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.
12
datasets available to search
ShareScore release 0.9.0
Dataset results
12 results for “emission spectrum”
Reproduction package for "A strong H− opacity signal in the near-infrared emission spectrum of the ultra-hot Jupiter KELT-9b"
<p>This is a basic reproduction package for the paper "A strong H− opacity signal</p><p>in the near-infrared emission spectrum of the ultra-hot Jupiter KELT-9b"</p><p>by [Jacobs, B.; Désert, J. -M.; Pino, L. et al. (2022)](https://doi.org/10.1051/0004-6361/202244533).</p><p> </p><p>Abstract:</p><p>We present the analysis of a spectroscopic secondary eclipse of the hottest transiting exoplanet detected to date, KELT-9b, obtained with the Wide Field Camera 3 aboard the <i>Hubble</i> Space Telescope. We complement these data with literature information on stellar pulsations and <i>Spitzer</i>/Infrared Array Camera and Transiting Exoplanet Survey Satellite eclipse depths of this target to obtain a broadband thermal emission spectrum. Our extracted spectrum exhibits a clear turnoff at 1.4 μm. This points to H− bound-free opacities shaping the spectrum. To interpret the spectrum, we perform grid retrievals of self-consistent 1D equilibrium chemistry forward models, varying the composition and energy budget. The model with solar metallicity and C/O ratio provides a poor fit because the H− signal is stronger than expected, requiring an excess of electrons. This pushes our retrievals toward high atmospheric metallicities ([M/H] = 1.98−0.21+0.19) and a C/O ratio that is subsolar by 2.4<i>σ</i>. We question the viability of forming such a high-metallicity planet, and therefore provide other scenarios to increase the electron density in this atmosphere. We also look at an alternative model in which we quench TiO and VO. This fit results in an atmosphere with a slightly subsolar metallicity and subsolar C/O ratio ([M/H] = −0.22−0.13+0.17, log (C/O) = −0.34−0.34+0.19). However, the required TiO abundances are disputed by recent high-resolution measurements of the same planet.</p>
Galactic Diffuse Emission Spectrum between 0.5 and 8.0 MeV and between 30 keV and 8 MeV for the search of PBH and Light Dark Matter
<p>Spectra and response files of the soft gamma-ray spectrum from Inverse Compton scattering in the Milky Way between 0.5 and 8.0 MeV, measured with INTEGRAL/SPI. The fluxes have been extracted with spimodfit assuming GALPROP v56 models according to Voyager 1, AMS-02, and Fermi/LAT data, plus different variants to change the interstellar radiation field, the diffusion properties, or the cosmic-ray halo size (<a href="https://ui.adsabs.harvard.edu/abs/2022A%26A...660A.130S/abstract">Siegert et al., 2022</a>). The respective galdef files are included. In particular:</p> <ul> <li>voyager: propagation model of Bisschoff et al. (2019), Table 2</li> <li>voyager_Dg10001: <span class="math-tex">\(\delta_1 = 0\)</span></li> <li>voyager_Dg1Dg205: <span class="math-tex">\(\delta_1 = \delta_2 = 0.5\)</span></li> <li>voyager_ISRFopt10: factor 10 stronger optical ISFR</li> <li>voyager_z8kpc_KL: thick halo with 8 kpc half-thickness</li> </ul> <p>In addition, there are spectra from 30 keV to 8 MeV (spec_0030-8000keV_<name>.fits, <a href="https://ui.adsabs.harvard.edu/abs/2022PhRvD.106b3030B/abstract">Berteaud et al., 2022</a>), separated into:</p> <ul> <li>CV: spectrum of unresolved point sources in the Galactic plane, mostly cataclysmic variables (strong systematics)</li> <li>IC: spectrum of Inverse Compton scattering of cosmic ray GeV electrons (see above)</li> <li>positronium: spectrum of positronium decay (annihilation of electrons with positrons after intermediate bound state)</li> <li>NFW: spectrum of dark matter contributions that would follow a Navarro Frenk White density profile (mostly consistent with zero)</li> <li>total: spectrum of the above combined</li> </ul> <p>The notebooks for dark matter related bounds when using this data as well as auxiliary files to create the