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8 results for “ultracool dwarf”
The UltracoolSheet: Photometry, Astrometry, Spectroscopy, and Multiplicity for 4000+ Ultracool Dwarfs and Imaged Exoplanets
<p>The UltracoolSheet is a catalog of 4000+ ultracool dwarfs (spectral types M6 and later) and imaged exoplanets, including photometry, absolute astrometry, proper motions, parallaxes, multiplicity, spectroscopic classifications, memberships, and ages.</p> <p>The catalog lives in a Google spreadsheet at</p> <p> <a href="http://bit.ly/UltracoolSheet"><strong>http://bit.ly/UltracoolSheet</strong></a></p> <p>where it will receive future updates. The README tab in the spreadsheet contains a detailed description of the contents of the catalog.</p> <p>UltracoolSheet started as a catalog of all spectroscopically confirmed objects of spectral type L0 or later in the extended solar neighborhood (out to ~100 pc) that were known as of April 15, 2015. It has subsequently been extended to include many late-M dwarfs and also augmented with more recent discoveries spanning all ultracool spectral types.</p> <p>The component spreadsheets of UltracoolSheet are posted here as CSV files, along with summary figures and (.dat) files containing ASCII tables to simplify figure plotting for users. The Summary Plots.pdf file shows the sky map, age distribution, publication dates, and proper motion since publication for all objects in UltracoolSheet, as well as the distribution of projected separations of companions.</p> <p>When using data from the UltracoolSheet, please cite the individual papers from which the data comes. Citations codes are included for all the data in the tables, and the References table translates the citation codes into ADS bibcodes, Papers citekeys, and publication titles.</p> <p>For research that benefits from this compilation, please cite this Zenodo post and include the following acknowledgment:</p> <p>"This work has benefited from The UltracoolSheet at <a href="http://bit.ly/UltracoolSheet">http://bit.ly/UltracoolSheet</a>, maintained by Will Best, Trent Dupuy, Michael Liu, Aniket Sanghi, Rob Siverd, and Zhoujian Zhang, and developed from compilations by <a href="http://adsabs.harvard.edu/abs/2012ApJS..201...19D">Dupuy & Liu (2012)</a>, <a href="http://adsabs.harvard.edu/abs/2013Sci...341.1492D">Dupuy & Kraus (2013)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2014ApJ...792..119D/abstract">Deacon et al. (2014)</a>, <a href="http://adsabs.harvard.edu/abs/2016ApJ...833...96L">Liu et al. (2016)</a>, <a href="http://adsabs.harvard.edu/abs/2018ApJS..234....1B">Best et al. (2018)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2021AJ....161...42B/abstract">Best et al. (2021)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2023ApJ...959...63S">Sanghi et al. (2023)</a>, and <a href="https://ui.adsabs.harvard.edu/abs/2023AJ....166..103S">Schneider et al. (2023)</a>."</p> <p>The UltracoolSheet itself can be cited by this Zenodo DOI: 10.5281/zenodo.4169084 </p> <p>Questions, comments, suggestions, or contributions?<br>Please send them to <a href="mailto:ultracool.sheet@gmail.com">ultracool.sheet@gmail.com</a> (especially contributions!)</p> <p> </p>
Synthetic JWST NIRCam, Euclid NISP, and Roman WFI Near-Infrared Photometry for 800+ Ultracool Dwarfs
<p>JWST NIRCam, Euclid NISP, and Roman WFI photometry (apparent magnitudes) for 800+ ultracool dwarfs synthesized using near-IR SpeX prism spectra. This is a supplementary data product to <a href="https://iopscience.iop.org/article/10.3847/2515-5172/acf864">Sanghi et al. 2023 (RNAAS, 7, 194)</a> and <a href="https://ui.adsabs.harvard.edu/abs/2024RNAAS...8..137S/abstract">Sanghi et al. 2024 (RNAAS, 8, 137)</a>. JWST photometry is presented in the Vega magnitude system and Euclid and Roman photometry are presented in the AB magnitude system.</p> <p>For research that benefits from this compilation, please cite <a href="https://iopscience.iop.org/article/10.3847/2515-5172/acf864">Sanghi et al. 2023 (RNAAS, 7, 194)</a> for JWST photometry, <a href="https://ui.adsabs.harvard.edu/abs/2024RNAAS...8..137S/abstract">Sanghi et al. 2024 (RNAAS, 8, 137)</a> for Euclid and Roman photometry, and include the following acknowledgment:</p> <p>"This work has benefitted from The UltracoolSheet, maintained by Will Best, Trent Dupuy, Michael Liu, Aniket Sanghi, Rob Siverd, and Zhoujian Zhang, and developed from compilations by <a href="https://ui.adsabs.harvard.edu/abs/2012ApJS..201...19D/abstract">Dupuy & Liu (2012, ApJS, 201, 19)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2013Sci...341.1492D/abstract">Dupuy & Kraus (2013, Science, 341, 1492)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2016ApJ...833...96L/abstract">Liu et al. (2016, ApJ, 833, 96)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2018ApJS..234....1B/abstract">Best et al. (2018, ApJS, 234, 1</a>), <a href="https://ui.adsabs.harvard.edu/abs/2021AJ....161...42B">Best et al. (2021, AJ, 161, 42)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2023ApJ...959...63S/abstract">Sanghi et al. (2023, ApJ, 959, 63)</a>, and <a href="https://ui.adsabs.harvard.edu/abs/2023AJ....166..103S/abstract">Schneider et al. (2023, AJ, 166, 103)</a>."</p> <p>Contact <a href="mailto:asanghi@caltech.edu">asanghi@caltech.edu</a> regarding questions.</p>
