THE FIRST HUNDRED BROWN DWARFS DISCOVERED BY THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE)
THE FIRST HUNDRED BROWN DWARFS DISCOVERED BY THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE)
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DOI：
10.1088/0067-0049/197/2/19
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发表时间：
2011-08
期刊：
影响因子：
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通讯作者：
J. Kirkpatrick;M. Cushing;C. Gelino;R. Griffith;M. Skrutskie;K. Marsh;E. Wright;A. Mainzer;
中科院分区：
文献类型：
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作者：
J. Kirkpatrick;M. Cushing;C. Gelino;R. Griffith;M. Skrutskie;K. Marsh;E. Wright;A. Mainzer;
我们提出了6 Y矮星的地基光谱验证（另见库欣等人），89颗T型矮星，8颗L型矮星，1颗M型矮星被宽视场红外巡天探测器（WISE）确认。其中80是冷棕矮星的光谱类型T1 T6，其中6个已宣布由Mainzer等人。和Burgasser等人。我们提出的颜色，颜色和颜色类型图显示的轨迹的M，L，T，Y矮星在WISE颜色空间。近红外光谱，在少数情况下，光学光谱为这些发现。近红外分类晚至早Y和特殊光谱的对象进行了讨论。利用这些新发现，我们还能够将光学T矮星分类方案从T8扩展到T9。在推导出WISE 4.6 μm（W2）绝对星等与光谱类型的关系后，我们估计了我们发现的分光光度距离。我们还利用现有的天体测量数据为我们发现的四个天体提供了初步的三角测量结果，这些天体有L9 pec（红色）、T8、T9和Y 0类型;所有这些天体都位于太阳的10 pc范围内。Y 0矮星WISE 1541−2250距离太阳最近，为2.8+1.3−0.6 pc;如果持续监测后仍保持2.8 pc的数值，WISE 1541−2250将成为第七个距离太阳最近的恒星系统。另外10个物体，类型在T6和> Y 0之间，具有分光光度距离估计，也将它们放置在10 pc内。其中最接近的是T6矮行星WISE 1506+7027，据信其距离为2.49秒差距。WISE多历元位置补充了主要来自斯皮策/红外阵列相机的位置信息，使我们能够计算大约一半新发现的自行和切向速度。这项工作代表了WISE完成全天空，体积有限的晚T和Y矮星普查的第一步。利用这次普查的早期结果，我们提出了初步的，这些对象的空间密度的下限和讨论的质量函数的函数形式和低质量限制的星星形成的限制。
We present ground-based spectroscopic verification of 6 Y dwarfs (see also Cushing et al.), 89 T dwarfs, 8 L dwarfs, and 1 M dwarf identified by the Wide-field Infrared Survey Explorer (WISE). Eighty of these are cold brown dwarfs with spectral types ⩾T6, six of which have been announced earlier by Mainzer et al. and Burgasser et al. We present color–color and color–type diagrams showing the locus of M, L, T, and Y dwarfs in WISE color space. Near-infrared and, in a few cases, optical spectra are presented for these discoveries. Near-infrared classifications as late as early Y are presented and objects with peculiar spectra are discussed. Using these new discoveries, we are also able to extend the optical T dwarf classification scheme from T8 to T9. After deriving an absolute WISE 4.6 μm (W2) magnitude versus spectral type relation, we estimate spectrophotometric distances to our discoveries. We also use available astrometric measurements to provide preliminary trigonometric parallaxes to four of our discoveries, which have types of L9 pec (red), T8, T9, and Y0; all of these lie within 10 pc of the Sun. The Y0 dwarf, WISE 1541−2250, is the closest at 2.8+1.3−0.6 pc; if this 2.8 pc value persists after continued monitoring, WISE 1541−2250 will become the seventh closest stellar system to the Sun. Another 10 objects, with types between T6 and >Y0, have spectrophotometric distance estimates also placing them within 10 pc. The closest of these, the T6 dwarf WISE 1506+7027, is believed to fall at a distance of ∼4.9 pc. WISE multi-epoch positions supplemented with positional info primarily from the Spitzer/Infrared Array Camera allow us to calculate proper motions and tangential velocities for roughly one-half of the new discoveries. This work represents the first step by WISE to complete a full-sky, volume-limited census of late-T and Y dwarfs. Using early results from this census, we present preliminary, lower limits to the space density of these objects and discuss constraints on both the functional form of the mass function and the low-mass limit of star formation.