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74 results for “white dwarfs”
Gaia Catalogue of Synthetic Photometry - White Dwarfs (GCSP-WD)
<p>GSPC-WD catalogue </p> <p>This catalogue contains objects described in detail in Gaia Collaboration, Montegriffo et al., 2022, A&A, in press. The description of the catalogue from the paper is given below.</p> <p>We have made the GSPC-WD synthetic photometry available<br> as a stand-alone catalogue27, including SDSS, JKC and JPLUS<br> XPSP and the DA classification probability. The photometry<br> of the individual J-PAS bands, used in the random forest<br> analysis, is not included due to their low signal-to-noise. For<br> WDs classified in SDSS, a subset of which were used in the<br> training/validation of the random forest algorithim, we also include<br> the full SDSS classifications as a separate column in the<br> GSPC-WD catalogue table. When the synthetic spectral bands are very narrow a<br> significant number of sources will have low signal-to-noise. Furthermore,<br> at the edges of the Gaia spectral range, away from<br> the peak of the effective area, this is also true for some stars<br> in the wider bands included in the catalogue. In some extreme<br> cases, there is no significant detection of the object. The random<br> forest algorithm is only able to classify a WD when valid<br> flux measurements are available for every photometric band we<br> include in the analysis. Therefore, no classification is recorded<br> in the catalogue when data for one or more bands is "missing".<br> In total 15,003 WDs from the total sample of 101,783 are not<br> classified. For completeness, we have made all the flux measurements<br> and corresponding magnitudes available for all objects in<br> the GSPC-WD. Hence magnitude/fluxes with very large errors,<br> up to several times the flux itself, are included. However, where<br> fluxes are negative, the magnitudes are not defined. When using<br> the catalogue, appropriate signal-to-noise cuts are advisable for<br> the specific work in-hand, to ensure data quality.</p> <p>Total number of objects = 101,786; Format 1 object per row, 73 columns of data as listed below.</p> <p>Column Description of contents<br> 1 Gaia source_id<br> 2 ra<br> 3 ra_error<br> 4 dec<br> 5 dec_error<br> 6 JohnsonStd_mag_U<br> 7 JohnsonStd_mag_B<br> 8 JohnsonStd_mag_V<br> 9 JohnsonStd_mag_R<br> 10 JohnsonStd_mag_I<br> 11 JohnsonStd_flux_U<br> 12 JohnsonStd_flux_B<br> 13 JohnsonStd_flux_V<br> 14 JohnsonStd_flux_R<br> 15 JohnsonStd_flux_I<br> 16 JohnsonStd_flux_error_U<br> 17 JohnsonStd_flux_error_B<br> 18 JohnsonStd_flux_error_V<br> 19 JohnsonStd_flux_error_R<br> 20 JohnsonStd_flux_error_I<br> 21 SdssStd_mag_u<br> 22 SdssStd_mag_g<br> 23 SdssStd_mag_r<br> 24 SdssStd_mag_i<br> 25 SdssStd_mag_z<br> 26 SdssStd_flux_u<br> 27 SdssStd_flux_g<br> 28 SdssStd_flux_r<br> 29 SdssStd_flux_i<br> 30 SdssStd_flux_z<br> 31 SdssStd_flux_error_u<br> 32 SdssStd_flux_error_g<br> 33 SdssStd_flux_error_r<br> 34 SdssStd_flux_error_i<br> 35 SdssStd_flux_error_z<br> 36 Jplus_mag_uJAVA<br> 37 Jplus_mag_J0378<br> 38 Jplus_mag_J0395<br> 39 Jplus_mag_J0410<br> 40 Jplus_mag_J0430<br> 41 Jplus_mag_gJPLUS<br> 42 Jplus_mag_J0515<br> 43 Jplus_mag_rJPLUS<br> 44 Jplus_mag_J0660<br> 45 Jplus_mag_iJPLUS<br> 46 Jplus_mag_J0861<br> 47 Jplus_mag_zJPLUS<br> 48 Jplus_flux_uJAVA<br> 49 Jplus_flux_J0378<br> 50 Jplus_flux_J0395<br> 51 Jplus_flux_J0410<br> 52 Jplus_flux_J0430<br> 53 Jplus_flux_gJPLUS<br> 54 Jplus_flux_J0515<br> 55 Jplus_flux_rJPLUS<br> 56 Jplus_flux_J0660<br> 57 Jplus_flux_iJPLUS<br> 58 Jplus_flux_J0861<br> 59 Jplus_flux_zJPLUS<br> 60 Jplus_flux_error_uJAVA<br> 61 Jplus_flux_error_J0378<br> 62 Jplus_flux_error_J0395<br> 63 Jplus_flux_error_J0410<br> 64 Jplus_flux_error_J0430<br> 65 Jplus_flux_error_gJPLUS<br> 66 Jplus_flux_error_J0515<br> 67 Jplus_flux_error_rJPLUS<br> 68 Jplus_flux_error_J0660<br> 69 Jplus_flux_error_iJPLUS<br> 70 Jplus_flux_error_J0861<br> 71 Jplus_flux_error_zJPLUS<br> 72 probability DA<br> 73 SDSS WD type</p>
A gap in the double white dwarf separation distribution caused by the common-envelope evolution: astrometric evidence from Gaia
