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48 results for “M Dwarfs”
A fading radius valley towards M-dwarfs, a persistent density valley across stellar types -- data
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Red-optical spectra of three nearby M dwarfs with SALT HRS
<p>We conducted observations of three nearby mid-M dwarfs with the High-Resolution Spectrograph (HRS) at the Southern African Large Telescope (SALT, DDT proposal code: 2019-2-DDT-006). We obtained spectra in its red arm over a wavelength range of 5,500-8,900 Angström with a spectral resolution of about 40,000 in medium-resolution mode. The observations were carried out on February 08 and February 09, 2020. The data were reduced with the PEPSI data reduction software (Strassmeier et al. 2018). The reduction followed the standard steps of bias overscan detection and subtraction, scattered light extraction from the inter-order space and subtraction, definition of échelle orders, optimal extraction of spectral orders, wavelength calibration, and a self-consistent continuum fit to the full two-dimensional (2D) image of extracted orders.</p> <p><strong>Files in this dataset</strong></p> <p>salt1.txt: TIC 44984200 (2MASS J08380224-5855583)<br> salt2.txt: TIC 277539431 (2MASS J10551532-7356091)<br> salt3.txt: TIC 300741820 (2MASS J07404497-6648318)</p> <p><strong>Columns in each file from left to right:</strong></p> <p>1 Wavelength in Angstrom<br> 2 Normalized flux<br> 3 Uncertainty on normalized flux</p> <p><strong>Corresponding author</strong></p> <p>Ekaterina Ilin, eilin@aip.de, Leibniz Institute for Astrophysics Potsdam (AIP)</p>
Exploring the age dependent properties of M and L dwarfs using Gaia and SDSS: The Sample
<p>Sample from "Exploring the age dependent properties of M and L dwarfs using Gaia and SDSS". We present a sample of 74,216 M and L dwarfs constructed from two existing catalogs of cool dwarfs spectroscopically identified in the Sloan Digital Sky Survey (SDSS). We cross-matched the SDSS catalog with Gaia DR2 to obtain parallaxes and proper motions and modified the quality cuts suggested by the Gaia Collaboration to make them suitable for late-M and L dwarfs. </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>
Light Curve and Target Data for "M-Dwarf Flare Candidates Simultaneously Observed by K2 and TESS"
<p>This repository contains light curves and data from the study conducted in the research note titled "M-Dwarf Flare Candidates Simultaneously Observed by K2 and TESS".</p> <p>Each file contains a light curve (produced outputs from PyVAN (<a href="https://ui.adsabs.harvard.edu/abs/2019AJ....158..119L/abstract" rel="nofollow">https://ui.adsabs.harvard.edu/abs/2019AJ....158..119L/abstract</a>, <a href="https://github.com/kdlawson/pyvan">https://github.com/kdlawson/pyvan</a>), modfied to easily distinguish between K2/TESS data) for each target flagged with a flaring event. Files titled #T indicate TESS data and #K indicates K2 data. </p> <p>Overlap plots are included (titled Shape#) for those which were clearly defined by TESS, but not seen by K2.</p> <p>See Table 1 for specific target identification and measurements.</p> <p>Targets 11, 20, 27, and 28 saw K2 detections that we believe to be false positives based on lack of structure and substanstial supporting evidence from TESS.</p> <p>Finally a .csv is included with the information for all targets observed in this study.</p>
Data associated with "The Role of Magma Oceans in Maintaining Surface Water on Rocky Planets Orbiting M-Dwarfs"
<p>The data included here involves all simulations outlined in the manuscript "The Role of Magma Oceans in Maintaining Surface Water on Rocky Planets Orbiting M-Dwarfs", submitted to MNRAS. Files are divided between models with and without a basal magma ocean, as well as different host stars, different magma ocean saturation limits, and different fringe/sensitivity analysis checks. Files are further sub-divided based on our studied parameter space: each is for a single orbital distance within the habitable zone, and a single initial water inventory. "MO_only" files correspond to the concurrent surface magma ocean/runaway greenhouse phase, while "combined_MO_cycling" files correspond to the deep-water cycling period.</p>
Starspot mapping with adaptive parallel tempering. II. Application to TESS data for M-dwarf flare stars, AU Microscopii, YZ Canis Minoris, and EV Lacertae (Flare Tables)
<p>For TESS PDC-SAP data of AU Mic (Sector 1 and 27), YZ CMi (Sector 7 and 34), and EV Lac (Sector 16), detected flare properties are listed: the peak time (BJD-2745000), amplitude, equivalent duration (sec), and e-folding time (day).</p>
