Find research datasets worth reusing
Search datasets from major research repositories and use ShareScore to quickly assess how well each record supports discovery, access, and reuse.
59
datasets available to search
ShareScore release 0.9.0
Dataset results
59 results for “JWST”
JWST reveals a rapid and strong day side variability of 55 Cancri e
<p>The plots are posterior distributions from atmospheric retrieval performed by <a href="https://arxiv.org/abs/2407.12898" target="_blank" rel="noopener">Patel et al. (2024)</a>. See, their Appendix C for more details. Image captions are as follows:</p> <p><em>post_co_v1_red2.png:</em> Posterior distributions of the free parameters for the first visit, representing the CO/CO2-atmosphere scenario. Results are shown for the <code>HANSOLO</code> reduction. The corresponding distributions for the <code>stark</code> reduction are depicted in Fig. 4 of Patel et al. (2024). We note that ξ_CO2 is not a free parameter in the retrieval but was calculated during a postprocess procedure following the requirement that in each posterior sample the sum of all ξ values must be zero.</p> <p><em>post_co_v2_red1.png</em> and <em>post_co_v2_red2.png</em>: Posterior distributions of the free parameters for Visit 2, representing the CO/CO2-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p> <p><em>post_co_v3_red1.png</em> and <em>post_co_v3_red2.png</em>: Posterior distributions of the free parameters for Visit 3, representing the CO/CO2-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p> <p><em>post_co_v4_red1.png</em> and <em>post_co_v4_red2.png</em>: Posterior distributions of the free parameters for Visit 4, representing the CO/CO2-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p> <p><em>post_co_v5_red1.png</em> and <em>post_co_v5_red2.png</em>: Posterior distributions of the free parameters for Visit 5, representing the CO/CO2-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p> <p><em>post_sio_v1_red1.png</em> and <em>post_sio_v1_red2.png</em>: Posterior distributions of the free parameters for Visit 1, representing the SiO/SiO2/MgO-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p> <p><em>post_sio_v2_red1.png</em> and <em>post_sio_v2_red2.png</em>: Posterior distributions of the free parameters for Visit 2, representing the SiO/SiO2/MgO-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p> <p><em>post_sio_v3_red2.png</em>: Posterior distributions of the free parameters for Visit 3, representing the SiO/SiO2/MgO-atmosphere scenario. Results are shown for the <code>HANSOLO</code> reduction. The corresponding distributions for the <code>stark</code> reduction are depicted in Fig. 5 of Patel et al. (2024).</p> <p><em>post_sio_v4_red1.png</em> and <em>post_sio_v4_red2.png</em>: Posterior distributions of the free parameters for Visit 4, representing the SiO/SiO2/MgO-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p> <p><em>post_sio_v5_red1.png</em> and <em>post_sio_v5_red2.png</em>: Posterior distributions of the free parameters for Visit 5, representing the SiO/SiO2/MgO-atmosphere scenario. Results are shown for the <code>stark</code> (red1) and <code>HANSOLO</code> (red2) reductions.</p>
JWST-TST DREAMS: Non-Uniform Dayside Emission for WASP-17b from MIRI/LRS
<p>Data and models accompanying the publication "JWST-TST DREAMS: Non-Uniform Dayside Emission for WASP-17b from MIRI/LRS". Here we include:</p> <ul> <li>ExoTiC-MIRI reductions of JWST MIRI LRS eclipse observations</li> <li>Eureka! reductions of JWST MIRI LRS eclipse observations</li> <li>PICASO forward atmospheric models </li> <li>ThERESA eclipse mapping outputs</li> <li>PHOENIX stellar model for WASP-17A</li> </ul> <p>Manuscript DOI: [10.3847/1538-3881/ad5c61] and [<a href="https://iopscience.iop.org/article/10.3847/1538-3881/ad5c61">Paper Link</a>]</p>
Data for: Tip of the Red Giant Branch Distances with JWST. II. I−band Measurements in a Sample of Hosts of 10 SN Ia Match HST Cepheids
<p>Data for: "Tip of the Red Giant Branch Distances with JWST. II. I−band Measurements in a Sample of Hosts of 10 SN Ia Match HST Cepheids". The photometry provided is after DOLPHOT quality cuts, foreground extinction corrections, and spatial cuts.</p>
Products and Models for "Early Release Science of the Exoplanet WASP-39b with JWST NIRSpec G395H"
