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15 results for “Gaia eDR3”
Catalog of GAIA eDR3 sources within 20 arcsec of pulsars
<p>Catalog of GAIA eDR3 sources within 20 arcsec of pulsars. Details on how the catalog was created can be found in <a href="https://arxiv.org/abs/2011.08075">Antoniadis (2021)</a></p> <p>The source code can be found <a href="https://zenodo.org/record/4378294#.X9-rR-lKjOQ">here</a></p>
UniDAM results with Gaia eDR3 parallaxes
<p>Results of UniDAM run with Gaia eDR3 parallaxes included.</p> <p>+------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | Survey | Input catalogue size | Stars with estimates | Reference |<br> | | | done using | |<br> | | | Gaia eDR3 parallaxes | |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | APOGEE (DR16) | 473307 | 326884 | Ahumada et al. (2020) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | Bensby | 714 | 547 | Bensby et al. (2014) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | Gaia-ESO (DR3) | 25533 | 20127 | Gilmore et al. (2012) G.Gilmore& S.Randich (2016) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | GALAH (DR3) | 564620 | 505403 | Buder et al. (2020) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | GCS | 13565 | 7633 | Casagrande et al. (2011) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | LAMOST (DR6) | 5581266 | 4377103 | Luo et al. (2015) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | LAMOST MRS (DR6) | 328187 | 223407 | Luo et al. (2015) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | RAVE (DR6) | 491349 | 347211 | Steinmetz et al. (2020) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | SEGUE | 235595 | 180012 | Yanny et al. (2009) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | Total (unique sources) | 5856273 | 4616931 | |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+</p>
Gaia EDR3 Catalogs of Machine-Learned Radial Velocities
<p><strong>Gaia EDR3 Catalogs of Machine-Learned Radial Velocities</strong></p> <p>Spatially complete Test-Set and Machine-Learned Radial Velocity (ML-RV) Catalogs described in Dropulic et al., arXiv:<a href="https://arxiv.org/abs/2205.12278">2205.12278</a>. The spatially complete Test-Set Catalog contains a total of 4,332,657 stars, while the spatially complete ML-RV Catalog contains 91,840,346 stars. We provide Gaia EDR3 Source IDs, the network-predicted line-of-sight velocity in km/s, and the network-predicted uncertainty in km/s. </p> <p>We have included a simple Jupyter notebook demonstrating how to import the data, and make a simple histogram with it.</p> <p>If you find this catalog useful in your work, please cite Dropulic et al. arXiv:<a href="https://arxiv.org/abs/2205.12278">2205.12278</a>, as well as Dropulic et al. <a href="https://doi.org/10.3847/2041-8213/ac09ef">ApJL 915, L14 (2021)</a> arXiv:<a href="https://arxiv.org/abs/2103.14039">2103.14039</a>. </p>
Catalogue of Wide Binaries from GAIA EDR3
<p>This dataset contains candidate wide binary systems from Gaia EDR3, used to perform tests of Modified Gravity theories in the low acceleration regime; as shown in the paper "Wide Binaries from GAIA EDR3: preference for GR over MOND ?" by Charalambos Pittordis & Will Sutherland. Accepted by Open Journal of Astrophysics, 31 Jan 2023.</p> <p>There are two files:</p> <p><strong>CleanedWB_EDR3_Prlx300pc_Gmag20_20230111_Size73087_ZenodoSample.csv</strong>: .CSV table with 73087 rows and 230 columns.</p> <p><br> <strong>00README_WideBinaries_EDR3_PS2023.txt : </strong>README file, describing the columns within the above dataset.</p>
An extended stellar halo discovered in Fornax dwarf spheroidal using Gaia EDR3
<p>We provide the catalog of Fornax member candidate, including the three final samples, as well as the data of surface density profiles, see the example python code of loading the data, as well as the explanation of each quantity.</p>
Gaia EDR3 in nearby galaxies
<p>Gaia EDR3 sources in the vicinity of nearby galaxies, as described in Barmby (2022, MNRAS submitted).</p>
The GALEX-Gaia-EDR3 Catalogue of Single and Binary White Dwarfs
