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10 results for “galactic binaries”
Supplementary material for the paper "DS Andromedae, A Detached Eclipsing Double-Lined Spectroscopic Binary in the Galactic Cluster NGC 752
<p>Supplementary material supporting the paper "DS Andromedae: A Detached Eclipsing Double-Lined Spectroscopic</p> <p>Binary in the Galactic Cluster NGC 752" by E. F. Milone, S. J. Schiller, Th. Mellergaard Amby, and S. Frandsen.</p> <p>It includes:</p> <p>A Read-me file in three formats (docx, rtf, pdf); Unabridged Section 3 with extended modeling details (pdf);</p> <p>Extended spreadsheet version of Table 3 of adjusted parameters (pdf); Extended spreadsheet version of Table 8 of absolute</p> <p>parameters (pdf); and Complete Table 15 of photometric data (txt): and a sample DC input file (for Model 41, used in the</p> <p>DS And modeling) in dat format.</p>
Binary fractions for Galactic globular clusters
<p>Binary fractions for Galactic globular clusters</p>
Galactic Populations of LISA DWD Binaries
<p>These COSMIC simulation outputs and assembled galactic populations of<br> Double White Dwarf (DWD) binaries<br> represent the work published by V. Delfavero et al,<br> in https://arxiv.org/abs/2409.15230</p> <p>The COSMIC version used in these simulations is 3.4.10</p> <p>The git repository for the accompanying code which built this dataset<br> will be available at https://gitlab.com/xevra/basil-cosmic<br> upon the publication of our article.</p> <p>Also useful is the fork of ldasoft used in this pipeline:<br> https://github.com/xevra/ldasoft</p> <p>Please cite this work if you use the included data in a publication.</p> <p>-------------------------------------------------------------------------------<br>Summary<br>-------------------------------------------------------------------------------<br>Params_[MODEL].ini<br> This initialization file was used for COSMIC, <br> for the runs tagged with [MODEL].</p> <p>[MODEL]_[KSTAR1]_[KSTAR2]_[METALLICITY_BIN].tar.gz<br> This tarball contains the outputs from one run of COSMIC,<br> using Params_[MODEL].ini, for a type of binary indicated by<br> [KSTAR1] and [KSTAR2] according to COSMIC syntax,<br> and for the [METALLICITY_BIN]'th metallicity bin.</p> <p>[MODEL]_COSMIC.hdf5<br> This hdf5 database holds the DWD population outputs for all 60<br> COSMIC simulations in a compressed format.<br> It only holds information about binary systems at the end<br> of evolution (conv, according to COSMIC syntax).<br> It does not contain the evolutionary history of individual binaries<br> (the bpp information, according to COSMIC syntax).</p> <p>[MODEL]_m12i-000_LISA.nal.hdf5<br> This hdf5 database holds the LISA "resolved" population of DWD binaries<br> for a single realization of a Milky-Way-like galaxy.<br> It also stores many attributes indicating assumptions and various<br> population statistics.<br> The "nal" extension indicates that this database contains<br> truncated Gaussian likelihood models for the resolved population<br> of LISA DWDs,<br> which can be loaded by the gwalk code (https://gitlab.com/xevra/gwalk).<br> This database can also be explored by any hdf5 library (such as h5py).</p> <p>[MODEL]_m12i-000_LISA.hdf5<br> This hdf5 database holds all of the LISA-band binaries (f_GW > 10^-4 Hz)<br> for a single galaxy realization.</p> <p>[MODEL]_m12i-000_LISA.txt.gz<br> This text file stores the inputs for ldasoft gbfisher analysis,<br> for a specific galaxy realization under assumptions<br> broadly described by [MODEL]<br><br>See README.txt for full description<br><br>-------------------------------------------------------------------------------<br>Funding<br>-------------------------------------------------------------------------------<br>VD is supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center administered by Oak Ridge Associated Universities under contract NPP-GSFC-NOV21-0031. ROS gratefully acknowledges support from NSF awards NSF PHY-1912632, PHY-2012057, PHY-2309172, AST-2206321, and the Simons Foundation. JB is supported by the NASA LISA Project Office.<br><br>We acknowledge software packages used in this publication, including NUMPY (Harris et al. 2020), SCIPY (Virtanen et al. 2020), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013, 2018), H5PY (Collette 2013), LEGWORK (Wagg et al. 2022), and ldasoft Littenberg et al. (2020). This research was done using resources provided by the Open Science Grid (Pordes et al. 2007; Sfiligoi et al. 2009), which is supported by the National Science Foundation awards #2030508 and #1836650, and the U.S. Department of Energy’s Office of Science</p>
Dataset from: Gravitational wave sources in our Galactic backyard - Predictions for BHBH, BHNS and NSNS binaries in LISA
