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10 results for “Large Magellanic Cloud”
Data Tables for Enrichment by Extragalactic First Stars in the Large Magellanic Cloud
<p>Machine-readable data tables for the article, "Enrichment by Extragalactic First Stars in the Large Magellanic Cloud"-- DOI: 10.1038/s41550-024-02223-w. Full descriptions of the tables are in the article, but we briefly summarize here-</p> <p>Table 1 (Table1.csv): This table provides general information on the stars for which we obtained long-exposure Magellan/MIKE data to derive their detailed elemental abundances. Columns include names, coordinates, SkyMapper g magnitudes from the Gaia XP spectra, and stellar parameters and metallicities with their respective random uncertainties.</p> <p>Table 2 (Table2.csv): This table provides names, radial velocities, metallicities, and selected elemental abundances with random uncertainties for stars listed in Table 1. [C/Fe]_c indicates carbon abundances that are corrected for the evolutionary state of the star following Placco et al. (2014). Abundances that are upper limits are flagged by the ul_[X/Fe] columns and have "nan" values for the uncertainty.</p> <p>Extended Data Table 1 (Extended_Data_Table1.csv): This table summarizes all of our observations, by providing names, coordinates, SkyMapper g magnitudes from the Gaia XP spectra, exposure times, dates of observation, and the instrument for these observations. This table includes stars observed with MagE, those observed with short-exposures with MIKE for just metallicities and carbon abundances, and those flagged as more metal-rich upon initial exposure and hence, not further observed. </p> <p>Extended Data Table 2 (Extended_Data_Table2.csv): This table provides names, followed by stellar parameters, metallicities, and carbon abundances, along with their respective uncertainties, for stars observed with MagE or MIKE for short exposures to just obtain a metallicity and carbon abundance. As in Table 2, abundances that are upper limits are flagged by the ul_[C/Fe] column and "nan" entries for the uncertainty.</p> <p>Supplementary Data 1 (Summary_Data_1.csv or Summary_Data_1.ascii): This table provides the suite of detailed element abundances and uncertainties from the long-exposure MIKE spectra of the stars in Table 1. Columns include the name, atomic number and ionization state of the element (element), the number of features used to estimate the elemental abundance (N), the solar abundance of that element (Solar), the absolute abundance (logeps), the chemical abundance scaled by the solar abundance relative to hydrogen ([X/H]), the ratio with respect to the iron abundance ([X/Fe]), the random uncertainty ([X/H]_err) and an upper limit flag (ul), and errors from propagating the uncertainties in the individual stellar parameters and the overall systematic and total uncertainty ([X/H]_errteff, [X/H]_errlogg, [X/H]_errvt, [X/H]_errsys, [X/H]_errtot). These are followed by the same columns, but with respect to iron (e.g., [X/Fe]_errteff, [X/Fe]_errlogg). Abundances of the CH molecule are indicated by 106.0 in the "element" column. This table is provided as a machine readable csv file and as an ascii file, the latter for easier visual readability.</p> <p>Supplementary Data 2 (Summary_Data_2.csv or Summary_Data_2.ascii): This table summarizes the chemical abundances from individual absorption features for the LMC stars with long-exposure MIKE spectra. The columns include the star name, the atomic number and ionization state of the element (species), the solar abundance of that element (Solar), followed by the wavelength, excitation potential, and loggf of the line (wavelength, expot, loggf), and then the measured equivalent width (EW), absolute abundance (logeps), and a flag indicating whether the abundance is an upper limit (ul). Abundances derived via spectral synthesis have "nan" entries for expot, loggf, and EW, and abundances of the CH molecular band are indicated by 106.0. This table is provided as a machine readable csv file and as an ascii file, the latter for easier visual readability. </p>
Science ready spectra of star clusters and their best-fitting models described in the research paper "Using Star Clusters as Tracers of Star Formation and Chemical Evolution: the Chemical Enrichment History of the Large Magellanic Cloud" by Chilingarian & Asa'd
