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59 results for “JWST”
JWST-TST DREAMS: Quartz Clouds in the Atmosphere of WASP-17b
<p>Data and models accompanying the publication "JWST-TST DREAMS: Quartz Clouds in the Atmosphere of WASP-17b". Here we include:</p> <ul> <li>Data, ExoTiC-MIRI reduction of JWST MIRI LRS transit observations</li> <li>Data, Eureka! reduction of JWST MIRI LRS transit observations</li> <li>Models, ATMO forward modelling.</li> <li>Models, PICASO+VIRGA forward modelling.</li> <li>Models, POSEIDON retrievals.</li> <li>Models, petitRADTRANS retrievals.</li> </ul> <p>Manuscript DOI: [10.3847/2041-8213/acfc3b] and [<a href="https://iopscience.iop.org/article/10.3847/2041-8213/acfc3b">Paper link</a>]</p>
Double Trouble (GJ 1132b JWST Transits NIRSpec G395H) — Supplementary Material
<p>Supplementary material for '<i>Double Trouble: Two Transits of the Super-Earth GJ 1132 b Observed with JWST NIRSpec G395H</i>' by May & MacDonald et al., ApJL (2023).</p><p>This repository contains four categories of data products:</p><ol><li><strong>Data reduction reproduction</strong> — Eureka! control files (.ecf) and parameter files (.epf) alongside saved Stage 3 output for both G395H visits. These allow replication of our data reduction, light curve fitting, and transmission spectra extraction using the <a href="https://github.com/kevin218/Eureka">open-source code Eureka</a>!</li><li><strong>Transmission spectra</strong> — Reduced transmission spectra from three data reduction codes (Eureka!, FIREFLy, and ExoTiC-JEDI) for both G395H visits.</li><li><strong>Stellar spectra </strong>— Flux calibrated observed stellar spectra of GJ 1132 from each G395H visit.</li><li><strong>Retrievals</strong> — Corner plots and parameter statistics summaries from atmospheric and stellar contamination retrievals applied to both G395H visits (Eureka! reduction). The retrievals used the <a href="https://github.com/MartianColonist/POSEIDON">open-source code POSEIDON</a>.</li></ol><p>For any additional data requests or questions, please contact: ryanjmac@umich.edu</p>
JWST-JupiterSPR-MIRI Rodriguez-Ovalle et al., 2024
Open the record for dataset details and reuse information.
The data for Reconstruction of Cosmic Black Hole Growth and Mass Distribution from Quasar Luminosity Functions at z>4: Implications for Faint and Low-mass Populations in JWST
<p>The data for Figure 1 in the AAS article: Reconstruction of Cosmic Black Hole Growth and Mass Distribution from Quasar Luminosity Functions at z>4: Implications for Faint and Low-mass Populations in JWST</p> <p>in each file, the column heads are x: M1450; y_f0: total Phi(Mpc^-3 mag^-1) for f_seed=1.0 y1_f0: unobscured Phi for f_seed=1.0 y_f1: total Phi for f_seed=0.1 y1_f1: unobscured Phi for f_seed=0.1</p>
Discovery of Carbon Dioxide and Hydrogen Peroxide on Charon's Stratified Surface with JWST
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JWST-JupiterSPR-MIRI benzene and Aerosol retrieval
<p>In this dataset you can find the benzene abundance for the three MIRI/JWST tiles, noted as obsX, where x is the number of the tile. In each directory, wou will find three folders noted as 'c6h6...' indicating the peak altitude for the c6h6 profile. In obs2 you will also find the results for the optical depth of the aerosols in the 'hazes...' directories.</p>
Model Spectra for Morley et al. 2017 (Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST)
<p>README</p> <p>This file contains the model spectra presented in Morley et al. 2017, Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST. </p> <p>The models are organized as follows: </p> <p>##########################<br> ## Transmission spectra ##<br> ##########################</p> <p>transmission_spectra contains 4 folders:<br> alb0.0_massradiusrel includes models with Bond albedo=0.0, and planet masses assuming the Weiss & Marcy 2014 mass-radius relationship<br> alb0.3_massradiusrel includes models with Bond albedo=0.3, and planet masses assuming the Weiss & Marcy 2014 mass-radius relationship<br> alb0.0_measured_masses includes models with Bond albedo=0.0, and observed planet masses, as described in Morley et al. 2017<br> alb0.3_measured_masses includes models with Bond albedo=0.3, and