The initial mass function in the Taurus star-forming region

被引:296
作者
Briceño, C
Luhman, KL
Hartmann, L
Stauffer, JR
Kirkpatrick, JD
机构
[1] Ctr Invest Astron, Merida 5101A, Venezuela
[2] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[3] CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA
[4] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA
关键词
infrared : stars; stars : evolution; stars : formation; stars; low-mass; brown dwarfs; stars : luminosity function; mass function; stars : pre-main-sequence;
D O I
10.1086/343127
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
By combining a deep optical imaging (I, z') survey of 8 deg(2) in the Taurus star-forming region with data from the Two-Micron All-Sky Survey (2MASS) and follow-up spectroscopy, we have performed a search for low-mass Taurus members that is complete to 0.02M. for reddenings of A(V) less than or similar to 4. We report the discovery of nine new members with spectral types of M5.75-M9.5, corresponding to masses of 0.1-0.015 M. by recent evolutionary models. The new M9.5 member is the least massive brown dwarf found to date in the Taurus star-forming region. We derive an initial mass function (IMF) for the fields surveyed in this work and in our previous studies, which encompass 54% of the known Taurus membership. We compare the Taurus IMF with a similarly derived one for the Trapezium Cluster and to mass functions for the M35 and Pleiades open clusters. While the IMFs in all of these regions flatten near similar to0.8M., the mass function in Taurus is more narrow and sharply peaked at this mass. Our survey indicates that Taurus has similar to2 x fewer brown dwarfs at 0.02-0.08 M. than the Trapezium. We discuss the implications of these results for theories of the IMF, and suggest that the lower frequency of brown dwarfs in Taurus relative to the Trapezium may result from the low-density star-forming environment, leading to larger minimum Jeans masses.
引用
收藏
页码:317 / 335
页数:19
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