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A Herschel and BIMA study of the sequential star formation near the W 48A H II region

Rygl, K. L. J. and Goedhart, S. and Polychroni, D. and Wyrowski, F. and Motte, F. and Elia, D. and Nguyen-Luong, Q. and Didelon, P. and Pestalozzi, M. and Benedettini, M. and Molinari, S. and André, Ph. and Fallscheer, C. and Gibb, A. and di Giorgio, A. M. and Hill, T. and Könyves, V. and Marston, A. and Pezzuto, S. and Rivera-Ingraham, A. and Schisano, E. and Schneider, N. and Spinoglio, L. and Ward-Thompson, D. and White, G. J. (2014) A Herschel and BIMA study of the sequential star formation near the W 48A H II region. Monthly Notices of the Royal Astronomical Society, 440 (1). pp. 427-447. ISSN 0035-8711. doi:10.1093/mnras/stu300.

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We present the results of Herschel HOBYS (Herschel imaging survey of OB Young Stellar objects) photometric mapping combined with Berkeley Illinois Maryland Association (BIMA) observations and additional archival data, and perform an in-depth study of the evolutionary phases of the star-forming clumps in W 48A and their surroundings. Age estimates for the compact sources were derived from bolometric luminosities and envelope masses, which were obtained from the dust continuum emission, and agree within an order of magnitude with age estimates from molecular line and radio data. The clumps in W 48A are linearly aligned by age (east-old to west-young): we find a ultra-compact (UC) H ii region, a young stellar object (YSO) with class II methanol maser emission, a YSO with a massive outflow and finally the NH_2D prestellar cores from Pillai et al. This remarkable positioning reflects the (star) formation history of the region. We find that it is unlikely that the star formation in the W 48A molecular cloud was triggered by the UC H ii region and discuss the Aquila supershell expansion as a major influence on the evolution of W 48A. We conclude that the combination of Herschel continuum data with interferometric molecular line and radio continuum data is important to derive trustworthy age estimates and interpret the origin of large-scale structures through kinematic information.

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Ward-Thompson, D.0000-0003-1140-2761
Additional Information:© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 February 12. Received 2014 February 12; in original form 2013 September 6. First published online: March 11, 2014. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is partially based on observations carried out with the IRAM 30m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The authors thank the anonymous referee for his/her detailed comments which lead to a significant improvement of the manuscript. Furthermore, the authors are very grateful to Gemma Busquet, Miguel Pereira-Santaella and Scige J. Liu. The staff of both the BIMA and IRAM 30m telescopes are acknowledged for their support during the observations. KLJR acknowledges funding by the Agenzia Spaziale Italiana (ASI) under contract number I/005/11/0. DP is funded through the Operational Program ‘Education and Lifelong Learning’ Ó and is co-financed by the European Union (European Social Fund) and Greek national funds. Part of this work was supported by the French National Agency for Research (ANR) project ‘PROBeS’, number ANR-08-BLAN-0241. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/ OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). The BIMA array was operated with support from the National Science Foundation under grants AST-9981308 to UC Berkeley, AST-9981363 to U. Illinois, and AST-9981289 to U. Maryland. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research and the National Research Council of Canada. This research has made use of the SIMBAD data base and the VizieR service, operated at CDS, Strasbourg, France.
Funding AgencyGrant Number
Agenzia Spaziale Italiana (ASI)I/005/11/0
Operational Program ‘Education and Lifelong Learning’ ÓUNSPECIFIED
European Union (European Social Fund)UNSPECIFIED
Greek national fundsUNSPECIFIED
French National Agency for Research (ANR)ANR-08-BLAN-0241
Subject Keywords: stars: formation ISM: clouds dust, extinction H ii regions ISM: individual objects: W 48A ISM: molecules
Issue or Number:1
Record Number:CaltechAUTHORS:20140602-061127288
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Official Citation: K. L. J. Rygl, S. Goedhart, D. Polychroni, F. Wyrowski, F. Motte, D. Elia, Q. Nguyen-Luong, P. Didelon, M. Pestalozzi, M. Benedettini, S. Molinari, Ph. André, C. Fallscheer, A. Gibb, A. M. di Giorgio, T. Hill, V. Könyves, A. Marston, S. Pezzuto, A. Rivera-Ingraham, E. Schisano, N. Schneider, L. Spinoglio, D. Ward-Thompson, and G. J. White A Herschel and BIMA study of the sequential star formation near the W 48A H ii region MNRAS first published online March 11, 2014 doi:10.1093/mnras/stu300
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46020
Deposited By: Ruth Sustaita
Deposited On:02 Jun 2014 14:52
Last Modified:10 Nov 2021 17:19

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