<p>Here we provide a supplementary dataset to our publication <em>A gap in the double white dwarf separation distribution caused by the common-envelope evolution: astrometric evidence from Gaia,</em> <a href="https://arxiv.org/abs/2203.03659">arXiv:2203.03659</a>. The dataset consists of 119 double white dwarf candidates selected in the Gaia Early Data Release 3 (EDR3) based on the sources' astrometric wobble amplitude. For each candidate we provide sky coordinates (RA, DEC), Gaia EDR3 ID, position on the HR diagram (G, BP-RP) and estimated astrometric wobble amplitude (delta a). Note that the astrometric wobble amplitude (delta a) is directly related to the binary’s orbital separation, as detailed in our paper.</p>
The Impact of White Dwarf Luminosity Profiles on Oscillation Frequencies
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018ApJ...867L..30T/abstract">The Impact of White Dwarf Luminosity Profiles on Oscillation Frequencies</a></p> <p> </p>
Spectral evolution of hot hybrid white dwarfs I. Spectral analysis
<p>Hydrogen-rich white dwarfs (WDs) comprise the majority of the WD population, but are only rarely found at the very hot end of the WD cooling sequence. A small subgroup that exhibits both hydrogen and helium lines in their spectra, the so-called hybrid (or DAO) WDs, represents the majority of hydrogen-rich WDs at effective temperatures <em>T</em>eff<em> ≈ </em>100 kK. We aim to understand the spectral evolution of hot hybrid WDs. Although small in number, they represent an evolutionary phase for most (≈ 75 %) WDs. We conducted a nonlocal thermodynamic equilibrium (NLTE) analysis with fully metal line blanketed model atmospheres for the ultraviolet (UV) and optical spectra of a sample of 19 DA and 13 DAO WDs with <em>Teff </em>> 60 kK. The UV spectra allow us to precisely measure the temperature through model fits to metal lines in different ionization stages, which enables us to place the WDs accurately on the cooling sequence. Here we present model fits to the UV and optical spectra in our sample. Aditionally, the <em>T</em>eff, log <em>g</em>, and abundance values of our sample objectss are compared to previous studies. </p>
Lithium Pollution of White Dwarfs and Other Secrets of MORDOR (CSV File of MORDOR Survey Objects)
<p>CSV file containing the Gaia DR2 data for the MORDOR Survey from Benjamin C. Kaiser's Ph.D. Dissertation. It also contains the spectral types and SED types that were identified.</p> <p>If you use this data please cite my dissertation, which should be accessible via the UNC Chapel Hill Library in some way. You should probably also cite Gaia DR2 if you use anything other than my spectral types pretty much because all the rest of the data is from Gaia DR2.</p>
Gravity modes on rapidly rotating accreting white dwarfs and their variation after dwarf novae
<p>MESA (r10398) inlist files and Gyre (5.2) files used in preparation of the paper "Gravity modes on rapidly rotating accreting white dwarfs and their variation after dwarf novae". More details for specific files are given in README.txt. </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>
Faint calcium-rich transient from a double-detonation of a 0.6 M⊙ carbon-oxygen white dwarf star: Complimentary material
<p>Complimentary material to the manuscript.<br> The videos show the hydrodynamical evolution of the merger leading to the double-detonation.</p> <p>The movie "overdensity_formation.mp4" shows slices through the orbital plane color coded with the density (left) and the temperature (right), displaying frame by frame the formation of a cold, overdense fluid parcel after the disruption of the HeWD. <br> <br> The remaining movies show the overall evolution of different quantities with slices through the orbital plane on the left and perpendicular to the orbital plane on the right.</p>
Convergence test: Double white dwarf merger (Octo-Tiger)
<p>Configuration files to reproduce the simulation for the convergence test.</p> <p> </p> <p>To generate the input files run:</p> <pre><code class="language-bash">octotiger --config_file=rcb_init.init --silo_num_groups=n</code></pre> <p> </p> <p>Octo-Tiger (b4c51431) and following dependencies were used</p> <ul> <li>HPX (1.4.0),</li> <li>hwloc (1.11.1),</li> <li>silo (4.10.2),</li> <li>jemalloc (5.1.0),</li> <li>hdf5 (1.8.12),</li> <li>cray-mpich/MVAPICH2 (7.7.10/2.3.2),</li> <li>gcc (8.3.0),</li> <li>APEX (8ba5090),</li> <li>and Papi (5.7.0)</li> </ul> <p>The Octo-Tiger source code is available on <a href="http://github.com/STEllAR-GROUP/octotiger">Github.</a></p> <p>To run the simulation run:</p> <pre><code class="language-bash">octotiger --config_file=rcb.ini --silo_num_groups=n</code></pre> <p> </p> <p>where n is the number of nodes.</p> <p> </p> <p> </p>
