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89 results for “tess”
Tess December 2016
<p>Dataset with the measures taken by STARS4ALL photometers network</p>
Supplementary material for "Stellar flare morphology with TESS across the main sequence"
<p>Online material for the paper titled "Stellar flare morphology with TESS across the main sequence". The dataset includes the manually flagged TESS light curves used to train the <em>flatwrm2</em> flare detection algorithm (<a href="https://github.com/vidakris/flatwrm2" target="_blank" rel="noopener">https://github.com/vidakris/flatwrm2</a>), the final manually vetted flare catalog, the extracted flare profiles, and Jupyter notebooks demonstrating how the data can be used.</p> <h2>Files</h2> <ul> <li><strong>flatwrm2_training_set.tar.gz</strong>: TESS 2-min cadence light curves used to train <em>flatwrm2</em> for flare detection. All files contain three columns, time in TBJD, PDCSAP flux, and a 1/0 flag for flare/not flare. Files are sorted into three directories:<br> <ul> <li>active_stars: Selected active stars up to sector 40 for the original training set of <em>flatwrm2</em>, 208 light curves.</li> <li>random_sample: Random stars up to sector 40 for the original training set of <em>flatwrm2</em>, 8000 light curves. Only a small fraction of them is flaring.</li> <li>new_selection: New selection of stars up to sector 69, 4631 light curves. It includes flaring and non-flaring stars, and also known astrophysical false positives (e.g., RR Lyrae stars). See Sect. 2.2 of the paper for details.</li> </ul> </li> <li><strong>Table2_flaring_star_catalog.csv</strong>: Catalog of flaring stars (Table 2 in the paper)</li> <li><strong>Table3_flare_catalog.csv</strong>: TESS flare catalog, including only the correctly extracted flares, with the same length as TESS_flare_shapes.dat (Table 3 in the paper)</li> <li><strong>Table3_flare_catalog_not_extracted.csv</strong>: Continuation of the TESS flare catalog, including only the incorrectly extracted flares (Table 3 in the paper). As most calculated parameters are probably erroneous, only the flare peak times are reported.</li> <li><strong>TESS_flare_shapes.dat</strong>: Scaled and interpolated TESS flare shapes, one flare profile for each entry in Table3_flare_catalog.csv</li> <li><strong>TESS_original_flare_shapes_time.dat</strong>: Times for the scaled, but not interpolated flares</li> <li><strong>TESS_original_flare_shapes_flux.dat</strong>: Fluxes for the scaled, but not interpolated flares</li> <li><strong>Table6_solar_flare_catalog.csv</strong>: Solar flare parameters from SDO/EVE (Table 6 in the paper). <em>Note:</em> the SDO/EVE data products have a version number in the URL. We used version 7 for the analysis, but it can change after major updates in the SDO data processing pipeline. Please change the URL accordingly, if you have issues accessing the data (e.g., 007 --> 008).</li> <li><strong>solar_flare_shapes.dat</strong>: Scaled and interpolated solar flare profiles from SDO/EVE, one flare profile for each entry in Table6_solar_flare_catalog.csv</li> <li><strong>01_Loading_data.ipynb</strong>: A Jupyter notebook demonstrating how the above datasets can be used</li> <li><strong>02_Sampling_flare_shapes.ipynb</strong>: A Jupyter notebook demonstrating how flare shapes can be sampled (Sect. 4.2 in the paper)</li> <li><strong>03_Locating_similar_flares.ipynb</strong>: A Jupyter notebook demonstrating how flares similar to an input shape can be located in the catalog (Sect. 4.3 in the paper)</li> </ul>
