The Infrared Surface Brightness technique applied to RR Lyrae stars from the solar neighborhood
Bartłomiej Zgirski, Wolfgang Gieren, Grzegorz Pietrzyński, Marek Górski, Piotr Wielgórski, Jesper Storm, Garance Bras, Pierre Kervella, Nicolas Nardetto, Gergel… 展开作者
Bartłomiej Zgirski, Wolfgang Gieren, Grzegorz Pietrzyński, Marek Górski, Piotr Wielgórski, Jesper Storm, Garance Bras, Pierre Kervella, Nicolas Nardetto, Gergely Hajdu, Rolf Chini, Martin Haas
The Baade-Wesselink method allows us to estimate distances to individual pulsating stars. Accurate geometric parallaxes obtained by the Gaia mission serve us in the calibration of the method and in the determination of its precision. The method also provides a way of determining mean radii of pulsating stars. The main aim of this work is to determine the scatter and possible dependence of p- factors of RR Lyrae stars on their pulsation periods. The secondary objective is to determine mean radius - period relations for these stars. Our calibrations for RR Lyrae stars are based on photometric data gathered at the Cerro Murphy Observatory. We obtained spectroscopic data specifically for this project using high resolution spectrographs. We use the Infrared Surface Brightness (IRSB) version of the method that relies on a surface brightness - color relation dependent on the (V-K) color. We obtain the spread of p- factors of around 0.07-0.08 for our sample of 9 RR Lyrae stars from the solar neighborhood. However, we also find relations between the p-factor and the pulsation period for RRab stars with the rms scatter around the relation of around 0.05, but with relatively large uncertainty of relations' parameters. We present relations between the mean radius and period for RR Lyrae pulsating in the fundamental mode with the rms scatter around the relation of $0.012R_{\odot}$. We observe a clear offset between p- factors obtained using the IRSB technique (with mean p between 1.39 and 1.45) and values inferred by Bras et al. (2024) using the SPIPS tool (Mérand et al. 2015). On the other hand, we obtain a similar scatter of p of as observed by Bras et al. (2024). Our period-radius relations are in a good agreement with both the inference of Bras et al. (2024) based on SPIPS and theoretical predictions of Marconi et al. (2005, 2015)
Distance to the Globular Cluster M 3 from the Infrared Surface Brightness Technique applied to RR Lyrae stars
Universidad de Concepción（孔塞普西翁大学）；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）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；Université Côte d’Azur（蔚蓝海岸大学）；Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸天文台，法国国家科学研究中心，拉格朗日实验室）；Instituto de Alta Investigación, Universidad de Tarapacá（塔拉帕卡大学高等研究院）；LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité（巴黎天文台低层大气研究、星体和宇宙学实验室，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎西岱大学）
Kepler Pixel Project -- background RR Lyrae stars in the primary Kepler mission field of view
在本文中，我们描述了一个项目，我们开始调查个人像素在下载的开普勒孔径，以找到对象的主要目标的背景中具有可变亮度。在本系列的第一篇论文中，我们发现并研究了547个短周期食双星（Bienias et al. 2021）。在这里，我们提出了26个新的RR天琴座恒星的开普勒背景像素在主要任务期间获得的独立发现，并提供这些对象的连续和精确的测光。这些恒星中有21颗已经被盖亚或泛星巡天发现。这个新的主要是微弱和遥远的RR天琴座恒星的人口增加了50%，很好地补充了52个已知的主要目标RR天琴座恒星在原来的开普勒领域。尽管它们很微弱，但这些恒星的四年准不间断光变曲线让我们可以前所未有地看到这些微弱的光环物体。我们提出了一个新的RR天琴座样本的光变曲线的分析，验证他们的分类使用傅立叶参数，并讨论这些新发现的脉动变星的属性。最值得注意的是，这是第一次在光度数据集的帮助下，以出色的节奏和精度对这种微弱的RR型天琴座恒星进行了研究。有趣的是，这些对象共享其较亮的兄弟姐妹在子类特征，附加模式内容和调制发生率方面的属性。
The Solar Neighborhood LIV: 54 Orbits of M Dwarf Multiples within 30 Parsecs with Speckle Interferometry at SOAR
Five College Astronomy Department, Smith College（史密斯学院五校天文系）；RECONS Institute（RECONS研究所）；Cerro Tololo Inter-American Observatory — NSF’s NOIRLab（塞罗托洛洛美际观测台—NSF的NOIRLab）；Bridgewater State University（布里奇沃特州立大学）；Department of Physics and Astronomy, Georgia State University（佐治亚州立大学物理与天文学系）；Department of Physics, Southern Connecticut State University（南康涅狄格州立大学物理系）
