A Caltech Library Service

Infall, outflow, and rotation in the G19.61-0.23 hot molecular core

Furuya, R. S. and Cesaroni, R. and Shinnaga, H. (2011) Infall, outflow, and rotation in the G19.61-0.23 hot molecular core. Astronomy and Astrophysics, 525 . Art. No. A72. ISSN 0004-6361.

PDF - Published Version
See Usage Policy.


Use this Persistent URL to link to this item:


Aims. We carried out sub-arcsecond resolution observations towards the high-mass star formation region G19.61−0.23, in both continuum and molecular line emission. While the centimeter continuum images, representing ultra compact HII regions, will be discussed in detail in a forthcoming paper, here we focus on the (sub)mm emission, devoting special attention to the hot molecular core (HMC). Methods. A set of multi wavelength continuum and molecular line emission data between 6 cm and 890 μm were obtained with the Very Large Array, Nobeyama Millimeter Array, Owens Valley Radio Observatory millimeter array, and Submillimeter Array (SMA). These data were analyzed in conjunction with previously published data. Results. Our SMA observations resolve the HMC into three cores whose masses are on the order of 10^1−10^3 M_⊙. No submm core exhibits detectable free-free emission in the centimeter regime, but appear to be associated with masers and thermal line emission from complex organic molecules. Towards the most massive core, SMA1, the CH_3CN (18_K−17_K) lines provide hints of rotation about the axis of a jet/outflow traced by H_2O maser and H^(13)CO^+(1−0) line emission. Inverse P-Cygni profiles of the ^(13)CO (3−2) and C^(18)O (3−2) lines seen towards SMA1 indicate that the central high-mass (proto)star(s) is (are) still gaining mass with an accretion rate ≥3 × 10^(−3) M_⊙ yr^(−1). Owing to the linear scales and high accretion rate, we hypothesize that we are observing an accretion flow towards a star cluster in the making, rather than towards a single massive star.

Item Type:Article
Related URLs:
URLURL TypeDescription
Additional Information:© 2010 ESO. Received 10 March 2010, Accepted 20 June 2010, Published online 02 December 2010. The authors are grateful to the referee, Dr. S. Curiel, and the editor, Dr. C. M. Walmsley, for their constructive comments to the manuscript. The authors sincerely acknowledge S. Takahashi, M. Momose, L. Testi, and C. Codella for their contribution at early stage of this study as co-authors of Paper I. In particular, S. Takahashi and M. Momose performed the NMA observations and calibrated most of the visibility data. The authors also acknowledge M. J. Claussen and G. V. Moorsel for their extensive help in VLA observations, especially handling the EVLA antenna data, D. Fong for his help in calibrating the SMA data, J. M. Carpenter and J. Lamb for their help in combining the OVRO and NMA visibilities, and A. I. Sargent and P. T. P. Ho for their fruitful comments and encouragement. R.S.F. is supported by a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science and Technology of Japan (No. 20740113).
Funding AgencyGrant Number
NSFAST 02-28955
Smithsonian InstitutionUNSPECIFIED
Academia SinicaUNSPECIFIED
Ministry of Education, Culture, Sports, Science and Technology (Japan)20740113
Subject Keywords:stars: early-type – evolution – HII regions – ISM: jets and outflows – ISM: individual objects: G19.61-0.23 – submillimeter: ISM
Record Number:CaltechAUTHORS:20110124-160759927
Persistent URL:
Official Citation:Infall, outflow, and rotation in the G19.61-0.23 hot molecular core R. S. Furuya, R. Cesaroni and H. Shinnaga A&A 525 A72 (2011) DOI: 10.1051/0004-6361/201014402
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21872
Deposited By: Benjamin Perez
Deposited On:25 Jan 2011 15:55
Last Modified:03 Oct 2019 02:30

Repository Staff Only: item control page