CONVERTING FROM 3.6 AND 4.5 μm FLUXES TO STELLAR MASS
CONVERTING FROM 3.6 AND 4.5 μm FLUXES TO STELLAR MASS
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DOI：
10.1088/0004-6256/143/6/139
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发表时间：
2012-06-01
影响因子：
5.3
通讯作者：
Meidt, Sharon
中科院分区：
文献类型：
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作者：
Eskew, Michael;Zaritsky, Dennis;Meidt, Sharon
我们利用大麦哲伦星云（LMC）的高空间分辨率恒星质量和红外通量图，校准了3.6和4.5 μ m通量与恒星质量（M ~* = 10）之间的转换F-3.6（2.85）F-4.5（-1.85）（D/0.05）（2）M圆点，其中通量以Jy为单位，D是到源的光度距离，以Mpc为单位，并提供分数内部不确定性的近似经验估计，M* 为0.3根N/10（6），其中N是该区域中的恒星数量。我们发现年轻恒星和热尘埃污染测量结果的证据，但尝试使用远优于未解析星系通常可用的数据的上级数据来消除这种污染，导致准确度略有提高。LMC中各区域的质量估计值之间的分散度与以前的研究人员在对复合种群建模时发现的分散度相当，因此我们得出结论，我们的简单转换对于目前可用的数据和模型来说是尽可能精确的。我们的研究结果允许一个合理的底部重的初始质量函数，如Salpeter或更重，并适度不赞成较轻的版本，如饮食Salpeter或Chabrier初始质量函数。
We use high spatial resolution maps of stellar mass and infrared flux of the Large Magellanic Cloud (LMC) to calibrate a conversion between 3.6 and 4.5 mu m fluxes and stellar mass, M-* = 10(5.65) F-3.6(2.85) F-4.5(-1.85) (D/0.05)(2) M-circle dot,where fluxes are in Jy and D is the luminosity distance to the source in Mpc, and to provide an approximate empirical estimate of the fractional internal uncertainty in M* of 0.3 root N/10(6), where N is the number of stars in the region. We find evidence that young stars and hot dust contaminate the measurements, but attempts to remove this contamination using data that are far superior to what are generally available for unresolved galaxies resulted in marginal gains in accuracy. The scatter among mass estimates for regions in the LMC is comparable to that found by previous investigators when modeling composite populations, and so we conclude that our simple conversion is as precise as possible for the data and models currently available. Our results allow for a reasonably bottom-heavy initial mass function, such as Salpeter or heavier, and moderately disfavor lighter versions such as a diet-Salpeter or Chabrier initial mass function.