我们的目的是测量与高质量X射线脉冲双星EXO 1722 -363发生食时的超巨星伴星的径向速度曲线，从而确定其组成部分的恒星质量。我们使用了一组档案K $_{\rm s}$波段红外光谱的对应EXO 1722 -363获得使用ISAAC的VLT，并互相关，以测量径向速度的恒星。由此产生的径向速度曲线的半振幅为$24.5 \pm 5.0$ km s $^{-1}$。当结合系统的其他测量参数时，这产生的质量范围为1.5 $\pm$ 0.4 - 1.6 $\pm$ 0.4 M $_{\odot}$（对于中子星）和13.6 $\pm$ 1.6 - 15.2 $\pm$ 1.9 M $_{\odot}$（对于B 0 - 1 Ia超巨星伴星）。这些下限和上限分别是在假设系统从侧面观察（i = 90 $^\circ$）和超巨星充满罗氏瓣（$β= 1$）的情况下得到的。系统倾角被限制为$i>75^{\circ}$，超巨星的罗氏瓣填充因子为$β>0.9$。此外，我们能够进一步限制我们的距离确定为7.1 $\le$ d $\le$ 7.9 kpc的EXO 1722 -363。该距离范围的X射线光度为4.7 $\times$ 10 $^{35}$ $\le$ L $_{\rm X}$ $\le$ 9.2 $\times$ 10 $^{36}$ erg s $^{-1}$。EXO 1722 -363因此成为十个已知的食X射线双星中的第七个，其中一个动态中子星质量解已经确定。此外，EXO 1722 -363是第一个利用近红外光谱测量中子星质量的系统。
英文摘要：
We intended to measure the radial velocity curve of the supergiant companion to the eclipsing high mass X-ray binary pulsar EXO1722-363 and hence determine the stellar masses of the components.
We used a set of archival K$_{\rm s}$-band infrared spectra of the counterpart to EXO1722-363 obtained using ISAAC on the VLT, and cross-correlated them in order to measure the radial velocity of the star.
The resulting radial velocity curve has a semi-amplitude of $24.5 \pm 5.0$ km s$^{-1}$. When combined with other measured parameters of the system, this yields masses in the range 1.5 $\pm$ 0.4 - 1.6 $\pm$ 0.4 M$_{\odot}$ for the neutron star and 13.6 $\pm$ 1.6 - 15.2 $\pm$ 1.9 M$_{\odot}$ for the B0--1 Ia supergiant companion. These lower and upper limits were obtained under the assumption that the system is viewed edge-on (i = 90$^\circ$) for the lower limit and the supergiant fills its Roche lobe ($β= 1$) for the upper limit respectively. The system inclination is constrained to $i>75^{\circ}$ and the Roche lobe-filling factor of the supergiant is $β>0.9$. Additionally we were able to further constrain our distance determination to be 7.1 $\le$ d $\le$ 7.9 kpc for EXO1722-363. The X-ray luminosity for this distance range is 4.7 $\times$ 10$^{35}$ $\le$ L$_{\rm X}$ $\le$ 9.2 $\times$ 10$^{36}$ erg s$^{-1}$.
EXO1722-363 therefore becomes the seventh of the ten known eclipsing X-ray binary pulsars for which a dynamical neutron star mass solution has been determined. Additionally EXO1722-363 is the first such system to have a neutron star mass measurement made utilising near-infrared spectroscopy.
CoronaGraph Instrument Reference stars for Exoplanets (CorGI-REx) I. Preliminary Vetting and Implications for the Roman Coronagraph and Habitable Worlds Observatory
University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）；NASA Ames Research Center（美国国家航空航天局艾姆斯研究中心）；Bay Area Environmental Research Institute（湾区环境研究所）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Cornell University（康奈尔大学）；University of Edinburgh（爱丁堡大学）；University of Notre Dame（圣母大学）；National Astronomical Observatory of Japan（日本国立天文台）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Northwestern University（西北大学）；European Southern Observatory（欧洲南方天文台）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
The Decline and Fall of ROME. V. A Preliminary Search for Star-Disrupted Planet Interactions and Coronal Activity at 5 GHz Among White Dwarfs within 25 pc