<p>We present a catalogue of white dwarf candidates constructed from the GALEX and Gaia EDR3 catalogues.<br> The catalogue contains 332,111 candidate binary white dwarf systems and 111,996 candidate single white dwarfs. Where available, the catalogue is augmented with photometry from Pan-STARRS DR1, SDSS DR12 and classifications from StarHorse. We fit photometric data with modeled white dwarf cooling sequences to derive mass, age and effective temperature of the white dwarf as well as mass estimates for the companion. We test our classifications against StarHorse, the Gentile-Fusillo Gaia EDR3 catalogue, and white-dwarf-main-sequence binaries identified in SDSS DR12. This catalogue provides a unique probe of the binarity of white dwarfs as well as the abundance of white-dwarf giant binaries and large mass-ratio stellar binaries which are difficult to probe otherwise.</p>
Wide binaries from Gaia eDR3
<p>This dataset contain the catalogs accompanying the paper "A million binaries from Gaia eDR3: sample selection and validation of Gaia parallax uncertainties" by Kareem El-Badry, Hans-Walter Rix, and Tyler M. Heintz, submitted to MNRAS in January 2021. </p> <p>There are two data files:</p> <p><strong>all_columns_catalog.fits.gz</strong>: fits table with 1,817,594 rows and 217 columns<br> <strong>all_columns_catalog_shift.fits.gz: </strong>fits table with 517,993 rows and 201 columns</p> <p>There are also two code files: </p> <p><strong>num_neighbors_edr3.py:</strong> python code to count the number of neighbors for each source <br> <strong>find_binaries_edr3.py</strong>: python code to assemble the binary catalog</p>
LISC catalogue of Galactic disk star clusters in Gaia EDR3
<p>This is a database of the color-magnitude diagrams (CMDs) and fundamental parameters of star clusters in LISC catalogue.</p> <p>It corresponds to the study of Zhongmu Li et al. in 2021, which was submitted to ApJS. When one use these data, please cite to that work.</p> <p>Note that (V-I) color and V magnitude in the observed CMD data which are given in the database are transformed from the Gaia EDR3 magnitudes using some fitting correlations. </p> <p>The database contains three directories. These directories are explained as follows.</p> <p>(1)The first directory "all_clusters" gives the basic information and the observed CMD data of 3597 clusters in the work of Li et al.(2021). These clusters are all searched clusters by FOF and compared with previous catalogs. It has two subfolders and two files with '.dat' suffix.</p> <p>The first subfolder "new_candidates" contains observed CMD data of 868 clusters. These clusters are the different clusters in the previous catalogues, i.e., Liu & Pang(2019), Kharchenko et al.(2013), Cantat-Gaudin et al.(2018), Cantat-Gaudin et al.(2019), Bica et al.(2019), Castro-Ginard et al.(2019), Castro-Ginard et al.(2020), and Casado(2021) ,and the catalogue proposed in this work. Each file is named "obcmd_LISC****. dat".There are 10 columns in each file. The colums are for V, V-I, BP, BP-RP, ra, dec, parallax, rv, e_ra, e_dec respectively. The first and second columns are for V magnitude and V-I color which are transformed from the Gaia EDR3 magnitudes using some fitting correlations, and the other columns are the information of single star from Gaia EDR3.</p> <p>The second subfolder "matched_clusters" contains observed CMD data of 2729 clusters. These clusters are the same cluster in the previous catalogues, i.e., Liu & Pang(2019), Kharchenko et al.(2013), Cantat-Gaudin et al.(2018), Cantat-Gaudin et al.(2019), Bica et al.(2019), Castro-Ginard et al.(2019), Castro-Ginard et al.(2020), and Casado(2021), and the catalogue proposed in this work. The name and content of each file are the same as the file in the first subfolders.</p> <p>The first file "new_candidates" gives basic information of 868 candidates which corresponds to the candidates in the first subfolder.</p> <p>The second file "match_clusters.dat" gives basic information of 2729 clusters which corresponds to the clusters in the second subfolder of this directory.</p> <p>(2)The second directory "new_clusters" gives observed CMD data, best-fitted CMD data and best-fit parameters of 61 unknown clusters before. These clusters come from 868 star clusters that have not been matched by other catalogues. They were identified as potential new clusters in Li et al.