Detection of an Earth-sized exoplanet orbiting the nearby ultracool dwarf star SPECULOOS-3
<p>Light curves and spectra of SPECULOOS-3 used in the research work presented in the Nature Astronomy article "Detection of an Earth-sized exoplanet orbiting the nearby ultracool dwarf star SPECULOOS-3"</p>
The Ultracool Dwarf Companion catalouge
<p>This dataset contains the catalogue accompanying the paper "The Gaia Ultracool<br> Dwarf Sample -- V: The Ultracool Dwarf Companion catalogue" by Sayan Baig et al., accepted by MNRAS in July 2024.</p>
Table A.10: M dwarfs + Ultracool dwarfs
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Best-fit Abundances, Observed Spectra and Spectral Models for the New Sample of Ultracool Dwarf Benchmarks with Detailed Chemical Characterization
<p>Dataset associated with Fisher et al. 2024 in RNAAS <a href="https://iopscience.iop.org/article/10.3847/2515-5172/ad79f0">[link to publication]</a></p> <p><code>summary.mrt</code> is a table of identifiers, photometry, fundamental stellar parameters and detailed chemical compositions for 13 candidate wide binary systems with FGK Main Sequence primaries (5100 K < Teff < 6300 K) and ultracool dwarf companions (2500 K < Teff < 3100 K). Refer to the file header for detailed description of columns and units.</p> <p><code>stars.zip</code> contains the high-resolution spectra of primaries observed with the Automated Planet Finder (APF, program <code>2021B_A010</code>), as well as the corresponding best-fit spectral models. Each FITS file in the archive represents an individual exposure of the primary. The files are arranged in directories by identifiers of the primaries. The total number of exposures varies from source to source.</p> <p>FITS files are composed of a primary HDU and 6 extensions.</p> <ul> <li>The primary HDU contains the unmodified sky-subtracted spectrum of the object as produced by the APF pipeline and published on <a href="https://jump.caltech.edu/">Jump</a>. The spectrum is stored as a 2D array organized by Echelle orders.</li> <li>The first extension contains the corresponding air wavelengths [in A] transformed to the rest frame of the source.</li> <li>The second extension is the boolean mask of pixels included in model fitting.</li> <li>The third extension is the adopted statistical weights of each pixel, estimated as inverse variances under the assumption of Poisson noise.</li> <li>The fourth extension contains the best-fit synthetic spectrum in CGS units of surface intensity per wavelength in A.</li> <li>The fifth extension is the best-fit spline continuum correction between the model and the data.</li> <li>The final extension contains the adopted FWHM of the line spread function in each pixel, estimated by combining in quadrature a wavelength-dependent component with λ/Δλ=120,000 and a best-fit wavelength independent component (the <code>quickblur</code> parameter of the <a href="https://github.com/Roman-UCSD/chemfit">chemfit</a> package)</li> </ul> <p>This repository is for the research note "New Sample of Ultracool Dwarf Benchmarks with Detailed Chemical Characterization" by Fisher et al. It is associated with manuscript number AAS58102.</p>
A Venus in the Making? Predictions for JWST Observations of the Ultracool M-Dwarf Planet LP 890-9 c
<p>This repository contains the pressure-temperature profiles and volume mixing ratio profiles used in a paper accepted in MNRAS Letters under the same name.</p>
A Uniform Retrieval Analysis of Ultracool Dwarfs. III. Properties of Y Dwarfs
<p>Posterior distributions for all model runs of <em>A Uniform Retrieval Analysis of Ultracool Dwarfs. III. Properties of Y-Dwarfs.</em></p> <p>To view, simply download the file and extract the tarball.</p> <p>Directory structure is as follows:</p> <p><strong>/free_retrieval/</strong>: All posteriors here result from the model assumptions stated in Section 4.2.1 in the manuscript and were used for the analysis in Sections 4.3 as well.</p> <p><strong>/constrained_retrieval/</strong>: All posteriors here result from the model assumptions stated in Section 4.2.2 of the manuscript.</p> <p><strong>/additional_retrievals/2212-6931_kirkpatrick2012/</strong>: Shows the results for both the "free" and "constrained" model assumptions using a distance estimate from Kirkpatrick et al. (2012) as mentioned in Section 4.2.3 of the manuscript.</p> <p><strong>/grid_model_fits/:</strong></p> <p>Contains directories for each grid model ran against our targets. Targets are specified by the first 4 numbers (RA) of their WISE/ALLWISE name. The subname specifies the free parameters of the grid model were and are as follows:</p> <p>_solar: Only Teff, log(g), radius, and log(Luminosity) are free parameters.</p> <p>_met: Same as solar, but now the metallicity of the system is a free parameter.</p> <p>_kzz: Same as solar, but now the eddy diffusion coefficient Kzz is also a free parameter.</p> <p>_CO: Same as solar, but now the elemental Carbon/Oxygen ratio is a free parameter.</p> <p>_full: All of the above are free parameters.</p> <p> </p>
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