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89 results for “tess”
TESS-APRIL-2018
<p>STARS4ALL Photometer Network (April 2018)</p>
TESS-MAY-2018
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). May 2018</p>
TESS-JUNE-2018
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). June 2018</p>
TESS-JULY-2018
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). July 2018</p>
TESS-SEPTEMBER-2018
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). September 2018</p>
A synthetic sample of short-cadence solar-like oscillators for TESS
<p>These are the simulated lightcurves for a synthetic sample of short-cadence solar-like oscillators as they might be observed by the Transiting Exoplanet Survey Satellite (TESS), as presented by Ball et al. (2018), "A synthetic sample of short-cadence solar-like oscillators for TESS". </p> <p>Each zip file contains the FITS lightcurves and mode data for stars observed in one sector, starting in the southern ecliptic hemisphere. The CSV file contains a selection of data contained in the FITS headers.</p> <p>For more detail, read the paper on <a href="https://arxiv.org/abs/1809.09108">arXiv</a>.</p> <p>Note that the FITS headers incorrectly report the units of the white noise level as <span class="math-tex">\(\mathrm{ppm}\)</span> rather than <span class="math-tex">\(\mathrm{ppm}\cdot\mathrm{hr}^{1/2}\)</span>. The white noise level excludes any systematic component, which should be added in quadrature if desired.</p>
TESS-OCTOBER-2018
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). October 2018</p>
TESS-DECEMBER-2018
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). December 2018</p>
TESS-FEBRUARY-2019
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). February 2019</p>
TESS-MARCH-2019
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). March 2019</p>
TESS-APRIL-2019
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). April 2019</p>
TESS-JUNE-2019
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). June 2019</p>
TESS-MAY-2019
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). May 2019</p>
Complementary figures for paper 'The ESO UVES/FEROS Large Programs of TESS OB pulsators II. On the physical origin of macroturbulence'
<p>These are figures from Appendices C and D of the paper <strong>'The ESO UVES/FEROS Large Programs of TESS OB pulsators II. On the physical origin of macroturbulence' (Serebriakova et al. Accepted on 17 Oct 2024 for publication in A&A)</strong>. Appendices C and D are moved to Zenodo following the request of the editor. The figures demonstrate MESA model properties used to compare with observed macroturbulent velocities in massive stars. Appendix C focuses on emphasising the role of opacity bumps and subsurface convection throughout evolution. Appendix D explores wave propagation in these models.</p> <p><strong>Appendix C: MESA internal profiles</strong>. Each figure contains a grid of model internal profiles of stellar properties computed with MESA. Initial mass varies in rows: 60, 20, 12, 7, and 3 Solar masses. In columns, three evolutionary stages are presented: MS, TAMS, and Hertzsprung gap. Models in Fig.1-4 were computed with Solar metallicity Z=0.014, and in Fig. 5-8 - with LMC metallicity Z=0.006. Fig. 1,5 - opacity and convective velocity VS temperature, Fig. 2,6 - opacity and convective velocity VS radius(zoomed), Fig. 3,7 - opacity and convective velocity VS radius(full), Fig. 4,8 - Sign of squared Brunt-Väisälä frequency and convective velocity as a fraction of sound speed VS radius. See the paper for details. </p> <p><strong>Appendix D: Propagation diagrams</strong>. Each figure contains a grid of propagation diagrams (shaded with g-modes and p-modes cavities) computed for the same models as before. Fig. 3 and 6 are complemented with tunnelling frequency omega_min - see 'Section 5: On wave tunnelling through subsurface convective layers' for details with examples in Fig. 8 of the paper. </p> <p> </p>
MOBSTER: Identifying Candidate Magnetic O Stars through Rotational Modulation of TESS Photometry
<p>O-type stars display rotational modulation of their photometric brightness due to surface features induced by fossil magnetic fields, and possibly through dynamos driven by subsurface convection. These features introduce wind perturbations that may drive large-scale structures and flows, including magnetospheres and corotating interaction regions. Until recently there has been a lack of high-precision, high-cadence photometry of O stars capable of detecting this variability. The wealth of new observations provided by the Transiting Exoplanet Survey Satellite (TESS) offers an unparalleled opportunity to conduct comprehensive studies of O-star variability at the sub-mmag level. Using the Galactic O-Stars Catalogue (GOSC) we have identified a sample of confirmed Galactic O stars observed by TESS with existing high-resolution spectroscopy from the IACOB and OWN surveys. Frequency analysis of the photometry is preceded by a careful examination of potential blending sources. Existing spectroscopy of each candidate is employed to test the rotational modulation hypothesis. In this presentation we describe the preliminary results of our study and outline plans for future analysis.</p>
Starspot mapping with adaptive parallel tempering. II. Application to TESS data for M-dwarf flare stars, AU Microscopii, YZ Canis Minoris, and EV Lacertae (Flare Tables)
<p>For TESS PDC-SAP data of AU Mic (Sector 1 and 27), YZ CMi (Sector 7 and 34), and EV Lac (Sector 16), detected flare properties are listed: the peak time (BJD-2745000), amplitude, equivalent duration (sec), and e-folding time (day).</p>
Supplement to "Transient Corotating Clumps Around Adolescent Low-Mass Stars From Four Years of TESS"
<p>This repository contains supplementary materials for the paper "Transient Corotating Clumps Around Adolescent Low-Mass Stars From Four Years of TESS", which will be submitted to the AAS journals in 2023.</p> <p><em>fig3_validation_plots.tar.gz</em> is a supplement to Figure 3 of the manuscript, and contains 240 pdf files for the 66 stars of interest.<br> <em>table1_MRT.csv</em> is a pipe-separated CSV version of Table 1 with all useful columns.<br> <em>table1_README.txt</em> is a README describing the columns in table1_MRT.csv and table1_short.csv.<br> <em>table1_short.csv</em> is a truncated version of <em>table_MRT.csv </em>with the columns displayed in the manuscript.</p>
TESS-NOVEMBER-2019
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). November 2019</p>
TESS-AUGUST-2020
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). August 2020</p>
TESS-JULY-2020
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). July 2020</p>
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