CARMENES input catalogue of M dwarfs V. Luminosities, colours, and spectral energy distributions
C. Cifuentes, J. A. Caballero, M. Cortes-Contreras, D. Montes, F. J. Abellan, R. Dorda, G. Holgado, M. R. Zapatero Osorio, J. C. Morales, P. Amado, V. M. Passeg… 展开作者
C. Cifuentes, J. A. Caballero, M. Cortes-Contreras, D. Montes, F. J. Abellan, R. Dorda, G. Holgado, M. R. Zapatero Osorio, J. C. Morales, P. Amado, V. M. Passegger, A. Quirrenbach, A. Reiners, I. Ribas, J. Sanz-Forcada, A. Schweitzer, W. Seifert, E. Solano
The relevance of M dwarfs in the search for potentially habitable Earth-sized planets has grown significantly in the last years. In our on-going effort to comprehensively and accurately characterise confirmed and potential planet-hosting M dwarfs, in particular for the CARMENES survey, we have carried out a comprehensive multi-band photometric analysis involving spectral energy distributions, luminosities, absolute magnitudes, colours, and spectral types, from which we have derived basic astrophysical parameters. We have carefully compiled photometry in 20 passbands from the ultraviolet to the mid-infrared, and combined it with the latest parallactic distances and close-multiplicity information, mostly from Gaia DR2, of a sample of 2479 K5V to L8 stars and ultracool dwarfs, including 2210 nearby, bright M dwarfs. For this, we made extensive use of Virtual Observatory tools. We have homogeneously computed accurate bolometric luminosities and effective temperatures of 1843 single stars, derived their radii and masses, studied the impact of metallicity, and compared our results with the literature. The over 40000 individually inspected magnitudes, together with the basic data and derived parameters of the stars, individual and averaged by spectral type, have been made public to the astronomical community. In addition, we have reported 40 new close multiple systems and candidates rho < 3.3 arcsec and 36 overluminous stars that are assigned to young Galactic populations. In the new era of exoplanet searches around M dwarfs via transit (e.g. TESS, PLATO) and radial velocity (e.g. CARMENES, NIRPS+HARPS), this work is of fundamental importance for stellar and therefore planetary parameter determination.
The CARMENES search for exoplanets around M dwarfs. A homogeneous catalogue of projected rotational velocities accounting for limb-darkening
Instituto de Astrofísica de Andalucía, CSIC（安达卢西亚天体物理研究所，西班牙高等科学研究委员会）；INAF- Palermo Astronomical Observatory（意大利国家天体物理研究所巴勒莫天文台）；Institut für Astrophysik und Geophysik, Georg-August-Universität Göttingen（哥廷根大学天体物理学与地球物理学研究所）；Centro de Astrobiología, CSIC-INTA（天体生物学中心，西班牙高等科学研究委员会-国家航空航天技术研究所）；Universidad de Granada（格拉纳达大学）；Landessternwarte, Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学中心州立天文台）
提出一种结合真实临边昏暗模型的过采样卷积方法，从 CARMENES 光谱精确测量 M 矮星的投影自转速度，构建了目前最大的均匀星表，测量精度显著优于文献。
The Gaia GSP-Spec catalogue of interstellar extinctions, and stellar luminosities, radii, and masses
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学、蔚蓝海岸天文台、法国国家科学研究中心、拉格朗日实验室）；I.N.A.F., Osservatorio Astronomico di Trieste（意大利国家天体物理研究所、的里雅斯特天文台）
A homogeneous distance catalogue for Galactic RV Tauri objects
后AGB（PAGB）天体的一个子集是高度发光的金牛座RV变星，它们与II型造父变星有相似之处。通过使用已知的RV金牛座恒星的麦哲伦云的样本，我们能够确定周期光度关系（PLR）已被用来确定其银河系同行的光度在各个波段。我们已经收集了所有可用的测光，以便为每个对象生成SED并确定总积分通量。这个总通量与计算或推断的固有光度相结合，导致距离（Vickers et al. 2015）。这个距离目录使我们能够开始限制这个知之甚少的演化阶段的物理参数，并确定这些物理特征之间的联系作为其恒星星族的函数。
The white dwarf population of open clusters and their tidal tails. Tracers of contamination and stellar interactions
Astronomical Institute, Faculty of Mathematics and Physics, Charles University（查理大学数学与物理学院天文研究所）；Helmholtz-Institut für Strahlen- und Kernphysik, Universität Bonn（波恩大学亥姆霍兹辐射与核物理研究所）；Department of Physics and Astronomy, University of British Columbia（不列颠哥伦比亚大学物理与天文学系）；Department of Physics, University of Warwick（华威大学物理系）；Physics Division, National Center for Theoretical Sciences, National Taiwan University（台湾大学理论科学中心物理组）
The Type I Superluminous Supernova Catalogue II: Spectroscopic Evolution in the Photospheric Phase, Velocity Measurements, and Constraints on Diversity
