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142 results for “Gravitational Waves”
Datasets for ``Numerical Simulations of Gravitational Waves from Early-Universe Turbulence''
<pre>The tar archive GW.tar contains an index.html file with links to the run directories for each run in Table 1 of the paper "Numerical Simulations of Gravitational Waves from Early-Universe Turbulence" by A. Roper Pol, S. Mandal, A. Brandenburg, T. Kahniashvili, &amp; A. Kosowsky with the temporary URL http://norlx55.nordita.org/~brandenb/tmp/GW. Corrections and updates are available on the active URL to this tar archive: https://www.nordita.org/~brandenb/projects/GW/</pre>
Submitted Completed pointings to the Gravitational Wave Treasure Map for event TEST_EVENT
Attached in a .json file is the completed pointing information for 2 observation(s) for the EM counterpart search associated with the gravitational wave event TEST_EVENT. These observations were taken on the DLT40 instrument.
Submitted Completed pointings to the Gravitational Wave Treasure Map for event TEST_EVENT
Attached in a .json file is the completed pointing information for 2 observation(s) for the EM counterpart search associated with the gravitational wave event TEST_EVENT. These observations were taken on the DECam instrument.
Submitted Completed pointings to the Gravitational Wave Treasure Map for event S190814bv
Attached in a .json file is the completed pointing information for 2293 observation(s) for the EM counterpart search associated with the gravitational wave event S190814bv. These observations were taken on the DECam instrument.
Stars Stripped in Binaries: The Living Gravitational-wave Sources
<p>Binary interaction can cause stellar envelopes to be stripped, which significantly reduces the radius of the star. The orbit of a binary composed of a stripped star and a compact object can therefore be so tight that the gravitational radiation the system produces reaches frequencies accessible to the Laser Interferometer Space Antenna (LISA). Two such stripped stars in tight orbits with white dwarfs are known so far (ZTF J2130+4420 and CD−30°11223), but many more are expected to exist. These binaries provide important constraints for binary evolution models and may be used as LISA verification sources. We develop a Monte Carlo code that uses detailed evolutionary models to simulate the Galactic population of stripped stars in tight orbits with either neutron star or white dwarf companions. We predict 0–100 stripped star + white dwarf binaries and 0–4 stripped star + neutron star binaries with a signal-to-noise ratio >5 after 10 yr of observations with LISA. More than 90% of these binaries are expected to show large radial velocity shifts of <span class="math-tex">\(\gtrsim\)</span>200 km s<sup>-1</sup>, which are spectroscopically detectable. Photometric variability due to tidal deformation of the stripped star is also expected and has been observed in ZTF J2130+4420 and CD−30°11223. In addition, the stripped star + neutron star binaries are expected to be X-ray bright with L<sub>X</sub> <span class="math-tex">\(\gtrsim\)</span> 10<sup>33</sup>–10<sup>36</sup> erg s<sup>-1</sup>. Our results show that stripped star binaries are promising multimessenger sources for the<br> upcoming electromagnetic and gravitational wave facilities.</p> <p> </p> <p>We provide detailed information about the run presented in Figures 2, 4, and 5 in the file named "entire_population_64.txt". We also provide information about sources with SNR > 4 in "pop_SNR4.txt" for 1000 runs of our standard model. The Jupyter notebook "Reading_stripped_star_compact_object_population.ipynb" reproduces figures of the manuscript and the Jupyter notebook "living_population.ipynb" shows how we model the Galactic population of stripped stars in tight orbit with compact objects.</p>
Submitted Galaxy Scores to the Gravitational Wave Treasure Map for event TEST_EVENT Preliminary
Attached in a .json file is the ranked galaxy information within the contour region of the EM counterpart search associated with the gravitational wave event TEST_EVENT Preliminary. A reference to these calculations can be found here: nicepaper
