The Spitzer survey of interstellar clouds in the Gould Belt. IV. Lupus V and VI observed with IRAC and MIPS

TY - JOUR

T1 - The Spitzer survey of interstellar clouds in the Gould Belt. IV. Lupus V and VI observed with IRAC and MIPS

AU - Spezzi, Loredana

AU - Vernazza, Pierre

AU - Merín, Bruno

AU - Allen, Lori E.

AU - Evans, Neal J.

AU - Jørgensen, Jes Kristian

AU - Bourke, Tyler L.

AU - Cieza, Lucas A.

AU - Dunham, Michael M.

AU - Harvey, Paul M.

AU - Huard, Tracy L.

AU - Peterson, Dawn

AU - Tothill, Nick F. H.

AU - Team, The Gould's Belt

PY - 2011/4/1

Y1 - 2011/4/1

N2 - We present Gould's Belt (GB) Spitzer IRAC and MIPS observations of the Lupus V and VI clouds and discuss them in combination with near-infrared (2MASS) data. Our observations complement those obtained for other Lupus clouds within the frame of the Spitzer "Core to Disk" (c2d) Legacy Survey. We found 43 young stellar object (YSO) candidates in Lupus V and 45 in Lupus VI, including two transition disks, using the standard c2d/GB selection method. None of these sources was classified as a pre-main-sequence star from previous optical, near-IR, and X-ray surveys. A large majority of these YSO candidates appear to be surrounded by thin disks (Class III; 79% in Lupus V and 87% in Lupus VI). These Class III abundances differ significantly from those observed for the other Lupus clouds and c2d/GB surveyed star-forming regions, where objects with optically thick disks (Class II) dominate the young population. We investigate various scenarios that can explain this discrepancy. In particular, we show that disk photoevaporation due to nearby OB stars is not responsible for the high fraction of Class III objects. The gas surface densities measured for Lupus V and VI lie below the star formation threshold (AV 8.6 mag), while this is not the case for other Lupus clouds. Thus, few Myr older age for the YSOs in Lupus V and VI with respect to other Lupus clouds is the most likely explanation of the high fraction of Class III objects in these clouds, while a higher characteristic stellar mass might be a contributing factor. Better constraints on the age and binary fraction of the Lupus clouds might solve the puzzle but require further observations.

AB - We present Gould's Belt (GB) Spitzer IRAC and MIPS observations of the Lupus V and VI clouds and discuss them in combination with near-infrared (2MASS) data. Our observations complement those obtained for other Lupus clouds within the frame of the Spitzer "Core to Disk" (c2d) Legacy Survey. We found 43 young stellar object (YSO) candidates in Lupus V and 45 in Lupus VI, including two transition disks, using the standard c2d/GB selection method. None of these sources was classified as a pre-main-sequence star from previous optical, near-IR, and X-ray surveys. A large majority of these YSO candidates appear to be surrounded by thin disks (Class III; 79% in Lupus V and 87% in Lupus VI). These Class III abundances differ significantly from those observed for the other Lupus clouds and c2d/GB surveyed star-forming regions, where objects with optically thick disks (Class II) dominate the young population. We investigate various scenarios that can explain this discrepancy. In particular, we show that disk photoevaporation due to nearby OB stars is not responsible for the high fraction of Class III objects. The gas surface densities measured for Lupus V and VI lie below the star formation threshold (AV 8.6 mag), while this is not the case for other Lupus clouds. Thus, few Myr older age for the YSOs in Lupus V and VI with respect to other Lupus clouds is the most likely explanation of the high fraction of Class III objects in these clouds, while a higher characteristic stellar mass might be a contributing factor. Better constraints on the age and binary fraction of the Lupus clouds might solve the puzzle but require further observations.

KW - ISM: clouds, ISM: individual objects: Lupus V and VI, stars: formation, stars: low-mass, stars: pre-main sequence

U2 - 10.1088/0004-637X/730/2/65

DO - 10.1088/0004-637X/730/2/65

M3 - Journal article

SN - 0004-637X

VL - 730

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 65

ER -