Find research datasets worth reusing

opencc-by-4.0Oct 2023View details →

Multiwavelength observations reveal a faint candidate black hole X-ray binary in IGR J17285-2922

<h2>Reproduction package for the paper "Multiwavelength observations reveal a faint candidate black hole X-ray binary in IGR J17285-2922"</h2><h4>This is a reproduction package with the internal API designation of 'silver'</h4><h4>Monthly Notices of the Royal Astronomical Society, Volume 507, Issue 1, October 2021, Pages 330–349</h4><h4>Authors: M. Stoop, J. van den Eijnden, N. Degenaar, A. Bahramian, S. J. Swihart, J. Strader, F. Jiménez-Ibarra, T. Muñoz-Darias, M. Armas Padilla, A. W. Shaw, T. J. Maccarone, R. Wijnands, T. D. Russell, J. V. Hernández Santisteban, J. C. A. Miller-Jones, D. M. Russell, D. Maitra, C. O. Heinke, G. R. Sivakoff, F. Lewis D. M. Bramich</h4><h4>Paper DOI: https://doi.org/10.1093/mnras/stab2127</h4><h4>Zenodo DOI: https://doi.org/10.5281/zenodo.4664505</h4> <h2>Raw Data</h2> - Uncalibrated X-ray data is given in ./raw_data - Radio data is too large in size to be stored on Zenodo. If you want to acquire these images, but can be found under https://data.nrao.edu searching for project code SF8027 - Raw data for the optical spectra can be acquired by contacting J. van den Eijnden <h2>Software</h2> - OS: MacOS Big Sur 11.6 Programming languages: - Python (3.9.7), matplotlib, numpy, pandas, scipy, linmix - Jupyter Notebook (6.3.0) NASA HEASARC's Software: - xrtpipeline (version 0.13.5) - caldb in the heasoft package (version 6.26.1) - xselect (version v2.4g) - xrtmkarf (version 0.6.3) - xspec (v. 12.10.1f) - casa pipeline (5.6.2) <h2>Figures and Tables</h2> - scripts and data to make the figures and tables can be found in ./figures_tables - figure 4, 5, 6, and 7 are made by collaborators. Please contact J. van den Eijnden if you would like access to data files or scripts for these figures. - X-ray lightcurve fit results in Table 3 is done by collaborators. Please contact J. van den Eijnden if you would like access to data files or scripts for this table. <h2>Intermediate data products  </h2> - Intermediate data products can be found in the directory ./intermediate_data - This includes the calibrated X-ray data, VLA imaging scripts to determine the flux density and spectral index. - Scripts can also be found here for intermediate data products for several figures (1, 2, 3, 8) <h2>Scientific-analysis</h2> - The directory ./scientific_analysis contains scripts and data to reduce the raw data to the intermediate data products. - ./Xray_files how to calibrate the Swift X-ray spectra - ./Xray_spectral_evolution contains how the intermediate data products for figure 3 - ./VLA_data_reduction how to reduce the VLA data and determine flux densities and spectral indices - ./Radio_Xray_Coupling contains the intermediate data products for figure 2 - ./Xray_lightcurve_fitting contains intermediate data products for Table 3 and fitting performed in section 3.4 - ./Orbital_Period contains intermediate data products for Table 4 and Figure 8 - ./xray contains backup files related to the x-ray spectra - ./radio contains backup files related to the radio data - the main results (intermediate data products) are the .txt files in this directory

opencc-by-4.0Dec 2021View details →

Optical polarimetric observations of low-mass X-ray black hole binary MAXI J1820+070 during 2019-2021

The dataset contains raw polarimetric FITS images of the low-mass X-ray black hole binary <a href="https://www.astronomerstelegram.org/?read=11399">MAXI J1820+070</a> (and surrounding field), obtained by the <a href="https://doi.org/10.3847/1538-3881/abc74f">DIPol-UF </a>optical CCD polarimeter in three (BVR) filters while mounted on the 2.56m <a href="https://www.not.iac.es">Nordic Optical Telescope</a>. The data were collected over 5 observing runs throughout 2019--2021. During each observing night, a set of calibration images were also obtained. These typically include 7 dark and 7 bias images per filter per night (sometimes more if weather conditions or instrument settings changed during observations). Bias and dark FITS files have `_bias` or `_dark` labels in their names, as well as FITS key `IMAGETYP` set to either `Bias Frame` or `Dark Frame`, respectively.

