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27 results for “X-ray:stars”
The detection of radio emission from known X-ray flaring star EXO 040830−7134.7
<p>This is the radio light curve of known X-ray flaring star EXO 040830−7134.7 observed by MeerKAT as part of ThunderKAT. These data are part of a publication in the Monthly Notice of the Royal Astronomical Society (Driessen et al., Accepted 2021 November 25. Received 2021 November 25; in original form 2021 August 25).</p> <p>The light curve is from the full-time-integration, full-frequency-integration images of VW Hyi, as processed by the LOFAR Transients Pipeline (<a href="https://tkp.readthedocs.io/en/latest/introduction.html">TraP</a>).</p> <p>The columns in the file are:</p> <ul> <li>mjd: the modified Julian Date (MJD) of the observation. The MJD is given by MJD=JD-2400000.5 where JD is the Julian Date</li> <li>f_int_Jy: the integrated flux density of the source in Jansky (Jy) determined by the LOFAR TraP</li> <li>f_int_err_Jy: the uncertainty on f_int_Jy in Jansky determined by the LOFAR TraP</li> <li>freq_eff_Hz: the effect frequency in Hertz (Hz) as determined by the LOFAR TraP</li> <li>taustart_ts: the ISO 8601 time of the observation in Coordinated Universal Time (UTC)</li> </ul> <p>The files were made using the Pandas package, so we recommend Python users load them using</p> <pre><code>import pandas as pd pd.read_csv(filename, comment='#')</code></pre> <p>If you use the data shared here please ensure that you cite the MNRAS paper (Driessen at al. 2021) and the Zenodo DOI: 10.5281/zenodo.5084298.</p> <p>The MeerKAT telescope is operated by the South African Radio Astronomy Observatory, which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation.<br> LND acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 694745).</p>
Constraining the properties of dense neutron star cores: The case of the transient low-mass X-ray binary HETE J1900.1-2455
<p>This is a basic reproduction package for the paper "Constraining the properties of dense neutron star cores: The case of the transient low-mass X-ray binary HETE J1900.1-2455" by <a href="https://doi.org/10.1093/mnras/stab2202">N. Degenaar et al. (2021)</a>. It provides reduced data products, simulated data and 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.</p>
X-ray and optical light curves of the M dwarf dipper star TIC 234284556
<p>We observed the star TIC 234284556 with XMM-Newton in soft X-rays and in the optical for ca. 35 hours (127.8 ks), starting 2022-04-16 22:58:46, ObsID 0881050101.</p> <p>We provide here two extracted soft X-ray light curves (energy band 0.2-2 keV) collected with XMM-Newton's PN camera, namely for a circular extraction region with 20 arcsec radius centered on the position of the M dwarf star TIC 234284556 (pn_lca_02_2.fits) with 100 seconds time binning, and a background light curve with the same energy range and time binning extracted for a PN background region with a three times larger radius (pn_lcabg_02_2.fits). We also provide optical light curves in the V band, collected with XMM-Newton's Optical Monitor with 10 seconds cadence (file names P0881050101OMS0**TIMESR0000.FIT).</p> <p>A barycentric correction, using the XMM-SAS task "barycen", has been applied to the PN and OM time columns. The time coordinate is given in seconds since BJD 2450814.5 (1998-01-01 00:00:00).</p>
Star Formation In Nearby Clouds (SFiNCs): X-ray And Infrared Source Catalogs And Membership. SPCM Atlas Dataset.
