By Rafael Rebolo, Maria Rosa Zapatero-Osorio, Editors
Here's a state of the art overview of our present wisdom of brown dwarfs and extremely low-mass stars. the quest for, and learn of, those elusive gadgets is at the moment essentially the most dynamic components of analysis in astronomy. This quantity provides evaluation articles from a staff of overseas experts who examine the striking growth during this box some time past few years. The contributed chapters overview either the newest observations and theories, making this an important connection with probably the most interesting fields in modern astronomy.
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Additional resources for Very Low-Mass Stars and Brown Dwarfs (Cambridge Contemporary Astrophysics)
However, such surveys only cover the cluster centre and are probably not representative of the cluster as a whole. Our data, by constrast, covers most of the effective area of the cluster. In addition, there is uncertainty in the distance and age of the cluster. 32 from Hipparcos data, while Basri et al. (1996) discuss the age problem. 1M© the IMF is critically dependent on the gradient of the ML function; hence any turn-over seen at these masses should be treated with caution. 26 N. C. Hambly: Proper motions of VLM Stars and BDs m/M 0 5.
We did not observe Li I 6708A at sufficient resolution to detect its presence in these stars. In any event, lithium could not have been used to distinguish a star from a brown dwarf as has been done for Calar 1 (Basri 1997) and others because at the estimated cluster age of 2 Myr, all stellar objects have lithium. Lithium was not a useful criterion for distinguishing cluster members from older background members of the Orion OB association either because all stellar objects are thought to possess lithium at the age of the oldest stars in the Orion OB association.
Steele, Jameson & Hambly 1993; Zapatero-Osorio, Martin & Rebolo 1997a). Such data were obtained for these candidates, and we produced a mass function for the cluster that, for the first time, samples a mass bin within the substellar regime to an easily quantifiable degree of completeness. 1. 875, ie. a conservative cut in the I, (R-I) colour-magnitude diagram to include all possible members, while at the same time minimising the non-member contamination. All images were required to be present on at least six I plates; images not present in the R stack (which reaches R ~ 21) were included as possible members with assumed large (R-I).
Very Low-Mass Stars and Brown Dwarfs (Cambridge Contemporary Astrophysics) by Rafael Rebolo, Maria Rosa Zapatero-Osorio, Editors