SPECTROSCOPIC FOLLOW-UP OF X-RAY SOURCES IN THE ChaMPlane SURVEY: IDENTIFICATION OF A NEW CATACLYSMIC VARIABLE
SPECTROSCOPIC FOLLOW-UP OF X-RAY SOURCES IN THE ChaMPlane SURVEY: IDENTIFICATION OF A NEW CATACLYSMIC VARIABLE
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Champlane 调查中 X 射线源的光谱跟踪：新灾难变量的识别
DOI：
10.1088/0004-637x/748/1/32
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
B. Allen
中科院分区：
文献类型：
--
作者：
M. Servillat;J. Grindlay;M. van den Berg;J. Hong;P. Zhao;B. Allen
本文介绍了钱德拉多波长平面巡天（ChaMPlane）的一部分--沿银道面（l = 327.°42，B = 2.°26）沿着区域X射线源的多目标光谱跟踪研究。我们获得了46颗恒星的光谱，其中包括15颗可能与X射线源对应的恒星，以及显示Hα色过剩的恒星。这导致了一个新的激变变星（CV）的发现，CXOPS J154305.5-522709，也被命名为ChaMPlane Bright Source 7（CBS 7），我们在该区域发现了8个活跃的晚型恒星。CBS 7的X射线光谱具有硬谱和两个周期：1.22 ± 0.08小时和2.43 ± 0.26小时。本文通过对它的光谱中H、He i和He ii发射线的探测，给出了它是CV源的明确证据。硬X射线谱和He ii λ4686的存在表明它具有磁性CV。近红外对应物是显著可变的，并且我们发现与最长X射线周期一致的周期为2.39 ± 0.05小时，但不是最短X射线周期。如果这个周期是轨道周期，这将使系统处于CV周期间隙中。可能的轨道周期表明它有一颗dM 4 ± 1的伴星星星。因此，距离估计为10.1 kpc。该系统可以是一个相对硬和X射线发光的极性或中间极性，可能几乎同步。
We present a multi-object optical spectroscopy follow-up study of X-ray sources in a field along the Galactic plane (l = 327.°42, b = 2.°26) which is part of the Chandra Multi-wavelength Plane survey (ChaMPlane). We obtained spectra for 46 stars, including 15 likely counterparts to X-ray sources, and sources showing an Hα color excess. This has led to the identification of a new cataclysmic variable (CV), CXOPS J154305.5-522709, also named ChaMPlane Bright Source 7 (CBS 7), and we identified eight X-ray sources in the field as active late-type stars. CBS 7 was previously studied in X-rays and showed a hard spectrum and two periods: 1.22 ± 0.08 hr and 2.43 ± 0.26 hr. We present here clear evidence that the source is a CV through the detection of H, He i, and He ii emission lines in its optical spectrum. The hard X-ray spectrum and the presence of the He ii λ4686 in emission with a large equivalent width suggest a magnetic CV. The near-infrared counterpart is significantly variable, and we found a period consistent with the longest X-ray period at 2.39 ± 0.05 hr but not the shortest X-ray period. If this period is the orbital period, this would place the system in the CV period gap. The possible orbital period suggests a dM4 ± 1 companion star. The distance is then estimated to be ∼1 kpc. The system could be a relatively hard and X-ray luminous polar or an intermediate polar, possibly nearly synchronous.