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Dataset results
18 results for “protoplanetary disk”
Data from "A multi-frequency ALMA characterization of substructures in the GM Aur protoplanetary disk"
<p>Image cubes, self-calibrated visibilities, and self-calibration and imaging scripts for data associated with Huang et al., 2020, "A multi-frequency ALMA characterization of substructures in the GM Aur protoplanetary disk," The Astrophysical Journal, 891, 48, arXiv:2001.11040</p> <p>The raw data are available on the ALMA archive under program IDs 2017.1.01151.S and 2018.1.01230.S (PI: Jane Huang). </p> <p><strong>Scripts:</strong></p> <p>reduction_utils.py: Set of helper functions for self-calibration scripts</p> <p>B4continuumreduction.py: Self-calibration and imaging script for Band 4 (2.1 mm) continuum (GMAurB4continuumfinal.image.fits) from GMAurB4continuum.final.ms.tgz</p> <p>B6continuumreduction.py: Self-calibration and imaging script for Band 6 (1.1 mm) continuum (GMAurB6continuumfinal.image.fits) from GMAurB6continuum.final.ms.tgz</p> <p>HCOp_imaging.py: Script producing GMAur_HCOp_continuumsubtracted.image.fits and GMAur_HCOp_withcontinuum.image.fits from GMAurB6_HCOp.ms.contsub.cvel and GMAurB6_HCOp.ms.cvel, respectively</p> <p><strong>Measurement sets:</strong></p> <p>GMAurB4continuumfinal.ms.tgz: Self-calibrated 2.1 mm continuum visibilities for GM Aur</p> <p>GMAurB6continuumfinal.ms.tgz: Self-calibrated 1.1 mm continuum visibilities for GM Aur</p> <p>GMAurB6_HCOp.ms.cvel.tgz: Self-calibrated HCO<sup>+ </sup>3-2 visibilities without continuum subtraction</p> <p>GMAurB6_HCOp.ms.contsub.cvel.tgz: Self-calibrated HCO<sup>+ </sup>3-2 visibilities with continuum subtraction</p> <p><strong>Images: </strong></p> <p>GMAurB6continuumfinal.image.fits: 1.1 mm continuum image of GM Aur</p> <p>GMAurB4continuumfinal.image.fits: 2.1 mm continuum image of GM Aur</p> <p>GMAur_HCOp_withcontinuum.image.fits: HCO<sup>+ </sup>3-2 image cube toward GM Aur without continuum subtraction</p> <p>GMAur_HCOp_continuumsubtracted.image.fits: HCO<sup>+ </sup>3-2 image cube toward GM Aur with continuum subtraction</p> <p> </p> <p> </p>
Far-infrared to millimeter data of protoplanetary disks: dust growth in the Taurus, Ophiuchus, and Chamaeleon I star-forming regions
<p>This repository contains the data set presented in the manuscript "Far-infrared to millimeter data of protoplanetary disks: dust growth in the Taurus, Ophiuchus, and Chamaeleon I star-forming regions" (Ribas et al. 2017), and includes a table with several sample properties (e.g. stellar properties, Herschel photometry, different spectral indices), spectral energy distributions, Spitzer/IRS and Herschel/SPIRE spectra, the median SEDs of Taurus, Ophiuchus and Chamaeleon I, and the Herschel maps used.</p> <p>ERRATUM: three Chamaeleon I sources (Hn 11, T45a, and WY Cha) were mislabeled in the original version of the manuscript, which resulted in their names, stellar parameters, extinction values, infrared slopes, and silicate feature properties being assigned to incorrect coordinates. Because the photometry and spectroscopy presented in the original article is coordinate- based, the provided SEDs and spectra were also missmatched: the data files labeled Hn 11 in the original manuscript correspond to T45a, those labeled T45a correspond to WY Cha, and those labeled WY Cha correspond to Hn 11. Additionally, due to a mislabeling issue in Manoj et al. 2011, the source formerly labeled UX Cha is actually CHSM 8284. Therefore, stellar parameters and photometry labeled UX Cha in our original manuscript correspond to CHSM 8284 The updated version of the repository fixes the issue both in the sample.csv file and in the individual SED and Spitzer/IRS spectra files. The published erratum is available here: <a href="https://iopscience.iop.org/article/10.3847/1538-4357/abb66e">https://iopscience.iop.org/article/10.3847/1538-4357/abb66e</a>.</p>
Radiative Transfer Edge-on Protoplanetary Disk Images
<p>Dataset used to train a Convolutional Autoencoder model to generate synthetic images of edge-on protoplanetary disks. The work is described in "A machine learning framework to predict images of edge-on protoplanetary disks", Telkamps et al. 2022, submitted to AAS. This image dataset was created using the radiative transfer (RT) modeling code MCFOST (Pinte et al. 2006; Pinte et al. 2009). </p>
A JWST inventory of protoplanetary disk ices. The edge-on protoplanetary disk HH 48 NE, seen with the Ice Age ERS program
<p>JWST NIRSpec G395H spectrum for HH 48 NE edge-on disk, as analyzed in Sturm et al. (2023). DOI: 10.1051/0004-6361/202347512</p>
