Tycho2星表中恒星的全天光谱匹配的UBVRI-ZY和u 'g' r 'i'z'星等
All-Sky spectrally matched UBVRI-ZY and u'g'r'i'z' magnitudes for stars in the Tycho2 catalog
摘要：
我们提出了拟合UBVRI-ZY和u 'g' r 'i'z'星等，光谱类型和距离的2.4M恒星，来自合成测光库光谱，最好的匹配Tycho 2 BtVt，NOMAD Rn和2 MASS JHK_{2/S}目录的星等。我们提出了类似的合成多滤波器的星等，类型和距离的4.8米的恒星与2 MASS和SDSS测光g<16的斯隆调查区域内，兰道尔特和斯隆的主要标准，以及斯隆北方（PT）和南方的二级标准。BtVt、UBVRI、ZvYv、JHK_{2/S}、JHK_{MKO}、Stromgren uvby、Sloan u 'g' r 'i'z'和ugriz的合成幅度零点在20个calspec分光光度标准上校准。对于覆盖-0.3 < V-I < 4.6的颜色范围的标准品，UBVRI和ugriz零点的分散度为1- 3%;对于其他滤光片，其分散度在2- 5%范围内。对Tycho 2星的光谱匹配拟合，在UBVRI或u 'g' r 'i' z '中，估计每星的1-sigma误差分别为~0.2，0.15，0.12，0.10和0.08 mags;对于至少70%的SDSS调查区域，g<16，在u 'g' r 'i'z'或UBVRI中，估计每星的1-sigma误差约为0.2，0.06，0.04，0.04，0.05。Tycho 2恒星的密度平均为每平方度60颗恒星，提供了足够的恒星，使大多数视场为0.5度或更大的数字图像能够自动进行通量校准。每个视场使用几个这样的标准，在任何滤光器、任何气团、大多数可行的观测条件下，自动通量校准可以达到百分之几，以便于对来自不同地点、望远镜和仪器的数据进行相互比较。
英文摘要：
We present fitted UBVRI-ZY and u'g'r'i'z' magnitudes, spectral types and distances for 2.4M stars, derived from synthetic photometry of a library spectrum that best matches the Tycho2 BtVt, NOMAD Rn and 2MASS JHK_{2/S} catalog magnitudes. We present similarly synthesized multi-filter magnitudes, types and distances for 4.8M stars with 2MASS and SDSS photometry to g<16 within the Sloan survey region, for Landolt and Sloan primary standards, and for Sloan Northern (PT) and Southern secondary standards. The synthetic magnitude zeropoints for BtVt, UBVRI, ZvYv, JHK_{2/S}, JHK_{MKO}, Stromgren uvby, Sloan u'g'r'i'z' and ugriz are calibrated on 20 calspec spectrophotometric standards. The UBVRI and ugriz zeropoints have dispersions of 1--3%, for standards covering a range of color from -0.3 < V-I < 4.6; those for other filters are in the range 2--5%. The spectrally matched fits to Tycho2 stars provide estimated 1-sigma errors per star of ~0.2, 0.15, 0.12, 0.10 and 0.08 mags respectively in either UBVRI or u'g'r'i'z'; those for at least 70% of the SDSS survey region to g<16 have estimated 1-sigma errors per star of ~0.2, 0.06, 0.04, 0.04, 0.05 in u'g'r'i'z' or UBVRI. The density of Tycho2 stars, averaging about 60 stars per square degree, provides sufficient stars to enable automatic flux calibrations for most digital images with fields of view of 0.5 degree or more. Using several such standards per field, automatic flux calibration can be achieved to a few percent in any filter, at any airmass, in most workable observing conditions, to facilitate inter-comparison of data from different sites, telescopes and instruments.
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