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23 results for “Gaia DR3”
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>
BASE-9 binarity and stellar masses from Gaia DR3, 2MASS, and Pan-STARRS data for six open clusters: NGC 2168, NGC 7789, NGC 6819, NGC 2682, NGC 188, NGC 6791
<h2>Data sets as described in "Goodbye to Chi-by-Eye: A Bayesian Analysis of Photometric Binaries in Six Open Clusters", Childs et al. 2023 <a href="https://ui.adsabs.harvard.edu/abs/2023arXiv230816282C/abstract">https://ui.adsabs.harvard.edu/abs/2023arXiv230816282C/abstract</a></h2>
Gaia Photometric Science Alerts Crossmatch with Gaia DR3 - Feb. 2024
<p>The <a href="http://gsaweb.ast.cam.ac.uk/alerts/home">Gaia Photometric Science Alerts</a> were crossmatched to the Gaia DR3 catalog on <strong>February 23rd, 2024</strong>. We assumed a 1" separation for each crossmatch. The crossmatch was conducted using the <a href="https://lsdb.readthedocs.io/en/latest/">Large Survey Database</a> (LSDB). </p>
An empirical model of the Gaia DR3 selection function
<p>Precomputed maps of the M10 parameter used to predict the completeness of the Gaia DR3 source catalogue.</p> <p><strong>allsky_M10_hpx7.hdf5 </strong>is a tessellation of the whole sky in Galactic nested healpix scheme of order 7.</p> <p><strong>allsky_uniq_10.fits</strong> uses an adaptive resolution and is based on the 'uniq' numbering of healpix tiles. Regions of higher density use a finer resolution, up to order 10, chosen so that every tile contains a minimum of twenty sources to compute M10 from.</p> <p>Paper: https://ui.adsabs.harvard.edu/abs/2023A%26A...669A..55C/abstract</p> <p>Tutorial using the GaiaUnlimited python package to query these maps: https://github.com/gaia-unlimited/gaiaunlimited/blob/main/docs/notebooks/dr3-empirical-completeness.ipynb</p> <p>Documentation for the GaiaUnlimited package: https://gaiaunlimited.readthedocs.io/en/latest/</p>
Gaia DR3 asteroid reflectance spectra: L-type families, memberships and ages
<p>The Gaia Data Release 3 (DR3) contains reflectance spectra at visible wavelengths for 60,518 asteroids over the range between 374-1034 nm, representing a large sample that is well suited to studies of asteroid families.</p> <p>We wanted to assess the potential of Gaia spectra in identifying asteroid family members. Here, we focus on two L-type families, namely Tirela/Klumpkea and Watsonia. These families are known for their connection to Barbarian asteroids, which are potentially abundant in calcium-aluminum rich inclusions (CAIs).</p> <p>The method we developed to establish family memberships is based (1) on a color taxonomy specifically built on Gaia data and (2) on the similarity of spectra of candidate members with the template spectrum of a specific family.</p> <p>Our work demonstrates the advantage of combining the classical hierarchical clustering method (HCM) approach to spectral properties obtained by Gaia for the study of asteroid families. Future data releases are expected to further expand the capabilities in this domain.</p> <p>The memberships for the Tirela/Klumpkea and Watsonia families are reported here. The columns report, from left to right: the identifier of the asteroid, the absolute magnitude, the proper elements (semi-major axis, eccentricity and sine of the inclination, taken from AFP, Novaković et al., 2022), NEOWISE albedo (Masiero et al., 2011) and spectral type from our color taxonomy. For the objects that are not directly classified into the S and L classes, their most probable spectral type is also reported. </p>