On following pages: 424. Black-and-orange Myotis (Myotis formosus); 425. Geoffroy's Myotis (Myotis emarginatus); 426. Temminck's Myotis (Myotis tricolon; 427. Welwitsch''s Myotis (Myotis welwitschii); 428. Reddish-black Myotis (Myotis rufonigen; 429. Scott's Myotis (Myotis scott); 430. Morris's Myotis (Myotis morrisi); 431. Bocage's Myotis (Myotis bocagil); 432. Malagasy Myotis (Myotis goudoti); 433. Anjouan Myotis (Myotis anjouanensis); 434. Kock's Myotis (Myotis dieteri); 435. Alcathoe Whiskered Myotis (Myotis alcathoe); 436. Hyrcanian Myotis (Myotis hyrcanicus); 437. Pond Myotis (Myotis dasycneme); 438. lkonnikov's Myotis (Myotis ikonnikovi); 439. Sichuan Myotis (Myotis altarium); 440. Common Whiskered Myotis (Myotis mystacinus); 441. David's Myotis (Myotis davidii); 442. Valley Myotis (Myotis ancricola); 443. Anna Tess's Myotis (Myotis annatessae);, 444. Gomantong Myotis (Myotis gomantongensis); 445. Peters's Myotis (Myotis ater); 446. Nepalese Whiskered Myotis (Myotis muricola); 447. Brown's Whiskered Myotis (Myotis brown); 448. Insular Myotis (Myotis insularum). in Vespertilionidae
On following pages: 424. Black-and-orange Myotis (Myotis formosus); 425. Geoffroy's Myotis (Myotis emarginatus); 426. Temminck's Myotis (Myotis tricolon; 427. Welwitsch''s Myotis (Myotis welwitschii); 428. Reddish-black Myotis (Myotis rufonigen; 429. Scott's Myotis (Myotis scott); 430. Morris's Myotis (Myotis morrisi); 431. Bocage's Myotis (Myotis bocagil); 432. Malagasy Myotis (Myotis goudoti); 433. Anjouan Myotis (Myotis anjouanensis); 434. Kock's Myotis (Myotis dieteri); 435. Alcathoe Whiskered Myotis (Myotis alcathoe); 436. Hyrcanian Myotis (Myotis hyrcanicus); 437. Pond Myotis (Myotis dasycneme); 438. lkonnikov's Myotis (Myotis ikonnikovi); 439. Sichuan Myotis (Myotis altarium); 440. Common Whiskered Myotis (Myotis mystacinus); 441. David's Myotis (Myotis davidii); 442. Valley Myotis (Myotis ancricola); 443. Anna Tess's Myotis (Myotis annatessae);, 444. Gomantong Myotis (Myotis gomantongensis); 445. Peters's Myotis (Myotis ater); 446. Nepalese Whiskered Myotis (Myotis muricola); 447. Brown's Whiskered Myotis (Myotis brown); 448. Insular Myotis (Myotis insularum).
CARMA determined light curves and PSDs to accompany ApJ publication Optical Variability Properties of Southern TESS Blazars
<p>A collection of all Figures included in Appendix D of Optical Variability Properties of Southern TESS Blazars (Dingler & Smith 2024).</p>
Quaver regressed light curves to accompany ApJ publication Optical Variability Properties of Southern TESS Blazars
<p>A collection of all Figures included in Appendix A of Optical Variability Properties of Southern TESS Blazars (Dingler & Smith 2024).</p>
Data for Exploration of Stellar Variability in 20-second Cadence TESS Data
<p>This repository contains code, data, and plots related to "Exploration of Stellar Variability in 20-second Cadence TESS Data" by DeVane-Purgh et al. 2024, associated with the RNAAS manuscript number AAS5813. </p> <p>This repository contains the light curves created in this process, the code necessary to create them, the code used for analysis, and the plotting script used in the paper (Final Corrections and Plots_JT.ipynb) . It also includes some of the validation plots and so forth used to examine the lightcurves, and scripts to download the data directly from MAST. README.md explains the purpose of each file. </p> <p>For ease of use, it is possible to download either individual files, or the entire (zipped) archive tess_zenodo.zip</p>
Contamination in TESS light curves: The case of the Fast Yellow Pulsating Supergiants
<p>MESA 22.11.1 inlist files used to create Fig. 1 of the paper "Contamination in TESS light curves: The case of the Fast Yellow Pulsating Supergiants".</p>
APOGEE-TESS Verification
<p>This dataset contains stars from NASA's TESS mission and APOGEE to test TESS's calibration comparatively to the Kepler scale. Link to publication: </p> <p>Arxiv:</p> <p><a href="https://arxiv.org/abs/2307.13853">https://arxiv.org/abs/2307.13853</a></p> <p>RNAAS:</p> <p><a href="https://iopscience.iop.org/article/10.3847/2515-5172/ace7af">https://iopscience.iop.org/article/10.3847/2515-5172/ace7af</a></p>
Study on Feasibility of Targeted Epidural Spinal Stimulation (TESS) to Improve Mobility in Patients With Parkinson's Disease
ClinicalTrials.gov study NCT04956770. IPD Sharing: NO. Countries: 1. Publications: 10.
Light curve analysis of Southern TESS blazars
Open the record for dataset details and reuse information.
