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What powers Lyα blobs?

Ao, Y. and Matsuda, Y. and Beelen, A. and Henkel, C. and Cen, R. and de Breuck, C. and Francis, P. J. and Kovács, A. and Lagache, G. and Lehnert, M. and Mao, M. Y. and Menten, K. M. and Norris, R. P. and Omont, A. and Tatemastu, K. and Weiss, A. and Zheng, Z. (2015) What powers Lyα blobs? Astronomy and Astrophysics, 581 . Arti. No.A132. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20151030-095317976

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Abstract

Lyα blobs (LABs) are spatially extended Lyα  nebulae seen at high redshift. The origin of Lyα emission in the LABs is still unclear and under debate. To study their heating mechanism(s), we present Australia Telescope Compact Array (ATCA) observations of the 20 cm radio emission and Herschel PACS and SPIRE measurements of the far-infrared (FIR) emission toward the four LABs in the protocluster J2143-4423 at z = 2.38. Among the four LABs, B6 and B7 are detected in the radio with fluxes of 67±17 μJy and 77±16 μJy, respectively, and B5  is marginally detected at 3σ (51±16 μJy). For all detected sources, their radio positions are consistent with the central positions of the LABs. Among them, B6 and B7 are obviously also detected in the FIR. By fitting the data with different templates, we obtained redshifts of 2.20^(+0.30)_(-0.35) for B6 and 2.20^(+0.45)_(-0.30) for B7, which are consistent with the redshift of the Lyα emission within uncertainties, indicating that both FIR sources are likely associated with the LABs. The associated FIR emission in B6 and B7 and high star formation rates strongly favor star formation in galaxies as an important powering source for the Lyα emission in both LABs. However, the other two, B1 and B5, are predominantly driven by the active galactic nuclei or other sources of energy still to be specified, but not mainly by star formation. In general, the LABs are powered by quite diverse sources of energy.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201424165DOIArticle
http://www.aanda.org/articles/aa/abs/2015/09/aa24165-14/aa24165-14.htmlPublisherArticle
http://arxiv.org/abs/1507.07627arXivDiscussion Paper
ORCID:
AuthorORCID
Ao, Y.0000-0003-3139-2724
de Breuck, C.0000-0002-6637-3315
Lagache, G.0000-0003-1492-2519
Lehnert, M.0000-0003-1939-5885
Menten, K. M.0000-0001-6459-0669
Omont, A.0000-0002-4721-3922
Weiss, A.0000-0003-4678-3939
Additional Information:© 2015 ESO. Received 9 May 2014. Accepted 20 July 2015. Published online 22 September 2015. We thank the anonymous referee for valuable comments that improved this manuscript. Y.A. acknowledges partial support by NSFC grant 11373007 and Youth Innovation Promotion Association CAS. R.C. is supported in part by NASA grant NNX11AI23G. Y.M. acknowledges support from JSPS KAKENHI Grant Number 20647268. Z.Z. was partially supported by NSF grant AST-1208891 and NASA grant NNX14AC89G. This research has made use of NASA’s Astrophysical Data System (ADS). 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); INAF-IFSI/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). 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, UKSA (UK); and NASA (USA).
Funders:
Funding AgencyGrant Number
National Natural Science Foundation of China11373007
Chinese Academy of SciencesUNSPECIFIED
NASANNX11AI23G
Japan Society for the Promotion of Science (JSPS)20647268
NSFAST-1208891
NASANNX14AC89G
Bundesministerium für Verkehr, Innovation und Technologie (BMVIT)UNSPECIFIED
ESA-PRODEX (Belgium)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Deutsches Zentrum für Luft- und Raumfahrt (DLR)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Comisión Interministerial de Ciencia y Tecnología (CICYT)UNSPECIFIED
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Ministerio de Economía y Competitividad (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB) UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Subject Keywords:galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies: active; infrared: galaxies
Record Number:CaltechAUTHORS:20151030-095317976
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20151030-095317976
Official Citation:What powers Lyα blobs? Y. Ao, Y. Matsuda, A. Beelen, C. Henkel, R. Cen, C. De Breuck, P. J. Francis, A. Kovács, G. Lagache, M. Lehnert, M. Y. Mao, K. M. Menten, R. P. Norris, A. Omont, K. Tatemastu, A. WeißY. Ao, Y. Matsuda, A. Beelen, C. Henkel, R. Cen, C. De Breuck, P. J. Francis, A. Kovács, G. Lagache, M. Lehnert, M. Y. Mao, K. M. Menten, R. P. Norris, A. Omont, K. Tatemastu, A. Weiß and Z. Zheng A&A, 581 (2015) A132 DOI: http://dx.doi.org/10.1051/0004-6361/201424165
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:61738
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:03 Nov 2015 00:53
Last Modified:17 Jul 2019 18:27

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