Submitted Galaxy Scores to the Gravitational Wave Treasure Map for event TEST_EVENT Preliminary
Attached in a .json file is the ranked galaxy information within the contour region of the EM counterpart search associated with the gravitational wave event TEST_EVENT Preliminary. A reference to these calculations can be found here: nicepaper
Observation of Gravitational Waves from the Coalescence of a 2.5-4.5 Msun Compact Object and a Neutron Star --- Data Release
<p>This data release contains the analysis results and data behind the figures of the GW230529 discovery paper (<a href="https://urldefense.com/v3/__https://dcc.ligo.org/LIGO-P2300352/public/__;!!Dq0X2DkFhyF93HkjWTBQKhk!W4i4x3JfGgemcFsnnEYP5qxiknddvrG1LWpTLjs_JGK907kTrEBkS8o6i5T6RUFMX0v04jCPhtTq9K2SLcv_4g$" target="_blank" rel="nofollow noreferrer noopener">https://dcc.ligo.org/LIGO-P2300352/public/</a>). Strain data for this event (the L1:GDS-CALIB_STRAIN_CLEAN_AR channel) can be downloaded on GWOSC (<a href="https://doi.org/10.7935/6k89-7q62" target="_blank" rel="noopener">https://doi.org/10.7935/6k89-7q62</a>).</p> <p>The PESummary metafile containing the parameter estimation posterior samples for all analyses performed in the paper (<strong>posterior_samples.h5</strong>) and skymap fits file (<strong>skymap_combined_PHM_high_spin.fits</strong>) for the preferred parameter estimation analysis (high-spin, combined samples using binary black hole waveforms) can be downloaded directly as individual files.</p> <p>The other analysis results are grouped by type: rates, populations, searches, and tidal. The <strong>figure_scripts.tar.gz</strong> file contains all the paper figures in jpeg format along with a Jupyter notebook to reproduce them and additional required helper scripts. Example code for working with the individual result files is given in the <strong>PaperPlots.ipynb</strong> notebook included in this tar file.</p> <p>In brief, the <strong>rates.tar.gz</strong> file contains two files that each include a subset of the rates probability distributions shown in Fig. 3 of the paper. The <strong>populations.tar.gz</strong> file contains all the data behind Figs. 4-8, with subdirectories for each of the three population analyses considered in the paper: Binned Gaussian Process, NSBH-pop, and Power-Law + Dip + Break. In addition to the data behind the figures, the Power-Law + Dip + Break subdirectory additionally includes two *result.json files for the hyper-parameter posterior samples. These files have the same format as the corresponding NSBH-pop *result.json files and can be manipulated in the same way, as shown in the figures notebook.</p> <p>The <strong>searches.tar.gz</strong> file contains the data behind Figs. 9-11 for each of the three search pipelines whose results are included in the paper. Finally, the <strong>tidal.tar.gz</strong> file contains the four probability distributions plotted in Fig. 14. All other figures are produced only using the posterior_samples.h5 file.</p>
Investigating the relation between gravitational wave tests of general relativity
<p>This data release accompanies the paper Johnson-McDaniel et al., Investigating the relation between gravitational wave tests of general relativity, arXiv:2109.06988.</p> <p>It provides the frame files containing the simulated observations of GR and non-GR signals (with no noise) analyzed in that paper. Specifically, these are simulated observations of binary black hole coalescences like GW150914 and GW170608.</p> <p>Each directory inside one of the tarballs corresponds to a given simulated observation and contains three frame files, one for each observatory (LIGO Hanford, LIGO Livingston, and Virgo). The GR cases contain simulated observations generated using the IHES EOB and IMRPhenomD models, while the non-GR cases contain the modified EOB, TIGER, FTA, and modified dispersion relation (MDR) simulated observations, as described in the paper. Specifically, the TIGER and FTA cases modify the 2PN coefficient, while the MDR cases are for a massive graviton. For the GW150914-like simulated observations, there are two selections (one large, one smaller) of the non-GR parameter for each non-GR case.