<p>Associated Publication: <a href="https://www.nature.com/articles/s41586-022-05591-3">https://www.nature.com/articles/s41586-022-05591-3</a></p> <p>Overview:<br> Measuring the abundances of carbon and oxygen in exoplanet atmospheres is considered a crucial avenue for unlocking the formation and evolution of exoplanetary systems. Access to an exoplanet’s chemical inventory requires high-precision observations, often inferred from individual molecular detections with low-resolution space-based and high-resolution ground-based facilities. Here we report the medium-resolution (R≈600) transmission spectrum of an exoplanet atmosphere between 3–5 𝛍m covering multiple absorption features for the Saturn-mass exoplanet WASP-39b, obtained with JWST NIRSpec G395H. Our observations achieve 1.46x photon precision, providing an average transit depth uncertainty of 221 ppm per spectroscopic bin, and present minimal impacts from systematic effects. We detect significant absorption from CO<sub>2</sub> (28.5<span class="math-tex">\(\sigma\)</span>) and H<sub>2</sub>O (21.5<span class="math-tex">\(\sigma\)</span>), and identify SO<sub>2</sub> as the source of absorption at 4.1 𝛍m (4.8<span class="math-tex">\(\sigma\)</span>). Best-fit atmospheric models range between 3 and 10x solar metallicity, with sub-solar to solar C/O ratios. These results, including the detection of SO<sub>2</sub>, underscore the importance of characterising the chemistry in exoplanet atmospheres, and showcase NIRSpec G395H as an excellent mode for time series observations over this critical wavelength range.<strong> </strong></p> <p> </p> <p> </p>
JWST Advanced Deep Extragalactic Survey: Thumbnail Images of Spectroscopically-Confirmed Galaxies at z>10.
<p>JWST NIRCam FITS image thumbnails for the spectroscopically-confirmed high-redshift galaxy sample in Robertson et al., arXiv:2212.04480. The tar file expands into the following directories:</p> <p>JADES-GS-z10-0/</p> <p>JADES-GS-z11-0/</p> <p>JADES-GS-z12-0/</p> <p>JADES-GS-z13-0/</p> <p>Each directory contains the F090W, F115W, F150W, F200W, F277W, F335M, F356W, F410M, and F444W FITS images of the galaxies. The FITS headers contain information about the observations, the units of the data, and the locations of the objects on the sky.</p>
JWST NIRSpec/MSA PSF libraries
<p>This dataset contains libraries of model PSFs for the JWST/NIRSpec MSA, as described in de Graaff et al. 2023 (https://arxiv.org/abs/2308.09742).<br> We provide one library for each NIRSpec disperser, for a single-shutter and triple shutter configuration (1x1 and 1x3, respectively). The PSFs were computed at the centre of MSA quadrant 3 (shutter (185,83)). The libraries contain PSF images at a range of different wavelengths and intrashutter positions.<br> Libraries can be used in combination with the software msafit, in particular the PFSLib class. The software is available publicly on github: https://github.com/annadeg/jwst-msafit</p>
JWST NIRSpec/MSA trace libraries and detector models
<p>Reference data needed for forward modelling of NIRSpec MSA data, as described in de Graaff et al. 2023 (https://arxiv.org/abs/2308.09742).<br> <br> This dataset contains a library of traces for each NIRSpec filter/disperser combination, providing a mapping from a microshutter s_{i,j} and wavelength to the position in the detector plane, and includes the rotation angle of the slitlet with respect to the trace in the detector plane.<br> Other files provide information on the detector, such as the pixel size and the kernels used to model the inter-pixel capacitance.</p> <p>These data are designed to be used together with the NIRSpec MSA forward modelling code msafit, which is available publicly on github: https://github.com/annadeg/jwst-msafit</p>
High Tide or Rip-Tide? GJ 486b JWST Transits with NIRSpec G395H - Supplementary Material
<p>Supplementary material for '<em>High Tide or Riptide on the Cosmic Shoreline? A Water-rich Atmosphere or Stellar Contamination for the Warm Super-Earth GJ 486b from JWST Observations</em>' by Moran & Stevenson et al., ApJL (2023).</p> <p>This repository contains four categories of data products:</p> <ol> <li><strong>White light curves</strong> — White light curves produced for Visit 1 and 2, for detectors NRS1 and NRS2 via the <a href="https://ui.adsabs.harvard.edu/abs/2023Natur.614..659R/abstract">FIREFLy pipeline</a> and the <a href="https://github.com/kevin218/Eureka">open-source codes Eureka</a>! and <a href="https://github.com/JamesKirk11/Tiberius">Tiberius</a></li> <li><strong>Transmission spectra</strong> — Reduced transmission spectra from three data reduction codes (Eureka!, FIREFLy, and Tiberius) for both G395H visits.</li> <li><strong>Stellar spectra and models </strong>— Flux calibrated observed stellar spectra of GJ 486 from each G395H visit, along with best-fit PHOENIX stellar models.</li> <li><strong>Atmospheric models</strong> — Atmospheric forward models used to interpret the data, produced from the open source <a href="https://natashabatalha.github.io/picaso/">PICASO</a> and <a href="https://github.com/mrline/CHIMERA">CHIMERA</a> codes.</li> </ol> <p>For any additional data requests or questions, please contact: sarahemoran@arizona.edu or kevin.stevenson@jhuapl.edu</p> <p> </p>
Data for: JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-836b
