3XMM J181923.7-170616: An X-Ray Binary with a 408 s Pulsar

doi:10.3847/1538-4357/aa8728

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	3XMM J181923.7-170616: An X-Ray Binary with a 408 s Pulsar
	Qiu, Hao 2; Zhou, Ping 1,2,3; Yu, Wenfei 4; Li, Xiangdong 1,2; Xu, Xiaojie 1,2
刊名	ASTROPHYSICAL JOURNAL
	2017-09-20
卷号	847 期号:1
关键词	Binaries: Symbiotic Stars: Individual (3xmm J181923.7-170616=swift J1819.2-1706) X-rays: Binaries
ISSN号	0004-637X
DOI	10.3847/1538-4357/aa8728
英文摘要	We carry out a dedicated study of 3XMM J181923.7-170616 with an approximate pulsation period of 400 s using the XMM-Newton and Swift observations spanning across nine years. We have refined the period of the source to 407.904(7) s (at epoch MJD 57142) and constrained the 1 sigma upper limit on the period derivative (P) over dot <= 1.1 x 10(-8)s s(-1). The source radiates hard, persistent X-ray emission during the observation epochs, which is best described by an absorbed power-law model (Gamma similar to 0.2-0.8) plus faint Fe lines at 6.4 and 6.7 keV. The X-ray flux revealed a variation within a factor of 2, along with a spectral hardening as the flux increased. The pulse shape is sinusoid-like and the spectral properties of different phases do not present significant variation. The absorption N-H (similar to 1.3 x 10(22) cm(-2)) is similar to the total Galactic hydrogen column density along the direction, indicating that it is a distant source. A search for the counterpart in optical and near-infrared surveys reveals a low-mass K-type giant, while the existence of a Galactic OB supergiant is excluded. A symbiotic X-ray binary (SyXB) is the favored nature of 3XMM. J181923.7-170616 and can essentially explain the low luminosity of 2.78 x 10(34)d(10)(2) erg s(-1), slow pulsation, hard X-ray spectrum, and possible K3 III companion. An alternative explanation of the source is a persistent Be X-ray binary (BeXB) with a companion star no earlier than B3-type.
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	IOP PUBLISHING LTD
WOS记录号	WOS:000411341100020
内容类型	期刊论文
源URL	[http://119.78.226.72/handle/331011/32571]
专题	中国科学院上海天文台
通讯作者	Zhou, Ping
作者单位	1.Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing, Jiangsu, Peoples R China 2.Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Jiangsu, Peoples R China 3.Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands 4.Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, 80 Nandan Rd, Shanghai 200030, Peoples R China
推荐引用方式 GB/T 7714	Qiu, Hao,Zhou, Ping,Yu, Wenfei,et al. 3XMM J181923.7-170616: An X-Ray Binary with a 408 s Pulsar[J]. ASTROPHYSICAL JOURNAL,2017,847(1).
APA	Qiu, Hao,Zhou, Ping,Yu, Wenfei,Li, Xiangdong,&Xu, Xiaojie.(2017).3XMM J181923.7-170616: An X-Ray Binary with a 408 s Pulsar.ASTROPHYSICAL JOURNAL,847(1).
MLA	Qiu, Hao,et al."3XMM J181923.7-170616: An X-Ray Binary with a 408 s Pulsar".ASTROPHYSICAL JOURNAL 847.1(2017).