Spectroscopic data set for an unusual white dwarf
<p>The tar file includes fits-formatted count (d*) and flux (ca*) spectra of an unusual white dwarf obtained at the MDM observatory. The spectra are wavelength calibrated. Users should exercise caution when quoting absolute flux. Heliocentric velocity corrections are not applied. The count spectra list the wavelength (angstrom) and the total count, and the flux spectra list the wavelength (angstrom) and the flux in units of erg/cm^2/s/angstrom.</p>
Neutron Star - White Dwarf Binaries: Probing Formation Pathways and Natal Kicks with LISA
<p>We present supplementary datasets accompanying our publication<em> </em><a href="https://arxiv.org/abs/2310.06559">Neutron Star - White Dwarf Binaries: Probing Formation Pathways and Natal Kicks with LISA</a>.<em> </em>These catalogues reperesent the Galactic population of double white dwarf (DWD) and neutron star - white dwarf (NSWD) binaries emitting gravitational waves (GWs) in the <em>Laser Interferometer Space Antenna</em> (LISA) frequency band (0.1 mHz - 1 Hz). The catalogues have been constructed based on binary evolution models <a href="https://arxiv.org/abs/1208.6446">Toonen et al. 2012</a> for DWDs and <a href="https://arxiv.org/abs/1804.01538">Toonen et al. 2018</a> for NSWD binaries, obtained using SeBa binary population synthesis code.</p> <p><strong>Data contents</strong></p> <p>The dataset consists of <strong>12 catalogues </strong>representing Galactic populations of NSWD and/or DWD binaries, which are expected to be the most numerous types of binaries amongt LISA's Galactic sources. Each catalogue is distinguished by its model ID, which specifies the presence of NSWD and/or DWD binaries, the CE model used, CE efficiency values, and the NS natal kick prescription applied (see table below).</p> <p>Each catalogue is structured to describe a binary systems with the following attributes:</p> <ul> <li><strong>Name*</strong>: binary identifier; this consist of a prefix indicating the binary type (<code>'MW_DWD'</code> for a DWD binary, <code>'MW_NSWD_ecc0'</code> for a circular NSWD bianry, or <code>'MW_NSWD_ecc1'</code> for an eccentric NSWD binary) followed by a unique ID number. For example, <code>'MW_DWD 28713637'</code>.</li> <li><strong>Frequency</strong>: present-day GW frequency (Hz).</li> <li><strong>Frequency Derivative</strong>: rate of change of GW frequency over time (Hz^2).</li> <li><strong>Ecliptic Latitude</strong>: in radians (rad).</li> <li><strong>Ecliptic Longitude</strong>: in radians (rad).</li> <li><strong>Amplitude</strong>: GW amplitude (dimensionless).</li> <li><strong>Inclination</strong>: angle between the binary's orbital plane and our line of sight, in radians (rad).</li> <li><strong>Polarization</strong>: Orientation of the GW's polarization, in radians (rad).</li> <li><strong>Initial Phase</strong>: initial phase (rad).</li> <li><strong>Eccentricity</strong>: orbital eccentricity (dimensionless).</li> </ul> <p><strong>*</strong>Note that the <strong>Name </strong>field for eccentric NS+WD binaries (staring with <code>'MW_NSWD_ecc1'</code>) is not unique because these binaries are represented by multiple harmonics sharing the same name ID. The number of harmonics included varies for each binary to ensure that at least 99% of the binary's total GW power is represented. Thus, for each binary, we added harmonics incrementally until this threshold is reached.