<p>Data and models accompanying the publication "JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-836b". Here we include:</p> <ul> <li>Data, ExoTiC-JEDI light curves and transmission spectrum of JWST NIRSpec/G395H transit observations</li> <li>Data, Eureka! light curves and transmission spectrum of JWST NIRSpec/G395H transit observations</li> <li>Models, PICASO models and data shown in Figure 5</li> </ul> <p>Manuscript DOI: [] and [paper link]</p>
JWST MIRI MRS spectrum of IC 348
<p>This spectrum was extracted from the IFU cube (which was downloaded via the MAST platform, from the GTO program ID 1236 (PI Michael Ressler) ) using a circular aperture of radius 1.15”, centered on coordinates (3:43:56.980,+32:03:03.98).</p> <p>First column correcponds to wavelength in microns, the second column to flux in MJy/sr.</p> <p>All JWST MIRI MRS channels are included in one single spectrum.</p> <p> </p>
Data for Estimate of water and hydroxyl abundance on asteroid (16) Psyche from JWST data
<p>The data as ASCII files used to produce the figures in the manuscript, " Estimate of water and hydroxyl abundance on asteroid (16) Psyche from JWST data". Almost all the files are ECSV files created from astropy Table. These files have complete metadata headers. Otherwise, the data, where appropriate, include s3d fits IFU data cubes used to produce 1D spectra, the solar spectra output by the Planetary Spectrum Generator, a thermophysical model output, asteroid reflectance measurements, and chondrite reflectance measurements all of which are described in further detail below. </p> <p>The Figures folder contains data behind the figures where data were used.</p> <p>For Figure 2 this corresponds to the NIRSpec and MIRI flux observations with a column for wavelength (in microns), flux (in Jansky), and error (in Jansky). </p> <p>For Figure 3 this corresponds to the normalized reflectance for the NIRSpec observations. The first column in each dataset corresponds to the wavelength in microns, the second column to the normalized reflectance (unitless), the third column to the error (unitless), and in the case of the .txt files the fourth column corresponds to the gaussian fit to the normalized reflectance. </p> <p>For Figure 4 these are the normalized reflectance divided by the continuum of the groups of data along wavelength ranges described in the manuscript for Figure 4. The first column corresponds to the wavelength in microns, the second column to the reflectance, the third column to the continuum fit to the data, the fourth column is the normalized reflectance divided by the continuum, and the error. </p> <p>For Figure 5 these are the data used to produce the 3-micron feature plot with the gaussian fit for each NIRSpec observation. The first column corresponds to the wavelength in microns, second column to the normalized reflectance divided by the continuum (unitless) and subtracted from the mean of the continuum between 3.6 and 3.7 microns such that the average of the continuum would be 0, the fourth column the error (unitless), and the fifth column the gaussian fit to the data. </p> <p>For Figure 6 the only additional data needed to produce this plot beyond what is provided for Figure 5 is the IRTF data which is provided as a text file. The first column corresponds to the wavelength in microns, the second column to the normalized reflectance divided by the continuum (unitless), and the third column to the error (unitless). </p> <p>For Figure 7 the additional data used to produce this plot beyond what is provided for Figure 5 includes laboratory reflectance measurements of various chondrites. The .scl files are the original laboratory measurements where the first column corresponds to the wavelength in microns, the second column to the normalized reflectance (unitless) and the third column to the error to 1 significant digit (unitless). The scaled_lab_reflectance.txt file has all the laboratory reflectance data used to produce the Figure 7 plot that includes the wavelength in microns, the normalized scaled reflectance for the CM chondrite, the normalized scaled reflectance for the CH/CBb chondrite, and the normalized scaled reflectance for the CY chondrite. </p> <p>For Figure 8 the additional data include original normalized reflectance data for asteroids interamnia, themis, bamberga, and europa as .trim files. The columns for these files correspond to wavelength in microns, normalized reflectance (unitless), and the error (unitless). The 'continuumremoved' .txt files correspond to the wavelength in microns and the normalized reflectance divided by the continuum (unitless). </p> <p>For Figure 9 these are the MIRI emissivity data for the two sets of observations. The first column corresponds to the wavelength in microns, the second column to the normalized emission by