<p>Science ready spectra of star clusters in the Large Magellanic Cloud and their best-fitting templates (alpha-enhanced MILES based simple stellar population models) obtained using the NBursts full spectrum fitting code. Each spectrum is presented as a binary FITS table, which contains a spectrum (wavelength, flux, uncertainties), best-fitting template, best-fitting parameters (radial velocity, age, metallicity), and a pixel mask used in the fitting procedure. For each cluster, 5 spectra are provided, which correspond to [alpha/Fe] values from 0.0 to 0.4 dex with a step of 0.1 dex. The only exception is NGC2249, for which only 3 models are provided. The alpha-enhancement value of a model grid used in the fitting procedure is given in the FITS keyword MGFEGRID.</p>
First Study of the Supernova Remnant Population in the Large Magellanic Cloud with eROSITA
<p>Aims. The all-sky survey carried out by the extended Roentgen Survey with an Imaging Telescope Array (eROSITA) on board Spektrum-Roentgen-Gamma (Spektr-RG, SRG) has provided us with spatially and spectrally resolved X-ray data of the entire Large Magellanic Cloud (LMC) and its immediate surroundings in the soft X-ray band down to 0.2 keV with an average angular resolution</p> <p>of 26′′ in the field of view. In this work, we have studied the supernova remnants (SNRs) and candidates in the LMC using data from the first four all-sky surveys (eRASS:4). From the X-ray data in combination with results at other wavelengths, we obtain information about the SNRs, their progenitors, and the surrounding interstellar medium (ISM). The study of the entire population of SNRs in a galaxy helps us to understand the underlying stellar populations, the environments, in which the SNRs are evolving, and the stellar feedback on the ISM.</p> <p>Methods. The eROSITA telescopes are the best instruments currently available for the study of extended soft sources like SNRs in an entire galaxy due to their large field of view and high sensitivity in the softer part of the X-ray band. We applied the Gaussian gradient magnitude (GGM) filter to the eROSITA images of the LMC to highlight the edges of the shocked gas in order to find new SNRs. We visually compared the X-ray images with those of their optical and radio counterparts to investigate the true nature of the extended emission. The X-ray emission is evaluated using the contours with respect to the background, while for the optical we used line ratio</p> <p>diagnostics, and non-thermal emission in the radio images. We used the Magellanic Cloud Emission Line Survey (MCELS) for the optical data. For the radio comparison, we used data from the Australian Square Kilometre Array Pathfinder (ASKAP) survey of the LMC. Using the star formation history (SFH) derived from the near-IR photometry of the VISTA survey of the Magellanic Clouds (VMC) we have investigated the possible progenitor type of the new SNRs and SNR candidates in our sample. Results. We present the most updated catalogue of SNRs in the LMC. Previously known SNRs and candidates were detected with 1σ significance down to a surface brightness of Σ [0.2–5.0 keV] = 3.0 × 10−15 erg s−1 cm−2 arcmin−2 and were examined. The eROSITA data have allowed us to confirm one of the previous candidates as an SNR. We confirm three newly detected extended sources as new SNRs, while we propose 13 extended sources as new X-ray SNR candidates. We also present the analysis of the follow-up</p> <p>XMM-Newton observation of MCSNR J0456–6533 discovered with eROSITA. Among the new candidates, we propose J0614–7251 (4eRASSU J061438.1−725112) as the first X-ray SNR candidate in the outskirts of the LMC.</p>
A 5% measurement of the gravitational constant in the Large Magellanic Cloud
<p><strong>Reproduction package for the paper "A 5% measurement of the gravitational constant in the Large Magellanic Cloud".</strong></p> <p><strong>The package contains inlist and run_star_extra.f files for MESA that can be used to simulate Cepheid variable stars under different values of the gravitational constant. Also included is a Python MCMC script for sampling MESA Cepheid models and comparing with measurements from Pilecki et al., ApJ 862 43 (2018).</strong></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>
