A 20-Second Cadence View of Solar-Type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Re-characterization of pi Men c
Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick Ball, Sarbani Basu, Timot… 展开作者
Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Joergen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. Garcia, Antonio Garcia Munoz, Charlotte Gehan, Lucia Gonzalez-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stephane Mathis, Savita Mathur, Mario J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakstiene, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Guenther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
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17 pages (excluding references), 13 figures, 6 tables; accepted for publication in AJ. Data and scripts to reproduce results are archived at https://zenodo.org/record/5555456
We present an analysis of the first 20-second cadence light curves obtained by the TESS space telescope during its extended mission. We find a precision improvement of 20-second data compared to 2-minute data for bright stars when binned to the same cadence (~10-25% better for T<~8 mag, reaching equal precision at T~13 mag), consistent with pre-flight expectations based on differences in cosmic ray mitigation algorithms. We present two results enabled by this improvement. First, we use 20-second data to detect oscillations in three solar analogs (gamma Pav, zeta Tuc and pi Men) and use asteroseismology to measure their radii, masses, densities and ages to ~1%, ~3%, ~1% and ~20% respectively, including systematic errors. Combining our asteroseismic ages with chromospheric activity measurements we find evidence that the spread in the activity-age relation is linked to stellar mass and thus convection-zone depth. Second, we combine 20-second data and published radial velocities to re-characterize pi Men c, which is now the closest transiting exoplanet for which detailed asteroseismology of the host star is possible. We show that pi Men c is located at the upper edge of the planet radius valley for its orbital period, confirming that it has likely retained a volatile atmosphere and that the "asteroseismic radius valley" remains devoid of planets. Our analysis favors a low eccentricity for pi Men c (<0.1 at 68% confidence), suggesting efficient tidal dissipation (Q/k <~ 2400) if it formed via high-eccentricity migration. Combined, these early results demonstrate the strong potential of TESS 20-second cadence data for stellar astrophysics and exoplanet science.
Asteroseismology of bright stars has become increasingly important as a method to determine fundamental properties (in particular ages) of stars. The Kepler Space Telescope initiated a revolution by detecting oscillations in more than 500 main-sequence and subgiant stars. However, most Kepler stars are faint, and therefore have limited constraints from independent methods such as long-baseline interferometry. Here, we present the discovery of solar-like oscillations in $α$ Men A, a naked-eye (V=5.1) G7 dwarf in TESS's Southern Continuous Viewing Zone. Using a combination of astrometry, spectro…
Context. There is currently a niche for providing high-cadence, high resolution, time-series optical spectroscopy from space, which can be filled by using a low-cost cubesat mission. The Belgian-led ESA CubeSpec mission is specifically designed to provide space-based, low-cost spectroscopy with specific capabilities that can be optimised for a particular science need. Approved as an ESA in-orbit demonstrator, the CubeSpec satellite's primary science objective will focus on obtaining high-cadence, high resolution optical spectroscopic data to facilitate asteroseismology of pulsating massive sta…
Over the last two decades, asteroseismology has increasingly proven to be the observational tool of choice for the study of stellar physics, aided by the high quality of data available from space-based missions such as CoRoT, Kepler, K2 and TESS. TESS in particular will produce more than an order of magnitude more such data than has ever been available before. While the standard TESS mission products include light curves from 120-sec observations suitable for both exoplanet and asteroseismic studies, they do not include light curves for the vastly larger number of targets observed by the missi…
The Transiting Exoplanet Survey Satellite (TESS) mission has provided photometric light curves for stars across nearly the entire sky. This allows for the application of asteroseismology to a pool of potential solar-like oscillators that is unprecedented in size. We aim to produce a catalogue of solar-like oscillators observed by TESS in the 120-second and 20-second cadence modes. The catalogue is intended to highlight stars oscillating at frequencies above the TESS 30-minute cadence Nyquist frequency with the purpose of encompassing the main sequence and subgiant evolutionary phases. We aim t…