taking the flux subtracting the solar flux and dividing by a thermophysical model (unitless), the error (unitless), and the gaussian fit to the normalized emission. </p> <p>For the supplemental figures these are the additional fit absorption features that are located in the appendix of the manuscript. For the 1.25 - 4.8 micron text files the columns correspond to the wavelength in microns, the continuum divided normalized reflectance (unitless), the error (unitless), and the gaussian fit. For the 5.74 - 5.98 micron text files the columns correspond to wavelength in microns, normalized emission divided by a linear fit to a region outside any potential features (unitless), the error (unitless), and the gaussian fit to the feature. </p> <p>The MIRI 1D spectra folder contains the ASCII files corresponding to the 1 arcsec aperture summed spectra from the MIRI observations. The columns correspond to wavelength in microns, flux in Jansky, and error in Jansky. </p> <p>The NIRSpec 1D spectra folder contains the ASCII files corresponding to the 1 arcsec aperture summed spectra from the NIRSpec observations. The columns correspond to wavelength in microns, flux in Jansky, and error in Jansky. </p> <p>The Solar Spectra folder contains the solar spectra flux used to reduce the data to produce the reflectance and emission spectra. The lbl text files are equivalent to the files with the same name without the lbl but also include the column information. The first column corresponds to the wavelength in microns, the second column to the total spectral irradiance in Jansky, the third column to the flux from the object in Jansky, the fourth column to the reflected sunlight in Jansky, and the fifth column to the thermal contribution in Jansky. The only column used for the solar reflectance used in the analysis corresponds to the fourth column. </p> <p>The ThermalModel folder contains the ASCII files with the data corresponding to the thermophysical model used to produce the reflectance (by subtracting the thermal contribution) and the emission (by dividing by the thermal contribution). The first column corresponds to the wavelength in microns, the second to the thermal flux in Jansky, the third to the smoothed thermal flux in Jansky, and the fourth column to the normalized thermal flux. Only column two corresponding to the thermal flux in Jansky was used in the analysis associated with the manuscript. </p>
Detection of carbon dioxide and hydrogen peroxide on the stratified surface of Charon with JWST
<p>This repository houses the JWST/NIRSpec grand-average spectrum of Charon, along with infrared absorption spectra that detail the effects of 5 keV electron irradiation on CO2 diluted in H2O ice films.</p>
Products for "An absolute mass, precise age, and hints of planetary winds for WASP-121 A and b from a JWST NIRSpec phase curve"
<p>The repository contains radial velocity data for WASP-121b from Sing, Evans-Soma, Rustamkulov, Lothringer, Mayne, & Schlaufman from the paper titled "An absolute mass, precise age, and hints of planetary winds for WASP-121 A and b from a JWST NIRSpec phase curve" (2024, AAS jounals). The record contains two data files corresponding to JWST/NIRSpec radial velocity data as shown in Figures 6 (NRS2) and 7 (NRS1). Each file contains five collumns, normalized time (BJD_TDB-2400000.5) in days, orbital phase, the planet radial velocity (km/s) and the 1-sigma uncertainties in the radial velocity (km/s).</p>
Data Products and Reduction Files For: JWST COMPASS: The 3-5 Micron Transmission Spectrum of the Super-Earth L 98-59 c
<p>Supplementary material for JWST COMPASS: The 3-5 Micron Transmission Spectrum of the Super-Earth L 98-59 c, Scarsdale et. al. 2024 (accepted). Included are:</p> <ol> <li>Control files necessary to reproduce the Eureka! reduction described in the paper</li> <li>Stage 4 (light curves) data products from Eureka!</li> <li>Final transmission spectra for the Eureka! and ExoTIC-JEDI reductions </li> </ol> <p>Please contact Nicholas Scarsdale (nscarsda at ucsc.edu) with any questions. </p>
JWST NIRISS WFSS Backgrounds
<p>JWST NIRISS Background for WFSS and Imaging created from available all public NIRISS data to mitigate residual issues present in. </p> <p>We note that files are denoted as "skyflats" to maintain compatability with <a href="https://github.com/gbrammer/grizli/">grizli</a> although they represent average astronomical backgrounds in NIRISS WFSS and Imaging data. <br><br>All files include the following extensions:</p> <ol> <li>SCI: Empirical Background Data</li> <li>ERR: Error array</li> <li>DQ: Data Quality Array (Binary flags)</li> <li>DQ_DEF: Table Description of DQ Array. </li> </ol> <p>Please see the GitHub for more details.</p>
JWST spectra and best-fit SED models of massive quiescent galaxies from the Blue Jay survey.