<p>The data from all simulations used in "<em><strong>Gravitational wave sources in our Galactic backyard: Predictions for BHBH, BHNS and NSNS binaries in LISA</strong></em>"</p> <p>Contents:</p> <ul> <li><strong>detections_and_totals.zip</strong> <ul> <li>Contains for .npy files that contain tables of the detections and total DCOs in Milky Way. These were calculated with <a href="https://github.com/TomWagg/detecting-DCOs-in-LISA/blob/main/simulation/postprocessing_notebooks/get_detection_rates.ipynb">this</a> and <a href="https://github.com/TomWagg/detecting-DCOs-in-LISA/blob/main/simulation/postprocessing_notebooks/get_total_DCOs_in_MW.ipynb">this</a> notebook and are included for convenience so you don't have to re-run these notebooks</li> </ul> </li> <li><strong>simulations_4yr.zip</strong> <ul> <li>Contains 60 .h5 files that contain the main simulations for a 4-year LISA mission. Each file contains the results for a single DCO type (BHBH, BHNS or NSNS) and model variation (20 variations) are labeled as <em>{DCO_type}_{variation}_all.h5</em><strong><em>. </em></strong></li> </ul> </li> <li><strong>simulations_10yr.zip</strong> <ul> <li>As simulations_4yr.zip but for a 10-year LISA mission</li> </ul> </li> <li><strong>simple_mw_simulations.zip</strong> <ul> <li>As simulations_4yr.zip but using a simple model for the Milky Way (discussed in Appendix D) and only for models A and F (hence only contains 6 .h5 files)</li> </ul> </li> </ul> <p>For a description of how to use these files to reproduce figures and results see the README.md in the associated GitHub repository: <a href="https://github.com/TomWagg/detecting-DCOs-in-LISA">https://github.com/TomWagg/detecting-DCOs-in-LISA</a></p> <p>Version 0.0.1 - Changes model E to E' as discussed in paper (now we allow HeHG donors to survive common-envelopes)</p> <ul> </ul>
Properties of Galactic B[e] supergiants. X. Refined orbit and fundamental parameters of the HD 327083 binary system.
<p>This dataset developed with MESA version r23.05.1 (May 30, 2023) and SDK version 23.7.3 (July 24, 2023), presents a comprehensive simulation of the binary system HD 327083, focusing on its evolution under specific initial conditions. </p>
Data release for "Discovering neutron stars with LISA via measurements of orbital eccentricity in Galactic binaries"
<p>Posterior samples and code to reproduce all figures associated with <em>Discovering neutron stars with LISA via measurements of orbital eccentricity in Galactic binaries</em>.</p> <p>The <code>parameter_estimation</code> folder contains the following:</p> <ul> <li><code>campaigns</code>: Analyses of eccentric quasi-monochromatic binaries, gridding over gravitational-wave frequency, eccentricty, and SNR. See the <code>README</code> inside for more information. The resulting posteriors are used in Figure 3, and the fitting formula Eq. 21. </li> <li><code>fiducial_source_checks</code>: Analyses that vary parameters other than SNR and frequency to investigate the effect on the minimum eccentricity that can be recovered. Used in Figure A1. Posteriors used for Figure 4 are also found in the <code>golden_binary</code> folder. </li> <li><code>nhat_runs</code>: Various analyses used for Figures 5, 6, B1, and C1. See the <code>README</code> inside for more information. Also see the <code>README</code> in <code>eccentric_gb_scripts</code> and links therein.</li> </ul> <p>Within each parameter estimation output folder there are <code>.dat</code> files for quantities such as the source SNR, log evidence, and posterior. There are also configuration <code>.yaml</code> files which are used by the BALROG code. These contain:</p> <ul> <li><code>lisa_config</code>: Parameters describing the LISA mission, including the duration in seconds. </li> <li><code>nessai_opts</code>: Settings used by nessai (the sampler used in this work). </li> <li><code>priors</code>: Lower and upper limits used for each source parameter. </li> <li><code>sources</code>: Injected values for each source parameter.</li> </ul> <p>The <code>notebooks</code> folder contains code to produce Figures 2, 3, 4, 6, and A1. Also included are notebooks to produce the fitting formula Eq. 21 (<code>emin_grid.ipynb</code>), and to inspect analyses in the <code>campaigns</code> and <code>fiducial_source_checks</code> folders.</p> <p>The <code>eccentric_gb_scripts</code> folder contains code to produce Figures 1, 5, B1 and C1. See the <code>README</code> inside for more information.</p>
Age determination of galactic B-type stars in double-lined eclipsing binaries