templates are given as (<a href="https://ui.adsabs.harvard.edu/abs/2022PhRvD.106b3030B/abstract">Berteaud et al., 2022</a>, <a href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.520.4167C/abstract">Calore et al., 2023</a>):</p> <ul> <li>DM_fsr.ipynb: Notebook for final state radiation bounds</li> <li>DM_fsr.py: astromodels function for final state radiation spectrum</li> <li>DM_2gamma.ipynb: Notebook for gamma gamma final state bounds</li> <li>DM_2gamma.py: astromodels function for gamma gamma spectrum</li> <li>Positronium_Spectrum.py: astromodels function for Positonium spectrum</li> <li>DM_pbh.py: script for obtaining PBH bounds</li> <li>diff_@@.csv: spectra for PBH evaporation</li> <li>total_spectrum.fits.gz: total Galactic spectrum</li> <li>NFW_spectrum.fits.gz: NFW-only spectrum</li> </ul>
Figure 1 in Description of the bioluminescent emission spectrum of Bicellonycha amoena Gorham, 1880 (Coleoptera: Lampyridae) in Guatemala
Figure 1. Dorsal and ventral view of B. amoena. A–B) Male and female from "Mayan Golf Club", Villa Nueva, Guatemala. C–D) Two males from Hacienda Sac Chich near Merida, Mexico (credit: Lynn Faust).
Figure 4 in Description of the bioluminescent emission spectrum of Bicellonycha amoena Gorham, 1880 (Coleoptera: Lampyridae) in Guatemala
Figure 4. Bioluminescence emission spectrum of B. amoena in comparison to that of some North American Photinus species. A) B. amoena. B) P. tanytoxus. C) P. consanguineus. D) P. consimilis. E) P. sabulosus. F) P. umbratus (Biggley et al. 1967).
Implementation of Aerosol Mie Scattering in POSEIDON with Application to the hot Jupiter HD 189733 b's Transmission, Emission, and Reflected Light Spectrum - Supplementary Material
<p>Supplementary material to 'Implementation of Aerosol Mie Scattering in POSEIDON with Application to the hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum'</p> <p>This zenodo repository corresponds to the updates to POSEIDON presented in Mullens et al 2024, as well as the benchmark retrievals preformed on archival HD 189733 b. </p> <p>In the upper level of the repository we have data products mentioned in the paper:</p> <p>aersosol_database.pdf <br>Aerosol-Database-Readme.txt<br>aerosol_database.hdf5</p> <p>There are then three directories (here as zip files): </p> <p>Aerosol-Datbase<br>- This folder contains the aerosol properties for aerosols in Table 1 in the paper. It contains the aerosol-database.hdf5 which contains the precomputed aerosol properties that POSEIDON utilizes in forward models and retrievals, a folder containing the npy files that have individual precomputed aerosol properties (used to generate the hdf5 file), a pdf containing the refractive indices + precomputed aerosol properties for each aerosol in the database (png versions of these figures are available in the Aerosol-Optical-Properties-Pngs folder), the refractive index txt files for each aerosol, and a readme file that contains information on each aerosol in the database (such as aerosol name, polymorph, crystalline or amorphous, crystal shape, information on samples used in refractive index references, and exoplanet/planetary science specific references). </p> <p>HD-189733b-Retrievals<br>- Contains retrieval scripts and retrieval results for the transmission, emission, and emission+reflection retrievals in the paper. Also has the notebooks used to make the figures in the paper.</p> <p>POSEIDO-V1-2<br>- Contains the POSEIDON module used to run retrievals and generate figures, and corresponds to POSEIDON version 1.2. Also contains a folder containing tutorial notebooks for new features introduced into POSEIDON version 1.2. Included in this repository for posterity.</p>
Products and Models for "A broadband thermal emission spectrum of the ultra-hot Jupiter WASP-18b"