observed planet masses, as described in Morley et al. 2017</p> <p>each file contains the wavelength and model transit depth from 0.3 to 250 microns, calculated at 1 cm-1 wavenumber resolution. </p> <p>The file name indicates the planet name, model surface pressure (in bar), Bond albedo, and the assumed composition (Earth-, Venus-, or<br> Titan-based compositions, calculated in chemical equilibrium at each layer of the model, as described in Morley et al. 2017). </p> <p>(e.g. trans_spect_massradiusrel_gj1132b_psurf0.1_alb0.0_chem_earth.p.txt is a model of GJ 1132b, assuming the Weiss/Marcy mass-radius relationship, with a surface pressure of 0.1 bar, Bond albedo of 0.0, and an Earth-based composition). </p> <p>##########################<br> ## Emission spectra ##<br> ##########################</p> <p>emission_spectra contains 4 folders:<br> alb0.0 includes models with Bond albedo=0.0<br> alb0.3 includes models with Bond albedo=0.3<br> alb0.7 includes models with Bond albedo=0.7<br> emission_spectra_dividestar includes models that have already been divided by a model stellar spectrum, for convenience. </p> <p><br> each file contains the wavelength and model thermal emission flux in W/m2/m from 0.3 to 250 microns, calculated at 1 cm-1 wavenumber resolution. </p> <p>The file name indicates the planet name, model surface pressure (in bar), Bond albedo, and the assumed composition (Earth-, Venus-, or<br> Titan-based compositions, calculated in chemical equilibrium at each layer of the model, as described in Morley et al. 2017). </p> <p>(e.g. gj1132b_psurf0.01_alb0.0_chem_earth.spec is a model of GJ 1132b with a surface pressure of 0.01 bar, Bond albedo of 0.0, and an Earth-based composition). </p> <p>The models in emission_spectra_dividestar instead contain the flux of the planet divided by the flux of the star. </p> <p> </p> <p>##########################<br> ## Eclipse Depths ##<br> ##########################</p> <p>eclipse_depths contains a file for each planet with calculated eclipse depths for each of the wide-band JWST MIRI filters (http://ircamera.as.arizona.edu/MIRI/pces.htm). </p> <p>(new version from Jan 29 2018 has fixed a bug in MIRI eclipse depths that affected the longest wavelength filter for GJ 1132b and LHS 1140b only). </p>
Statistical trends in JWST transiting exoplanet atmospheres
<p>Spectra shown in Figure 1</p> <p>Columns are: Wavelength(micron), Wavelength err(micron), Transit Depth, Transit Depth err</p>
Sonora Cholla: A Grid of Cloud-free, Solar Metallicity Models in Chemical Disequilibrium for the JWST Era
<p>Exoplanet and brown dwarf atmospheres commonly show signs of disequilibrium chemistry. In the James Webb Space Telescope era high resolution spectra of directly imaged exoplanets will allow the characterization of their atmospheres in more detail, and allow systematic tests for the presence of chemical species that deviate from thermochemical equilibrium in these atmospheres. Constraining the presence of disequilibrium chemistry in these atmospheres as a function of parameters such as their effective temperature and surface gravity will allow us to place better constrains in the physics governing these atmospheres.</p> <p>This database contains a grid of cloud-free, solar metallicity atmospheres for brown dwarfs and wide separation giant planets with key molecular species such as CH<sub>4</sub>, H<sub>2</sub>O, CO and NH<sub>3</sub> in disequilibrium. The grid covers atmospheres with T<sub>eff</sub>~[500 K,1300 K], log<em>g</em>~[3.0,5.5] (cgs) and an eddy diffusion parameter of log K<sub>zz</sub>=2, 4 and 7 (cgs). A description of the code and a study of the effect of different parameters within the grid on the temperature and composition profiles of our atmospheres is presented in the accompanying paper "The Sonora Substellar Atmosphere Models. II. Cholla: A Grid of Cloud-free, Solar Metallicity Models in Chemical Disequilibrium for the<em> JWST </em>Era" (accepted to ApJ, Oct. 2021)</p>
"An atlas of color-selected quiescent galaxies at z>3 in public JWST fields" (Supplementary material)
