A Common Proper Motion Companion to the Exoplanet Host 51 Pegasi
J. Greaves
系外行星飞马座51有一颗距离很远的红矮星伴星。另外两颗更遥远的恒星也与这颗恒星共同运动，这表明它们至少由于共同的起源而处于共同的银河系轨道上。
The exoplanet host 51 Pegasi has a widely separated red dwarf companion. Two other, far more distant, stars are also co-moving with this star, showing that they are at least of common Galactic orbit due to a common origin.
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In this work, the photometric data from the American Association of Variable Star Observers are collected and analyzed on the SX Phoenicis star DY Pegasi (DY Peg). From the frequency analysis, we get three independent frequencies: $f_0 = 13.71249\ \rm{c\ days^{-1}}$, $f_1 = 17.7000\ \rm{c\ days^{-1}}$, and $f_2 =18.138\ \rm{c\ days^{-1}}$, in which $f_0$ and $f_1$ are the radial fundamental and first overtone mode, respectively, while $f_2$ is detected for the first time and should belong to a nonradial mode. The $O-C$ diagram of the times of maximum light shows that DY Peg has a period change…
New analysis on the period changes of Type II Cepheid AU Peg is presented. The available recent photometric measurements were collected and analysed with various methods. The period has been found to be constant for certain time intervals, although increasing in overall, in contrast with the previous expectations, which suggested the period change to reverse. Superimposed on overall period change, a formerly unknown periodic behaviour has been found in the $O-C$ diagram of AU Peg, which cannot be matched to the radial velocity variations. Since the Cepheid is a member of a binary system, it is…
The planet-hosting subdwarf B star V391 Pegasi is a hybrid pulsator
一部分明显的亚矮星B星表现出短周期（p模式）或长周期（g模式）的光度变化，其中两个物体迄今为止已知表现出混合行为，即同时显示两种类型的模式。脉动次矮星B星飞马座V391（或HS 2201 +2610），靠近log g-Teff平面中的两个已知的混合双星，最近被发现拥有一颗行星伴星。为了更多地了解行星伴星及其对主星演化的可能影响（亚矮星B的形成仍然没有很好的理解），需要对主星进行准确的描述。作为正在进行的努力，以显着改善的宿主星的星震特性的一部分，我们调查的低频行为的HS 2201 +2610。我们在2 m级望远镜上获得了快速的高信噪比测光CCD（B滤光片）和PMT（透明滤光片）数据，并对光变曲线进行了仔细的频率分析。除了已知的342 s-367 s范围内的短周期光度变化外，我们还发现了一个周期为54 min，振幅为0.15%的长周期变化，这最有可能被确认为g模式脉动，因此HS 2201 +2610是混合sdB振荡器名单上的一个新成员。除了先前已知的脉动次矮星B星HS 0702 +6043和表现出混合行为的超新星090100001外，新的混合恒星HS 2201 +2610是这个类别的第三个成员。HS 2201 +2610的这一重要性质可以更好地描述这颗行星宿主恒星，也有助于描述它的行星伴侣。目前的脉动模型还不能特别好地再现混合sdBV星，为此目的改进的脉动模型必须包括混合行为。
Rediscussion of Eclipsing Binaries. Paper XXX. The Slightly Evolved F-type System BK Pegasi
研究BK天琴座双星系统，利用TESS光变曲线和光谱数据精确测定其质量与半径，发现其与理论模型相符，年龄约2.65亿年。
An Outer Giant Planet or Brown Dwarf in the 51 Pegasi System?
研究通过径向速度、绝对视差和高对比度成像数据，探讨51 鹭星系外伴星的质量和轨道距离，发现可能的超木星或棕矮星，但质疑长期信号的真实性。
Rediscussion of eclipsing binaries. Paper XVIII. The F-type system OO Pegasi
本文基于TESS光变曲线和已发表光谱数据重新分析分离食双星OO Peg，测定两子星质量与半径，发现主星更热更大更亮但质量略低，并给出与Gaia DR3一致的距离，未探测到脉动。
IK Pegasi and the Double-merger Path to Type Ia Supernovae
IK佩加西型系统通过双合并路径揭示II型Ia超新星的中间阶段，利用s过程富集识别白矮星的形成机制。
On the Nature of the Purported Common Proper Motion Companions to the Exoplanet Host Star 51 Peg
Greaves（2006）提出，在51 Peg（NLTT 54007、54064和55547）的10度范围内，有三颗红色的高自行恒星是这颗著名的系外行星的伴星。虽然这两颗恒星的自行与51 Peg相似，但它们的运动学视差产生了极不一致的色星等位置，比主序低2到4等。这三颗恒星都可能是背景恒星，与51 Peg无关。
Context. Spectroscopy of exoplanet atmospheres at high resolving powers is rapidly gaining popularity to measure the presence of atomic and molecular species. While this technique is robust against contaminant absorption in the Earth's atmosphere, the non stationary stellar spectrum creates a non-negligible source of noise that can alter or even prevent detection. Aims. We aim at using three-dimensional stellar simulations to directly remove the signature of the star from observations, and prior to cross correlation with templates for the planet's atmosphere Methods. We compute synthetic spect…
