Optical Spectroscopy of the Surface Population of the rho Ophiuchi Molecular Cloud: The First Wave of Star Formation

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dc.creatorWilking, Bruce A.
dc.creatorMeyer, Michael R.
dc.creatorRobinson, John G.
dc.creatorGreene, Thomas P.
dc.date2005-06-10
dc.date.accessioned2026-07-07T11:24:28Z
dc.date.available2026-07-07T11:24:28Z
dc.descriptionWe present the results of optical spectroscopy of 139 stars obtained with the Hydra multi-object spectrograph. The objects extend over a 1.3 square degree area surrounding the main cloud of the rho Oph complex. The objects were selected from narrowband images to have H alpha in emission. Using the presence of strong H alpha emission, lithium absorption, location in the Hertzsprung-Russell diagram, or previously reported x-ray emission, we were able to identify 88 objects as young stars associated with the cloud. Strong H alpha emission was confirmed in 39 objects with line widths consistent with their origin in magnetospheric accretion columns. Two of the strongest emission-line objects are young, x-ray emitting brown dwarf candidates with M8 spectral types. Comparisons of the bolometric luminosities and effective temperatures with theoretical models suggest a medianage for this population of 2.1 Myr which is signifcantly older than the ages derived for objects in the cloud core. It appears that these stars formed contemporaneously with low mass stars in the Upper Scorpius subgroup, likely triggered by massive stars in the Upper-Centaurus subgroup.
dc.description35 pages of postscript which includes seven figures (some of which are multi-panel) and four postscript tables. Astronomical Journal (in press)
dc.identifierhttps://arxiv.org/abs/astro-ph/0506251
dc.identifierhttp://arxiv.org/abs/astro-ph/0506251
dc.identifierAstron.J.130:1733-1751,2005
dc.identifierdoi:10.1086/432758
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/195200
dc.subjectAstrophysics
dc.titleOptical Spectroscopy of the Surface Population of the rho Ophiuchi Molecular Cloud: The First Wave of Star Formation
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