</p> <p>The frame files in the GW150914-like (GW170808-like) cases contain 8 (16) seconds of data, starting from a GPS time of 1126259456 (1180922480). In both cases, the peak of the waveform (the "trigger time") is placed 2 seconds from the end of the data segment, so at GPS times of 1126259462 and 1180922494 for the GW150914-like and GW170608-like cases, respectively.</p> <p>Any publication that uses these data should cite the aforementioned paper that describes them (arXiv:2109.06988), as well as this Zenodo release, doi:10.5281/zenodo.5637361.</p> <p>Contents:</p> <p>GW150914_like_GR.tgz:<br> - GW150914_like_IHES_EOB_GR<br> - GW150914_like_IMRPhenomD_GR</p> <p>GW150914_like_nonGR_larger.tgz:<br> - GW150914_like_IHES_EOB_modGR_a2_400<br> - GW150914_like_IMRPhenomD_TIGER_dchi4_m13<br> - GW150914_like_IMRPhenomD_FTA_dchi4_m13<br> - GW150914_like_IMRPhenomD_MDR_alpha0_A_5em44</p> <p>GW150914_like_nonGR_smaller.tgz:<br> - GW150914_like_IHES_EOB_modGR_a2_40<br> - GW150914_like_IMRPhenomD_TIGER_dchi4_m2<br> - GW150914_like_IMRPhenomD_FTA_dchi4_m2<br> - GW150914_like_IMRPhenomD_MDR_alpha0_A_1em44</p> <p>GW170608_like_GR.tgz:<br> - GW170608_like_IHES_EOB_GR<br> - GW170608_like_IMRPhenomD_GR</p> <p>GW170608_like_nonGR.tgz:<br> - GW170608_like_IHES_EOB_modGR_a2_40<br> - GW170608_like_IMRPhenomD_TIGER_dchi4_m2<br> - GW170608_like_IMRPhenomD_FTA_dchi4_m2<br> - GW170608_like_IMRPhenomD_MDR_alpha0_A_1em43</p>
Submitted Completed pointings to the Gravitational Wave Treasure Map for event TEST_EVENT
Attached in a .json file is the completed pointing information for 1 observation(s) for the EM counterpart search associated with the gravitational wave event TEST_EVENT. These observations were taken on the DLT40 instrument.
Submitted Completed pointings to the Gravitational Wave Treasure Map for event TEST_EVENT
Attached in a .json file is the completed pointing information for 1 observation(s) for the EM counterpart search associated with the gravitational wave event TEST_EVENT. These observations were taken on the DLT40 instrument.
Submitted Completed pointings to the Gravitational Wave Treasure Map for event TEST_EVENT
Attached in a .json file is the completed pointing information for 2 observation(s) for the EM counterpart search associated with the gravitational wave event TEST_EVENT. These observations were taken on the DLT40 instrument.
Backward Population Synthesis: Mapping the Evolutionary History of Gravitational-Wave Progenitors dataset
<p>Dataset release accompanying Backward Population Synthesis: Mapping the Evolutionary History of Gravitational-Wave Progenitors.</p> <p>Note that A22_02_rerun.hdf, A22_5_rerun.hdf, A22_rerun.hdf, KW_rerun.h5 are not directly used in generating the plots in the paper.</p>
The Large Magellanic Cloud Revealed in Gravitational Waves with LISA: Population Release
<p>The Large Magellanic Cloud (LMC)’s binary populations for study by the <em>Laser Interferometer Space Antenna (LISA)</em> as generated by Keim et al. in a paper submitted to MNRAS (Keim, M. A., Korol, V., Rossi, E. M. The Large Magellanic Cloud Revealed in Gravitational Waves with LISA. <em>Monthly Notices of the Royal Astronomical Society</em>, 2022, submitted). The files include all current double white dwarfs in the LISA band (‘LISABand’), all which will be detectable with a S/N>7 after 4 yrs (‘Detect’), and all which are detached/non-accreting, i.e. sure LISA sources (‘Detached’). This release represents a 2.7*10^9 stellar mass LMC, and includes distribution models based on observation (‘M1’) and simulation (‘M3’). For more information, please refer to Keim et al. (2022). We request that researchers utilising any of these populations cite Keim et al. (2022).</p> <p>The data columns are as follows:</p> <p>Column 1 = Right Ascension (Degrees)</p> <p>Column 2 = Declination (Degrees)</p> <p>Column 3 = Age (Myr, since formation of Main Sequence Pair)</p> <p>Column 4 = Mass of White Dwarf One (Msun)</p> <p>Column 5 = Mass of White Dwarf Two (Msun)</p> <p>Column 6 = Radius of White Dwarf One (Rsun)</p> <p>Column 7 = Radius of White Dwarf Two (Rsun)</p> <p>Column 8 = Orbital Radius (Rsun)</p> <p>Column 9 = Frequency (Hz)</p> <p>Column 10 = Chirp (Hz^2)</p> <p>Column 11 = Latitude (Radians)</p> <p>Column 12 = Longitude (Radians)</p> <p>Column 13 = Amplitude (Defined with a prefactor of 2)</p> <p>Column 14 = Inclination (Radians)</p> <p>Column 15 = Polarization (Radians)</p> <p>Column 16 = Orbital Phase (Radians)</p> <p>Column 17 = Distance (kpc)</p> <p>Column 18 = Mass Transfer (1= Yes, i.e. Roche Lobe Overfill, 0= No)</p>