opencc-by-4.0Oct 2022View details →

The Missing Link Between Black Holes in High-Mass X-ray Binaries and Gravitational-Wave Sources: Observational Selection Effects

Data tables containing the calculated binary parameters used to acquire all results in <a href="https://arxiv.org/abs/2210.01825v1">arXiv:2210.01825v1</a>. The file "xrb_params_illustris_z0.05_sample.csv" contains data for the z<0.05 sampled population and the file xrb_params_illustris_z20_sample.csv contains data for the z<20 sampled population.

opencc-by-4.0Aug 2024View details →

Reproduction package for the paper 'Evidence for a dynamic corona in the short-term time lags of black hole X-ray binary MAXI J1820+070'

This is a basic reproduction package for the paper 'Evidence for a dynamic corona in the short-term time lags of black hole X-ray binary MAXI J1820+070', Bollemeijer et al., 2024, MNRAS, 528, 558-576. <ul> <li>This reproduction package aims for open science, with the internal API designation of 'Gold'.</li> <li>Authors: Niek Bollemeijer, Phil Uttley, Arkadip Basak, Adam Ingram, Jakob van den Eijnden, Kevin Alabarta, Diego Altamirano, Zaven Arzoumanian, Douglas J.K. Buisson, Andrew C. Fabian, Elizabeth Ferrara, Keith Gendreau, Jeroen Homan, Erin Kara, Craig Markwardt, Ronald A. Remillard, Andrea Sanna, James F. Steiner,  Francesco Tombesi, Jingyi Wang, Yanan Wang  and Abderahmen Zoghbi</li> <li>Paper DOI: https://doi.org/10.1093/mnras/stad3912</li> <li>Arxiv DOI: https://doi.org/10.48550/arXiv.2312.09835</li> <li>Published in the Monthly Notices of the Royal Astronomical Society (date of acceptance: 2023/12/12)</li> </ul> <h2>Raw Data</h2> <ul> <li>Raw event files for the described NICER observations can be obtained from the HEASARC at https://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3browse.pl. Select NICER as the telescope and search for MAXI_J1820+070.</li> <li>We used HEASoft v6.28 with standard reprocessing settings to obtain event lists to make light curves. See paper for details.</li> </ul> <h2>Software</h2> <ul> <li>Linux Ubuntu 22.04.</li> <li>Jupyter Notebook (7.0.7)</li> <li>Programming languages used: Python (3.12.1)</li> <li>Python packages used: numpy (1.26.3), matplotlib (3.8.2), scipy (1.12.0),  astropy (6.0.0)</li> </ul> <h2>Figures and Tables</h2> <ul> <li>Figures can be reproduced from the ./figures/ folder.</li> <li>All material and data used are available as intermediate data products.</li> <li>Jupyter notebooks (.ipynb files) can be used to make all figures. Running all cells at once does not work, but you can choose the figure you want to remake and executing the relevant cells will result in those figures.</li> </ul> <h2>Intermediate data products</h2> <ul> <li>The light curve arrays that are made in the first few cells of the main Jupyter Notebook can be found in 'datafiles.zip'. </li> <li>The parameters for the Lorentzian fits of the power spectra and the grouping of different observations can be found in 'qpofitsc.txt' and 'obsidsa.txt', respectively, in the same zipped folder.</li> </ul> <h2>End-to-End analysis scripts</h2> <ul> <li>The three Jupyter notebooks that have been added can be used to make the figures and reproduce the main results of the paper. Evidence_for_a_dynamic_corona_main.ipynb is about the main body of the paper, Evidence_for_a_dynamic_corona_energy_bands.ipynb is used for a part of the Discussion involving multiple narrow energy bands and Evidence_for_a_dynamic_corona_sim.ipynb is about the simulations described in Appendix A.</li> </ul>

opencc-by-4.0Sep 2021View details →

Modeling of the optical spectra of the High-mass X-ray binaries IGR J17544-2619 and IGR J21343+4738

