Moraux, E. and Bouvier, J. and Stauffer, J. R. and Barrado y Navascués, D. and Cuillandre, J.-C. (2007) The lower mass function of the young open cluster Blanco 1: from 30 M_(Jup) to 3 M_☉. Astronomy and Astrophysics, 471 (2). pp. 499-513. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20100419-141213308
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Aims. We performed a deep wide field optical survey of the young (~100−150 Myr) open cluster Blanco 1 to study its low mass population well down into the brown dwarf regime and estimate its mass function over the whole cluster mass range. Methods. The survey covers 2.3 square degrees in the I and z-bands down to I ≃ z ≃ 24 with the CFH12K camera. Considering two different cluster ages (100 and 150 Myr), we selected cluster member candidates on the basis of their location in the (I, I − z) CMD relative to the isochrones, and estimated the contamination by foreground late-type field dwarfs using statistical arguments, infrared photometry and low-resolution optical spectroscopy. Results. We find that our survey should contain about 57% of the cluster members in the 0.03−0.6 M_☉ mass range, including 30–40 brown dwarfs. The candidate’s radial distribution presents evidence that mass segregation has already occured in the cluster. We took it into account to estimate the cluster mass function across the stellar/substellar boundary. We find that, between 0.03 M_☉ and 0.6 M_☉, the cluster mass distribution does not depend much on its exact age, and is well represented by a single power-law, with an index α = 0.69 ± 0.15. Over the whole mass domain, from 0.03 M_☉ to 3 M_☉, the mass function is better fitted by a log-normal function with m_0 = 0.36 ± 0.07 M_☉ and σ = 0.58 ± 0.06. Conclusions. Comparison between the Blanco 1 mass function, other young open clusters’ MF, and the galactic disc MF suggests that the IMF, from the substellar domain to the higher mass part, does not depend much on initial conditions. We discuss the implications of this result on theories developed to date to explain the origin of the mass distribution.
|Additional Information:||© 2007 ESO. Received 28 August 2006; accepted 7 June 2007. The authors thank Isabelle Baraffe who calculated the NEXTGEN and DUSTY models for the CFH12K filter set, as well as Sylvain Guieu for computing the isodensity contours. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.|
|Subject Keywords:||stars: low-mass, brown dwarfs; stars: luminosity function, mass function; Galaxy: open clusters and associations: individual: Blanco 1|
|Official Citation:||The lower mass function of the young open cluster Blanco 1: from 30 M_(Jup) to 3 M_☉ E. Moraux, J. Bouvier, J. R. Stauffer, D. Barrado y Navascués and J.-C. Cuillandre A&A 471 (2) 499-513 (2007) DOI: 10.1051/0004-6361:20066308|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||19 Apr 2010 22:47|
|Last Modified:||26 Dec 2012 11:58|
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