Liu, HB, Dunham, MM, Pascucci, I, Bourke, TL, Hirano, N, Longmore, SN, Andrews, S, Carrasco-González, C, Forbrich, J, Galván-Madrid, R, Girart, JM, Green, JD, Juárez, C, Kóspál, Á, Manara, CF, Palau, A, Takami, M, Testi, L and Vorobyov, EI (2017) A 1.3 mm SMA Survey of 29 Variable Young Stellar Objects. Astronomy and Astrophysics. ISSN 0004-6361

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Abstract

Young stellar objects (YSOs) may undergo periods of active accretion (outbursts), during which the protostellar accretion rate is temporarily enhanced by a few orders of magnitude. Whether or not these accretion outburst YSOs possess similar dust/gas reservoirs to each other, and whether or not their dust/gas reservoirs are similar as quiescent YSOs, are issues not yet clarified. The aim of this work is to characterize the millimeter thermal dust emission properties of a statistically significant sample of long and short duration accretion outburst YSOs (i.e., FUors and EXors) and the spectroscopically identified candidates of accretion outbursting YSOs (i.e., FUor-like objects). We have carried out extensive Submillimeter Array (SMA) observations mostly at $\sim$225 GHz (1.33 mm) and $\sim$272 GHz (1.10 mm), from 2008 to 2017. We covered accretion outburst YSOs located at $<$1 kpc distances from the solar system. We analyze all the existing SMA data of such objects, both published and unpublished, in a coherent way to present a millimeter interferometric database of 29 objects. We obtained 21 detections at $>$3-$\sigma$ significance. Detected sources except for the two cases of V883 Ori and NGC 2071 MM3 were observed with $\sim$1$"$ angular resolution. Overall our observed targets show a systematically higher millimeter luminosity distribution than those of the $M_{*}>$0.3 $M_{\odot}$ Class II YSOs in the nearby ($\lesssim$400 pc) low-mass star-forming molecular clouds (e.g., Taurus, Lupus, Upp Scorpio, and Chameleon I). In addition, at 1 mm our observed confirmed binaries or triple-system sources are systematically fainter than the rest of the sources even though their 1 mm fluxes are broadly distributed. We may have detected $\sim$30-60\% millimeter flux variability from V2494 Cyg and V2495 Cyg, from the observations separated by $\sim$1 year.

Item Type:	Article
Uncontrolled Keywords:	astro-ph.SR; astro-ph.SR
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	EDP Sciences
Related URLs:	http://arxiv.org/abs/1710.08686v1
Date Deposited:	10 Nov 2017 12:59
Last Modified:	04 Sep 2021 11:01
URI:	https://researchonline.ljmu.ac.uk/id/eprint/7530

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