SPECTRAL ENERGY DISTRIBUTION AND BOLOMETRIC LUMINOSITY OF THE COOL BROWN DWARF GLIESE 229B
SPECTRAL ENERGY DISTRIBUTION AND BOLOMETRIC LUMINOSITY OF THE COOL BROWN DWARF GLIESE 229B
复制标题
冷棕矮星 Gliese 229B 的光谱能量分布和辐射光度
DOI：
--
复制
发表时间：
1996
期刊：
影响因子：
--
通讯作者：
B. Oppenheimer
中科院分区：
文献类型：
--
作者：
K. Matthews;T. Nakajima;S. Kulkarni;B. Oppenheimer
报道了波长从0.8微米到10.5微米的凉爽棕矮星Gliese229B的红外宽带测光。这些结果是从新数据和重新分析的先前发布的数据中得出的。已报道的现有光谱数据已被重新推导和重新校准。明亮的Gliese229A离暗淡的Gliese229B很近，需要使用特殊的技术进行观测和数据分析。我们对这些步骤进行了详细描述。在0.8到10.5微米之间观测到的光度为(4.9+/-0.6)×10(exp-6)太阳光度。观测到的光谱能量分布与Tsuji等人的无尘模型光谱总体上是一致的。对于T(Ef)约为等于900K，如果用这个模型来推导辐射热校正值，则测辐射光度的最佳估计值是6.4×10(exp-6)太阳光度，其中50%的光度在1到2.5微米之间。我们对有效温度的最佳估计是900K，根据观测到的近红外光谱和光谱能量分布，估计了亮度温度(T(B))。最高的T(亚B)=1640K位于J带光谱的峰值，而最低的T(亚B)小于或等于600K，在3.4微米处，对应于基本甲烷带的位置。
Infrared broadband photometry of the cool brown dwarf Gliese 229B extending in wavelength from 0.8 to 10.5 micron is reported. These results are derived from both new data and reanalyzed, previously published data. Existing spectral data reported have been rereduced and recalibrated. The close proximity of the bright Gliese 229A to the dim Gliese 229B required the use of special techniques for the observations and also for the data analysis. We describe these procedures in detail. The observed luminosity between 0.8 and 10.5 micron is (4.9 +/- 0.6) x 10(exp -6) solar luminosity. The observed spectral energy distribution is in overall agreement with a dust-free model spectrum by Tsuji et al. for T(eff) approx. equal to 900 K. If this model is used to derive the bolometric correction, the best estimate of the bolometric luminosity is 6.4 x 10(exp -6) solar luminosity and 50% of this luminosity ties between 1 and 2.5 microns. Our best estimate of the effective temperature is 900 K. From the observed near-infrared spectrum and the spectral energy distribution, the brightness temperatures (T(sub B) are estimated. The highest, T(sub B) = 1640 K, is seen at the peak of the J band spectrum, while the lowest, T(sub B) is less than or equal to 600 K, is at 3.4 microns, which corresponds to the location of the fundamental methane band.