Know The Star, Know the Planet. IV. A Stellar Companion to the Host star of the Eccentric Exoplanet HD 8673b
HD 8673拥有一颗大质量的系外行星，其轨道高度偏心（e=0.723）。基于两个时代的斑点干涉测量，以前的出版物确定了一个候选的恒星伴侣。我们用10米凯克II望远镜、5米黑尔望远镜、3.63米AEOS望远镜和1.5米帕洛马望远镜在各种滤光器中多次观测HD 8673，目的是确认和表征恒星伴星。我们没有探测到候选伴星，我们现在得出结论，这是一个错误的探测，但我们确实探测到了一个更暗的伴星。我们收集了天体测量和测光的同伴在六个时代在各种过滤器。测量的差示测光使我们能够确定伴星是一颗早期M矮星，质量估计为0.33-0.45 M？。伴星的预计距离为10天文单位，这是系外行星主双星系统中最小的预计距离之一。基于有限的天体测量收集，我们能够约束的轨道的恒星同伴的半长轴为35{60 AU，偏心率？0.5以及75{85？}的倾角。这颗恒星伴星可能强烈影响了系外行星的轨道，很可能解释了它的高偏心率。
The Mass of the Candidate Exoplanet Companion to HD136118 from Hubble Space Telescope Astrometry and High-Precision Radial Velocities
我们使用哈勃空间望远镜精细制导传感器天体测量和来自HET的HD 136118的高节奏径向速度以及Lick的存档数据来确定HD 136118 b的完整轨道参数。我们发现候选系外行星的轨道倾角为i_{b} = 163.1 +- 3.0度。这确定了物体的实际质量，M_{b} = 42^{+11}-{-18} MJup，而仅根据径向速度数据确定的最小质量M_{b} sin{i} ~ 12 MJup。因此，HD 136118的低质量伴星现在被确定为可能居住在“棕矮星沙漠”中的棕矮星。
Red Asymmetry of H$_α$ Line Profiles during the flares on the active RS CVn-type star II Pegasi
本文通过对 RS CVn 型恒星飞马座 II 的高分辨率光谱观测，在两次耀斑期间发现 H$_α$ 线红不对称性及高速红移发射成分，推断其可能对应一次日珥爆发并发展为 CME，同时估算了 CME 的质量和动能。
We calculate the dynamical tides raised by a close planetary companion on non-rotating stars of $1$ $\text{M}_{\odot}$ and $1.4$ $\text{M}_{\odot}$. Using the Henyey method, we solve the fully non-adiabatic equations throughout the star. The horizontal Lagrangian displacement is found to be 10 to 100 times larger than the equilibrium tide value in a thin region near the surface of the star. This is because non--adiabatic effects dominate in a region that extends from below the outer edge of the convection zone up to the stellar surface, and the equilibrium tide approximation is inconsistent wi…
The extreme contrast ratios between stars and their planets at optical wavelengths make it challenging to isolate the light reflected by exoplanet atmospheres. Yet, these reflective properties reveal key processes occurring in the atmospheres, and they also span wavelengths that include the potential O$_2$ biosignature. High resolution cross-correlation spectroscopy (HRCCS) offers a robust avenue for developing techniques to extract exoplanet reflection spectra. We aimed to extract the optical reflected light spectrum of the non-transiting hot Jupiter 51 Peg b by adapting techniques designed t…
The Origin of the Exoplanets
我们探索行星质量的物体形成的两种方式。一个是在像太阳系这样的圆盘系统中。另一个是在恒星和褐矮星形成的密集星团中。我们还没有仪器的精确度来探测像太阳系那样质量的多行星系统;用我们目前的技术从遥远的地方，只能探测到木星的影响。我们表明，恒星，褐矮星，太阳系外行星同伴的太阳型恒星的轨道特性（偏心率和半长轴）是在我们的测量精度都是相同的，是非常不同的比太阳系中的行星。多行星系统中的周期比并不能区分这两种模型。我们得出的结论是，迄今为止发现的大部分系外行星都是像恒星同伴一样形成的，而不是像太阳系这样的圆盘系统。这一结论解释了为什么贫金属恒星没有行星：因为贫金属恒星缺乏周期短的伴星。对于[Fe/H]< -0.3的主星，系外行星周期的分布符合贫金属恒星的伴星的分布，而不是富金属恒星的伴星。
Detectability of Exoplanets in the Beta Pic Moving Group with the Gemini Planet Imager
我们使用双子座行星成像仪（GPI），一种旨在通过成像检测同伴的日冕仪，对Beta Pic移动群（BPMG）中恒星周围系外行星的可探测性进行了建模。BPMG的成员被认为是系外行星搜索的有希望的目标，因为他们的年轻（~12 MY）和接近（中位数距离~35 pc）。我们编写了一个建模程序来生成给定质量、年龄、偏心率和半长轴的假设同伴，并将它们放置在GPI V波段范围内的BPMG成员周围。我们计数作为可能的检测同伴躺在GPI的视野和H-波段通量，有一个主机伴侣通量比将它们放置在其灵敏度。能够被探测到的伴星的比例取决于它们在1200万年前的亮度，以及它们的形成机制，以及它们的半长轴分布。我们使用亮度模型形成磁盘不稳定性和核心吸积。我们考虑了半长轴分布的两种极端情况--附近F型和G型恒星的对数正态分布和径向速度技术探测到的系外行星的幂律分布。我们发现，GPI可以检测到所有的F和G光谱型恒星的系外行星的BPMG样本的概率取决于亮度模型和半长轴分布。在光谱类型K到M1，系外行星的可探测性取决于亮度和宿主恒星的距离。GPI将能够检测到比M1晚的M星的伴星，只有当它们比10 pc更接近时。在BPMG样本中的四颗A星中，只有一颗的V波段亮度在GPI范围内，其他的都太亮了。