<ul> <li>The JWST/NIRSpec spectra are stored as FITS tables which include wavelength (in angstrom, in rest-frame), calibrated flux, uncertainty, and best-fit model (in 1e-19 erg/s/cm^2/AA).</li> </ul>
JWST MIRI MRS dataset
<p>These are x1d test files for the JWST's MIRI MRS mode. They are used by specutils' unit tests to test the reader code.</p>
Products and Models for "Early Release Science of the Exoplanet WASP-39b with JWST NIRSpec PRISM"
<p>Associated publication: <a href="https://nam02.safelinks.protection.outlook.com/?url=https%3A%2F%2Fwww.nature.com%2Farticles%2Fs41586-022-05677-y%2520&data=05%7C01%7Czafar%40jhu.edu%7C70cefcf501224b8d305708daed9f9533%7C9fa4f438b1e6473b803f86f8aedf0dec%7C0%7C0%7C638083566905963125%7CUnknown%7CTWFpbGZsb3d8eyJWIjoiMC4wLjAwMDAiLCJQIjoiV2luMzIiLCJBTiI6Ik1haWwiLCJXVCI6Mn0%3D%7C3000%7C%7C%7C&sdata=gyY0O%2FyMHX0paZC60ZCiQAif%2F0O8K2QKAuuF9%2FjtRpA%3D&reserved=0">https://www.nature.com/articles/s41586-022-05677-y</a></p> <p> </p> <p>OVERVIEW: Transmission spectroscopy of exoplanets has revealed signatures of water vapor, aerosols, and alkali metals in a few dozen exoplanet atmospheres. However, these previous inferences with the Hubble and Spitzer Space Telescopes were hindered by the observations’ relatively narrow wavelength range and spectral resolving power, which precluded the unambiguous identification of other chemical species—in particular the primary carbon-bearing molecules. Here we report a broad-wavelength 0.5–5.5 µm atmospheric transmission spectrum of WASP-39 b, a 1200 K, roughly Saturn-mass, Jupiter-radius exoplanet, measured with JWST NIRSpec’s PRISM mode as part of the JWST Transiting Exoplanet Community Early Release Science Team program. We robustly detect multiple chemical species at high significance, including Na (19σ), H<sub>2</sub>O (33σ), CO<sub>2</sub> (28σ), and CO (7σ). The non-detection of CH<sub>4</sub>, combined with a strong CO<sub>2</sub> feature, favours atmospheric models with a super-solar atmospheric metallicity. An unanticipated absorption feature at 4 µm is best explained by SO<sub>2</sub> (2.7σ), which could be a tracer of atmospheric photochemistry. These observations demonstrate JWST’s sensitivity to a rich diversity of exoplanet compositions and chemical processes.</p>
Products and Models for "Early Release Science of the Exoplanet WASP-39b with JWST NIRISS"
<p>Associated Publication: <a href="https://www.nature.com/articles/s41586-022-05674-1">https://www.nature.com/articles/s41586-022-05674-1</a></p> <p> </p> <p>Transmission spectroscopy provides insight into the atmospheric properties and consequently the formation history, physics, and chemistry of transiting exoplanets. However, obtaining precise inferences of atmospheric properties from transmission spectra requires simultaneously measuring the strength and shape of multiple spectral absorption features from a wide range of chemical species. This has been challenging given the precision and wavelength coverage of previous observatories. Here, we present the transmission spectrum of the Saturn-mass exoplanet WASP-39b obtained using the SOSS mode of the NIRISS instrument on the JWST. This spectrum spans 0.6−2.8μm in wavelength and reveals multiple water absorption bands, the potassium resonance doublet, as well as signatures of clouds. The precision and broad wavelength coverage of NIRISS-SOSS allows us to break model degeneracies between cloud properties and the atmospheric composition of WASP-39b, favoring a heavy element enhancement ("metallicity") of ∼10−30× the solar value, a sub-solar carbon-to-oxygen (C/O) ratio, and a solar-to-super-solar potassium-to-oxygen (K/O) ratio. The observations are best explained by wavelength-dependent, non-gray clouds with inhomogeneous coverage of the planet's terminator.</p>
JWST MIRI channel1 spectrum of d203-506
<p>This is the JWST MIRI channel1 spectrum of d203-506 protoplanetary disk (ON and OFF position). The data are described in Berné et al. Nature 2023. </p>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.