Faint calcium-rich transient from a double-detonation of a 0.6 M⊙ carbon-oxygen white dwarf star: Complimentary material
<p>Complimentary material to the manuscript.<br> The videos show the hydrodynamical evolution of the merger leading to the double-detonation.</p> <p>The movie "overdensity_formation.mp4" shows slices through the orbital plane color coded with the density (left) and the temperature (right), displaying frame by frame the formation of a cold, overdense fluid parcel after the disruption of the HeWD. <br> <br> The remaining movies show the overall evolution of different quantities with slices through the orbital plane on the left and perpendicular to the orbital plane on the right.</p>
FUMES III: Ultraviolet and Optical Variability of M Dwarf Chromospheres
<p>We obtained ultraviolet and optical spectra for 9 M dwarfs across a range of rotation periods to determine whether they showed stochastic intrinsic variability distinguishable from flares. The ultraviolet spectra were observed during the Far Ultraviolet M Dwarf Evolution Survey <em>Hubble Space Telescope</em> program using the Space Telescope Imaging Spectrograph. The optical observations were taken from the Apache Point Observatory 3.5-meter telescope using the Dual Imaging Spectrograph and from the Gemini South Observatory using the Gemini Multi-Object Spectrograph. We used the optical spectra to measure multiple chromospheric lines: the Balmer series from H$\alpha$ to H$10$ and the Ca II H and K lines. We find that after excising flares, these lines vary on the order of $1-20\%$ at minute-cadence over the course of an hour. The absolute amplitude of variability was greater for the faster rotating M dwarfs in our sample. Among the 5 stars for which measured the weaker Balmer lines, we note a tentative trend that the fractional amplitude of the variability increases for higher order Balmer lines. We measured the integrated flux of multiple ultraviolet emission features formed in the transition region: the N V, Si IV, and C IV resonance line doublets, and the C II and He II multiplets. The signal-to-noise (S/N) ratio of the UV data was too low for us to detect non-flare variability at the same scale and time cadence as the optical. We consider multiple mechanisms for the observed stochastic variability and propose both observational and theoretical avenues of investigation to determine the physical causes of intrinsic variability in the chromospheres of M dwarfs.</p> <p>All code associated with the analysis and plots for this paper are included in .py scripts. All raw data for the optical spectra are its files compressed into a tar.gzip archive while all reduced spectra are in fits files. All tables are provided in the astropy ASCII text ecsv file format.</p> <ul> <li><strong>Optical Reduction Code</strong>: The reduction code is divided into two folders, one labelled "pydis" and another labelled "pygemini".</li> <li><strong>Equivalent Width Measurements:</strong> The equivalent widths are measured using a combination of two tables for each exposure: one ending with the suffix "ew_windows.ecsv" that lists the boundaries of the blue and red continua windows and the continuum flux density value, and another ending with the suffix "ew_lines.ecsv" that lists the boundaries of the wavelength window, the integrated line flux with its error, and the equivalent width with its error. These tables are in a subdirectory named "fit_tables".</li> <li><strong>spectralPhoton:</strong> The version of spectralPhoton code and the scripts we use to split the <em>Hubble</em> x1d spectra are in a directory named "uv".</li> <li><strong>Line-fitting Tables:</strong> The parameter values and associated errors are recorded in tables structured similarly to the equivalent width tables, ending with suffixes "windows.ecsv" and "lines.ecsv".</li> <li><strong>Time Series Tables:</strong> The equivalent widths and integrated line fluxes are collated into time series tables in the subdirectory "time_series". Entries with cosmic ray hits in the middle of the line or other spectral defects have been commented out using a # symbol.</li> <li><strong>Posterior Distributions:</strong> All posterior samples and their log-likelihood values are recorded in numpy binary .npy files that can be read using the numpy.load() function. These files are divided into two subdirectories named ``abs" and ``frac" for the absolute and fractional flux fits respectively.</li> </ul>
THE FLARING ACTIVITY OF M DWARFS IN KEPLER FIELD