We present the results of our long-term photometric and spectroscopic observations at the Russian–Turkish RTT-150 telescope for the optical counterparts of the High-mass X-ray binaries IGR J17544-2619 and IGR J21343+4738. Based on our optical data, we have determined for the first time the orbital and physical parameters of the IGR J17544-2619 by the methods of Doppler spectroscopy. We have calculated theoretical spectra for the optical counterpart by applying non-LTE corrections for selected lines and obtained the parameters of the stellar atmosphere (Teff = 33 000 K, log g = 3.85, RV = 9.5 Rsun, and MV = 23Msun). The variability of the Hα line in the optical Be star spectra of the IGR J21343+4738 is studied. It reflects the dynamic evolution of the equatorial disk of the optical star. Decrease of the equivalent width of the central absorption of the Hα line from 2006 to 2012 and from 2014 to 2019 is accompanied by a decrease in the photometric brightness of the system, which is explained by an increase in the radius of the equatorial disk of the Be star, which eclipses the star itself. In 2013, the disk size reached its maximum value and was destroyed. From 2014 to 2019 the process of accumulation of matter again began in the equatorial disk of the star, and it can be assumed that in the near future the source will again flare up in the X-ray range.

opencc-by-4.0Jul 2024View details →

The Symbiotic X-ray Binary IGR J16194-2810: Magellan Inamori Kyocera Echelle (MIKE) Spectra

Optical high-resolution spectra taken with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph for the symbiotic X-ray binary IGR J16194-2810.

Formation of Black Hole X-Ray Binaries with Non-degenerate Donors in Globular Clusters

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017ApJ...843L..30I">Formation of Black Hole X-Ray Binaries with Non-degenerate Donors in Globular Clusters</a>

Low-mass X-ray binaries: the effects of the magnetic braking prescription

MESA inlists associated with Formation of <a href="https://ui.adsabs.harvard.edu/?#abs/2019MNRAS.483.5595V/abstract">Low-mass X-ray binaries: the effects of the magnetic braking prescription</a>

Novel modelling of ultracompact X-ray binary evolution - stable mass transfer from white dwarfs to neutron stars

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2017MNRAS.470L...6S/abstract">Novel modelling of ultracompact X-ray binary evolution - stable mass transfer from white dwarfs to neutron stars</a>

Evolution of Transient Low-mass X-Ray Binaries to Redback Millisecond Pulsars

MESA inists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2015ApJ...814...74J">Jia & Li (2015)</a>. MESA version 7624. Publication DOI: <a href="https://doi.org/10.1088/0004-637X/814/1/74">10.1088/0004-637X/814/1/74</a>

Ultra-luminous X-ray sources and neutron-star-black-hole mergers from very massive close binaries at low metallicity

MESA inlists, run_star_extras, and data associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017A&A...604A..55M">Marchant et al. (2017)</a>. MESA version 8118. Publication DOI: <a href="https://doi.org/10.1051/0004-6361/201630188">10.1051/0004-6361/201630188</a> Files are also available in a gihub repository <a href="https://github.com/orlox/mesa_input_data/tree/master/2016_ULX">here</a> Upload includes post-processed simulation output in the files Z-XX.tar.xz, where XX represents the metallicity (Z-25.tar.gz is for a metallicity of log10(Z)=-2.5). Each folder inside the archive corresponds to a single MESA simulation, with the name indicating the value of log10(M_1), q=M2/M1 and the orbital period in days. For example, the directory 1.600_0.500_0.900 corresponds to the simulation with log10(M1/Msun)=1.6, M2/M1=0.5 and Porb=0.9 days. Each folder is also a MESA template folder, containing all input files neccesary to reproduce that individual simulation. The file summary_tables.tar.gz contains summarized information for each simulation in ascii format.

opencc-by-4.0Sep 2024View details →

Inlists for "Rethinking Thorne-Żytkow Object Formation: The Fate of X-ray Binary LMC X-4 and Implications for Ultra-long Gamma-ray Bursts"