Exploring Supernova Gravitational Waves with Machine Learning
<p>The gravitational wave strain from сore-collapse supernova simulations used in our analysis. The file contains 402 signals labeled as <em>s00A0O00</em> or s00A0O00.0, where:</p> <p><em>s00</em> -- corresponds to (zero-age) progenitor mass, e.g. s27 means 27 solar mass</p> <p><em>A0</em> -- corresponds for a degree of differential rotation</p> <p><em>O00 </em>or <em>O00.0 </em>-- corresponds to central angular velocity, e.g. O07 or O07.5 means that our model has a central angular velocity of 7 or 7.5 rad/s, respectively</p> <p>Our waveforms are represented as a quadrupole wave amplitude. One can get a strain <em>h</em> multiplied by the distance <em>D </em>(= 10 kpc) by the following formula: <em>hD</em> = <strong><em>our_data</em></strong>/3.66 cm; see Eq (20) of Dimmelmeier et al 2008 [<a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.78.064056">link</a>] for more information. All waveforms are represented in the time range from -15 to 20 ms with a 0.001 ms step size. The time of zero corresponds to the time of bounce. See [<a href="https://arxiv.org/abs/2209.14542">https://arxiv.org/abs/2209.14542</a>] for more information.</p>
Submitted Completed pointings to the Gravitational Wave Treasure Map for event S240422ed
<p>Attached in a .json file is the completed pointing information for 55 observation(s) for the EM counterpart search associated with the gravitational wave event S240422ed. These observations were taken on the ZTF, and WINTER instruments.</p>
Submitted Completed pointings to the Gravitational Wave Treasure Map for event S240422ed
<p>Attached in a .json file is the completed pointing information for 24 observation(s) for the EM counterpart search associated with the gravitational wave event S240422ed. These observations were taken on the MLS10KCCD-CSS instrument.</p>
Submitted Completed pointings to the Gravitational Wave Treasure Map for event S240422ed
<p>Attached in a .json file is the completed pointing information for 306 observation(s) for the EM counterpart search associated with the gravitational wave event S240422ed. These observations were taken on the Sinistro, and MuSCAT instruments.</p>
Submitted Completed pointings to the Gravitational Wave Treasure Map for event MS240429t
Attached in a .json file is the completed pointing information for 2 observation(s) for the EM counterpart search associated with the gravitational wave event MS240429t. These observations were taken on the DLT40 instrument.
Mass-redshift dependency of Supermassive Black Hole Binaries for the Gravitational Wave Background
<p>These show the posterior distributions as supplementary material for arXiv:2305.18293 and doi:10.1093/mnras/stae1219</p> <p>The corner plots for the complete 20 parameters with amplitudes hc = 0.5e-15, 1e-15, 2e-15, 3e-15, and 4e-15 for both circular and eccentric population of SMBHBs are presented in the 'free_parameters' folder.</p> <p>The corner plots for the 16 parameters with amplitudes hc = 0.5e-15, 2e-15, and 4e-15 for both circular and eccentric population of SMBHBs using the fitted BH-bulge mass parameters from the simulations can be found in the 'simulation_parameters' folder.</p> <p>The posterior distributions are shown as black contours, while the prior distributions are denoted by light green lines. The top right inlay figure shows the median and central 2sigma range of the recovered characteristic spectrum, where the 5 points denote the frequency bins of 1/(25years), 2/(25years), 3/(25years), 4/(25years) and 5/(25years), which are used as the input data for the Bayesian analysis. To guide the eye the analytic sensitivity curve from the IPTA DR2 is also plotted.</p>
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