It is well established that roughly half of all nearby solar-type stars have at least one companion. Stellar companions can have significant implications for the detection and characterization of exoplanets, including triggering false positives and masking the true radii of planets. Determining the fraction of exoplanet host stars that are also binaries allows us to better determine planetary characteristics as well as establish the relationship between binarity and planet formation. Using high angular resolution speckle imaging, we detect stellar companions within ~1 arcsec of K2 planet candi…
Know the Star, Know the Planet. II. Speckle Interferometry of Exoplanet Host Stars
研究系外行星的宿主恒星对于了解它们的环境很重要。为此，我们报告新的斑点观测的一个样本的系外行星主机原色。明亮的系外行星宿主HD 8673（= HIP 6702）被发现有一个伴星，尽管目前我们还不能确定伴星是物理的还是光学的。行星搜索和这些观测的观测列表在很大程度上已经预先筛选了已知的双重性，因此检测到的双星分数低于预期。因此，为了验证和质量控制的目的，同时观测了大量的双星，以确保没有发现系外行星宿主的伴星是有效的。在这些额外的观测中，首次解析了10对，确认了60对。这些观测是在2001年至2010年期间在KPNO和CTIO的NOAO 4 m望远镜上使用USNO斑点相机获得的。
Context: The influence of stellar multiplicity on planet formation is not yet well determined. Most planets are found using indirect detection methods via the small radial velocity or photometric variations of the primary star. These indirect detection methods are not sensitive to wide stellar companions. High-resolution imaging is thus needed to identify potential (sub)stellar companions to these stars. Aims: In this study we aim to determine the (sub)stellar multiplicity status of exoplanet host stars, that were not previously investigated for stellar multiplicity in the literature. For syst…
We are studying the influence of stellar multiplicity on exoplanet systems, in particular systems that have been detected via radial-velocity searches. We are in particular interested in the closest companions as they would have a strong influence on the evolution of the original planet forming disks. In this study we present new companions detected during our ongoing survey of exoplanet hosts with VLT/SPHERE. We are using the extreme adaptive optics imager SPHERE at the ESO/VLT to search for faint (sub)stellar companions. We utilized the classical coronagraphic imaging mode to perform a snaps…
Stellar companions to exoplanet host stars: Lucky Imaging of transiting planet hosts
观测到的双星/多星系统中恒星和行星的性质为行星形成和演化提供了线索。我们将我们对视觉恒星同伴的调查扩展到21颗恒星的凌日系外行星的主机，使用两台AstraLux仪器的幸运成像技术：Calar Alto 2.2米望远镜的AstraLux Norte和La Silla ESO 3.5米新技术望远镜的AstraLux Sur。我们对凌日行星宿主星HAT-P-8和WASP-12的两颗以前未知的二元候选伴星进行了观测，并推导出伴星候选者的光度和天体测量特性。先前发现的与系外行星宿主恒星TrES-4和WASP-2的候选伴星的共同自行从后续观测中得到证实。对AstraLux观测到的31颗凌日系外行星的主星进行的贝叶斯统计分析表明，行星主星的伴星比例与太阳型场星的伴星比例没有显着差异，但行星主星的双星分离平均较大。
Search for Stellar Companions of Exoplanet Host Stars with AstraLux/CAHA 2.2 m
本文使用AstraLux/CAHA 2.2 m对212颗系外行星宿主恒星进行Lucky Imaging巡天，探测到46颗共动伴星，确定最小多重性率为20±3%，并强调在研究系外行星宜居性时必须考虑恒星多重性。
Know the Star, Know the Planet. III. Discovery of Late-Type Companions to Two Exoplanet Host Stars
我们讨论了两个拥有已知系外行星的多恒星系统：HD 2638和30 Ari B。自适应光学图像显示了两颗恒星的额外伴星。我们在Palomar天文台收集了Robo-AO和PALM-3000自适应光学系统的多历元图像，并提供了相对测光和天体测量。天体测量表明，伴星与它们各自的主星有共同的自行。这两颗新的伴星都预计与系外行星宿主恒星的距离小于30 AU。使用投影的分离来计算新伴星的轨道周期，HD 2638的周期为130年，而30 Ari B的周期为80年。以前的研究表明，真实的周期很可能在这些估计值的三倍之内。30 Ari的额外组成部分使其成为第二个确认的四重系统，已知拥有系外行星。HD 2638拥有一颗热木星，新伴星的发现加强了热木星和双星之间的联系。我们把系统的颜色星等图，并得出质量的同伴，原来是大约0.5太阳质量的恒星。
