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7 results for “tidal disruption events”
Dataset for article "From X-rays to physical parameters: a comprehensive analysis of thermal tidal disruption event X-ray spectra"
<p>This repository contains the data used in the modeling of TDE X-ray emission within the article: Mummery et al. 2023, " From X-rays to physical parameters: a comprehensive analysis of thermal<br> tidal disruption event X-ray spectra" published as Mummery et al. 2023, MNRAS, 519, 5828</p>
Reproduction package for the article "Accretion disc cooling and narrow absorption lines in the tidal disruption event AT 2019dsg"
<p>This is the reproduction package for the MNRAS Article "Accretion disc cooling and narrow absorption lines in the tidal disruption event AT 2019dsg" by Cannizzaro et al (2021). It contains the reduced optical data, the scripts used for the emission lines fitting and the code used to perform the host galaxy subtraction.</p>
Reproduction package for the article "Spectroscopic Monitoring of the Candidate Tidal Disruption Event in F01004–2237"
<p>This is the reproduction package for the Article "Spectroscopic Monitoring of the Candidate Tidal Disruption Event in F01004-2237" by Cannizzaro et al (2021). It contains the reduced optical data and the scripts used for the emission lines fitting.</p>
Strong lensing of tidal disruption events: Detection rates in imaging surveys
<p>The unlensed and strongly lensed tidal disruption event (TDE) catalogs at the fiducial temperature of T = 20,000 K for the L1 and L2 luminosity models separately. The L1 luminosity model is an observationally driven upper limit defined by 1% of stellar fallback material (produced in the disruption of a 0.1 Msun main-sequence star) turning into radiation. The L2 luminosity model is defined by self-crossing shocks of stellar debris. Each line of a file represents a TDE (unlensed or lensed), so to compute the TDE detection rate one would need to iterate through the entire file, sum over the TDE weighting factors, and apply magnitude cuts according to the desired survey limit. For the lensed catalogs, further normalization by any oversampling factors is needed. These catalogs assume a survey area of 20,000 deg^2; the observational limiting magnitude is 27.0 (AB) for each band, so one can choose a brighter limiting survey magnitude with mag (AB) < 27.0. </p>
Reproduction package for the publication "Tidal disruption event AT2020ocn: early-time X-ray flares caused by a possible disc alignment process"
<p>This package contains the data analysed in the paper "Tidal disruption event AT2020ocn: early–time X–ray flares caused by a possible disc alignment process". The software XSPEC (Arnaud 1996) is needed to perform the spectral analysis and reproduce the results shown in the paper.</p> <p>The structure is as follows:</p> <p>./reproduction_ocn/nicer: contains all processed NICER data used in the paper, grouped by their epochs. "speclist-early.dat" lists all the early-time epochs before MJD 59130. "en_range.dat" lists the selected energy range at each epoch during the early-time period for X-ray spectral analysis. Within each epoch-specific folder, "src.fits" and "bkg.fits" are the source+background and background spectra re-binned using the FTOOL "ftgrouppha"; "*.arf" and "*.rmf" are ancillary file and response file for spectral analysis; rest files are direct products of the NICER data reduction process. See the paper for details.</p> <p>./reproduction_ocn/swift: contains all Swift/UVOT data used in the paper, grouped by their observation IDs. "m2.fits", "w1.fits", and "w2.fits" contain the UV lightcurves from three UV filters, produced by Swift task "uvotproduct". "swfxraypclc.dat" is the Swift/XRT lightcurve, produced by the online Swift pipeline: https://www.swift.ac.uk/user_objects/ (Evans et al. 2009). "./reproduction_ocn/MOSFiT-products/" includes MCMC products from the MOSFiT package (Mockler et al. 2019).</p> <p>./reproduction_ocn/xmm: contains the reduced XMM-Newton/EPIC-pn spectra of three epochs used in the paper. "1and2-slim.xcm" is fitting the XMM#1 and XMM#2 spectra using the slim disc model. "3-phenmnlgcl.xcm" and "3-relxillCp.xcm", are fitting the XMM#3 spectrum with, a powerlaw+zbbody model and a slim disc+relxillCp model, respectively.</p>
The mass fallback rate in relativistic stellar tidal disruption events
<p>MESA inlist files for the paper "The mass fallback rate in relativistic stellar tidal disruption events". Versions 15140 of MESA and MESA SDK 20.3.1 were used for the simulations. More details are in the README.txt file and in the paper.</p>
Data for 'Partial Tidal Disruption Events: The Elixir of Life'
<p>This folder includes all the data for the paper titled: Partial Tidal Disruption Events: The Elixir of Life</p> <p>Simulations were run with publicly available phantom code (https://github.com/danieljprice/phantom; https://phantomsph.readthedocs.io/en/latest/) and Kepler code (https://2sn.org/kepler/doc/Setup.html)</p> <p>We used splash (https://github.com/danieljprice/splash.git) for making Figures 2, 7, 8, 9, 10, 12, 14, B2, F1.</p> <p>We have three folders called s1_kepler, s3_kepler and s10_kepler. They contain the KEPLER models .wnd and .cnv files along with the dumps for ZAMS, MAMS and TAMS</p> <p>We have saved the PHANTOM relaxed models in star_(mass_of_star)_(evolution_stage) along with mapping back evolution in KEPLER files (link.dat, .wnd, .cnv). We have also saved Makefile, star.in, star.setup, tde.comp files, linkg.