Data from the Transiting Exoplanet Survey Satellite (TESS) has produced of order one million light curves at cadences of 120 s and especially 1800 s for every ~27-day observing sector during its two-year nominal mission. These data constitute a treasure trove for the study of stellar variability and exoplanets. However, to fully utilize the data in such studies a proper removal of systematic noise sources must be performed before any analysis. The TESS Data for Asteroseismology (T'DA) group is tasked with providing analysis-ready data for the TESS Asteroseismic Science Consortium, which covers…
Diverse Variability of O and B Stars Revealed from 2-minute Cadence Light Curves in Sectors 1 and 2 of the TESS Mission: Selection of an Asteroseismic Sample
The NASA Transiting Exoplanet Survey Satellite (TESS) is observing tens of millions of stars with time spans ranging from $\sim$ 27 days to about 1 year of continuous observations. This vast amount of data contains a wealth of information for variability, exoplanet, and stellar astrophysics studies but requires a number of processing steps before it can be fully utilized. In order to efficiently process all the TESS data and make it available to the wider scientific community, the TESS Data for Asteroseismology working group, as part of the TESS Asteroseismic Science Consortium, has created an…
Unveiling the properties of pulsating low-mass helium-core white dwarfs through TESS asteroseismology I. First results
Universidad Nacional de La Plata（拉普拉塔国立大学）；CONICET-UNLP（阿根廷国家科学研究委员会-拉普拉塔国立大学）；City University of New York Graduate Center（纽约市立大学研究生院）；KU Leuven（荷语鲁汶大学）；Queens College, City University of New York（纽约市立大学皇后学院）；Universitat Politècnica de Catalunya（加泰罗尼亚理工大学）；Boston University（波士顿大学）
Luminaries in the Sky: The TESS Legacy Sample of Bright Stars. I. Asteroseismic detections in naked-eye main-sequence and sub-giant solar-like oscillators
1D stellar evolution codes employ rudimentary treatments of turbulent convection. For stars with convective envelopes, this leads to systematic errors in the predicted oscillation frequencies needed for asteroseismology. One way of mending these structural inadequacies is through patching, whereby the outermost layers of 1D models are replaced by the mean stratifications from 3D simulations. In order to viably implement this approach in asteroseismic analysis, interpolation throughout precomputed 3D envelopes is required. We present a method that interpolates throughout precomputed 3D envelope…
We present the first near all-sky yield of oscillating red giants from the prime mission data of NASA's Transiting Exoplanet Survey Satellite (TESS). We apply machine learning towards long-cadence TESS photometry from the first data release by the MIT Quick-Look Pipeline to automatically detect the presence of red giant oscillations in frequency power spectra. The detected targets are conservatively vetted to produce a total of 158,505 oscillating red giants, which is an order of magnitude increase over the yield from Kepler and K2 and a lower limit to the possible yield of oscillating giants …
Asteroseismology and interferometry of the F7V spectroscopic binary $χ$ Draconis A in the TESS CVZ
Aarhus University（奥胡斯大学）；University of Sydney（悉尼大学）；Macquarie University（麦考瑞大学）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）
The Pan-Pacific Planet Search -- IX. A menagerie of companions orbiting evolved stars
University of Southern Queensland（南昆士兰大学）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Department of Astronomy & Astrophysics, University of Chicago（芝加哥大学天文与天体物理系）；Department of Physical Sciences, Kutztown University（库茨敦大学物理科学系）；Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney（悉尼大学物理学院悉尼天体物理研究所）；Institute for Astronomy, University of Hawai‘i（夏威夷大学天体物理研究所）；School of Physics, UNSW Sydney（新南威尔士大学悉尼分校物理学院）；Department of Physics, National University of Singapore（新加坡国立大学物理系）
Chronos --- Taking the pulse of our Galactic neighbourhood (ESA Voyage 2050 White Paper)
欧空局航行长期计划中考虑的2035- 2050年期间，将与银河系恒星成分表征方面的一系列可预见的进展相吻合。盖亚任务与大规模光谱调查相结合，正在帮助建立一个前所未有的银河系恒星星族天体测量、运动学和化学性质的普查。在十年内，对数亿颗恒星的这种性质的精确测量将成为可能。与此同时，由CoRoT和Kepler/K2发起并由TESS和PLATO等空间任务或LSST等地面项目进行的时域调查将使星震学达到高度成熟。将来自星震学的精确年龄与大型恒星样本的天体测量和光谱数据相结合，使银河系考古学家能够对银河系的组装历史获得新的见解。最近的突破-基于在数万颗红巨星中探测到类似太阳的振荡-证明了这种方法的潜力。因此，我们相信，全天空、高节奏、长时间的恒星变率调查将成为2035-50年期间的科学优先事项。这里提出的克罗诺斯概念是对盖亚的时域扩展。它将允许对距离太阳1.7千秒差距内的50万颗红巨星进行质量和年龄估计，从而为我们对银河系动力学和考古学的理解提供新的视角。在目标恒星方面，克罗诺斯将通过测量从亚巨星分支到早期AGB的恒星，弥合PLATO和LSST之间的差距。最后，它将在综合天空覆盖范围和观测持续时间（整个天空2 x 3.75个月，CVZ>5年）方面超过以前能够进行星震学的所有调查。
A Homogeneous Catalog of Oscillating Solar-Type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Columbia University（哥伦比亚大学）；University of Hawai‘i（夏威夷大学）；University of Sydney（悉尼大学）；Princeton University（普林斯顿大学）
Asteroseismology is used to infer the interior physics of stars. The \textit{Kepler} and TESS space missions have provided a vast data set of red-giant light curves, which may be used for asteroseismic analysis. These data sets are expected to significantly grow with future missions such as \textit{PLATO}, and efficient methods are therefore required to analyze these data rapidly. Here, we describe a machine learning algorithm that identifies red giants from the raw oscillation spectra and captures \textit{p} and \textit{mixed} mode parameters from the red-giant power spectra. We report algori…