<p>The SPCM (SFiNCs Possible Cluster Member) Atlas dataset accompanies the article entitled ``Star Formation In Nearby Clouds (SFiNCs): X-ray And Infrared Source Catalogs And Membership,'' by Getman, Broos, Kuhn, Feigelson, Richert, Ota, Bate, and Garmire, to appear in The Astrophysical Journal Supplement Series. The paper is also available on-line on astro-ph at: https://arxiv.org/abs/1612.05282 . SPCM Atlas is a collection of 25 PDF files. Four pdf files are associated with the SFiNCs star forming region (SFR) Cep OB3b, and 21 pdf files are associated with the remaining 21 SFiNCs SFRs. Full description of SPCM Atlas is given in the Appendix B section of the article. This upload is superseded by a new version, http://doi.org/10.5281/zenodo.345398 .</p>
Constraining the Neutron Star Mass-Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set
<p>This deposit includes the cleaned, filtered and phase folded NICER event data set for the millisecond pulsar (MSP) PSR J0030+0451 in the 0.25-3 keV band. The data processing and filtering was performed using HEASoft 6.251 and NICERDAS version 5.0; the specific parameters and filtering criteria used are detailed in the ApJ Letter listed above. This event list was used to produce what is shown for PSR J0030+0451 in Figures 2, 3, and 4 in the accepted ApJ Letter listed above and was also used for the neutron star mass-radius and equation of state inference analyses presented in the companion papers (Miller et al. 2019, Riley et al. 2019, and Raaijmakers et al. 2019).</p> <p>The event file and its MD5 checksum is:<br> J0030+0451_merged_phase_0.25-3keV.fits (463bbac7203bb45bb02ea0deed49f083)<br> </p>
MCMC samples for X-ray spectra fits summarised in the paper "A strangely light neutron star"
<p>Posterior samples for NS mass and radius described based on fitting of XMM-Newton and Suzaku spectra of the CCO in HESS J1731-347 and described in the paper the paper "A strangely light neutron star" (DOI: <a href="https://doi.org/10.21203/rs.3.rs-1509469/v1">10.21203/rs.3.rs-1509469/v1</a>). Two files uploaded contain posterior samples based based </p> <p>a) on fitting X-ray data alone using single temperature carbon atmosphere model and Gaia parallax priors (xray_only_carbatm.txt)</p> <p>b) on fitting the same X-ray data but including also all additional priors described in the main text and full priors on distance rather than inverted parallax value (full_priors_carbatm.txt). Note that initial version contained wrong file uploaded by error, so the correct file to use in this case is full_priors_carbatm_corr.txt. We urge, however, to use a) as a baseline, i.e. as input for incorporating of other constraints for two reasons: first, the procedure of incorporating other constraints adopted by us and you may be different, and second, this file contains relatively small number of samples as it was mainly meant as illustration putting our results in context of other constraints and to give an idea of impact which our measurement has on EOS selection for a particular family of EOSs, so the result would be different if other set of EOSs is considered. </p> <p>in addition a file with updated weights for EOSs used by Dietrich et al 2021 (2020Sci...370.1450D, available on https://github.com/diettim/NMMA) which take into the account constrains from X-ray spectral fitting presented in our work for the CCO and constrains based on modeling of the 4U 1702-429 bursts reported by Nattila et al 2017 (2017A&A...608A..31N) are included in file chiralEFT_MTOV_NICER_GW170817_AT2017gfo_cco_weights.txt. This file is based on and has the same syntax as file chiralEFT_MTOV_NICER_GW170817_AT2017gfo_weighting.dat provided by Dietrich et al 2021 available on https://github.com/diettim/NMMA along with the corresponding tabulated EOS files.</p> <p> </p>
Star Formation In Nearby Clouds (SFiNCs): X-ray And Infrared Source Catalogs And Membership. SPCM Atlas Dataset (Version 2).