Main Sequence + Compact Object binary candidates from Gaia DR3 astrometric and spectroscopic excess noise
<p>MS+CO systems selected from Gaia DR3 via inferred periods and mass ratios derived from astrometric and spectroscopic errors.</p> <p>The sample is split into a bronze list (significant astrometric and spectroscopic RUWE, mass ratio > 1 and companion mass > 3 Msun). </p> <p>A subset of these is chosen as a silver list (propagating errors on mass ratio and companion mass to deselect systems which are not significantly above the previous criteria)</p> <p>Finally, a gold list is constructed from the subset of the silver list which shows no evidence of being significantly brighter than a single MS star and with no significant excess photometric noise.</p> <p>We include the most relevant Gaia data for the system, as well as our inferred spectroscopic and photometric errors and RUWEs, and the inferred periods and mass ratios. Gaia's DR3 source id, and the ra, dec position are included and thus other Gaia data, or data from other astronomical catalogs, can be found for these systems.</p> <p>The catalog and the underlying methods are explained in more detail in <a href="https://arxiv.org/abs/2206.04392">Andrew et al. 2022</a>.</p>
Gaia DR3 detectability of unresolved binary systems
<p>This upload contains the necessary data to construct the selection of unresolved binary systems in Gaia DR3 based on RUWE.</p> <p>The tutorial showing how to work with these data can be found here: </p> <p>https://gaiaunlimited.readthedocs.io/en/latest/notebooks/dr3-unresolved-binaries.html</p> <p>The paper describing the data and methods is:</p> <h2>Gaia DR3 detectability of unresolved binary systems</h2> <div>Alfred Castro-Ginard, Zephyr Penoyre, Andrew R. Casey, Anthony G.A. Brown, Vasily Belokurov, Tristan Cantat-Gaudin, Ronald Drimmel, Morgan Fouesneau, Shourya Khanna, Evgeny P. Kurbatov, Adrian M. Price-Whelan, Hans-Walter Rix and Richard L. Smart</div> <div> </div> <div>https://ui.adsabs.harvard.edu/abs/2024arXiv240414127C/abstract</div>
The data for Newly Detected Old Galactic Globular Cluster Candidates Using Gaia DR3
<pre><br><br></pre> <p>GAIA_input - Raw data downloaded by GAIA</p> <p>GAOSI - Gaussian interpolation and testing AND concer fits correlational graph values</p> <p>The result after clustering_output</p> <p>mh_gspphot - [Fe/H] ag_gspphot - AG m_M - distance modulus - This is also the header of GC01.csv and GC02.csv under .data\gaosi\GAOS, which are copied from the csv file in .data\gaosi\GAOSI\output2</p> <p>Because GAIA lacked part of the data of [Fe/H] and AG after clustering, we adopted the Gaussian RV completion method of Qin et al. (2023) doi: 10.3847/1538-4365/acadd6 to supplement the data of [Fe/H] and AG. The data in these 3 folders is the result of the process we performed. .data\gaosi\GAOSI\output and .data\gaosi\GAOSI\output1 and .data\gaosi\GAOSI\output2 </p> <p>.data\gaosi\GAOSI\output3 - Test the data after we finish the Gaussian interpolation</p> <p>.data\gaosi\GAOSI\medain.csv -The median of the data before Gaussian interpolation</p> <p>.data\gaosi\GAOSI\pyngc01_1sigma.csv and .data\gaosi\GAOSI\pyngc02_1sigma.csv -The mean, standard deviation, and error range of m_M and mh_gspphot and ag_gspphot</p> <p> </p>
Appendix Figures A.1 - A.15 of the paper "Advanced classification of hot subdwarf binaries using artificial intelligence techniques and Gaia DR3 data". This work has been accepted for publication in the journal Astronomy & Astrphysics (A&A) on September 24, 2024.