<p>The Kepler flux, M dwarfs that include flares,the format consist of four columns:<br> <br> BKJD Relative Flux Fit line Flare Flux</p> <p>the Relative flux wil be empty when flares occur, the flares flux will be empty when quiescent flux.</p> <p>the file lamost_obsid is the spectra used in this work, one can use the obsid to download the fits through the following website: http://dr4.lamost.org/</p>
The SPHINX M-dwarf Spectral Grid. I. Benchmarking New Model Atmospheres to Derive Fundamental M-Dwarf Properties
<p><strong>NEW UPDATE:::::::::::::VERSION 4</strong></p> <p>MODEL GRID AND SUPPLEMENTARY FIGURES for <strong>The SPHINX M-dwarf Spectral Grid. I. Benchmarking New Model Atmospheres to Derive Fundamental M-Dwarf Properties:</strong></p> <p><strong>(1) MODEL GRID:</strong> Zip file titled 'SPHINX_MODELS_MLT_1.zip' contains a directory (376MB on disk) that is divided into three folders: ATMS, SPECTRA, and ABUNDANCES. All models here assume mixing length parameter of 1. For more info, we direct the reader to the paper.</p> <p>The ATMS directory contains thermal profiles/atmospheres of all models. (Temperature in K, Pressure in bars)</p> <p>The SPECTRA directory contains synthetic spectra. (Wavelength--0.1 to 20 microns, Flux in W/m2/m, R~250)</p> <p>The ABUNDANCES directory contains mixing ratios of all atomic and molecular species included in these models.</p> <p><strong>(2) SUPPLEMENTARY FIGURES:</strong></p> <p>The plot files are named as 'target name' _ corner.</p> <p>Each file is a corner plot of posterior probability distributions from grid-model fit of low-resolution spectra of benchmark M dwarfs using the SPHINX model grid. We also include posterior distributions of Starfish (Czekala et al.2015) hyperparameters to properly constrain model and data systematics. The vertical blue lines in the plots indicate values from observations (empirically derived [M/H] from Mann et al. 2013 and interferometrically measured radii from Boyajian et al. 2012b).</p> <p>File named Gl436_mixinglength shows difference in grid model fit assuming mixing length parameter 1 vs 0.5.</p> <p>File named Gl725B_spot shows difference in grid model fit assuming stellar photospheric heterogeneity vs without.</p> <p><strong>If you use our stellar atmosphere models, please remember to cite both the zenodo doi for the open source data as well as the paper. Thank you!</strong></p> <p> </p> <p>--> link to <a href="https://iopscience.iop.org/article/10.3847/1538-4357/acabc2/meta">published paper</a></p>
GCM simulations of Earth-like M- and K-dwarf planets
<p>Simulations are described in papers:</p> <ul> <li> <div>Lobo, A. H., Shields, A. L., Palubski, I. Z., & Wolf, E. (2023). <strong>Terminator Habitability: The Case for Limited Water Availability on M-dwarf Planets</strong>. <em>The Astrophysical Journal</em>, <em>945</em>(2), 161. https://doi.org/10.3847/1538-4357/aca970</div> </li> <li>Lobo, A. H., Shields, A. L., (in press, 2024). <strong>Climate Regimes Across the Habitable Zone: a Comparison of Synchronous Rocky M- and K-dwarf Planets</strong>. <em>The Astrophysical Journal. </em></li> </ul> <p> </p>
Stellar Parameter Estimation for Half a Million M Dwarfs based on Cycle-StarNet
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Inlist Files for Effects of Full Sphere Convection On M-Dwarf Dynamo Action, Flux Emergence, and Spin-Down
<p>Inlist files for a model of a ZAMS 0.3 M_sun star used as background for global convection simulations in <em>Effects of Full Sphere Convection On M-Dwarf Dynamo Action, Flux Emergence, and Spin-Down</em>. Run using MESA version r12115.</p>
M Dwarf Flare Continuum Variations on One-Second Timescales: Calibrating and Modeling of ULTRACAM Flare Color Indices
<p>These files contain the ULTRACAM light curves, the ULTRACAM flare color indices, the APO/DIS spectral data, and the NMSU 1-m U-band photometry from "M Dwarf Flare Continuum Variations on One-Second Timescales: Calibrating and Modeling of ULTRACAM Flare Color Indices", Kowalski, A. F., Mathioudakis, M., Hawley, S. L., Wisniewski, J. P., Dhillon, V. S., Marsh, T. R., Hilton, E. J., & Brown, B. P., 2016, Astrophysical Journal in press. See the included ReadMe file for detailed information on the files.</p>
Table A.11: M dwarfs + Planets
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Table A.10: M dwarfs + Ultracool dwarfs
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Table A.9: M dwarfs + White dwarfs
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Table A.8: M dwarfs + FGK stars
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Stellar Parameter Estimation for Half a Million LAMOST M Dwarfs based on Cycle-StarNet
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