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89 results for “tess”
TESS-validated Gaia DR3 Pulsating Variables of δ Scuti and γ Doradus: II. 360+ Eclipsing Binaries with δ Scuti and γ Doradus Components
<div> <div> <div> <p>I present serendipitous discoveries of 380 eclipsing binaries with δ Scuti and γ Doradus pulsators, 46 eclipsing binaries exhibiting rotational variability, and 8 new RR Lyrae stars, identified for the first time during a validation project of pulsating variables from Gaia Data Release 3. Gaia DR3 Part 4 Variability released 12.4 million variables, including 748,058 pulsating variable stars of `DSCT|GDOR|SXPHE' types among the variability classification results of all classifiers -- 9,976,881 objects (in the file vclassre.dat, https://cdsarc.cds.unistra.fr/viz-bin/cat/I/358}). Among 75,369 analyzed stars, I confirmed 12,145 δ Scuti stars (including 8,710 new) and 8,192 γ Doradus stars (including 7,531 new). This work has significantly expanded the bona fide DSCT and GDOR catalogs to include 98,968 and 19,466 stars, respectively, providing a valuable resource for future studies. The discovery of the remarkable number of pulsating binaries underscores the significance of this project in validating Gaia’s variable star catalog. </p> </div> </div> </div> <p>The attached CSV files report the current validation results. If you use any data from the catalogs in your research, I appreciate your citation to the paper: </p> <p><strong>Zhou, A.-Y., 2024, Research Notes of the AAS, Volume 8, Number 4, 110 (ADS bibcode: 2024RNAAS...8..110Z) </strong></p> <ul> <li>CSV file GaiaDR3_vari_DSCTgDorSXPhe_Validated_R2_NewEB_Pul.csv for the newly identified Eclipsing Binaries with Pulsating components;</li> <li>CSV file GaiaDR3_vari_DSCTgDorSXPhe_Validated_R2.csv for the entire validated and newly identified results from 75,369 analyzed samples.</li> </ul> <p>This is a developing story. Check back for updates.</p>
TESS Network Motivation Survey
<p>The TESS Network motivation study was conducted within the ongoing H2020 project named <a href="https://actionproject.eu/">ACTION</a> (pArticipatory sCience Toolkit agaInst pollutiON) on citizen science. Volunteers participate to citizen science initiatives for multiple reasons: personal enjoyment, desire for improvement or achievement, establishment of personal relationships, care for the environment, etc.</p> <p>Studying motivation and investigating the factors influencing people participation to citizen science projects is an essential aspect in the analysis of citizen science communities. Understanding the reasons that foster people to engage can support the successful design and implementation of effective participant involvement tasks, as well as pave the way for long-term engagement.</p> <p>The goal of the study is to analyse the motivation to participate of a specific citizen science community focused on fighting light pollution: the network of around 120 hosts of the <a href="https://tess.stars4all.eu/">TESS photometers</a>. Volunteers of this network accepted to host and install sensors to monitor sky brightness in order to collect data for measuring the level of light pollution in many areas of the Earth.<br> The volunteers are very diverse: professional astronomers, amateur astronomers, light pollution fighters, astronomical outreach (museum, planetarium, dark sky association, etc.), astro-tourism actors, public administrations and others.</p> <p>The TESS Network Survey motivation study is part of the study about motivation in citizen science projects conducted within the ACTION project (<a href="https://doi.org/10.5281/zenodo.5753092">https://doi.org/10.5281/zenodo.5753092</a>). The survey was designed and administered using the <a href="https://coney.cefriel.com/">Coney</a> toolkit.</p> <p>The research object adopts the <a href="https://www.researchobject.org/ro-crate/1.0/">RO-Crate</a> specification. Files made available within the research object are:</p> <ul> <li><em>*-procedure.ttl</em> contains the RDF representation of the structure of the conversational survey (questions, answers, etc.) using the <a href="https://w3id.org/survey-ontology">Survey Ontology</a></li> <li><em>*-results.ttl </em>contains the RDF representation of the answers collected using the <a href="https://w3id.org/survey-ontology">Survey Ontology</a></li> <li><em>*-survey.tll </em>contains a comprehensive RDF representation of the survey data using the <a href="https://w3id.org/survey-ontology">Survey Ontology</a></li> <li><em>*-results.csv </em>contains the CSV of the collected answers</li> <li>*-<em>script.R</em> is the R script developed to analyse the collected answers</li> <li>*-<em>mean-var-motivating-questions.csv </em>contains the computed mean and average for each question considered (observable variables)</li> <li>*-<em>mean-var-motivating-factor.csv </em>contains the computed mean and average for each motivation factor considered (latent variables)</li> <li>*-<em>correlation-factors-global-motivation.csv </em>contains the correlation analysis between each motivation factor and the global motivation </li> </ul> <p>A <a href="https://doi.org/10.5281/zenodo.4066914">poster</a> and a <a href="https://doi.org/10.22323/2.20060203">paper</a> describing the study are additional resources referenced by the research object.</p>