<p><strong>Figure captions:</strong></p> <p> </p> <p><strong>Fig. A.1.</strong> Heatmap with the number of common stars (true positives) labeled as binary for the five methods used.</p> <p> </p> <p><strong>Fig. A.2.</strong> Heatmap with the number of common stars (true negatives) labeled as single for the five methods used.</p> <p> </p> <p><strong>Fig. A.3.</strong> Color-magnitude diagrams, showing the 2815 stars of our sample from Sect. 3. Colors indicate the label predictions by SOM (left panel) and CNN (right panel).</p> <p> </p> <p><strong>Fig. A.4.</strong> K-S test comparing radial SOM (black) and CNN (blue).</p> <p> </p> <p><strong>Fig. A.5.</strong> Spectra of the star "LAMOSTJ112914.11+471501.7" (blue color) and in the background (gray color) the 35 stars classified as binary by Solano et al. (2022) with VOSA tools.</p> <p> </p> <p><strong>Fig. A.6.</strong> Spectra of the star "HD14829" (red color) and in the background (gray color) the 53 stars classified as single by Drilling et al. (2013).</p> <p> </p> <p><strong>Fig. A.7.</strong> Spectra of the star "Feige98" (red color) and in the background (gray color) the 53 stars classified as single by Drilling et al. (2013).</p> <p> </p> <p><strong>Fig. A.8.</strong> Spectra of the star "PG0304+184" (red color) and in the background (gray color) the 53 stars classified as single by Drilling et al. (2013).</p> <p> </p> <p><strong>Fig. A.9.</strong> Spectra of the star "PG1510+635" (red color) and in the background (gray color) the 53 stars classified as single by Drilling et al. (2013).</p> <p> </p> <p><strong>Fig. A.10.</strong> Cluster 0 of spectra (blue color) with the other spectra in the background (gray color).</p> <p> </p> <p><strong>Fig. A.11.</strong> Cluster 4 of spectra (brown color) with the other spectra in the background (gray color).</p> <p> </p> <p><strong>Fig. A.12.</strong> Cluster 1 of spectra (yellow color) with the other spectra in the background (gray color).</p> <p> </p> <p><strong>Fig. A.13.</strong> Cluster 3 of spectra (red color) with the other spectra in the background (gray color).</p> <p> </p> <p><strong>Fig. A.14.</strong> Cluster -1 of spectra (pink color) with the other spectra in the background (gray color).</p> <p> </p> <p><strong>Fig. A.15.</strong> Cluster 2 of spectra (green color) with the other spectra in the background (gray color).</p>
Phase spiral in Gaia DR3
<p>Movies of the evolution of the phase spiral in Gaia DR3, supplementing the publication:</p> <p>The phase spiral in Gaia DR3, Astronomy and Astrophysics, 673, A115, Antoja, T., Ramos, P., García-Conde, B., Bernet, M., Laporte, C. F. P., & Katz, D. (2023), https://ui.adsabs.harvard.edu/abs/2023A&A...673A.115A</p> <p><a href="https://doi.org/10.1051/0004-6361/202245518">https://doi.org/10.1051/0004-6361/202245518</a></p> <p> </p> <p> </p>
A Bayesian Estimation of the Milky Way's Circular Velocity Curve using Gaia DR3
<p>The derived input dataset of approximately 0.6 million RGB stars used in the work "A Bayesian Estimation of the Milky Way’s Circular Velocity Curve using Gaia DR3" . The authors kindly ask to cite the original work described in (<a href="https://doi.org/10.1051/0004-6361/202346474">https://doi.org/10.1051/0004-6361/202346474</a>) should one make use of this catalogue.</p> <p> </p> <p> </p>
Catalogues of active galactic nuclei from Gaia and unWISE data (updated to Gaia DR3 astrometric solution)
<p>This is a minor update to the Gaia-unWISE AGN catalogue published in Shu et al. 2019, MNRAS, 489, 4741. It contains the same 2.7 million AGN candidates selected from the Gaia DR2 and unWISE data using a random forest classifier. In addition to the original columns (which are explained in detail in Shu et al. 2019), a few new columns that correspond to Gaia DR3 astrometric solutions are appended, i.e. dr3_source_id, dr3_pmra, dr3_pmra_err, dr3_pmdec, dr3_pmdec_err, dr3_plx, dr3_plx_err, dr3_pmsig, and dr3_plxsig. </p>
Cataloging Distant Galactic Open Clusters: Identification of 739 New Star Clusters Beyond 5 kpc Utilizing GAIA DR3 Data
<p><span>The figures of the 739 open clusters that report in our paper (Cataloging Distant Galactic Open Clusters: Identification of 739 New Star Clusters Beyond 5 kpc Utilizing GAIA DR3 Data)</span></p> <p><span> complete King's model<span> </span>profile fitting, sky charts and 5-panels ( spatial distribution, proper-motion distribution,</span></p> <p><span><span>parallax statistics, parallax distribution, and CMD)</span> .</span></p>
