$β$ Pictoris' inner disk in polarized light and new orbital parameters for $β$ Pictoris b
Maxwell A. Millar-Blanchaer, James R. Graham, Laurent Pueyo, Paul Kalas, Rebekah I. Dawson, Jason Wang, Marshall Perrin, Dae-Sik Moon, Bruce Macintosh, S. Mark … 展开作者
Maxwell A. Millar-Blanchaer, James R. Graham, Laurent Pueyo, Paul Kalas, Rebekah I. Dawson, Jason Wang, Marshall Perrin, Dae-Sik Moon, Bruce Macintosh, S. Mark Ammons, Travis Barman, Andrew Cardwell, Christine H. Chen, Eugene Chiang, Jeffrey Chilcote, Tara Cotten, Robert J. De Rosa, Zachary H. Draper, Jennifer Dunn, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen J. Goodsell, Alexandra Z. Greenbaum, Markus Hartung, Pascale Hibon, Sasha Hinkley, Patrick Ingraham, Rebecca Jensen-Clem, Quinn Konopacky, James E. Larkin, Douglas Long, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Katie M. Morzinski, Eric L. Nielsen, David W. Palmer, Rebecca Oppenheimer, Lisa Poyneer, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Naru Sadakuni, Leslie Saddlemyer, Adam C. Schneider, Anand Sivaramakrishnan, Remi Soummer, Sandrine Thomas, Gautam Vasisht, David Vega, J. Kent Wallace, Kimberly Ward-Duong, Sloane J. Wiktorowicz, Schuyler G. Wolff
We present $H$-band observations of $β$ Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ~0.3" (~6 AU) and ~1.7" (~33 AU), while simultaneously detecting $β$ Pic $b$. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best fit model indicates a disk inclined to the line of sight ($ϕ=85.27°^{+0.26}_{-0.19}$) with a position angle $θ_{PA}=30.35°^{+0.29}_{-0.28}$ (slightly offset from the main outer disk, $θ_{PA}\approx29°$), that extends from an inner disk radius of $23.6^{+0.9}_{-0.6}$ AU to well outside GPI's field of view. In addition, we present an updated orbit for $β$ Pic $b$ based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semi-major axis of $a=9.2^{+1.5}_{-0.4}$AU, with an eccentricity $e\leq 0.26$. The position angle of the ascending node is $Ω=31.75°\pm0.15$, offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of $β$ Pic to $1.60\pm0.05 M_{\odot}$. Dynamical sculpting by $β$ Pic $b$ cannot easily account for the following three aspects of the inferred disk properties: 1) the modeled inner radius of the disk is farther out than expected if caused by $β$ Pic b; 2) the mutual inclination of the inner disk and $β$ Pic $b$ is $4°$, when it is expected to be closer to zero; and 3) the aspect ratio of the disk ($h_0 = 0.137^{+0.005}_{-0.006}$) is larger than expected from interactions with $β$ Pic $b$ or self-stirring by the disk's parent bodies.
Discovery of an Exterior Third Planet Orbiting $β$ Pictoris
University of California, San Diego（加州大学圣地亚哥分校）；Space Telescope Science Institute（太空望远镜科学研究所）；The University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）；Center for Interdisciplinary Exploration and Research in Astrophysics（天体物理学跨学科探索与研究中心）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of California Observatories（加州大学天文台）
The $β$ Pictoris b Hill sphere transit campaign. Paper II: Searching for the signatures of the $β$ Pictoris exoplanets through time delay analysis of the $δ$ Scuti pulsations
The Birth of Minor-Body Populations in the $β$ Pictoris System I: The First 25 Myr
Universidad de La Laguna (ULL)（拉古纳大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），CSIC-INTA）；Universidad Complutense de Madrid（马德里康普顿斯大学）；Lund University（隆德大学）
The multi-wavelength vertical structure of the archetypal $β$ Pictoris debris disk
California Institute of Technology（加州理工学院）；University of Cambridge（剑桥大学）；University of Belgrade（贝尔格莱德大学）；University of Oxford（牛津大学）；ALMA JAO（阿塔卡马大型毫米波/亚毫米波阵列联合运营办公室）；Wesleyan University（卫斯理安大学）；Trinity College Dublin, the University of Dublin（都柏林三一学院，都柏林大学）
Direct Imaging Discovery of Giant Exoplanet $β$ Pictoris d: A Decade-Long Game of Hide-and-Seek
Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；Centre for Exoplanet Science, University of Edinburgh（爱丁堡大学系外行星科学中心）；European Southern Observatory（欧洲南方天文台）；Max Planck Institute for Intelligent Systems（马克斯·普朗克智能系统研究所）；Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）
通过VLT/ERIS、JWST/NIRCam和VLT/SPHERE的档案数据，直接成像发现了β Pictoris系统的第三颗系外行星d，其轨道半长轴26.0 au，质量2.4 M_Jup，温度600 K，与51 Eri b相似。
Two inner dust clumps in PDS 70. A third protoplanet traced by trojan material or a substructured inner disk?
KU Leuven（荷语鲁汶大学）；Université de Liège（列日大学）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、天体物理学和信息研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；LIRA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（拉格朗日力学实验室、巴黎天文台、巴黎文理研究大学、索邦大学、巴黎西岱大学、塞吉-蓬图瓦兹大学、法国国家科学研究中心）；European Southern Observatory（欧洲南方天文台）；University of Victoria（维多利亚大学）；NRC Herzberg Astronomy and Astrophysics（加拿大国家研究委员会赫尔伯格天体物理研究所）
The inner structure of the TW Hya Disk as revealed in scattered light
利用哈勃空间望远镜/STIS和NICMOS的非偏振多波长图像，在0 \farcs 4（22天文单位）的内工作角下，观测到TW Hya盘内部在40天文单位的显著变化。我们的图像显示了在每个波长下具有类似行为的清除的外边缘，表明该特征是结构性的，而不是由于圆盘中的偏振光的某些特性。我们将我们的观测结果与Akiyama et al.（2015）和Rapson et al.（2015）的观测结果进行了比较，并讨论了80~AU圆盘内部的光谱演化。我们建立了一个模型，两个间隙：一个在30~AU和一个在80~AU，拟合观测到的表面亮度轮廓，但高估了磁盘的绝对亮度。我们的模型需要一个额外的调光与观察一致，我们暂时归因于阴影。在散射光中看到的间隙结构在空间上与CO和N $_2$ H $^+$的亚毫米检测一致，并且接近这些分子种类的预期凝结前沿，提供了在散射光中看到的结构可能与盘中的化学变化相关的初步证据。