(2021). These clusters are fitted via ASPS model and Powerful CMD code. Three parts of this directory are as follows.</p> <p>The first subfolder "obcmd" contains observed CMDs of 61 newly found clusters. The name and content of each file are the same as the file in the first subfolders of the first directory.</p> <p>The second subfolder "fitcmd" contains best-fitted CMDs of 61 new found clusters. These clusters are fitted by the ASPS model and Powerful CMD code. Each file is named "fitcmd_LISC****. dat". The first two lines give the best fitting parameters of the cluster. Note that "age0" is the age of the youngest star in the cluster if the stellar population type of cluster is composite stellar population(CSP). The first and second columns from the fourth row are for (V-I) color and V magnitude.</p> <p>The file "fit_parameter.dat" contains best-fit parameters of 61 new found clusters. There are 16 columns in this file. The colums are for id, ra, dec, plx,sig_plx, μαcosδ,sig_μαcosδ, μδ,sig_μδ, rsc, m-M, E(V-I), Z, t/t_range, f_bin and f_rot respectively. These parameters are the best-fit parameters by the ASPS model and Powerful CMD code. They correspond to the contents of a manuscript that was submitted to ApJS.</p> <p>(3)The third directory "known_clusters" gives observed CMD data, best-fitted CMD data and best-fit parameters of 594 known clusters. These clusters come from 2729 star clusters that have been matched by other catalogues. They have relatively clear CMDs structure and be fitted via ASPS model and Powerful CMD code. This directory have two subfolders.</p> <p>The first subfolder "good_fit" have the same structure with the second directory "new_clusters" but for 309 known clusters that have high quality CMDs and are fitted well. </p> <p>The second subfolder "other" have the same structure with the second directory "new_clusters" but for 285 known clusters that did not have high quality CMDs or are not well fitted.</p> <p>If you have any problems when using these data, send an email to Prof. Dr. Zhongmu LI, at email: zhongmuli@126.com.</p>
The C-19 Stream: Gaia EDR3 Member list
<p>The Gaia EDR3 memberlist of the C-19 stream</p> <p>source_id: Gaia EDR3 id</p> <p>feh_pr: the phtometric metallcities from Pristine</p> <p>rv: The best radial velocity measured</p> <p>feh: The spectroscopic metallicities from the best measurements. [FeII/H] values from HR spectra are listed if available, otherwise [FeI/H]_LTE (HR) values are used. If neither measurement is available, [FeI/H]_LTE (LR) derived from OSIRIS spectra are listed. See details in Table 1.</p> <p>note: We list the instruments used to obtain spectra. NEW specifies the new members confirmed in this paper. For the BHB stars, we notify those unlikely candidates based on their on-sky positions and proper motion measurements.</p>
White-Dwarf Wide Binaries from Gaia EDR3
<p>This dataset contain the catalogs accompanying the paper "Hydrogen-Atmosphere White Dwarfs Are Less Likely To Be Found with Wide-Binary Companions" by Jeremy Heyl, submitted to Open Journal of Astrophysics in July 2024. </p> <p>There are five data files:</p> <p><strong>HAtmo.fits.gz</strong>: fits table with 53,364 rows and 160 columns</p> <p> objects in the Gentile-Fusillo catalogue best fit by hydrogen atmospheres</p> <p><strong>HAtmoBinary.fits.gz: </strong>fits table with 3,219 rows and 408 columns</p> <p> objects in HAtmo.fits.gz that match to objects in the El Badry binary catalogue (<a href="../records/4435257">https://zenodo.org/records/4435257</a>)</p> <p><strong>HeAtmo.fits.gz</strong>: fits table with 7,662 rows and 160 columns</p> <p> objects in the Gentile-Fusillo catalogue best fit by helium atmospheres</p> <p><strong>HeAtmoBinary.fits.gz: </strong>fits table with 975 rows and 408 columns</p> <p> objects in HeAtmo.fits.gz that match to objects in the El Badry binary catalogue (<a href="../records/4435257">https://zenodo.org/records/4435257</a>)</p> <p><strong>MWDDB-binary.fits.gz:</strong> fits table with 3,784 rows and 228 columns,</p> <p> contains all matches between the MWDDB and the El Badry catalogue (<a href="../records/4435257">https://zenodo.org/records/4435257</a>), not only the spectral types discussed in the paper</p>