<p>Close-in giant exoplanets with temperatures greater than 2,000 K (“ultra-hot Jupiters”) have been the subject of extensive efforts to determine their atmospheric properties using thermal emission measurements from the Hubble and Spitzer Space Telescopes1–3. However, previous studies have yielded inconsistent results because the small sizes of the spectral features and the limited information content of the data resulted in high sensitivity to the varying assumptions made in the treatment of instrument systematics and the atmospheric retrieval analysis3–12. Here we present a dayside thermal emission spectrum of the ultra-hot Jupiter WASP-18b obtained with the NIRISS13 instrument on JWST. The data span 0.85 to 2.85 μm in wavelength at an average resolving power of 400 and exhibit minimal systematics. The spectrum shows three water emission features (at <6σ confidence) and evidence for optical opacity, possibly due to H-, TiO, and VO (combined significance of 3.8σ). Models that fit the data require a thermal inversion, molecular dissociation as predicted by chemical equilibrium, a solar heavy-element abundance (“metallicity”, M/H = 1.03-0.51+1.11 x solar), and a carbon-to-oxygen (C/O) ratio less than unity. The data also yield a dayside brightness temperature map, which shows a peak in temperature near the sub-stellar point that decreases steeply and symmetrically with longitude toward the terminators.</p>
Figure 3 in Description of the bioluminescent emission spectrum of Bicellonycha amoena Gorham, 1880 (Coleoptera: Lampyridae) in Guatemala
Figure 3. Bioluminescence emission spectrum of B. amoena. A) SS population. B) MGC population.
Figure 2 in Description of the bioluminescent emission spectrum of Bicellonycha amoena Gorham, 1880 (Coleoptera: Lampyridae) in Guatemala
Figure 2. Sampling locations for both populations of B. amoena in Guatemala and Sacatepéquez.
Size spectrum, time series and atom number distribution of macroalgal emission vapors and oxidation products
<p>We conducted oxidation and NPF experiments with vapor emissions from real-world coastal macroalgae in a bag reactor. The dataset showed the measurement results of volatile precursors and their oxidation products. The dataset was organized by the order of figures in our submitted manuscript.</p>
Chandra HETG Spectrum of Quiescent Emission from Sgr A*
<p>Dataset from "The Chandra High Resolution X-ray Spectrum of Quiescent Emission from Sgr A*", by Corrales et al. (2020).</p> <p>This article has been accepted to the Astrophysical Journal. A copy of the article pre-print is also uploaded for reference, and is also available on the astro-ph arXiv: <a href="https://arxiv.org/abs/2002.07198">https://arxiv.org/abs/2002.07198</a></p> <p>The dataset is available through the Chandra contributed datasets website: <a href="http://cxc.cfa.harvard.edu/cda/Contrib/2020/CORR1/">http://cxc.cfa.harvard.edu/cda/Contrib/2020/CORR1/</a></p> <p>Zenodo is being used for backup legacy storage, as there is no guarantee that the Chandra website will be maintained beyond the mission end date.</p>
Emission spectrum of the plasma source at different powers (gas flow:3 L/min) (a)280nm-420nm (b)720nm-860nm.
Open the record for dataset details and reuse information.
The Emission Spectrum of the Hot Jupiter WASP-79b from HST/WFC3
<p>Supplementary material for '<strong><em>The Emission Spectrum of the Hot Jupiter WASP-79b from HST/WFC3</em></strong>'.</p> <p>This repository contains posterior probability distributions for the two cases that were investigated using the 'white' light data of WASP-79b captured by the Hubble Space Telescope using the Wide Field Camera 3. It also contains the posterior probability distributions for three spectroscopic channels. </p> <p>The two 'white' light corner plots consider two scenarios: a fixed mid-eclipse time based on the expected occurrence time and a mid-eclipse time set as a free parameter. The three spectroscopic corner plots then look at the observations divided into three equal wavelength bins of width 0.20 μm centered at 1.18, 1.38, and 1.58 μm. The spectroscopic analysis was done under the scenario of a free mid-eclipse time.</p> <p> </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.