<p>The SPCM (SFiNCs Possible Cluster Member) Atlas dataset accompanies the article entitled ``Star Formation In Nearby Clouds (SFiNCs): X-ray And Infrared Source Catalogs And Membership,'' by Getman, Broos, Kuhn, Feigelson, Richert, Ota, Bate, and Garmire, to appear in The Astrophysical Journal Supplement Series. The paper is also available on-line on astro-ph at: https://arxiv.org/abs/1612.05282 . SPCM Atlas is a collection of 25 PDF files. Four pdf files are associated with the SFiNCs star forming region (SFR) Cep OB3b, and 21 pdf files are associated with the remaining 21 SFiNCs SFRs. Full description of SPCM Atlas is given in the Appendix B section of the article. This is an update of the previous zenodo.231216 upload. This update includes revised PDF atlases for Be59 and IC348 (with revised vales of the SED slope and [3.6] and [4.5]-band magnitudes).</p>
X-ray Variability of the Massive O star zeta Pup
<p>Analysis of very deep, high resolution X-ray spectroscopy of the early O supergiant zeta Pup, acquired by Chandra in 2018-9, is presented. The cumulative spectrum has an exposure time of 820 kiloseconds (almost 10 days) and covers the wavelength range 3-20 Å. The X-ray broad-band light curve displays significant variability with one clear period, 1.78d, which has been previously detected in optical. The correlation with optical and UV data is discussed, notably in the context of CIRs and (possibly magnetic?) spots on the stellar surface with at least one stable period. The possible correlation of periods with optical and UV data is discussed. The X-ray spectrum is divided into several wavelength bands which are explored for variability. These divisions allow construction of light curves for hard, medium, and soft bands individually (which allows calculations of time-dependent hardness ratios), along with independently investigating the temporal behavior of strong X-ray emission lines. New constraints on the structure of stellar winds for the most massive stars are discussed.</p>
Ptychographic X-ray speckle tracking (PXST) scan of the Siemens star test sample
<p>The PXST scan of the Siemens star test sample measured at P11 beamtime of the PETRA III synchrotron radiation facility. The beam was focused with a pair of MLLs with focal lengths of 1.25 mm and 1.15 mm and numerical apertures of 0.014 and 0.015, in the vertical and horizontal directions, respectively. The X-ray beam photon energy was 17.5 keV.</p>
Novel modelling of ultracompact X-ray binary evolution - stable mass transfer from white dwarfs to neutron stars
<p>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></p>
Ultra-luminous X-ray sources and neutron-star-black-hole mergers from very massive close binaries at low metallicity
<p>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.</p> <p>Publication DOI: <a href="https://doi.org/10.1051/0004-6361/201630188">10.1051/0004-6361/201630188</a></p> <p>Files are also available in a gihub repository <a href="https://github.com/orlox/mesa_input_data/tree/master/2016_ULX">here</a></p> <p>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.</p> <p>The file summary_tables.tar.gz contains summarized information for each simulation in ascii format.</p>
X-ray Emission of Nearby Low-mass and Sun-like Stars with Directly Imageable Habitable Zones: X-ray Spectra and Light Curves
<p>This repository contains the X-ray light curves extracted from the XMM-Newton and Chandra observations and the best-fit X-ray spectral models (with and without emission lines) from all stars detected at high significance in Binder et al. (2024), ApJS, ..., ...</p> <p>Description of Files:</p> <h3>LightCurves.zip</h3> <p>Summary: Light curve files (327) for all stars detected at high significance; in FITS (BinTableHDU) format with 7-14 extensions. The following types of data are included:</p> <ul> <li>"*_source.lc" : EPIC/PN source light curves of stars detected with more than ~500 net counts in an XMM-Newton observation</li> <li>"*_bkg.lc" : EPIC/PN background light curves of stars detected with more than ~500 net counts in an XMM-Newton observation</li> <li>"*_sub_lc.fits" : Background-subtracted light curves of stars detected with more than ~50 net counts in a Chandra observation</li> </ul> <h3>Spectra.zip</h3> <p>Summary: Spectra (152) for all stars detected at high significance (with >500 net counts in Chandra observations and >2000 net counts in XMM-Newton observations) in ASCII (ECSV format). We provide both the continuum spectra and spectra containing line emission. For stars that exhibit X-ray count rate variability, we provide spectra for specific variability types (see Binder et al. 2024 for details). The following types of data are included:</p> <ul> <li>"*_continuum.dat" : Continuum-only best-fit spectra</li> <li>"*_lines.dat" : Best-fit spectra containing line emission</li> </ul>
Reproduction package for the paper "A strongly changing accretion morphology during the outburst decay of the neutron star X-ray binary 4U 1608-52"
<p>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. </p> <p>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>.</p>
X-ray properties of early-type stars in the Tarantula Nebula from T-ReX
<p>X-ray data related to paper with same title.</p>
The miniJPAS Survey: The Radial Distribution of Star Formation Rate in Faint X-ray AGN