MCMC samples of the posterior distribution from the paper "TESS spots a mini-neptune interior to a hot saturn in the TOI-2000 system"
<p>This dataset contains the Hamiltonian Monte Carlo samples of the posterior distribution of the planetary and stellar parameters from the paper "TESS Spots a Mini-Neptune Interior to a Hot Saturn in the TOI-2000 System". The file format, NetCDF, is based on HDF5, and is meant to be read by the Python package <a href="https://python.arviz.org/en/latest/">ArviZ</a>.</p> <p>Hot jupiters (<em>P</em> < 10 d, <em>M</em> > 60 M<sub>⊕</sub>) are almost always found alone around their stars, but four out of hundreds known have inner companion planets. These rare companions allow us to constrain the hot jupiter's formation history by ruling out high-eccentricity tidal migration. Less is known about inner companions to hot Saturn-mass planets. We report here the discovery of the TOI-2000 system, which features a hot Saturn-mass planet with a smaller inner companion. The mini-neptune TOI-2000 b (2.70 ± 0.15 R<sub>⊕</sub>, 11.0 ± 2.4 M<sub>⊕</sub>) is in a 3.10-day orbit, and the hot saturn TOI-2000 c (<span class="math-tex">\(8.14^{+0.31}_{-0.30}\)</span> R<sub>⊕</sub>, <span class="math-tex">\(81.7^{+4.7}_{-4.6}\)</span> M<sub>⊕</sub>) is in a 9.13-day orbit. Both planets transit their host star TOI-2000 (TIC 371188886, <em>V</em> = 10.98, <em>TESS</em> magnitude = 10.36), a metal-rich ([Fe/H] = <span class="math-tex">\(0.439^{+0.041}_{-0.043}\)</span>) G dwarf 174 pc away. <em>TESS</em> observed the two planets in sectors 9–11 and 36–38, and we followed up with ground-based photometry, spectroscopy, and speckle imaging. Radial velocities from HARPS allowed us to confirm both planets by direct mass measurement. In addition, we demonstrate constraining planetary and stellar parameters with MIST stellar evolutionary tracks through Hamiltonian Monte Carlo under the PyMC framework, achieving higher sampling efficiency and shorter run time compared to traditional Markov chain Monte Carlo. Having the brightest host star in the <em>V</em> band among similar systems, TOI-2000 b and c are superb candidates for atmospheric characterization by the JWST, which can potentially distinguish whether they formed together or TOI-2000 c swept along material during migration to form TOI-2000 b.</p>
15000 Ellipsoidal Binary Candidates in TESS: Associated Tables
<p>A catalogue of 15779 candidate ellipsoidal binary systems, identified from the first two years of TESS full-frame images.</p> <p>Table 2 contains the 'BEER' score applied to approximately 8,000,000 input TESS targets.</p> <p>Table 3 contains the details of the 15779 selected candidates.</p> <p>Full details of both tables, and the selection process, can be found in the associated paper.</p> <p>https://arxiv.org/abs/2211.06194</p>
TESS Confirmed and First Identified SuperWASP Variable Stars
<p>This catalog consists of the TESS-confirmed and First Identified SuperWASP Variable Stars of types $\delta$ Scuti, $\gamma$ Doradus, RR Lyrae, eclipsing binary systems with pulsating components, rotating variables, and others. This dataset is part of a short summary submitted to RNAAS entitled "Identifying SuperWASP Detected Candidate Variables with TESS" (Zhou, A.-Y., 2023 Research Notes of the AAS, vol.7). </p><p> </p>
Tess dataset - September 2016
<p>This datasets corresponds to the measures taken by the STARS4ALL photometer network during the month of September(2016).</p>
Data affiliated with "Evolution of Flare Activity in GKM Stars Younger than 300 Myr over Five Years of TESS Observations"
<p>Data and Python scripts affiliated with the publication "Evolution of Flare Activity in GKM Stars Younger than 300 Myr over Five Years of TESS Observations" in the American Astronomical Journals. The manuscript pre-print can be found on <a href="https://arxiv.org/abs/2405.00850">arXiv</a>.</p> <p>This repository contains all of the data used to complete the analysis of the aforementioned manuscript, along with the Python scripts used to create all of the figures in the manuscript. Many of the data products from this manuscript are saved as CSVs, with appropriate column names and units, when applicable.</p> <p>Additionally, we include the light curves for all targets in this sample, along with the 'probability light curves,' which were used to identify flares in the TESS data. These data products can be found in the zip file 'TESS_stella_outputs.zip'. The rest of the data product is structured as it is on the <a href="https://github.com/afeinstein20/young-stellar-flares/tree/paper">associated GitHub repository</a>.</p>