Confronting sparse Gaia DR3 photometry with TESS for a sample of around 60,000 OBAF-type pulsators
<p>This listing contains the results produced as part of the paper "Confronting sparse Gaia DR3 photometry with TESS for a sample of around 60,000 OBAF-type pulsators" by Hey & Aerts, 2024.</p> <p>A description of the tables is as follows;</p> <ol> <li><strong>prewhiten_all.json</strong>: The frequencies, amplitudes, and phases of all targets in the sample prewhitened to a 1% false alarm level.</li> <li><strong>prewhiten_all_cleaned.json</strong>: The same as Table 1, where combination frequencies have been removed.</li> <li><strong>full_sample_prediction_paper.csv</strong>: The results of the classification for each variability class.</li> <li><strong>ranked_table_revised.csv:</strong> The final ranking of the targets for future studies.</li> </ol>
Low-amplitude long-period variable (OSARGs) candidates in Gaia DR3 LPV catalogue
<p>The low-amplitude long-period variable (LA-LPV) candidates in Gaia DR3 LPV catalogue. The selection is described in <a href="https://ui.adsabs.harvard.edu/abs/2024arXiv240606678Z/abstract">Zhang et al. 2024</a>. The heliocentric distances is in column "luminosity_dist" in unit of kpc. Other astrometric measurements are from Gaia DR3 and has the save column name as Gaia DR3. </p>
Gravitationally Bound Wide Pairs Hosting Unresolved Astrometric Binaries in Gaia DR3
<p>We present a catalog of 14,791 gravitationally bound wide pairs where one of the components is an unresolved binary with an astrometric orbital or acceleration solution in Gaia DR3. The catalog is separated into two tables corresponding to orbital solutions and acceleration solutions, respectively. </p>
Rotation Period Predictions for Low-mass Stars with Kinematic Information from Gaia DR3
<pre><strong>DR3_kine_prot_pred.csv:</strong> 17.6 million predicted periods for all stars with Gaia DR3 RVs. This data should only be used to vet periods and not directly as period measurements. Works best for stars with GBP-GRP > 1.5 and rotation period > 20 days. Do not work for fast-rotating low-mass stars. Column descriptions see below </pre> <p><strong>source_id</strong>: Gaia DR3 source_id</p> <p><strong>ra</strong>: Gaia DR3 ra measurements</p> <p><strong>dec</strong>: Gaia DR3 dec measurements</p> <p><strong>parallax</strong>: Gaia DR3 parallax measurements</p> <p><strong>bp_rp</strong>: Gaia DR3 G<sub>BP</sub>-G<sub>RP</sub> measurements</p> <p><strong>phot_g_mean_mag</strong>: Gaia DR3 G mag</p> <p><strong>abs_G</strong>: absolute Gaia G magnitude derived from Gaia DR3 G mag and parallax</p> <p><strong>ruwe</strong>: Gaia DR3 ruwe measurements </p> <p><strong>Prot_pred</strong>: Predicted periods using Gaia DR3 parameters and kinematics</p> <p> </p> <p><strong>vet_ztf_lowmass.csv</strong>: 65k vetted ZTF period measurements for stars with G<sub>BP</sub>-G<sub>RP</sub> > 1.5. Column descriptions see below</p> <p><strong>source_id</strong>: Gaia DR3 source_id</p> <p><strong>ra</strong>: Gaia DR3 ra measurements</p> <p><strong>dec</strong>: Gaia DR3 dec measurements</p> <p><strong>parallax</strong>: Gaia DR3 parallax measurements</p> <p><strong>bp_rp</strong>: Gaia DR3 G<sub>BP</sub>-G<sub>RP</sub> measurements</p> <p><strong>gmag</strong>: Gaia DR3 G mag</p> <p><strong>abs_G</strong>: absolute Gaia G magnitude derived from Gaia DR3 G mag and parallax</p> <p><strong>rv</strong>: Gaia DR3 rv measurements</p> <p><strong>Prot</strong>: measured and vetted periods from ZTF </p>
Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
<p>The data of 77 clusters with eMSTO.</p>
Gaia DR3 in nearby galaxies
<p>Data files for "Gaia DR3 and nearby galaxies: where do foregrounds matter?" (2022, MNRAS submitted)</p>
GAIA DR3 6D Kinematics
<p>Processed data from GAIA DR3 with available 6D kinematics (positions, proper motions and radial velocities), including propagated uncertainties and various useful coordinate systems. Also included is the pipeline of scripts used to produce this dataset.</p> <p> </p> <p>Details of the data format and usage can be found in the pipeline README.md which is also available on <a href="https://github.com/CianMRoche/GAIA-DR3-6D-Kinematics/tree/v1.0">Github</a>.</p>
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