Chandra Multiwavelength Plane (ChaMPlane) Survey: An Introduction
Chandra Multiwavelength Plane (ChaMPlane) Survey: An Introduction
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钱德拉多波长平面 (ChaMPlane) 巡天：简介
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发表时间：
2005
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通讯作者：
A. Rogel
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作者：
J. Grindlay;Jaesub Hong;P. Zhao;Silas Laycock;M. V. D. Berg;X. Koenig;E. M. Schlegel;H. Cohn;P. Lugger;A. Rogel
我们介绍了钱德拉多波长平面 (ChaMPlane) 巡天，旨在测量或限制在银道面和核球中吸积白矮星、中子星和恒星质量黑洞的低光度 (LX ≳ 1031 ergs s-1) 种群。 ChaMPlane 包含两项调查：X 射线（钱德拉）和光学（NOAO 4 m 马赛克成像），以及后续光谱和红外识别程序。该调查现已扩展到 Chandra 数据的前 6 年，使用在 154 个指向中观察到的 105 个不同 ACIS-I 和 ACIS-S 场中检测到的偶然来源，并由 V、R、I 和 Hα 中的 65 个深度马赛克图像覆盖。 ChaMPlane 包含银河纬度 ≲ 12° 的场，并选择没有亮点或漫射源，曝光时间 ≳20 ks 和（如果可能）最小 NH。我们描述科学目标并介绍 X 射线和光学/红外处理和数据库。我们从银河系反中心 14 个场的 X 射线/光学数据中得出了对灾难变量 (CV) 的空间密度或光度函数的初步约束。这些反中心场中缺乏 ChaMPlane CV，表明它们的空间密度比之前 X 射线巡天发现的太阳邻域值 (3 × 10-5 pc-3) 低约 3 倍。配套论文详细描述了 X 射线和光学处理、选定反中心场中 ChaMPlane 源的光谱以及银河系中心场的红外成像结果。附录介绍了 ChaMPlane 虚拟天文台 (VO)，用于在线访问 X 射线和光学图像以及源目录，以便随时显示和进一步分析。
We introduce the Chandra Multiwavelength Plane (ChaMPlane) survey, designed to measure or constrain the populations of low-luminosity (LX ≳ 1031 ergs s-1) accreting white dwarfs, neutron stars, and stellar mass black holes in the Galactic plane and bulge. ChaMPlane incorporates two surveys, X-ray (Chandra) and optical (NOAO 4 m Mosaic imaging), and a follow-up spectroscopy and IR identification program. The survey has now extended through the first 6 yr of Chandra data using serendipitous sources detected in 105 distinct ACIS-I and ACIS-S fields observed in 154 pointings and covered by 65 deep Mosaic images in V, R, I, and Hα. ChaMPlane incorporates fields with Galactic latitude ≲ 12° and selected to be devoid of bright point or diffuse sources, with exposure time ≳20 ks and (where possible) minimum NH. We describe the scientific goals and introduce the X-ray and optical/IR processing and databases. We derive preliminary constraints on the space density or luminosity function of cataclysmic variables (CVs) from the X-ray/optical data for 14 fields in the Galactic anticenter. The lack of ChaMPlane CVs in these anticenter fields suggests that their space density is ~3 times below the value (3 × 10-5 pc-3) found for the solar neighborhood by previous X-ray surveys. Companion papers describe the X-ray and optical processing in detail, optical spectroscopy of ChaMPlane sources in selected anticenter fields, and IR imaging results for the Galactic center field. An appendix introduces the ChaMPlane Virtual Observatory (VO) for online access to the X-ray and optical images and source catalogs for ready display and further analysis.