<p>Figures show the AGN host galaxies accompanied by their observed J-spectra within their Kron radii and the fitted spectrum with \texttt{CIGALE} to determine their physical properties. We note that \texttt{CIGALE} does not fit AGN emission for 1 source with miniJPAS object ID 2241-18160. This object fell in the composite area in the BPT diagram, and in the LINER area in the WHAN diagram. This could represent a case where the AGN is obscured due to dust and \texttt{CIGALE} fails to fit optical AGN emission for this case. This further emphasizes the importance of X-ray emission to identify AGN systems that are optically obscured and are seen as normal galaxies without X-ray detections. We report that the inclusion or emission of this object from our AGN sample does not produce any differences in the results obtained in this paper.</p>
UV and X-ray observations of the neutron star LMXB EXO 0748-676 in its quiescent state
<p>Data used in the manuscript "UV and X-ray observations of the neutron star LMXB EXO 0748-676 in its quiescent state" submitted to MNRAS</p>
The input files and associated data products for "Modeling High Mass X-ray Binaries to Double Neutron Stars through Common Envelope Evolution"
<p>Simulations were made using the version 12115 of the MESA code together with the x86_64-linux-20190830 MESA SDK. "template.zip" provides the MESA inlist files to reproduce our simulations. "CE_1.zip" provides our simulated results for a grid of binary systems with common envelope ejection efficiencies set to be 1.0. Different folders indicate the binary systems with different initial parameters. Inside each folder information can be found for binary properties in the "history.data" file. Each folder also contains the "result.txt" file with the terminal output of the simulation. "CE_3.zip", "CE_0.3.zip" and "CE_0.1.zip" are the same as "CE_1.zip" but with common envelope ejection efficiencies set to be 3.0, 0.3 and 0.1, respectively.</p>
Star-forming nucleus with an X-ray source
<p>Cloudy model grid for the MULTIGRIS framework. See Lebouteiller & Ramambason 2022, Beck et al. 2023 for details.</p>
LkH-alpha 101 Star Formation Region Chandra X-Ray Point Source Catalog
This table contains some of the results from a multi-wavelength study of a partially embedded region of star formation centered on the Herbig Be star LkH-alpha 101. Using two 40 ks Chandra observations, The authors have detected 213 X-ray sources in the ~ 17' x 17' ACIS-I field. They combine the X-ray data with Two Micron All Sky Survey (2MASS) near-IR observations and Spitzer Space Telescope (SST) IRAC and MIPS 24-micron observations to obtain a complete picture of the cluster. A total of 158 of the X-ray sources have infrared counterparts. Of these, the authors find nine protostars, 48 Class II objects, five transition objects, and 72 Class III objects. From the Spitzer data, they identify an additional 10 protostars, 53 Class II objects, and four transition disk candidates which are not detected by Chandra. (These objects are not included in this HEASARC table which contains the multi-wavelength data for only the 213 detected X-ray sources). The authors obtained optical spectra of a sample of both X-ray-detected and non-X-ray-detected objects. Combining the X-ray, Spitzer, and spectral data, they obtain independent estimates of cluster distance and the total cluster size - excluding protostars. The authors obtain consistent distance estimates of 510 (+100,-40) pc and a total cluster size of 255 (+50,-25) stars. They find the Class II:III ratio is about 5:7 with some evidence that the Class III sources are spatially more dispersed. The cluster appears very young with three sites of active star formation and a median age of about 1 Myr. The field was observed by Chandra on 2005 March 6 starting at 17:16 UT for 40.2 ks of total time and 39.6 ks of the so-called good time (Chandra ObsID 5429). It was observed again on 2005 March 8 starting at 17:43 UT for essentially the same duration (Chandra ObsID 5428). The ACIS was used in the nominal imaging array (chips I0-I3) which provides a field of view of approximately 17' x 17'. The aimpoint was at RA, Dec = 04:30:14.4, +35:16:22.2 (J2000.0) with a roll angle of 281 degrees. In addition, the S2 and S3 chips were active; however, the analysis of these data is not presented here. For purposes of point-source detection, the data from the two observations were merged into a single event list following established CIAO procedures to create a merged event list. To identify point sources, photons with energies below 300 eV and above 8.0 keV were filtered out from this merged event list. This excluded energies which generally lack a stellar contribution. By filtering the data as described, contributions from hard, non-stellar sources such as X-ray binaries and active galactic nuclei (AGNs) are attenuated, as is noise. A monochromatic exposure map was generated in the standard way using an energy of 1.49 keV which is a reasonable match to the expected peak energy of the stellar sources and the Chandra mirror transmission. The CIAO tool WavDetect was then run on a series of flux-corrected images binned by 1, 2, and 4 pixels. The output source lists were combined and this resulted in the detection of 231 sources. The authors defined false detections as any sources with < 4 net counts or any sources more than 5' off-axis with < 7 net counts. By this definition, 18 of the 231 detections were rejected as false detections. A post facto check confirmed that none of these (spurious) sources had an infrared counterpart. This table was created by the HEASARC in July 2010 based on the versions of Tables 1, 2, 3, 7 and 9 from the paper which were obtained from the electronic ApJ web site. This is a service provided by NASA HEASARC .