<p>The files are organized as follows:</p> <p>0) "<em>readme_atlas_jwst_paper.txt"</em><br> This file describes the content of the file "<em>supplementary_atlas_jwst_paper.tar</em>" containing supplementary figures and tables for the manuscript <em>"An atlas of color-selected quiescent galaxies at z>3 in public JWST fields" </em>by Valentino, Brammer, Gould et al. (2023, ApJ).<br> The information is also provided here below.</p> <p>1) supplementary_figures/</p> <p>1.1) Depth in NIRCam/F150W, F200W, F277W, and F356W equivalent to Figure A.1 in Appendix A:</p> <ul> <li>f150w_flux_aper_1_observed_magnitude_sn_5.0_completeness_kde_allfields.png</li> <li>f200w_flux_aper_1_observed_magnitude_sn_5.0_completeness_kde_allfields.png</li> <li>f277w_flux_aper_1_observed_magnitude_sn_5.0_completeness_kde_allfields.png</li> <li>f356w_flux_aper_1_observed_magnitude_sn_5.0_completeness_kde_allfields.png</li> </ul> <p>These figures are also collected in a Figure Set available on the journal webpage.</p> <p>1.2) Comoving number densities of <em>UVJ</em>-selected galaxies falling in the standard selection box by Williams+2009 and not accounting for the uncertainties on colors:</p> <ul> <li>uvj_number_densities_mass_bins_strict_nouncertainties.png</li> </ul> <p>The purple and green colors mark the <em>p(z)</em> of individual robust "standard" <em>UVJ</em> quiescent candidates with M* ≥ 10<sup>10.6</sup> M<sub>⊙</sub> and 10<sup>9.5</sup> ≤ M* < 10<sup>10.6</sup> M<sub>⊙</sub>, respectively. The <em>p(z) </em>are normalized by their area (∫<sub>z</sub> <em>p(z)</em> d<em>z</em> = 1). The sky coverage of each field is as labeled. We included the effect of gravitational lensing at these redshifts in the calculation of the areas around galaxy clusters (Sunrise, SMACS0723), for which the masses should be intended as observed (not delensed). The comoving number densities in units of 10<sup>-5</sup> Mpc<sup>-3</sup> obtained from the integration of <em>p(z)</em> within the 3 < <em>z</em> < 4, 4 < <em>z</em> < 5, and 5 < <em>z</em> < 6.5 bins marked by dotted lines are reported. The errors mark the 68% Poissonian confidence intervals. Estimates of the uncertainties from bootstrapping are within brackets. The first and second rows indicate <em>n</em> in the 10<sup>9.5</sup> ≤ M* < 10<sup>10.6 </sup>M<sub>⊙</sub> and M* ≥ 10<sup>10.6</sup> M⊙ bins, respectively.</p> <p>2) uvj/</p> <p>Folder containing the SEDs (seds/) and positions in the <em>UVJ</em> diagram (uvj_single/) of the UVJ-selected samples described in the manuscript. The latter include both the initial pool of candidates and the visually selected sample.</p> <p>Tables containing the basic properties of both samples described in the text are available in fits and html formats.</p> <p>By downloading the folder and clicking on the .html tables, the reader can visualize the content in a web browser. This feature allows to automatically visualize the properties, SEDs, position in the <em>UVJ</em> diagram, and generate RGB cutouts in the SW and LW NIRCam channels on-the-fly. The latter operation takes a few seconds.</p> <p>A .reg file compatible with DS9 is provided for the visually selected sample. The coordinates are aligned with GAIA DR3.</p> <p>3) nuvuvj/</p> <p>The content is similar to that of the uvj/ folder, but for the <em>NUVUVJ</em> selection in Gould, Brammer, Valentino et al. (2023, ApJ). Separate tables for "robust" and "probable" samples before and after the visual inspections are distributed in .fits and .html format.</p> <p>4) carnall22_selection/</p> <p>The content is similar to that of the nuvuvj/ folder, but for the sample selected by Carnall, McLeod, McLure et al. 2023 (2023MNRAS.tmp..383C, arXiv:2208.00986). The information is provided to allow for a rapid comparison with this work.</p> <p><br> For further information or details, please write at: francesco.valentino@eso.org.</p>
JWST imaging and spectroscopy of a z=9.51 galaxy
<p>HST and JWST Imaging and JWST spectroscopy of a z=9.51 galaxy. </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>
Nebular spectra from Type Ia supernova explosion models compared to JWST observations of SN 2021aefx
<p>Hydrodynamical models and synthetic spectra from Blondin et al. (2023).</p>
PEARLS: Near Infrared Photometry in the JWST North Ecliptic Pole Time Domain Field