Data for `Identifying New Pulsating Variables and Eclipsing Binaries Using TESS Data'
<p>This study presents a series of surveys using TESS data to identify new δ Scuti and γ Doradus stars, as well as eclipsing binaries with pulsating components. Preliminary catalogs of newly discovered variables are being made publicly available to encourage community use as the project progresses. Please visit this website for updates. </p> <p> 1. New δ Scuti stars, γ Doradus stars, and eclipsing binaries from a subset of 709,000 selected AF-type stars observed by TESS. Version 4.5 is an update to Version 4.0 (the first release for Part IV), while Part III was provided in Version 3.0.</p> <p> The attached CSV file <strong>NewVar_AF50w_R2.csv,</strong> contains the catalog of newly identified variables from Phases I and II of the survey (i.e. R2 includes R1 from Version 3.0). The accompanying file <strong>ms2RNAAS_2025AF50w_IV.pdf</strong> is the initial draft describing the Phase-II identifications. The published paper can be found in 2025 <em>Research Notes of the AAS</em>, <strong>Vol. 9, No. 1, 23</strong> (Zhou 2025, https://iopscience.iop.org/article/10.3847/2515-5172/adaf8c (ADS code: 2025RNAAS...9...23Z). These unpublished discoveries have been compiled into catalogs of δ Scuti and γ Doradus stars available at Zenodo https://zenodo.org/records/17096360 (DOI: <a href="https://doi.org/10.5281/zenodo.17096360">10.5281/zenodo.17096360</a>) -- which currently include <strong>118,410</strong> and <strong>41,622</strong> entries, respectively, as of the release date.</p> <p> 2. New Pulsating Variable Stars and Eclipsing Binaries around BL Cam (added in Version 2.0)</p> <p> The attached CSV file NewVar_BLCam_R2D.csv provides a catalog of the new variables with the following columns: TIC ID, Simbad main ID, Gaia DR3 ID, RA_deg Dec_deg(J2000), Tmag, Teff, SpType, Lum, logg, mass, VarType_Notes</p> <p> 3. New Pulsating Variable Stars and Eclipsing Binaries near NGC 6302 (Version 1.0)</p> <p> Check corresponding files containing the string "NGC 6302".</p>
Variability of OB stars from TESS southern Sectors 1-13 and high-resolution IACOB and OWN spectroscopy
<p>Typical MESA and GYRE inlists associated with <a href="https://arxiv.org/abs/2005.09658">Burssens et al. 2020</a>. MESA v. 12155, GYRE version v. 5.2.</p> <p><em>Context:</em> Lack of high-precision long-term continuous photometric data for large samples of stars has prevented the large-scale exploration of pulsational variability in the OB star regime. As a result, the candidates for in-depth asteroseismic modelling remained limited to a few tens of dwarfs. The TESS nominal space mission has surveyed the southern sky, including parts of the galactic plane, yielding continuous data of at least 27 d for hundreds of OB stars.<br> <em>Aims:</em> We aim to couple TESS data in the southern sky with ground-based spectroscopy to study the variability in two dimensions, mass and evolution. We focus mainly on the presence of coherent pulsation modes that may or may not be present in the predicted theoretical instability domains and unravel all frequency behaviour in the amplitude spectra of the TESS data.<br> <em>Methods: </em>We compose a sample of 98 OB-type stars observed by TESS in Sectors 1-13 and with available multi-epoch, high-resolution spectroscopy gathered by the IACOB and OWN surveys. We present the short-cadence 2-min light curves of dozens of OB-type stars, that have one or more spectra in the IACOB or OWN database. Based on these light curves and their Lomb-Scargle periodograms we perform variability classification and frequency analysis. We place the stars in the spectroscopic Hertzsprung-Russell diagram to interpret the variability in an evolutionary context.<br> <em>Results:</em> We deduce diverse origins of the mmag-level variability found in all of the 98 OB stars in the TESS data. We find among the sample several new variable stars, including three hybrid pulsators, three eclipsing binaries, high frequency modes in a Be star, and potential heat-driven pulsations in two Oe stars. <br> <em>Conclusions:</em> We identify stars for which future asteroseismic modelling is possible, provided mode identification is achieved. By comparing the position of the variables to theoretical instability strips we discuss the current shortcomings in non-adiabatic pulsation theory, and the distribution of pulsators in the upper Hertzsprung-Russell diagram.</p> <p> </p> <p> </p>