Processd TESS light curves of stars with known ages
<p>We present light curves of ~100,000 stars (most within 500 pc) with ages inferred from membership of the nearby moving groups from Untangling The Galaxy series of papers. The light curves are generated from TESS full frame images using Eleanor (Feinstein+19). The nine zip files are split based on the first digit of TIC id, with the nested folders inside corresponding to the first three digits.</p>
Modelling OB stars with TESS: Construction of an asteroseismic sample
<p>Lack of high-precision continuous space-photometry has slowed the unlocking of OB star interiors in large numbers from asteroseismology. TESS is now providing data for large samples of stars allowing us to calibrate interior physics such as core overshooting, interior rotation and envelope mixing from pulsation frequencies. Calibrations of this kind are of major importance to quantitatively describe and predict subsequent evolutionary stages and ultimately their stellar remnants. In this talk I will present new results on the largest OB asteroseismic sample with TESS, which focuses on high frequency pulsators. The sample is characterised by a diverse variability, including pulsations, binarity, and rotational modulation connected to spots induced by magnetic fields. As an important test against theory I discuss the placement of the stars in the theoretical pulsation instability strips, computed using the stellar evolution code MESA and the stellar pulsation code GYRE. This test reveals that several stars show pulsational variability not predicted by current models and additional physics needs to be taken into account. This includes rotation, which is especially important as many OB stars are known to rotate at significant fractions of their critical rotation rates and has a profound effect on their pulsation physics. Identifying signatures of rotational modulation in the TESS photometry is therefore of paramount importance as it allows us to measure the surface rotation rate accurately, assess the influence of rotation on the pulsation physics, and remove degeneracies in asteroseismic modelling. The new TESS results of pulsating OB stars allow their pulsational and structural properties to be determined for the first time ever for such a large sample.</p>
Internal rotation and buoyancy travel time of 60 gamma Doradus stars from uninterrupted TESS light curves spanning 352 days
<p>Description:<br> Electronic versions of Table A.1 and A.2 from the Appendix of<br> Garcia et al. (2022b), as well as all analysed g-mode period-spacing<br> patterns from this work.</p> <p>Abstract:<br> Context. Gamma Doradus (hereafter gamma Dor) stars are gravity-mode<br> pulsators whose periods carry information about the internal structure of<br> the star. These periods are especially sensitive to the internal rotation<br> and chemical mixing, two processes that are currently not well constrained<br> in the theory of stellar evolution.<br> Aims. We aim to identify the pulsation modes and deduce the internal<br> rotation and buoyancy travel time for 106 gamma Dor stars observed<br> by the TESS mission in its southern continuous viewing zone (hereafter<br> S-CVZ). We rely on 140 previously detected period-spacing patterns, that is,<br> series of (near-)consecutive pulsation mode periods.<br> Methods. We used the asymptotic expression to compute gravity-mode<br> frequencies for ranges of the rotation rate and buoyancy travel time that<br> cover the physical range in γ Dor stars. Those frequencies were fitted to<br> the observed period-spacing patterns by minimizing a custom cost function.<br> The effects of rotation were evaluated using the traditional approximation<br> of rotation, using the stellar pulsation code GYRE.<br> Results. We obtained the pulsation mode identification, internal rotation<br> and buoyancy travel time for 60 TESS gamma Dor stars. For the remaining 46<br> targets, the detected patterns are either too short or contained too many<br> missing modes for unambiguous mode identification, and longer light curves<br> are required. For the successfully analysed stars, we found that<br> period-spacing patterns from 1-yr long TESS light curves can constrain the<br> internal rotation and buoyancy travel time to a precision of 0.03 d^{−1} and<br> 400s, respectively, which is about half as precise as literature results<br> based on 4-yr Kepler light curves of gamma Dor stars.</p>
Multi Centre Study on TESS V2 Shoulder System
ClinicalTrials.gov study NCT03431857. IPD Sharing: Not stated. Countries: 2. Publications: 0.
UniDAM: TESS-HERMES
<p>UniDAM results for TESS-HERMES data with Gaia DR2 parallaxes</p>
TESS-DECEMBER-2019
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). December 2019</p>
TESS-APRIL-2020
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). April 2020</p>
TESS-MARCH-2020
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). March 2020</p>
TESS-JUNE-2020
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). June 2020</p>
TESS-MAY-2020
<p>Measurements taken by the European Photometer Network (Project STARS4ALL). May 2020</p>
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