<p>We make public visible and near-infrared images and derived catalogues obtained as part of the ground-based observations targetting the North Ecliptic Pole Time Domain Field. This is one of the prime targets of the PEARLS collaboration (Windhorst+ 2023, AJ 165, 13 (https://doi.org/10.3847/1538-3881/aca163), and was designed to identify transient objects (outer Solar System objects, variable stars, Active Galactic Nuclei, Supernovae). These data complement the already extensive coverage this field has had from space and ground-based observatories ranging from hard X-rays to radio.</p>
Products and Models for "A JWST transmission spectrum of the nearby Earth-sized exoplanet LHS 475 b"
<p>OVERVIEW: The critical first step in the search for life on exoplanets over the next decade is to determine whether rocky planets transiting small M-dwarf stars possess atmospheres and, if so, what processes sculpt them over time. Because of its broad wavelength coverage and improved resolution compared to previous instruments, spectroscopy with JWST offers a new capability to detect and characterize the atmospheres of Earth-sized, M-dwarf planets. Here we use JWST to independently validate the discovery of LHS 475 b, a warm (586 K), 0.99 Earth-radius exoplanet, interior to the habitable zone, and report a precise 2.9 − 5.3 μm transmission spectrum using the NIRSpec G395H instrument. With two transit observations, we rule out primordial hydrogen-dominated and cloudless pure methane atmospheres. Thus far, the featureless transmission spectrum remains consistent with a planet that has a high-altitude cloud deck (similar to Venus), a tenuous atmosphere (similar to Mars), or no appreciable atmosphere at all (akin to Mercury). There are no signs of stellar contamination due to spots or faculae. Our observations demonstrate that JWST has the requisite sensitivity to constrain the secondary atmospheres of terrestrial exoplanets with absorption features < 50 ppm, and that our current atmospheric constraints speak to the nature of the planet itself, rather than instrumental limits.</p>
JWST NIRSpec spectrum of the d203-506 protoplanetary disk
<p>This zip file contains the NIRSpec spectrum of d203-506 from Berné O. et al. Science 2024. First column is wavelength, second column is intensity in MJy/sr, third column is the uncertainty (MJy/sr). File with ON extension is the on source spectrum. OFF extension is the OFF source spectrum. ON_OFF extension is the difference between the two. See Berné et al. for details on the extraction region and coordinates. </p>
JWST ERS Ice Age NIRCam WFSS initial team release, Version 1
<p>Initial repository for the full set of "working" version Ice Age NIRCam data, as of December 2023.</p> <p>This repository contains the best representative subset of the spectra from the WFSS extraction, that will be published in Noble et al. (2024, in prep.) and Smith et al. (2024, in prep.). See the included README file for more details.</p> <p>At this stage, the NIRCam WFSS spectra extracted using the Ice Age pipeline are a proprietary science product and will be publically embargoed until the publication of the final NIRCam team paper in the Nature Astronomy series that we are working on this year. Usage of these NIRCam science products for a project or proposal prior to the public data release requires registering that project or proposal with the Ice Age management team so that they can coordinate between projects/proposals, and an opt-out option for key members of the NIRCam science team. A Zenodo account is necessary to access these data. These data are only available at present to Ice Age team members.</p> <p>A request to access these data implies acknowledgement and acceptance of these access conditions.</p> <p> </p> <p> </p>
A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree The Atmosphere of WASP-77A b is Metal-Poor
<p>Supplementary material for <em>A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree The Atmosphere of WASP-77A b is Metal-Poor</em>, accepted for publication in the Astronomical Journal 2023.</p>
JWST ERS Ice Age working version internal repository
<p>Test version of the eventual repository for the full set of "working" version of the Ice Age data, as of December 2023.</p>
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