<p>We present the results of age determination for galactic B-type main sequence stars which are components of double-lined eclipsing binaries. Only detached systems are considered. We analyze 38 binary systems that meet such criteria. The analysis is based on evolutionary computations and we consider that the age is determined if there is a common value from the radius−age diagrams and the agreement in the position of both components in the Hertzsprung-Russell diagram. In some cases, to meet these two conditions, it was necessary to adjust the value of the metallicity, Z or/and the parameter of overshooting from the convective core, αov. We determine the consistent age for 33 binaries out of 38. Besides, we made an extensive computations and for each system we give the range of αov and Z, for which the consistent solutions exist. The age of the studied B-type main sequence stars ranges, as counted from the Zero Age Main Sequence, from about 2.5 Myr to about 200 Myr.</p>
Data release for "Identifying LISA verification binaries among the Galactic population of double white dwarfs"
<p>Posterior samples and SNR calculations associated with <em>Identifying LISA verification binaries among the Galactic population of double white dwarfs</em> (<a href="https://arxiv.org/abs/2210.10812">arxiv:2210.10812</a>, <a href="https://doi.org/10.1093/mnras/stad1288">MNRAS, 522, 5358 (2023)</a>).</p> <p>The <code>data</code> folder contains the following:</p> <ul> <li><code>vb_table</code>: Verification binary (VB) candidate properties obtained from electromagnetic (EM) observations. This data was compiled by Kupfer et al. and is available at <a href="https://gitlab.in2p3.fr/LISA/lisa-verification-binaries">https://gitlab.in2p3.fr/LISA/lisa-verification-binaries</a> (accessed on 2022 September 2). Used in Table 1.</li> <li><code>snr</code>: SNR calculations for each VB candidate as a function of mission duration. Used in Figure 2.</li> <li><code>basic</code>: Gravitational-wave (GW) parameter estimation study of each VB candidate. Used in Table 2 and Figure 3.</li> <li><code>detection_time</code>: VB SNR calculations with source property (and LISA launch time) uncertainty taken into account. Used in Figure 1 and Figure 4.</li> <li><code>em_priors</code>: GW parameter estimation study with EM information included in the priors. Used in Figure 5.</li> <li><code>unknown_noise</code>: GW parameter estimation study with the inclusion of noise parameters to vary the PSD. Used in Figure 6.</li> <li><code>filtered_populations</code>: Source properties of DWDs nearby in frequency to each VB candidate. See the <code>confused_sources.ipynb</code> notebook. Used in Figure 7.</li> <li><code>confusion_snr</code>: SNR calculations of the above confusion sources. Used in Figure 7.</li> <li><code>confusion</code>: A analysis of V803Cen with a realistic Galactic population of DWDs included in the data. Used in Figure 8.</li> </ul> <p>Code to reproduce every figure from the paper is available in <code>plots</code>.</p> <p>Supplementary notebooks associated with the generation of a realistic data instance (i.e. including a simulated Galactic population of DWDs nearby in frequency to V803Cen) can be found in <code>notebooks</code>.</p>
{Core-Collapse Supernovae in Binaries as the Origin of Galactic Hyper-Runaway Stars
<p>Several stars detected moving at velocities near to or exceeding the Galactic escape speed likely originated in the Milky Way disc. We quantitatively explore the `binary supernova scenario' hypothesis, wherein these stars are ejected at large peculiar velocities when their close, massive binary companions undergo a core-collapse supernova and the binary is disrupted. We perform an extensive suite of binary population synthesis simulations evolving massive systems to determine the assumptions and parameters which most impact the ejection rate of fast stars. In a simulation tailored to eject fast stars, we find hyper-runaway star progenitor binaries composed of a massive (~30 M<sub>sun</sub>) primary and a ~3-4 M<sub>sun</sub> companion on an orbital period that shrinks to <1 day prior to the core collapse following a common envelope phase. The black hole remnant formed from the primary must receive a natal kick >1000 km/s to disrupt the binary and eject the companion at a large velocity. We compare the fast stars produced in these simulations to a contemporary census of early-type Milky Way hyper-runaway star candidates. We find that these rare objects may be produced in sufficient number only when poorly-constrained binary evolution parameters related to the strength of post-core collapse black hole natal kicks and common envelope efficiency are adjusted to values currently unsupported -- but not excluded -- by the literature. We discuss observational implications that may constrain the existence of these putative progenitor systems.</p>
X-ray Binary Luminosity Function Scaling Relations in Elliptical Galaxies: Evidence for Globular Cluster Seeding of Low-Mass X-ray Binaries in Galactic Fields
<p>Processed Chandra images, Chandra source catalog, and extended Figure 2 for Lehmer et al. (2020)</p>
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