基本造父变星Calif Zeta Gem主星系团的发现
Discovery of the Host Cluster for the Fundamental Cepheid Calibrator Zeta Gem
摘要：
新的和现有的CORAVEL，UBVJHKs，HST，HIP/Tycho，ARO，KPNO和DAO的观测表明，基本的造父变星校准器Zeta Gem是一个星团成员。以下参数是从星团成员关系中推断出的，并与为26颗附近恒星建立的新光谱分类（DAO）相关联（例如，HD53588/B7.5IV，HD54692/B9.5IV）：E（B-V）=0.02 ± 0.02，logt =7.85 ± 0.15，d=355 ± 15 pc.从集群成员到Zeta Gem的平均距离和六个最近的估计（例如，IRSB）为d=363+-9（se）+-26（sd）pc。这里给出的结果支持Benedict等人（2007）推导出的造父变星的颜色过剩和HST视差。即将到来的精确自行（DASCH）和钱德拉/XMM-牛顿观测更广泛的领域可以用来识别集群成员，支持集群的存在，并提供更强的约束造父变星的基本参数。
英文摘要：
New and existing CORAVEL, UBVJHKs, HST, HIP/Tycho, ARO, KPNO, and DAO observations imply that the fundamental Cepheid calibrator Zeta Gem is a cluster member. The following parameters were inferred for Zeta Gem from cluster membership and are tied to new spectral classifications (DAO) established for 26 nearby stars (e.g., HD53588/B7.5IV, HD54692/B9.5IV): E(B-V)=0.02+-0.02, log t=7.85+-0.15, and d=355+-15 pc. The mean distance to Zeta Gem from cluster membership and six recent estimates (e.g., IRSB) is d=363+-9(se)+-26(sd) pc. The results presented here support the color-excess and HST parallax derived for the Cepheid by Benedict et al. (2007). Forthcoming precise proper motions (DASCH) and Chandra/XMM-Newton observations of the broader field may be employed to identify cluster members, bolster the cluster's existence, and provide stronger constraints on the Cepheid's fundamental parameters.
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