Internal proper motion dispersion profiles for 37 Milky Way globular clusters extracted from Gaia EDR3
<p>Internal proper motion dispersion profiles, in the radial and tangential components, extracted from Gaia EDR3 data for 37 Milky Way globular clusters.</p> <p>Created for, and used for model fitting in, the submitted manuscript: "Multimass modelling of Milky Way globular clusters - I. Implications on their stellar initial mass function above 1 M$_{\odot}$". Details on the creation of this dataset are available within this article.</p>
Catalogue of stars in Milky Way Dwarf Spheroidal Galaxies from Gaia EDR3
<p>Pace, Erkal, and Li 2022. </p> <p>Summary Table (including fits, csv, and npy file formats)</p> <p>(1) Catalogs</p> <p>(2) Diagnostic Plot Figures</p> <p>(3) Comparison Plot Figures</p> <p>v2 changes:</p> <ul> <li>The input velocity of Tucana V had the incorrect sign and has been corrected. All orbit models and values that depended on the velocity have been updated. </li> <li>the column "rhalf_sph_physical_mcmc_error" had the same values for each galaxy.</li> <li>The error columns (ep/em) for the following columns have been updated: average_density, m_l, mhalf, density_ratio. The errors are now the difference between the 16/84 confidence interval and the 50 confidence interval which follows the format of the rest of the summary file. </li> </ul> <p>v3 changes:</p> <ul> <li>The correlation errors between pmra, pmdec where incorrectly computed (named edr3_pmra_pmdec_error and edr3_gauss_pmra_pmdec_error in the catalogs here) and have been fixed. Only the summary files have been updated. </li> </ul>
Precise dynamical masses of new directly imaged companions from combining relative astrometry, radial velocities, and HIPPARCOS-Gaia eDR3 accelerations
<p>The VLT/SPHERE reduced images using the Geneva reduction pipeline, GRAPHIC, used to obtain the astrometry and photometry as published in Rickman et al. 2022. Each .fits file has been cosmetically corrected (i.e. bad pixels), background-subtracted, and flat-fielded. These files correspond to the 'flux frames' of the imaging observing sequence that was used to calculate the astrometry and photometry for each companion. The raw data are also available on the ESO archive with the relevant program numbers as listed in Rickman et al. 2022.</p>
Pleiades member candidates via STARGO with Gaia EDR3
<p>Members of the Pleiades open cluster are selected by using the STARGO method (Yuan et al. 2018) with Gaia early data release 3 (EDR3; Gaia Collaboration et al. 2021) data. See Li et al. 2021 (in prep. for Research Note of the AAS) for a detailed description. </p> <p>We downloaded the Gaia EDR3 data 100 pc from the center of Pleiades (X, Y, Z) = (−121.38, +29.17, −54.47) pc in Heliocentric Cartesian coordinates (Galli et al. 2017; Olivares et al. 2018). After removing artifacts and poor quality photometric sources (Lindegren et al 2018), we select stars within a radius of 10.8 mas yr^−1 from the center of the mean proper motion (μα cos δ, μδ ) = (+19.997, −45.548) mas yr<sup>-1</sup> of Pleiades (Gaia Collaboration et al. 2018) and input the 5D parameters (X, Y, Z, μα cosδ, μδ) into STARGO. We allow a 5% field star contamination rate in our identified members.</p> <p>We correct the distance of individual stars in Pleiades for the pseudo-elongation generated by parallax errors, via a Bayesian approach described in Carrera et al. (2019) and Pang et al. (2020, 2021). The mass of individual members in Pleiades is computed via the k-D tree method by taking the mass of the nearest point in the isochrone of 125 Myr (Lodieu et al. 2019) with AV = 0.11 mag and [Fe/H] = 0.08 (Gossage et al. 2018).</p> <p>"x_c", "y_c", "z_c" are the cluster position with distance correction in Heliocentric Cartesian coordinates. "Mass" represents the mass estimate of each star member via k-D tree method (Millman & Aivazis 2011). The descriptions of other parameters are found by opening the fits. file in TOPCAT.</p>
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