Simulation data for the model of the Sagittarius stream in the presence of the Large Magellanic Cloud
<p>This archive contains simulations of the disrupting Sagittarius galaxy in the combined potential of the Milky Way and the Large Magellanic Cloud.</p> <p><strong>Sgr_snapshot</strong><br> contains the final (present-day) snapshot from the fiducial simulation with a triaxial Milky Way halo and M_LMC=1.5e11 Msun (see the readme file in that folder for details).</p> <p><strong>Sgr_snapshot_noLMC</strong><br> contains the same data but for a model without the LMC (which does not reproduce some aspects of the observations, but is nevertheless useful for a comparison with the other one).</p> <p><strong>potentials_triax</strong><br> contains the initial and subsequently evolving potentials of both the Milky Way and LMC, represented by multipole expansions, as well as the trajectory of the LMC and the reflex motion-induced acceleration of the Milky Way -- everything that is needed to study the dynamics of the Sgr stream and other objects in a time-dependent potential of the interacting Milky Way and LMC. This model corresponds to the stream simulation in the previous folder.</p> <p><strong>potentials_axisym</strong><br> contains the same data, but for another Milky Way halo model, which is axisymmetric rather than triaxial (note that in either case, its axis ratios vary with radius). It may be more convenient in certain applications, and produces a stream that fits the observations almost as well as the triaxial model.</p> <p><strong>scripts</strong><br> contains the Python scripts illustrating how to integrate orbits in a time-dependent potential, and how to construct initial conditions for these simulations (the parameter files for various choices of Milky Way halo potentials are also included). These scripts use the Agama framework, available at http://agama.software</p>
Simulation data for the article "On the Effect of the Large Magellanic Cloud on the Orbital Poles of Milky Way Satellite Galaxies"
<p>This archive contains the data shared in the context of the "On the Effect of the Large Magellanic Cloud on the Orbital Poles of Milky Way Satellite Galaxies" article.</p> <p>In particular, it contains the initial conditions and final snapshots of our N-body simulation.</p>
The TRAPUM Large Magellanic Cloud pulsar survey with MeerKAT I: Survey setup and first seven pulsar discoveries (Archive files)
<p>PSRCHIVE archive files of the seven new LMC radio pulsars as described in the paper <em>The TRAPUM Large Magellanic Cloud pulsar survey with MeerKAT I: Survey setup and first seven pulsar discoveries </em>(Prayag et al. 2024).</p>
Fit summary of "X-Shooting ULLYSES: Massive Stars at low metallicity IX: Empirical constraints on mass-loss rates and clumping parameters for OB supergiants in the Large Magellanic Cloud"
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Large Magellanic Cloud Extended Objects Catalog
A survey of extended objects in the Large Magellanic Cloud (LMC) was carried out on the ESO/SERC R and J Sky Survey Atlases, checking entries in previous catalogs and searching for new objects. The census provided 6659 objects including star clusters, emission-free associations, and objects related to emission nebulae. Each of these classes contains three subclasses with intermediate properties, which are used to infer total populations. The survey includes cross-identifications among catalogs, and includes 3246 new objects (~49% of the unified catalog). The authors have provided accurate positions, classification, and homogeneous measurements of sizes and position angles, as well as information on cluster pairs and hierarchical relation for superimposed objects. This unification and enlargement of catalogs is important for future searches of fainter and smaller new objects. The present catalog together with its previous counterpart for the SMC and the inter-Cloud region provide a total population of 7847 extended objects in the Magellanic System. The angular distribution of the ensemble reveals important clues on the interaction between the LMC and SMC. This table was created by the HEASARC in March 2007 based on the CDS table J/AJ/117/238, file table2.dat and contains the 6659 extended objects found in this LMC survey. This is a service provided by NASA HEASARC .
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