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Title:
Properties of free-free, dust and CO emissions in the starbursts of blue compact dwarf galaxies
Authors:
Hirashita, Hiroyuki
Affiliation:
AA(Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, Taipei 10617, Taiwan; )
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 429, Issue 4, p.3390-3401 (MNRAS Homepage)
Publication Date:
03/2013
Origin:
OUP
Astronomy Keywords:
dust, extinction, galaxies: dwarf, galaxies: evolution, galaxies: individual: He 2-10, galaxies: individual: NGC 5253, galaxies: individual: II Zw 40, submillimetre: galaxies
Abstract Copyright:
2013 The Author Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/sts602
Bibliographic Code:
2013MNRAS.429.3390H

Abstract

The central star-forming regions in three blue compact dwarf galaxies (He 2-10, NGC 5253 and II Zw 40) were observed in the 340 GHz (880mum) band at ˜5 arcsec resolution with the Submillimetre Array (SMA). Continuum emission associated with the central star-forming complex was detected in all these galaxies. The SMA 880 mum flux is decomposed into free-free emission and dust emission by using centimetre-wavelength data in the literature. We find that free-free emission contributes half or more of the SMA 880 mum flux in the central starbursts in those three galaxies. In spite of the dominance of free-free emission at 880 mum, the radio-to-far-infrared (FIR) ratios in the central star-forming regions are not significantly higher than those of the entire systems, showing the robustness of radio-FIR relation. Based on the robustness of the radio-FIR relation, we argue that the free-free fraction in the 880 mum emission is regulated by the dust temperature. We also analyse the CO (J = 3-2) emission data. We find that CO is a good tracer of the total gas mass in solar-metallicity object He 2-10. Low-metallicity objects, NGC 5253 and II Zw 40, have apparently high star formation efficiencies; however, this may be an artefact of significant dissociation of CO in the low-metallicity environments. We also point out a potential underestimate of dust mass, since the dust traced by emission is biased to the most luminous high-temperature regions, particularly when a system hosts a compact star-forming region where the dust temperature is high.
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