TESS November 2016
<p>Dataset with the measures taken by STARS4ALL photometers network.</p>
TESS January 2017
<p>Dataset with the measures taken by STARS4ALL photometers network</p>
Planetary perturbers: Flaring star-planet interactions in Kepler and TESS
<p>This data set contains:</p> <p>a. almost 13,000 de-trended Kepler and TESS light curves used in the publication with the same title (Ilin et al. 2024). Each light curve is a fits file with the Kepler or TESS identifier, Quarter or Sector, and, if there are multiuple light curves per Quarter/Sector, the number of the light curve. The light curves can be read with any fits file handler (e.g., astropy), or with the lightkurve package. Each light curve contains arrays for the flux, detrended flux, time, and orbital phase of the innermost planet. Note that for transiting planets the orbital phase is set to zero around transit midtime, while for non-transiting planets, the phase zero is set arbitrarily. There is no particular reason for splitting the data in the zip files except for easier upload.</p> <p>b. Tables 1-4 from Ilin et al. (2024). Tables 1 and 3 are combined into one. Each table includes a description of its columns at the top.</p> <p><a href="https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.3395I/abstract"><strong>Ilin et al. (2024)</strong></a> Ilin, E., Poppenhäger, K., Chebly, J., Ilić, N., Alvarado-Gómez, J.~D.</p> <p>Planetary perturbers: flaring star-planet interactions in Kepler and TESS.</p> <p>Monthly Notices of the Royal Astronomical Society 527, 3395–3417.</p> <p>doi:10.1093/mnras/stad3398</p>
Signal-to-Noise Ratios, DYNAMITE Posteriors, and Combined Detectability Plots for 173 TESS Multi-Planet Systems
<p>Collection of figures for 173 TESS Multi-Planet Systems. Each figure (titled with the system's TOI number) has 2 rows of planets, corresponding to results from the clustered period model (upper) and period ratio model (lower) predictions for an additional planet in each system. The left-most column of the plots show the signal-to-noise ratios (SNR) of simulated transits for planets with a given radius and period in the corresponding TESS light curve. The middle column shows the dot product of the radius and period posteriors generated by DYNAMITE using TESS light curves up to and including Sector 76. The right-most column shows the detectability (SNR) modulated by the DYNAMITE posteriors, showing the location in (P, Rp) space where an additional planet in this system is most likely to be detected under each model.</p>
scatterbrain: TESS Sector 2 Backdrop Files
<p>This is a preliminary upload of the driver files for scatterbrain, for TESS sector 2, camera1. </p>
supplementary materials: Classifying Be star variability with TESS I: the southern ecliptic
<p>The archived files contain ascii light curves (LC_data.tgz) and plots (LC_plots.tgz) from TESS cycle 1 for the Be star sample of "Classifying Be star variability with TESS I: the southern ecliptic". The light curve files have columns: 1) TESS JD (JD - 2457000), 2) relative flux, 3) photometric error. </p>
TESS-September-2017
<p>Measurements of the STARS4ALL Photometers Network</p>
Light Curve and Target Data for "M-Dwarf Flare Candidates Simultaneously Observed by K2 and TESS"
<p>This repository contains light curves and data from the study conducted in the research note titled "M-Dwarf Flare Candidates Simultaneously Observed by K2 and TESS".</p> <p>Each file contains a light curve (produced outputs from PyVAN (<a href="https://ui.adsabs.harvard.edu/abs/2019AJ....158..119L/abstract" rel="nofollow">https://ui.adsabs.harvard.edu/abs/2019AJ....158..119L/abstract</a>, <a href="https://github.com/kdlawson/pyvan">https://github.com/kdlawson/pyvan</a>), modfied to easily distinguish between K2/TESS data) for each target flagged with a flaring event. Files titled #T indicate TESS data and #K indicates K2 data. </p> <p>Overlap plots are included (titled Shape#) for those which were clearly defined by TESS, but not seen by K2.</p> <p>See Table 1 for specific target identification and measurements.</p> <p>Targets 11, 20, 27, and 28 saw K2 detections that we believe to be false positives based on lack of structure and substanstial supporting evidence from TESS.</p> <p>Finally a .csv is included with the information for all targets observed in this study.</p>
TESS-January-2018
<p>STARS4ALL Photometer Network (January 2018)</p>
TESS-MARCH-2018
<p>STARS4ALL Photometer Network (March 2018)</p>
TESS-FEBRUARY-2018
<p>STARS4ALL Photometer Network (February 2018)</p>
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