , Russia

3. Visiting astronomer, Laboratoire Lagrange, Université Côte d’ Azur , Observatoire de la Côte d’ Azur, CNRS, Boulevard de l’ Observatoire, CS 34229, F-06304, Nice Cedex 4 , France

Abstract

ABSTRACT The S254-258 star-forming complex is a place of massive star formation where five OB-stars have created H ii regions, visible as optical nebulae, and disrupted the parental molecular gas. In this work, we study the 3D structure of these H ii regions using optical spectroscopy and tunable-filter photometry with the 6- and 1-m telescopes of the Special Astrophysical Observatory of the Russian Academy of Sciences. We construct maps of the optical extinction and find that the H ii emission is attenuated by neutral material with 2 ≤ AV ≤ 5 mag. The typical electron density in S255, and S257 is ≈100 cm−3, with enhancements up to 200 cm−3 in their borders, and up to 400 cm−3 toward the dense molecular cloud between them, where active star formation is taking place. We show that either a model of a clumpy dense neutral shell, where UV photons penetrate through and ionize the gas, or a stellar wind, can explain the shell-like structure of the ionized gas. S255 is surrounded by neutral material from all sides, but S257 is situated on the border of a molecular cloud and does not have dense front and rear walls. The compact H ii regions S256 and S258 are deeply embedded in the molecular clouds.

Funder

Russian Science Foundation

Ministry of Science and Higher Education of the Russian Federation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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