Exploring the RCrA environment with SPHERE: Discovery of a new stellar companion
D. Mesa, M. Bonnefoy, R. Gratton, G. Van Der Plas, V. D'Orazi, E. Sissa, A. Zurlo, E. Rigliaco, T. Schmidt, M. Langlois, A. Vigan, M. G. Ubeira Gabellini, S. De… 展开作者
D. Mesa, M. Bonnefoy, R. Gratton, G. Van Der Plas, V. D'Orazi, E. Sissa, A. Zurlo, E. Rigliaco, T. Schmidt, M. Langlois, A. Vigan, M. G. Ubeira Gabellini, S. Desidera, S. Antoniucci, M. Barbieri, M. Benisty, A. Boccaletti, R. Claudi, D. Fedele, D. Gasparri, T. Henning, M. Kasper, A. -M. Lagrange, C. Lazzoni, G. Lodato, A. -L. Maire, C. F. Manara, M. Meyer, M. Reggiani, M. Samland, M. Van den Ancker, G. Chauvin, A. Cheetham, M. Feldt, E. Hugot, M. Janson, R. Ligi, O. Moller-Nilsson, C. Petit, E. L. Rickman, F. Rigal, F. Wildi
Aims. R Coronae Australis (R CrA) is the brightest star of the Coronet nebula of the Corona Australis (CrA) star forming region. It has very red colors, probably due to dust absorption and it is strongly variable. High contrast instruments allow for an unprecedented direct exploration of the immediate circumstellar environment of this star. Methods. We observed R CrA with the near-IR channels (IFS and IRDIS) of SPHERE at VLT. In this paper, we used four different epochs, three of them from open time observations while one is from the SPHERE guaranteed time. The data were reduced using the DRH pipeline and the SPHERE Data Center. On the reduced data we implemented custom IDL routines with the aim to subtract the speckle halo.We have also obtained pupil-tracking H-band (1.45-1.85 micron) observations with the VLT/SINFONI near-infrared medium-resolution (R~3000) spectrograph. Results. A companion was found at a separation of 0.156" from the star in the first epoch and increasing to 0.18400 in the final one. Furthermore, several extended structures were found around the star, the most noteworthy of which is a very bright jet-like structure North-East from the star. The astrometric measurements of the companion in the four epochs confirm that it is gravitationally bound to the star. The SPHERE photometry and the SINFONI spectrum, once corrected for extinction, point toward an early M spectral type object with a mass between 0.3 and 0.55 M?. The astrometric analyis provides constraints on the orbit paramenters: e~0.4, semi-major axis at 27-28 au, inclination of ~ 70° and a period larger than 30 years. We were also able to put constraints of few MJup on the mass of possible other companions down to separations of few tens of au.
Exploring the optical properties of redback pulsars: The case of J1717+4308A in the globular cluster M92
Beijing Normal University（北京师范大学）；Alma Mater Studiorum Università di Bologna（博洛尼亚大学）；INAF-Osservatorio di Astrofisica e Scienze dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；Norwegian University of Science and Technology（挪威科技大学）
On the formation of subdwarf B stars via engulfment of substellar companions I. Conditions for and occurrence of envelope ejection events
Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège（列日大学空间科学、技术与天体物理研究研究所）；Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles (ULB)（布鲁塞尔自由大学天文与天体物理研究所）
Finding the elusive RR Lyrae companions via speckle imaging
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天体物理中心）；Gemini Observatory/NSF’s NOIRLab（Gemini 天文台 / NSF 的 NOIRLab）；European Southern Observatory（欧洲南方天文台）；Instituto de Física y Astronomía, Universidad de Valparaíso（瓦尔帕莱索大学物理与天文学研究所）；Institute of Astrophysics, Pontificia Universidad Católica de Chile（智利天主教大学天体物理研究所）；Centro de Astroingeniería, Pontificia Universidad Católica de Chile（智利天主教大学天体工程中心）；NASA Ames Research Center（美国宇航局艾姆斯研究中心）；Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University in Toruń（托伦尼古拉·哥白尼大学物理、天文学和信息技术学院天体物理研究所）
Exploring the radial velocity variations of RY Lup with VLT/ESPRESSO: Binary versus spot hypotheses
European Southern Observatory（欧洲南方天文台）；INAF – Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；INAF – Osservatorio Astrofisico di Catania（意大利国家天体物理研究所卡塔尼亚天文台）；Dipartimento di Fisica, Université degli Studi di Milano（米兰大学物理系）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；University Observatory, Faculty of Physics, Ludwig-Maximilians- Universität München（慕尼黑大学物理学院天文台）
A Binary Flux Calibrator Reveals the Scientific Potential of Short-integration JWST MIRI Imaging to Directly Detect sub-Jupiter Exoplanets
Eureka Scientific Inc.（Eureka科学公司）；University of Michigan（密歇根大学）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；University of California Santa Cruz（加州大学圣克鲁兹分校）；Massachusetts Institute of Technology（麻省理工学院）；Johns Hopkins APL（约翰斯·霍普金斯大学应用物理实验室）
ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS): II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-Mass Companion 2MASS 1207 b