<div> <div> <div> We use the MESA Isochrones and Stellar Tracks (MIST) package (Dotter 2016; Choi et al. 2016) with MESA v7503 (Paxton et al. 2011, 2013, 2015) and mesasdk x86_64-linux-20141212 revision 245.  </div> </div> </div>

opencc-by-4.0Jul 2023View details →

Investigating the Lower Mass Gap with Low Mass X-ray Binary Population Synthesis

Title: Investigating the Lower Mass Gap with Low Mass X-ray Binary Population Synthesis  Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry,          Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera,          Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra,          Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing,          and Emmanouil Zapartas           Table: Summary of Population Synthesis Models Columns:     Population parameters:         CE: efficiency of common envelope unbinding, either:             * 1 or 5         CE merge: stars without a distinct core-envelope boundary that instigate a CE                    event are either assumed to survive the CE (Optimistic) or are                    assumed to merge (Pessimistic).         QMIN: minimum ZAMS ratio, either:             * 0.01             * Lifetime limited (pre-main-sequence lifetime of the secondary is shorter               than the main-sequence lifetime of the primary)         BRK: prescription for magnetic braking of a tidally coupled magnetic wind, either:             * H02: Hurley et al. 2002             * IT03: Ivanova & Taam 2003         ACC: amount of mass accreted during Roche-lobe overflow, either:             * 50% efficiency             * State dependent: (i) limited to ten-times the thermal rate if the accretor is a main-sequence,                Hertzsprung gap or core helium burning star, or (ii) unlimited if the accretor is a giant branch,                early asymptotic giant branch or asymptotic giant branch star.                Compact objects also experience conservative mass transfer, provided the                mass-transfer rate is sub-Eddington.              Selection effect parameters:         weighting: logs what selection effects were considered for the detection weighted results, either:             *prob_occ: the probability that an outburst occurs and turns off during the survey             *prob_see: the probability that the outburst is bright enough to be detected             *prob: the product of prob_occ and prob_see                             RIA_nu: determines when the transition to radiatively inefficient accretion occurs, either:             *0 (no transition) or 0.05                  Results:         f_gap_N: fraction of LMXB systems with a mass gap BH (M<4.5Msol)         f_AIC_N: fraction of LMXB systems where the BH formed through accretion induced collapse of a NS         f_AIC_gap_N: fraction of LMXB systems where the BH formed through accretion induced collapse of a NS and                      the BH is in the mass gap         fw_X_N: detection weighted fraction of X (e.g., gap, AIC, AIC_gap)          Notes:      Each quantity is calculated for 5000 snapshots of the evolution tracks.       Here we report the Nth percentiles (e.g., 16, 50, 84) of each quantity.

opencc-by-4.0Jul 2020View details →

Reproduction package for the paper "A strongly changing accretion morphology during the outburst decay of the neutron star X-ray binary 4U 1608-52"

This is a basic reproduction package for the paper "A strongly changing accretion morphology during the outburst decay of the neutron star X-ray binary 4U 1608-52" by J. van den Eijnden et al. (2020). It provides reduced data sets, simulation scripts, X-ray spectral fits, and plotting scripts to allow the reproduction of the work performed in this paper. It also lists software used and data archives containing the public observational data.  An open access version of the paper can be found at <a href="https://arxiv.org/abs/2002.04003">https://arxiv.org/abs/2002.04003</a>.

opencc-by-4.0Jul 2022View details →

Do high-spin high mass X-ray binaries contribute to the population of merging binary black holes?

Input files and data used in the paper "Do high-spin high mass X-ray binaries contribute to the population of merging binary black holes?". MESA models were computed with version 12115 of MESA. COSMIC models new computed with version 3.4. README file included.

opencc-by-4.0Jan 2022View details →

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

This is the data repository for the paper "Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries"

opencc-by-4.0May 2024View details →

Inlists for "An Alternative Channel to Black Hole Low-Mass X-ray Binaries: Dynamical Friction of Dark Matter? "

In this work, we employ MESA code to diagnose whether the dynamical friction between dark matter and the companion stars can drive BH binaries to evolve toward the observed BH LMXBs and alleviate the effective temperature problem. Assuming that there exists a density spike of dark matter around BH, the dynamical friction can produce an efficient angular momentum loss, driving BH binaries with an intermediate-mass companion star to evolve into BH LMXBs for a spike index higher than $\gamma = 1.58$. MESA version: r12115; SDK compiler: mesasdk-x86_64-linux-20190830

Are there pre-main-sequence/black hole X-ray binaries?

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.480.3856X/abstract">Are there pre-main-sequence/black hole X-ray binaries?</a>

On the Origin of Black Hole Spin in High-mass X-Ray Binaries

MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2019ApJ...870L..18Q">On the Origin of Black Hole Spin in High-mass X-Ray Binaries</a>