</p> <p>We have saved the PHANTOM simulation data in folders named star(mass_of_star)_(evolution_stage)_(beta_val). These include the .in, .tdeparams, ptok file, tde dump file used for analysis, KEPLER mapping back files (link.dat, .wnd, .cnv), .ev files. </p> <p>We have saved the KEPLER models that had the same mass as the remnants in star(mass_of_star)_(evolution_stage)_(beta_val)_kepler folders. We provide the generator file, .wnd, .cnv files. </p> <p>We have saved the KEPLER models that were generated by replacing the composition in the ptok files with the original star composition in the star_(mass_of_star)_(evolution_stage)_(beta_val)_strip</p> <p>We have saved the KEPLER models that were run until the He4 in the central bin was same as remnant He4 in centre, in the star(mass_of_star)_(evolution_stage)_(beta_val)_he4_same</p> <p>We have saved the PHANTOM simulation data for zero energy orbits run in star(mass_of_star)_(evolution_stage)_(beta_val)_zero folders. </p> <p>We have saved the geodesic files in the geodesic folder. It includes the .py files used to run jobs in parallel, and interpolation files. We have also saved the rp values used in the simulations run. </p> <p>We have saved the scripts used to run the KEPLER models (mapping back and stripping) in the python_code folder. We have also saved an EXCEL file which includes all the PHANTOM simulations data, along with the correct beta values shown in the paper. </p> <p><br>-----------------------------------------------------------------------------------------------------</p> <p>For the figures from the publication, </p> <p>Figure 1 uses the data from s1_kepler, s3_kepler and s10_kepler folders. </p> <p>Figure 2 uses data files present in the star(mass_of_star)_(evolution_stage)_(beta_val) folders. The folders for 3 solar MID have sub-folders starting with fig2 which contain the PHANTOM dump files. </p> <p>Figure 3 uses the data from solar3_mid_beta(value) folders. We have included the .ev files which were used to make this plot. </p> <p>Figure 4 uses the mass of the remnant as function of time. We have included the dump_info files that can be used to make this plot. </p> <p>Figure 5 and 6 use the mass of the remnant. You can access this information from Table 1 and 2 of the paper. </p> <p>Figure 7 uses the remnant files from the star1, star3 and star10 MID models. </p> <p><br>Figure 8 uses the ptok files and tde dump files. These are all included in the folders. </p> <p>Figure 9 uses dump files which are included in a sub-folder in the star3_mid_beta18 folder. </p> <p>Figure 10 requires the dump files along with files including the binned rotation profile and the break-up velocities. All of this is present in the folders where .exact1 and .exact2 are the binned and break-up profiles.</p> <p>Figure 11 can be generated by using the ptok files as they include binned rotation profile and radius.</p> <p>Figure 12 uses data files from the star3_mid_beta18 folder. We have included the remnant files. The same folder includes vphi files for Figure 13. </p> <p>Figure 14 requires the dump files along with tde.comp files. All tde.comp files are present in star_(mass_of_star)_(evolution_stage) folders. Dumps are in star_(mass_of_star)_(evolution_stage)_beta(value)folders. </p> <p>Figure 15 uses the files provided in the folders ending with _he4_same. </p> <p>Figure 16 and 17 can be generated by using the .wnd files provided in the star_(mass_of_star)_(evolution_stage) and star_(mass_of_star)_(evolution_stage)_beta(value) folders. The same files can be used for Figure 18 and Figure 19. </p> <p>Figure 20 can be generated by using the files present in folders ending with _kepler. </p> <p>Figure 21 uses files from folders ending with _strip. </p> <p>Figure 22 uses ptok files which have been provided for all star10_tams_beta(value) folders</p> <p>Figures A1, A2 can be generated using the ptok files and the original model files. </p> <p>Figure B2 uses files from sub-folder called cut_plot in the star3_mid_beta15 folder.</p> <p>Figure E1 uses .wnd files present in star(mass_of_star)_(evolution_stage) folders. </p> <p>Figure E2 uses .wnd files from the star3_tams_beta25 (sub-folder, time_run).</p> <p>Figure F1 uses files from zero and hyperbolic folders. </p> <p><br>-----------------------------------------------------------------------------------------------------</p> <p>To load the .wnd and .cnv, use windata and conv modules from python/source code written by Alexander Heger (KEPLER).<br>To load files starting with tde_0* use splash or sarracen (https://sarracen.readthedocs.io/en/latest/quick-start.html). <br>To load files starting with ptok (ASCII files), you can use splash or python. <br>To load .ev (ASCII files), you can use splash or python. <br>To load rem_* files or exact* files (ASCII) splash or python can be used. <br>To load link.dat file (ASCII) one can use splash or python. <br>To load KEPLER files containing @ one can use python. These are ASCII files. To convert any KEPLER files containing #, one would need to use Le-data filename to get it into ASCII form. </p> <p>-----------------------------------------------------------------------------------------------------<br>orbit.tdeparams files contain the initial position and velocities required for zero energy orbit. <br>tde.tdeparams files contain the beta, pericentre and starting distance along with mass of SMBH (in code units). </p> <p>star_00000.tmp files are the relaxed stellar profiles that were disrupted by the SMBH. <br>dump_info file is an ASCII file with information about the dumps such as the mass of the remnant, escape velocity, and maximum radius. <br> </p> <p> </p>
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