Most Sub-Arcsecond Companions of Kepler Exoplanet Candidate Host Stars are Gravitationally Bound
使用已知的高分辨率成像观测的检测极限和真正的二进制和视线的同伴的统计特性，我们估计的二进制分数{ \it开普勒}系外行星宿主恒星。我们在WIYN 3.5-m和Gemini North 8.1-m望远镜上的散斑成像计划已经观测了600多个{ \it Kepler}感兴趣的物体（KOI），并在$\sim$ 1角秒内探测到49个恒星伴星。假设双星在3000 ~ 10000 K的有效温度范围内遵循对数正态周期分布，那么模型预测绝大多数检测到的亚弧秒伴星都是长周期（$P>50$年）的引力束缚伴星。在比较两个观测项目中的模型预测与实际探测的数量时，我们得出结论，宿主星的总体双星比例与观测到的场星的40- 50%相似。
The majority of stars have one or more stellar companions. As exoplanets continue to be discovered, it is crucial to examine planetary systems to identify their stellar companions. By observing a change in proper motion, companions can be detected by the acceleration they induce on their host stars. We selected 701 stars from the Hipparcos-Gaia Catalog of Accelerations (HGCA) that have existing adaptive optics imaging data gathered with Gemini/NIRI. Of these, we examined 21 stars known to host planet candidates and reduced their archival NIRI data with Gemini's DRAGONS software. We assessed th…
We present high angular resolution imaging observations of 517 host stars of TESS exoplanet candidates using the `Alopeke and Zorro speckle cameras at Gemini North and South. The sample consists mainly of bright F, G, K stars at distances of less than 500 pc. Our speckle observations span angular resolutions of ~20 mas out to 1.2 arcsec, yielding spatial resolutions of <10 to 500 AU for most stars, and our contrast limits can detect companion stars 5-9 magnitudes fainter than the primary at optical wavelengths. We detect 102 close stellar companions and determine the separation, magnitude diff…
The Kepler mission and subsequent ground-based follow-up observations have revealed a number of exoplanet host stars with nearby stellar companions. This study presents speckle observations of 57 Kepler objects of interest (KOIs) that are also double stars, each observed over a 3 to 8 year period, which has allowed us to track their relative motions with high precision. Measuring the position angle and separation of the companion with respect to the primary can help determine if the pair exhibits common proper motion, indicating it is likely to be a bound binary system. We report on the motion…
On the Stellar Companion to the Exoplanet Hosting Star 30 Arietis B
理解行星形成的一个关键方面是确定宿主恒星的双星性。径向速度调查和开普勒系外行星候选者的后续行动的结果表明，恒星双星当然不排除稳定轨道上行星的存在，而且这种配置实际上可能相对常见。在这里，我们提出了新的结果30白羊座系统，这证实了B组件主机行星和恒星的同伴。凯克AO成像提供了恒星伴星的直接检测和额外的径向速度数据是一致的轨道恒星。我们提出了一个修订后的轨道的已知行星随着测光在预测过境时间。最后，我们提供的恒星伴侣的轨道稳定性考虑的基础上的属性的限制。
Know the Star, Know the Planet. V. Characterization of the Stellar Companion to the Exoplanet Host HD 177830
HD 177830是一颗演化的K 0 IV恒星，有两颗已知的系外行星。除了行星伴星之外，它还有一颗晚型恒星伴星是用自适应光学成像发现的。我们用PHARO近红外相机和Project 1640日冕仪观测了双星系统。使用Project 1640日冕仪和积分场摄谱仪，我们提取了恒星伴星的光谱。这使我们能够确定恒星伴星的光谱类型是M4 $\pm$ 1V。我们用这两种仪器来测量双星系统的天体测量。结合这些数据和已发表的数据，我们确定该双星的周期可能约为800年，半长轴为100-200 AU。这意味着恒星伴星对系外行星的动力学几乎没有影响。应继续监测该系统的天体测量，但由于该系统的缓慢性质，可以每5-10年进行一次观测。
We have obtained the highest resolution images available of TRAPPIST-1 using the Gemini-South telescope and our speckle imaging camera. Observing at 692 and 883 nm, we reached the diffraction limit of the telescope providing a best resolution of 27 mas or, at the distance of TRAPPIST-1, a spatial resolution of 0.32 AU. Our imaging of the star extends from 0.32 to 14.5 AU. We show that to a high confidence level, we can exclude all possible stellar and brown dwarf companions, indicating that TRAPPIST-1 is a single star.
