APERTURE SYNTHESIS OBSERVATIONS OF CO, HCN, AND 89 GHz CONTINUUM EMISSION TOWARD NGC 604 IN M33: SEQUENTIAL STAR FORMATION INDUCED BY A SUPERGIANT H II REGION

Journal Article · Wed Dec 01 04:00:00 EST 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/724/2/1120· OSTI ID:21474484

Miura, Rie; Okumura, Sachiko K; Kurono, Yasutaka; Nakanishi, Kouichiro ^[1]; Tosaki, Tomoka ^[2]; Tamura, Yoichi ^[3]; Kuno, Nario; Kawabe, Ryohei ^[4]; Sakamoto, Seiichi ^[5]; Hasegawa, Takashi ^[6]

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1. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
2. Joetsu University of Education, Yamayashiki-machi, Joetsu, Niigata 943-8512 (Japan)
3. Department of Astronomy, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo 133-0033 (Japan)
4. Nobeyama Radio Observatory, Minamimaki, Minamisaku, Nagano 384-1805 (Japan)
5. Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara-shi, Kanagawa 252-5210 (Japan)
6. Gunma Astronomical Observatory, Nakayama, Takayama, Agatsuma, Gunma 377-0702 (Japan)

We present the results from new Nobeyama Millimeter Array observations of CO(1-0), HCN(1-0), and 89 GHz continuum emission toward NGC 604, known as the supergiant H II region in the nearby galaxy M33. Our high spatial resolution images (4.''2 x 2.''6, corresponding to 17 pc x 11 pc physical size) of CO emission allowed us to uncover 10 individual molecular clouds that have masses of (0.8-7.4) x10{sup 5} M{sub sun} and sizes of 5-29 pc, comparable to those of typical Galactic giant molecular clouds. Moreover, we detected for the first time HCN emission in the two most massive clouds and 89 GHz continuum emission at the rims of the 'H{alpha} shells'. The HCN and 89 GHz continuum emission are offset from the CO peak and are distributed in the direction of the central cluster. Three out of ten CO clouds are well correlated with the H{alpha} shells both in spatial and velocity domains, implying an interaction between molecular gas and the expanding H II region. The CO clouds show varieties in star formation efficiencies (SFEs), which are estimated from the 89 GHz emission and combination of H{alpha} and Spitzer 24 {mu}m data. Furthermore, we found that the SFEs decrease with increasing projected distance measured from the heart of the central OB star cluster in NGC 604, suggesting radial changes in the evolutionary stages of the molecular clouds in the course of stellar cluster formation. Our results provide further support to the picture of sequential star formation in NGC 604 initially proposed by Tosaki et al. with the higher spatially resolved molecular clouds, in which an isotropic expansion of the H II region pushes gases outward, which accumulates to form dense molecular clouds, and then induces massive star formations.

• OSTI ID: 21474484
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 724; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
CARBON COMPOUNDS
CARBON MONOXIDE
CARBON OXIDES
CHALCOGENIDES
EMISSION
GALAXIES
HYDROCYANIC ACID
HYDROGEN COMPOUNDS
INORGANIC ACIDS
INORGANIC COMPOUNDS
OXIDES
OXYGEN COMPOUNDS
RESOLUTION
SPATIAL RESOLUTION
STAR CLUSTERS
STARS