2 MASS、SDSS和BVRI测光系统之间的转换：桥接近红外和光学
Transformations between 2MASS, SDSS and BVRI photometric systems: bridging the near infrared and optical
摘要：
我们提出的颜色转换转换的{ \em 2 MASS}测光系统的约翰逊-费因斯$UBVRI$系统，并进一步到{ \em SDSS} $ugriz$系统。我们从$SDSS$数据发布5（DR 5）中获取了用2.5米望远镜测量的恒星的{ \em SDSS} $gri$星等，并分别从Stetson星表和\citet{Cu03}中获取了$BVRI$和$JHK_{s}$星等。我们通过坐标匹配了三个测光系统中的数千颗恒星，并通过以下约束获得了825颗恒星的均匀样本，这些约束在以前的转换中没有使用：1）数据被去红化，2）忽略巨星，3）选择的样本恒星质量最高。我们给金属丰度，人口类型，和转换依赖于两种颜色。这些变换提供了绝对星等和距离测定，可用于短距离的空间密度估算，其中部分或全部{ \em SDSS} $ugriz$星等饱和。将这些密度与使用{ \em SDSS} $ugriz$测光法在更远距离上评估的密度相结合，将提供精确的银河模型参数，特别是每个种群的局部空间密度。
英文摘要：
We present colour transformations for the conversion of the {\em 2MASS} photometric system to the Johnson-Cousins $UBVRI$ system and further into the {\em SDSS} $ugriz$ system. We have taken {\em SDSS} $gri$ magnitudes of stars measured with the 2.5-m telescope from $SDSS$ Data Release 5 (DR5), and $BVRI$ and $JHK_{s}$ magnitudes from Stetson's catalogue and \citet{Cu03}, respectively. We matched thousands of stars in the three photometric systems by their coordinates and obtained a homogeneous sample of 825 stars by the following constraints, which are not used in previous transformations: 1) the data are de-reddened, 2) giants are omitted, and 3) the sample stars selected are of the highest quality. We give metallicity, population type, and transformations dependent on two colours. The transformations provide absolute magnitude and distance determinations which can be used in space density evaluations at short distances where some or all of the {\em SDSS} $ugriz$ magnitudes are saturated. The combination of these densities with those evaluated at larger distances using {\em SDSS} $ugriz$ photometry will supply accurate Galactic model parameters, particularly the local space densities for each population.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