We present the latest results of an ongoing multiplicity survey of exoplanet hosts, which was initiated at the Astrophysical Institute and University Observatory Jena, using data from the second data release of the ESA-Gaia mission. In this study the multiplicity of 289 targets was investigated, all located within a distance of about 500 pc from the Sun. In total, 41 binary, and 5 hierarchical triple star systems with exoplanets were detected in the course of this project, yielding a multiplicity rate of the exoplanet hosts of about 16 %. A total of 61 companions (47 stars, a white dwarf, and …
We have been conducting a exoplanet search survey using Bohyunsan Observatory Echelle Spectrograph (BOES) for the last 18 years. We present the detection of exoplanet candidate in orbit around HD 18438 from high-precision radial velocity (RV) mesurements. The target was already reported in 2018 (Bang et al. 2018). They conclude that the RV variations with a period of 719 days are likely to be caused by the pulsations because the Lomb-Scargle periodogram of HIPPARCOS photometric and Ha EW variations for HD 18438 show peaks with periods close to that of RV variations and there were no correlatio…
On the Orbits of Low-mass Companions to White Dwarfs and the Fates of the Known Exoplanets
由于最近发现了越来越多的低质量的白矮星伴星，因此双星伴星的最终命运（包括伴星是否幸存以及双星的最终轨道）是一个有趣的问题。在这封信中，我们研究了一个两体系统的演化，其中轨道调整由于结构变化的主要，通过潮汐轨道能量的耗散，和质量损失在巨大的阶段;以前的研究没有纳入变化的主要的自旋。对于从木星的质量到~0.3 Msun和从1-3 Msun的初级恒星的伴星，我们确定了伴星在主序后演化过程中避免被初级恒星吞没所需的最小初始半长轴，并强调了已知系外行星最终生存的影响。我们目前的区域在二级质量和轨道周期空间，一个被吞没的同伴可能会生存的共同包络相（CEP），并与已知的M矮+WD短周期双星比较。最后，我们注意到被吞没的类地行星无法在CEP中幸存下来。在白矮星宜居带探测第一代类地行星需要从几个天文单位的轨道散射到一个高偏心率的轨道（近星点为~Rsun），然后通过潮汐摩擦将其阻尼到圆形轨道，可能使其成为一个不适合居住的烧焦的行星。
The vast majority of extrasolar planets are detected by indirect detection methods such as transit monitoring and radial velocity measurements. While these methods are very successful in detecting short-periodic planets, they are mostly blind to wide sub-stellar or even stellar companions on long orbits. In our study we present high resolution imaging observations of 63 exoplanet hosts carried out with the lucky imaging instrument AstraLux at the Calar Alto 2.2m telescope as well as with the new SPHERE high resolution adaptive optics imager at the ESO/VLT in the case of a known companion of sp…
Prioritizing High-Precision Photometric Monitoring of Exoplanet and Brown Dwarf Companions with JWST -- Strategic Exoplanet Initiatives with HST and JWST White Paper
本文主张利用 JWST 的高稳定性和高对比度星冕成像对系外行星与褐矮星伴星开展高精度测光监测，以探测大气特征、自转周期及多波段大气结构差异，实现亚百分级光变刻画。
Validation of the Exoplanet Kepler-21b using PAVO/CHARA Long-Baseline Interferometry
我们使用CHARA阵列的PAVO光束组合器对Kepler系外行星宿主恒星HD 179070（Kepler-21）进行了长基线干涉测量。可见度数据与单个恒星一致，不包括距离约1-1000 mas（约0.1-113 AU）和对比度< 3.5等的伴星。这一结果支持了Howell等人（2012年）对1.6 R_{earth}系外行星开普勒-21 b的验证，并补充了自适应光学成像、斑点干涉测量和径向速度观测所设置的限制，以排除由于恒星伴星造成的误报。我们的结论是，长基线干涉测量有很强的潜力，以验证凌日系外行星，特别是未来的项目，旨在更明亮的恒星和宿主恒星的径向速度后续是不可用的。
Dynamical Masses of Young M Dwarfs: Masses and Orbital Parameters of GJ 3305 AB, the Wide Binary Companion to the Imaged Exoplanet Host 51 Eri
我们结合新的高分辨率成像和光谱从凯克/NIRC 2，发现频道望远镜/DSSI，和凯克/HIRES与公布的天体测量和径向速度，以测量个别的质量和轨道要素的GJ 3305 AB系统，一个年轻的（~20百万年）M+M二进制（未解析光谱类型M0）的成员β风景如画的移动群与成像的系外行星主机51 Eri。我们测量的总系统质量为1.11 \pm 0.04 M_太阳，周期为29.03 \pm 0.50$ yr，半长轴为9.78 \pm 0.14 AU，偏心率为0.19 \pm 0.02。主组件的动力学质量为0.67 \pm 0.05 M_sun，次级组件的质量为0.44 \pm 0.05 M_sun。最近更新的BHAC 15模型与两颗恒星的质量一致，在1.5 sigma内。根据观测到的质量，模型预测GJ 3305 AB系统的年龄为37 \pm 9百万年。根据观测到的系统结构和我们的动力学质量测量，51 Eri b的轨道不太可能被Kozai-Lidov机制显著改变。