Data from "CO Line Emission Surfaces and Vertical Structure in Mid-Inclination Protoplanetary Disks"
<p>CO line emission image cubes ("[DISK]_CO_cube.fits"), line+continuum image cubes ("[DISK]_CO_cube_wcont.fits"), and zeroth moment maps ("[DISK]_CO_M0.fits") associated with Law et al., 2022, "CO Line Emission Surfaces and Vertical Structure in Mid-Inclination Protoplanetary Disks," The Astrophysical Journal</p> <p>CO line emission image cubes from the DSHARP ALMA Large Program (for HD 142666, MY Lup, GW Lup, WaOph 6, DoAr 25) can be found at: https://bulk.cv.nrao.edu/almadata/lp/DSHARP/ and are not included here.</p> <p>The raw data are available on the ALMA archive (see Table 1 in the paper for a listing of the relevant ALMA project codes).</p>
Formation of super-Earths in a protoplanetary disk
<p>This is a simulation of the process of formation for a planetary system with close-in super-Earths.</p> <p>The simulation begins with 125 planetary embryos, each with 0.4 times the mass of the Earth. The gray region shows the height of the protoplanetary disk. At the beginning of the simulation the embryos have strong gravitational encounters that increase their orbital inclinations (y-axis) and leads to collisions. After the embryos merge into larger bodies, interactions with the disk cause the eccentricities and inclinations to drop and the planets form a chain of mean motion resonances. Planets also experience torques from the disk that remove orbital angular momentum which causes the planets to drop to lower orbits. While the planets migrate through the disk, they accrete gas from the disk. The color of each body shows the fraction of their mass that is in the gaseous envelope.</p> <p>The disk dissipates after 5 Myr. With the disk gone, the planetary system becomes dynamically unstable and two new waves of giant impacts occur. This leaves behind a planetary system with larger planet masses, smaller gas envelopes, and higher mutual inclinations.</p>
Data from "Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission"
<p>CO isotopologue line emission image cubes ("[DISK]_[LINE]_cube.fits"), line+continuum image cubes ("[DISK]_[LINE]_cube_wcont.fits"), and zeroth moment maps ("[DISK]_[LINE]_M0.fits") associated with Law et al., 2023, "Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission," The Astrophysical Journal</p> <p>The raw data are available on the ALMA archive (see Table 2 in the paper for a listing of the relevant ALMA project codes).</p>
Observational Signatures of Tightly Wound Spirals Driven by Buoyancy Resonances in Protoplanetary Disks
<p>These are simulated CO data cubes presented in "Observational Signatures of Tightly Wound Spirals Driven by Buoyancy Resonances in Protoplanetary Disks" by Bae, Teague and Zhu. They represent simulated 12CO and 13CO ALMA observations using the standard model (see Section 3.1.1 of the paper), with three different planet masses (0.5, 1, and 2 Jupiter-mass) and five different disk inclination values (5, 15, 30, 45, and 60 degrees).</p>
Shadowing and multiple rings in the protoplanetary disk of HD 139614
<p>This is a basic reproduction package for the paper 'Shadowing and multiple rings in the protoplanetary disk of HD 139614' by Muro-Arena et al (2022). It aims to provide the most important data products to check and reproduce the main results of the paper, listing all software used and data archives containing the public data used.</p> <p> </p> <p>It is available at - arXiv: https://ui.adsabs.harvard.edu/abs/2020A%26A...635A.121M/abstract and has been published by Astronomy and Astrophysics at https://www.aanda.org/articles/aa/full_html/2020/03/aa36509-19/aa36509-19.html</p>
A unified intensity of the magnetic field in the protoplanetary disk from the Winchcombe meteorite
<p>Alternating field demagentisation data for the Winchcombe meteorite, published in 'A unified intensity of the magnetic field in the protoplanetary disk from the Winchcombe meteorite' (2023) <em>Meteoritics and Planetary Science</em>, <strong>59</strong>, 1194-1215, 10.1111/maps.14079</p>
Data from "Molecular Mapping of DR Tau's Protoplanetary Disk, Envelope, Outflow, and Large-Scale Spiral Arm"