</p> <table> <tbody> <tr> <td>Model ID</td> <td>WD+WD</td> <td>NS+WD</td> <td>CE model</td> <td>CE efficiency</td> <td>NS natal kick</td> </tr> <tr> <td>1_0</td> <td>Yes</td> <td>No</td> <td>αα</td> <td>αλ=2.00</td> <td>N/A</td> </tr> <tr> <td>1_1</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Verbunt</td> </tr> <tr> <td>1_2</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Arzoumanian</td> </tr> <tr> <td>1_3</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Hobbs</td> </tr> <tr> <td>1_4</td> <td>Yes</td> <td>Yes</td> <td>αα</td> <td>αλ=2.00</td> <td>Blaauw</td> </tr> <tr> <td>2_0</td> <td>Yes</td> <td>No</td> <td>αα2</td> <td>αλ=0.25</td> <td>N/A</td> </tr> <tr> <td>2_1</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Verbunt</td> </tr> <tr> <td>2_2</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Arzoumanian</td> </tr> <tr> <td>2_3</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Hobbs</td> </tr> <tr> <td>2_4</td> <td>Yes</td> <td>Yes</td> <td>αα2</td> <td>αλ=0.25</td> <td>Blaauw</td> </tr> <tr> <td>3_0</td> <td>Yes</td> <td>No</td> <td>αγ</td> <td>αλ=2.00, γ=1.75</td> <td>N/A</td> </tr> <tr> <td>3_1</td> <td>Yes</td> <td>Yes</td> <td>αγ</td> <td>αλ=2.00, γ=1.75</td> <td>Verbunt</td> </tr> </tbody> </table> <p> </p> <h4><strong>Citing the Dataset</strong></h4> <p>When utilising these catalogues in your research, please cite <a href="https://arxiv.org/abs/2310.06559">Korol et al. 2024.</a> We also note our companion data-analysis-focused paper <a href="https://arxiv.org/abs/2310.06568">Moore et al. 2024</a>.</p>
On Trapped Modes In Variable White Dwarfs As Probes Of The 12C(α, γ)16O Reaction Rate
<p>The files in this dataset should have everything to re-produce figure 10, the summary plot in the manuscript.</p>
Applying the metallicity-dependent binary fraction to double white dwarf formation: Implications for LISA -- COSMIC + Ananke data
<p>This dataset contains all data required to run the pipeline which produces the results and figures in Thiele+2022 including:</p> <p>- results of all COSMIC simulations for the fiducial, alpha25, alpha5, and q3 models for each double white dwarf type and binary fraction assumption</p> <p>- metallicities, ages, positions and star particle kernel lengths from the Ananke framework of galaxy m12i in the Latte suite of the FIRE-2 simulations.</p>
Using 3.4-micron Variability towards White Dwarfs as a Signpost of Remnant Planetary Systems
<p>Here we provide the catalog of variables (Catalog_of_3p4um_Variable_WDs_Guidry+2024.csv) and full sample (Full_Variable_WDs_in_WISE_Sample_Guidry+2024.csv) generated by our analysis in <a href="https://arxiv.org/abs/2406.18646">https://arxiv.org/abs/2406.18646</a>.</p> <p>We also provide all of the light curves used in our analysis. Light curve files generated using 2-pixel circular apertures are available in .csv format in AP_Phot_LCs.tar.gz. Our PSF photometry extracted light curves (which we do not analyze in our study) are also provided in PSF_Phot_LCs.tar.gz.</p> <p> </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>
A Search for a Surviving White Dwarf Companion in SN~1006 - photometric dataset
<p>This is a photometry catalogue obtained by DECam to find hot surviving WD companions to the SN1006 supernova. Please acknowledge the science paper Kerzendorf et al. 2017 if you use this dataset. </p>
Polluted White Dwarfs: Mixing Regions and Diffusion Timescales
<p>Tables of diffusion timescales and surface mass fractions in MESA models for polluted DA white dwarfs.</p> <p>Includes python interpolation routines and and example plotting script, along with inlists and instructions for reproducing the MESA runs that built these tables.</p> <p>If you wish to make use of these tables in your work, please cite this paper: <a href="http://adsabs.harvard.edu/abs/2019ApJ...872...96B">http://adsabs.harvard.edu/abs/2019ApJ...872...96B</a> </p>
Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-nova Supersoft Phase
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2013ApJ...777..136W">Hydrogen Burning on Accreting White Dwarfs: Stability, Recurrent Novae, and the Post-nova Supersoft Phase</a></p>
The outcomes of carbon-oxygen white dwarfs accreting CO-rich material
<p>MESA inlist associated files for <a href="https://ui.adsabs.harvard.edu/#abs/2019MNRAS.483..263W/abstract">The outcomes of carbon-oxygen white dwarfs accreting CO-rich material</a></p>
Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs
<p>Inlists and data for "<a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.474..427Z/abstract">Evolution models of helium white dwarf-main-sequence star merger remnants: the mass distribution of single low-mass white dwarfs</a>"</p>
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