The orbital eccentricities of directly imaged exoplanets and brown dwarf companions provide clues about their formation and dynamical histories. We combine new high-contrast imaging observations of substellar companions obtained primarily with Keck/NIRC2 together with astrometry from the literature to test for differences in the population-level eccentricity distributions of 27 long-period giant planets and brown dwarf companions between 5-100 AU using hierarchical Bayesian modeling. Orbit fits are performed in a uniform manner for companions with short orbital arcs; this typically results in …
Keck Observations in the INfrared of Taurus and $ρ$ Oph Exoplanets And Ultracool dwarfs (KOINTREAU) II: Two Young Bound Companions to Ophiuchus Stars
凯克望远镜发现两颗年轻恒星的伴星，其中一颗质量为3.4±0.7 M_Jup，另一颗可能为11.5±1.2或15.3±0.8 M_Jup。
High-Resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-In Stellar Companions to Exoplanet Host Stars
本研究通过斑点干涉测量验证TESS控制样本中系外行星宿主恒星近距离伴星缺失，发现TIC选择偏差导致高质量比双星被排除，修正后伴星频率与经典值一致。
The stable oscillations of pulsating stars can serve as accurate timepieces, which may be monitored for the influence of exoplanets. An external companion gravitationally tugs the host star, causing periodic changes in pulsation arrival times. This method is most sensitive to detecting substellar companions around the hottest pulsating stars, especially compact remnants like white dwarfs and hot subdwarfs, as well as delta Scuti variables (A stars). However, it is applicable to any pulsating star with sufficiently stable oscillations. Care must be taken to ensure that the changes in pulsation …
We present high-resolution speckle interferometric imaging observations of TESS exoplanet host stars using the NN-EXPLORE NESSI instrument the at the 3.5-m WIYN telescope. Eight TOIs, that were originally discovered by Kepler, were previously observed using the Differential Speckle Survey Instrument (DSSI). Speckle observations of 186 TESS stars were carried out and 45 (24%) likely bound companions were detected. This is approximately the number of companions we would expect to observe given the established 46% binarity rate in exoplanet host stars. For the detected binaries, the distribution …
Mind the Companion : Demographics of Transiting S-type Exoplanets
利用Gaia DR3数据构建S型系外行星参考星表，通过对比单星和双星系统中的行星，发现双星中巨行星质量更大、轨道更近、半径更膨胀，且M矮星周围存在伴星分离<1000 AU的巨行星过量。
Carbon and Oxygen Abundances in the Hot Jupiter Exoplanet Host Star XO-2N and its Binary Companion
为了将恒星和行星的组成联系起来，我们给出了凌日系外行星宿主恒星XO-2N及其宽分离双星XO-2S的碳和氧以及铁和镍的丰度。恒星参数来自高分辨率，高信噪比的光谱，这两颗星被发现是相似的Teff，log g，铁（[Fe/H]），镍（[Ni/H]）丰度。它们的碳（[C/H]）和氧（[O/H]）丰度也在误差范围内重叠，尽管XO-2N可能比XO-2S略富碳和富氧。这两颗恒星的碳氧比（~0.60+/-0.20）也可能比太阳的碳氧比（~0.50）稍大。XO-2系统有一个过境的热木星围绕一个双星组成，但不是另一个，使我们能够探测行星形成可能对宿主恒星组成的潜在影响。此外，通过对其大气层的多次观测，凌日系外行星XO-2b有助于成分分析，这可以与我们的双星元素丰度建立的出生化学环境进行比较。这项工作的阶段，确定如何相似/不同的系外行星和宿主恒星的组成，以及行星形成的影响，通过讨论的C/O比测量的独特环境中的视觉双星系统与一个恒星托管过境热木星。
Extrasolar planets in stellar multiple systems
通过分析由径向速度或凌日观测探测到的系外行星，我们确定了系外行星宿主恒星的多样性，以研究恒星伴星对行星候选者性质的影响。通过径向速度或凌日观测发现的系外行星候选者的主恒星与在线多重性目录相匹配，除了文献搜索外，还确定了57颗系外行星主恒星具有恒星伴星。由此产生的至少12%的系外行星宿主恒星的多重性比一般的类太阳恒星的多重性小四倍。在恒星复合系统中，行星的质量和数量取决于它们的主星和它最近的伴星之间的距离，例如行星的质量随着恒星距离的增加而减少。我们提出了恒星多系统中系外行星候选者的最新概述，包括15个新系统（与2009年的最新摘要相比）。
Search for exoplanet around northern circumpolar stars - Four planets around HD 11755, HD 12648, HD 24064, and 8 Ursae Minoris
