Mañana, JUEVES, 24 DE ABRIL, el sistema se apagará debido a tareas habituales de mantenimiento a partir de las 9 de la mañana. Lamentamos las molestias.
Disk evolution in ob associations: Deep Spitzer/IRAC observations of IC 1795
Entity
UAM. Departamento de Física TeóricaPublisher
The American Astronomical Society.Date
2011-06-01Citation
10.1088/0004-637X/733/2/113
The Astrophysical Journal 733.2 (2013): 113
ISSN
0004-637X (print); 1538-4357 (online)DOI
10.1088/0004-637X/733/2/113Editor's Version
http://dx.doi.org/10.1088/0004-637X/733/2/113Subjects
ISM: individual objects (W3); open clusters and associations: individual (W3 IC1795); protoplanetary disks; stars: formation; stars: pre-main sequence; X-rays: stars; FísicaNote
The Astrophysical Journal 773.2 (2011): 113 reproduced by permission of the AASRights
© 2011. The American Astronomical Society.Abstract
We present a deep Spitzer/Infrared Array Camera (IRAC) survey of the OB association IC 1795 carried out to investigate the evolution of protoplanetary disks in regions of massive star formation. Combining Spitzer/IRAC data with Chandra/Advanced CCD Imaging Spectrometer observations, we find 289 cluster members. An additional 340 sources with an infrared excess, but without X-ray counterpart, are classified as cluster member candidates. Both surveys are complete down to stellar masses of about 1 M⊙. We present pre-main-sequence isochrones computed for the first time in the Spitzer/IRAC colors. The age of the cluster, determined via the location of the Class III sources in the [3.6]-[4.5]/[3.6] color-magnitude diagram, is in the range of 3-5Myr. As theoretically expected, we do not find any systematic variation in the spatial distribution of disks within 0.6 pc of either O-type star in the association. However, the disk fraction in IC 1795 does depend on the stellar mass: sources with masses >2 M⊙ have a disk fraction of ∼ 20%, while lower mass objects (2-0.8 M⊙) have a disk fraction of ∼ 50%. This implies that disks around massive stars have a shorter dissipation timescale.
Files in this item
Google Scholar:Roccatagliata, Veronica
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Bouwman, Jeroen
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Henning, Th H E
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Gennaro, Mario
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Feigelson, Eric D.
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Jinyoung Serena, Kim
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Sicilia-Aguilar, Aurora
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Lawson, Warrick A.
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