Massive Star-Forming Regions Omnibus X-Ray Catalog
This table contains the Massive Star-forming Regions (MSFRs) Omnibus X-ray Catalog (MOXC), a compendium of X-ray point sources from Chandra/ACIS observations of a selection of MSFRs across the Galaxy, plus 30 Doradus in the Large Magellanic Cloud. MOXC consists of 20,623 X-ray point sources from 12 MSFRs with distances ranging from 1.7 kpc to 50 kpc, and comprises Table 3 of the reference paper. In their paper, the authors show the morphology of the unresolved X-ray emission that remains after the cataloged X-ray point sources are excised from the ACIS data, in the context of Spitzer and WISE observations that trace the bubbles, ionization fronts, and photon-dominated regions that characterize MSFRs. In previous work, they have found that this unresolved X-ray emission is dominated by hot plasma from massive star wind shocks. This diffuse X-ray emission is found in every MOXC MSFR, clearly demonstrating that massive star feedback (and the several-million-degree plasmas that it generates) is an integral component of MSFR physics. The Chandra observations used for the Massive Star-forming Regions Omnibus X-ray Catalog (MOXC) are summarized in Table 2 of the reference paper and have dates ranging from 2000-04-03 to 2013-01-31 for the 12 MSFRs: the 7 MYStIX targets NGC 6334, NGC 6357, M 16, M 17, W 3, W 4 and NGC 3576, and the 5 "beyond-MYStIX" targets G333.6-0.2, W 51A, G29.96-0.02, NGC 3603 and 30 Doradus. A similar table to MOXC for other MYStIX targets was presented by Kuhn et al. (2013, ApJS, 209, 27, available as the HEASARC MYSTIXXRAY table). The main difference between that table and the MOXC version is that the present authors have chosen to omit absorption-corrected X-ray source luminosities from the XPHOT algorithm (Getman et al. 2010, ApJ, 708, 1760) herein, because those quantities are given in Broos et al. (2013, ApJS, 209, 32, available as the HEASARC MYSTIXMPCM table) for relevant MYStIX X-ray sources (those classified as pre-main sequence stars). For beyond-MYStIX targets, the authors chose to postpone XPHOT calculations until the X-ray sources were classified, since XPHOT estimates are only appropriate for pre-MS stars. The XPHOT code is available (Getman et al. 2012, Astrophysics Source Code Library, record ascl.soft12002) if others wish to use it on MOXC sources. All photometric quantities in this table are apparent (not corrected for absorption). The HEASARC has used prefixes 'fb_', 'sb_' and 'hb_' (replacing the suffixes '_t', '_s' and '_h' used in the reference paper) on the names of the X-ray photometric quantities which designate the full (total, 0.5 - 8 keV), soft (0.5 - 2.0 keV) and hard (2-8 keV) energy bands. Correction for finite extraction apertures is applied to the ancillary reference file (ARF) calibration products (see Broos et al. 2010, ApJ, 714, 1582, Section 5.3); the total_counts and counts quantities characterize the extraction and are not aperture-corrected. The only calibrated quantities presented are the apparent photon fluxes, in units of photon cm<sup>-2</sup> s<sup>-1</sup> (see Broos et al. 2010, ApJ, 714, 1582, Section 7.4), and estimates for the apparent energy fluxes, in units of erg cm<sup>-2</sup> s<sup>-1</sup> (Getman et al. 2010, ApJ, 708, 1760). This table was created by the HEASARC in October 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/213/1">CDS Catalog J/ApJS/213/1</a> files table3.dat (the MOXC X-ray Source Catalog) and table6.dat (the list of MOXC sources in previously published Chandra catalogs). This is a service provided by NASA HEASARC .
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Allen Brain Atlas
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International Brain Laboratory public data
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OpenNeuro
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