目标。该方案最初是利用宝玄山光学天文台1.8米望远镜进行的系外行星观测的北极区域延伸。本文的目的是通过精确的径向速度（RV）调查在北极绕极星中找到系外行星。方法.我们选择了大约200颗北极环极星，标准是：Dec> 70度，0.6 < B-V < 1.6，HIPPARCOS_scat < 0.05等，5.0 < mv < 7.0。高分辨率、光纤馈入的Bohyunsan天文台Echelle摄谱仪（BOES）用于RV调查。通过对色球活动、依巴谷光度测量和分光线的分析，排除了RV变化的其他原因。结果2010年，我们开始对候选人进行监测，并在过去五年中完成了对所有明星的初步筛选。我们发现了四颗新的系外行星。恒星HD 11755、HD 12648、HD 24064和8 UMi都显示出巨行星在开普勒运动的证据。HD 11755的伴星在433天的轨道上的最小质量为6.5 M_Jup，离心率为0.19。HD 12648的伴星最小质量为2.9 M Jup，周期为133天，离心率为0.04。怀疑HD 24064的表面活性较弱。然而，没有发现与RV变异相关的证据。它的伴星最小质量为9.4 M_Jup，周期为535天，离心率为0.35。最后，8 UMi的最小质量为1.5 M_Jup，周期为93天，偏心率为0.06。
We study the multiplicity of host stars to known transiting extra-solar planets to test competing theories on the formation mechanisms of hot Jupiters. We observed 45 exoplanet host stars using VLT/SPHERE/IRDIS to search for potential companions. For each identified candidate companion we determined the probability that it is gravitationally bound to its host by performing common proper motion checks and modelling of synthetic stellar populations around the host. We detected new candidate companions around K2-38, WASP-72, WASP-80, WASP-87, WASP-88, WASP-108, WASP-118, WASP-120, WASP-122, WASP1…
Know the Star, Know the Planet. I. Adaptive Optics of Exoplanet Host Stars
本文介绍了对系外行星主星进行伴星自适应光学观测的结果。我们利用AEOS望远镜及其自适应光学系统在$I$波段采集了恒星的深空图像。观测到62颗系外行星的宿主恒星，并解析出15个多恒星系统。这八个是已知的倍数，而七个是新的候选二进制。对于所有双星，我们测量了双星对的相对星等和$I$波段的差星等。我们改进了HD 19994和$τ$ Boo的轨道。这些观测将提供有关系外行星宿主恒星的双重性的更好的统计数据，并加深对已知双星系外行星宿主的动态的理解。
Wide low-mass substellar companions are known to be very rare among low-mass stars, but appear to become increasingly common with increasing stellar mass. However, B-type stars, which are the most massive stars within ~150 pc of the Sun, have not yet been examined to the same extent as AFGKM-type stars in that regard. In order to address this issue, we launched the ongoing B-star Exoplanet Abundance Study (BEAST) to examine the frequency and properties of planets, brown dwarfs, and disks around B-type stars in the Scorpius-Centaurus (Sco-Cen) association; we also analyzed archival data of B-ty…
The Young Suns Exoplanet Survey (YSES) consists of a homogeneous sample of 70 young, solar-mass stars located in the Lower Centaurus-Crux subgroup of the Scorpius-Centaurus association with an average age of $15\pm3\,$Myr. We report the detection of a co-moving companion around the K3IV star TYC 8998-760-1 (2MASSJ13251211-6456207) that is located at a distance of $94.6\pm0.3\,$pc using SPHERE/IRDIS on the VLT. Spectroscopic observations with VLT/X-SHOOTER constrain the mass of the star to $1.00\pm0.02\,M_{\odot}$ and an age of $16.7\pm1.4\,$Myr. The companion TYC 8998-760-1 b is detected at a …
We conducted speckle imaging observations of 53 stellar systems that were members of long-term radial velocity (RV) monitoring campaigns and exhibited substantial accelerations indicative of planetary or stellar companions in wide orbits. Our observations were made with blue and red filters using the Differential Speckle Survey Instrument at Gemini-South and the NN-Explore Exoplanet Stellar Speckle Imager at the WIYN telescope. The speckle imaging identifies eight luminous companions within two arcseconds of the primary stars. In three of these systems (HD 1388, HD 87359, and HD 104304), the p…
We report results from the Wide-orbit Exoplanet search with InfraRed Direct imaging (WEIRD), a survey designed to search for Jupiter-like companions on very wide orbits (1000 to 5000 AU) around young stars ($<$120 Myr) that are known members of moving groups in the solar neighborhood ($<$70 pc). Sharing the same age, distance, and metallicity as their host while being on large enough orbits to be studied as "isolated" objects make such companions prime targets for spectroscopic observations and valuable benchmark objects for exoplanet atmosphere models. The search strategy is based on deep ima…