<p>Data associated with Huang et al., 2023, "Molecular Mapping of DR Tau's Protoplanetary Disk, Envelope, Outflow, and Large-Scale Spiral Arm," ApJ, 943, 107</p> <p>The raw data can be obtained by requesting data from program W20BE (PI: J. Huang) from the NOEMA archive. </p> <p><strong>Images</strong></p> <p>images.tar: FITS files of image cubes and moment maps as shown in Figs. 2, 3, 5, 9, and 10 (see also finalimagingscript.py)</p> <p><strong>Spectra</strong></p> <p>spectra.tar: ASCII files of spectra shown in Figs. 1 and 9 (see also finalimagingscript.py) </p> <p><strong>Measurement sets (CASA format)</strong></p> <p>drtau_LINENAME_corrected.ms.tar: Measurement set for a given line, corresponding to drtau_LINENAME_selfcal-contsub.uvt in lines_contsub_uvt.tar </p> <p>drtau_ui_cont_corrected.ms.tar: Continuum measurement set corresponding to the UI baseband, generated from w20be-ui-cont-selfcal.uvt in continuum_uvt.tar </p> <p><strong>UV tables (GILDAS format)</strong></p> <p>LR_uvt.tar: Pipeline-calibrated UV tables of low-resolution data (see w20be-tables-LR.clic)</p> <p>HR_uvt.tar: Pipeline-calibrated UV tables of high-resolution data (see w20be-tables-HR.clic)</p> <p>continuum_uvt.tar: Self-calibrated, spectrally averaged continuum UV tables generated from LR_uvt.tar</p> <p>lines_contsub_uvt.tar: Self-calibrated, continuum-subtracted line UV tables generated from the UV tables in HR_uvt.tar</p> <p><strong>Scripts</strong></p> <p>w20be-tables-LR.clic: CLIC script used to output UV tables of low-resolution data from the pipeline-calibrated data (output contained in LR_uvt.tar)</p> <p>w20be-tables-HR.clic: CLIC script used to output UV tables of high-resolution data from the pipeline-calibrated data (output contained in HR_uvt.tar)</p> <p>uvfitstoms.py: Script to export uvfits files to measurement sets and to correct the metadata in the measurement sets </p> <p>finalimagingscript.py: CASA script used to generate imaging products in images.tar and spectra in spectra.tar </p> <p><strong>Other:</strong></p> <p>calib.tar: Files output by NOEMA pipeline </p> <p> </p>
Modest dust settling in the IRAS04302+2247 Class I protoplanetary disk
<p>Continuum VLA images of IRAS04302+2247, from projects 21B-183 and 21B-100. For the Q and Ka observations, we also include images after correction for free-free emission.</p>
Theoretical water binding energy distribution and snowline in protoplanetary disks
<p>Zip file containing all the structures and input obtained in our accepted article for publication in ApJ, 2023</p> <p>To easily handle all these structures an online interactive page is created: <a href="https://tinaccil.github.io/Jmol_BE_H2O_visualization/">https://tinaccil.github.io/Jmol_BE_H2O_visualization/</a></p>
Dust rings as a footprint of planet formation in a protoplanetary disk
<p>Simulation outputs of "Dust rings as a footprint of planet formation in a protoplanetary disk".</p> <p>average_output*.dat: azimuthally averaged surface density of gas</p> <p>average_output_dust0*.dat azimuthally averaged surface density of dust grains</p> <p>output*.dat: 2D data for gas</p> <p>output_dust0*.dat: 2D data for dust grains</p> <p>The number of the file indicates the time of output (10xnumber orbit)</p> <p>Regarding to planet0.dat and orbit0.dat, please see http://fargo.in2p3.fr/Output</p>
ALMA cubes and integrated maps of the d203-506 protoplanetary disk
<p>These are the ALMA reduced data of the d203-506 protoplanetary disk. The data was obtained as part of the project 2017.1.01478.S (PI J.~Champion). The data was reduced at the ALMA regional node in Grenoble thanks to the help of Edwige Chapillon. </p>
Modeling protoplanetary disk SEDs with artificial neural networks: Revisiting the viscous disk model and updated disk masses
<p>This repository contains the cornerplots of relevant parameters for the 23 protoplanetary disks modeled in the manuscript "Modeling protoplanetary disk SEDs with artificial neural networks: Revisiting the viscous disk model and updated disk masses" (Ribas et al. 2020).</p>
Determining Dust Properties in Protoplanetary Disks: SED-derived Masses and Settling With ALMA
<p>This zip file contains the cornerplots of relevant parameters for the 338 protoplanetary disks modeled in the manuscript "Determining Dust Properties in Protoplanetary Disks: SED-derived Masses and Settling With ALMA" (Rilinger et al. 2022). This version includes the most up-to-date sample of disks. The disk masses are now displayed logarithmically for clarity.</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>
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Allen Brain Atlas
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Annotated Behaviour and Observability Dataset (ABODe)
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DANDI Archive for NWB datasets
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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.