Distinguishing exoplanet companions from field stars in direct imaging using Gaia astrometry
本文提出结合 Gaia 天体测量与 2MASS 测光、基于似然比较场星与共同运动伴星模型的方法，并在 BEAST 样本中识别出 7 个高置信伴星候选体。
Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS
本研究利用高分辨率成像与Gaia天体测量，分析TESS发现的M型矮星双星系外行星宿主星的人口统计学特征，测定伴星参数，修正行星半径，并发现3个近距双星中的多行星系统。
Ruling Out Possible Secondary Stars to Exoplanet Host Stars Using the CHARA Array
在迄今为止已知的450多颗系外行星中，有420多颗是通过径向速度研究发现的，这种方法对行星轨道的倾角一无所知。由于伴星更有可能是中等至高倾角轨道上的行星质量物体，而不是几乎面对面轨道上的低质量恒星物体，因此二级天体被推定为行星。干涉测量观测使我们能够检查角直径拟合残差校准vibrium，以排除在一个非常低的倾角轨道上的低质量恒星伴侣的可能性。我们使用高角分辨率天文学中心（CHARA）阵列干涉仪观察了20颗系外行星的宿主恒星，并考虑了五种潜在的次级光谱类型：G5 V，K0 V，K5 V，M0 V和M5 V。对于7颗主星，所有的次级类型都可以从考虑中排除，而对于另外7颗主星，任何光谱类型的次级恒星都不能排除。剩下的6颗主星显示出一系列可能的次级类型。
Connecting planets around horizontal branch stars with known exoplanets
我们研究了主序（MS）恒星周围系外行星的分布，并将我们的结果应用于极端水平分支（EHB; sdO; sdB;热次矮星）恒星形成的二元模型。通过双星模型，我们指的是恒星和亚恒星的同伴，提高质量损失率，其中亚恒星的同伴代表大质量行星和褐矮星。我们的结论是sdB（EHB）恒星是行星搜索的主要目标。我们得出这一结论是因为我们注意到，行星围绕恒星的双峰分布相对于参数M_p*a^2在质量范围为1 Mo < M < 1.5Mo的恒星中最为显著; 'a'是轨道间距，'M'是恒星质量，'M_p'是行星质量。这也是EHB恒星的祖先的质量范围，这些恒星是通过它们的祖先与行星的相互作用形成的（假设EHB的形成机制是双星模型）。在EHB星形成的双星模型中，与双星伴星或亚恒星物体（行星或棕矮星）的相互作用，导致其前身在红巨星分支（RGB）阶段失去了大部分的包层质量。因此，后代HB星是热的，即，一颗EHB（sdB）星。双峰分布表明，即使形成EHB恒星的近距离行星没有在其RGB共同包层演化中幸存下来，也可能有一颗或多颗行星在>1AU的位置幸存下来。此外，如果一颗或更多的行星在大于1AU的位置被观测到，那么有可能是一颗更近的大质量行星在共同包层阶段幸存下来，并且它以数小时到数天的轨道周期绕着EHB运行。
Planetary companions orbiting M giants HD 208527 and HD 220074
目标。本研究的目的是通过精确的视向速度（RV）测量来研究行星伴星的起源。方法. 2008年9月至2012年6月，在宝贤山光学天文台（BOAO）使用了光纤馈入宝贤山天文台Echelle光谱仪（BOES）的高分辨率光谱。结果我们报告了在HD 208527和HD 220074周围的轨道上探测到两颗系外行星，它们的RV周期变化为875.5 +/- 5.8和672.1 +/- 3.7天。RV的变化与表面的不均匀性没有明显的关系，行星伴星的开普勒运动是最可能的解释。假设可能的恒星质量为1.6 +/- 0.4和1.2 +/- 0.3 M太阳，我们得到了HD 208527和HD 220074周围系外行星的最小质量分别为9.9 +/- 1.7和11.1 +/- 1.8 M_Jup，轨道半长轴分别为2.1 +/- 0.2和1.6 +/-0.2。0.1 AU，偏心率分别为0.08和0.14。我们还发现，先前已知的HD 208527和HD 220074的光谱分类是错误的：我们对恒星参数的新估计表明，HD 208527和HD 220074都是M巨星。因此，HD 208527和HD 220074是迄今为止第一个拥有行星伴星的M巨星候选者。
ExoCat-1: The Nearby Stellar Systems Catalog for Exoplanet Imaging Missions
我们提出了第一个版本的系外行星成像任务（被称为直接成像社区为“ExoCat”）的附近恒星系统目录，用于系外行星直接成像任务规划。这个版本，ExoCat-1，包括2347颗取自依巴谷星表的恒星，测量的视差> 33.33 mas（对应于30 pc的距离）。这个样本几乎是完整的，直到V=8，对应的恒星亮度超过~0.5太阳光度（晚期G-/早期K-型矮星在30 pc的距离限制）。对于每颗恒星，我们提供天体测量（包括赤道和银河系坐标，视差和自行），约翰逊B和V星等（从依巴谷或第谷数据转换或从文献中获取），以及从2 MASS（对于较暗的恒星）或从文献中获取的K波段星等转换为2 MASS Ks星等（对于明亮的恒星）的KS波段星等。使用这些数据，我们估计恒星的光度，有效温度，恒星半径（太阳和角度单位），地球等效日射距离（在AU和角度单位），和分数行星亮度外=地球在地球等效日射距离。我们提供已公布的光谱类型和简单的恒星类型标签，用于快速评估设计参考任务选定的目标列表。已知的系外行星伴星的数量是为每颗恒星标示的，对于明亮的恒星（V<7），我们提供了10角秒内最亮恒星伴星的距离和δ星等。其他重要的恒星数据，如log（g），色球活动水平和年龄估计提供了现成的。ExoCat-1可以通过Exoplanets Exploration Program（ExEP）网站找到。
Keck Observations in the INfrared of Taurus and $ρ$ Oph Exoplanets And Ultracool dwarfs (KOINTREAU) I: A Planetary-Mass Companion and a Disk-Obscured Stellar Companion Discovered in Taurus
凯克望远镜在塔罗斯发现行星质量伴星和被盘遮挡的恒星伴星，通过近红外观测确定其光谱和质量特性。
The quest to discover exoplanets is one of the most important missions in astrophysics, and is widely performed using the transit method, which allows for the detection of exoplanets down to the size of Mercury. However, to confirm these detections, additional vetting is mandatory. We selected six K2 targets from campaigns #1 to #8 that show transit light curves corresponding to Earth-sized to Neptune-sized exoplanets. We aim to discard some scenarios that could mimic an exoplanetary transit, leading to a misinterpretation of the data. We performed direct imaging observations using the SPHERE/…
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