Find research datasets worth reusing

opencc-by-4.0Jan 2021View details →

Datasets associated with the publication of the "satuRn" R package

On this Zenodo link, we share the data that is required to reproduce all the analyses from our publication "satuRn: Scalable Analysis of differential Transcript Usage for bulk and single-cell RNA-sequencing applications". This repository includes input transcript-level expression matrices and metadata for all datasets, as well as intermediate results and final outputs of the respective DTU analyses. For a more elaborate description of the data, we refer to the companion GitHub for our publications; https://github.com/statOmics/satuRnPaper. Note that this is version 1.0.3 of the data (uploaded on 2022-07-08). If any changes were to be made to the datasets in the future, this will also be communicated on our companion GitHub page.

opencc-by-4.0Oct 2024View details →

Saturn's magnetospheric proton and electron intensities from Cassini

Differential intensities of 3keV – 40MeV protons and 10eV – 10MeV electrons in Saturn’s magnetosphere and radiation belts at L-shell distances between 1 and 20 Saturn radii from mission-averages of the MIMI/LEMMS, MIMI/CHEMS, and CAPS/ELS instruments on the Cassini spacecraft that was in orbit between 2004 and 2017.

opencc-by-4.0Mar 2023View details →

Selection of Low Frequency Extensions of Saturn Kilometric Radiation detected by Cassini/RPWS.

Selection of Low Frequency Extensions (LFEs) of Saturn Kilometric Radiation (SKR) observed by Cassini RPWS. The catalogue of LFES are presented in TFCAT format (Time-Frequency Catalogue, https://gitlab.obspm.fr/maser/catalogues/tfcat/-/tree/master/). This work was funded by Science Foundation Ireland grant 18/FRL/6199.

opencc-by-4.0Jun 2023View details →

Image-based Classification of Intense Radio Bursts from Spectrograms: An Application to Saturn Kilometric Radiation

A catalogue of 4874 of the Low Frequency Extensions (LFEs) of Saturn Kilometric Radiation (SKR) detected by Cassini/RPWS from the beginning of 2004 until mission end in 2017. The LFEs presented in this catalogue were identified using a modified U-Net architecture that applied semantic segmentation to spectrogram images in order to extract the exact frequency-time coordinates of the LFE. The files consist of a .json file with the coordinates of each LFE in Time Frequency Catalogue (TFCat) format (Cecconi et. al. 2023). We also include a .csv file with the start and stop times of each LFE in the form of python datetime timestamps, with the average predicted probability per LFE as an accompanying column.

opencc-by-4.0Dec 2023View details →

HPF data for "A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation"

Data from the Habitable Zone Planet Finder (HPF) Spectrograph at McDonald Observatory, in the form of high resolution infrared echelle spectra.  The target is HAT-P-67, a planet host star.  The spectra were acquired by Queue observations with the Hobby Eberly Telescope in the period 2020-2022.  The data were reduced with the "Goldilocks" pipeline.  The full dataset is described in detail in the paper "A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation".   The abstract for that paper is reproduced below: <div> <div>Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass-radius-insolation distribution. Here we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder (HPF) spectra show a detection of up to 10% absorption depth of the 10833 Angstrom Helium triplet. The 13.8 hours of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess Helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar---and not planetary---rest frame, consistent with the Doppler velocity structure seen in the Helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/night- side asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ 1D Parker wind models to estimate the mass loss rate, finding values on the order of 2x10^13 g/s, with large uncertainties owing to the unknown XUV flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: Ohmic dissipation and XUV irradiation, slightly favoring the latter.</div> </div>

opencc-by-4.0Mar 2024View details →

Cassini Magnetometer Data Products Associated With Ring-Saturn Electromagnetic Coupling

This dataset shows the measurements made by the Cassini magnetometer as it traversed ring-connected magnetic field lines during the Cassini Grand Finale orbits. The L-shell mapping of the azimuthal magnetic field component and associated field-aligned currents are provided, and can be used to regenerate the Cassini magnetometer data products in Figure 2 of the manuscript "Current Events at Saturn: Ring-Planet Electromagnetic Coupling" (Agiwal et al., 2024).

opencc-by-4.0Jan 2022View details →

List of Saturn magnetopause and bow shock crossings by the Cassini spacecraft

This is an updated list of magnetopause (MP) and bow shock (BS) crossings from Cassini, based on the list presented in Jackman et al. [2019] <a href="https://doi.org/10.1029/2019JA026628">https://doi.org/10.1029/2019JA026628</a>. This uploaded list has the following changes from the list first presented in that paper (and included in that supplementary material):   I = inbound O = outbound Amendments to Cassini MP/BS crossing list Changes made 26/01/2021 Total #MP crossings: 2118 (some times changed) Total #BS crossings: 1247 (3 pairs added, 1 pair removed, some times changed) Change list below: Change #1: Note the following crossings come from a list on MAPSView which was originally collated based on MAG and CAPS data.  MAG data gap spans these dates so crossings are based on other instruments at these times. ELS and SNG data available 2004 181-185 and 195-196 (except 196 13-23 UT). 2004    181    02    43    MP    I     2004    186    04    42    MP    O    2004    186    10    24    MP    I     2004    186    17    57    MP    O    2004    186    20    17    MP    I     2004    188    07    06    MP    O   2004    188    08    11    MP    I     2004    188    13    14    MP    O   2004    188    15    13    MP    I     2004    188    19    39    MP    O   2004    189    14    05    BS    O   2004    189    16    15    BS    I     2004    189    21    46    BS    O   2004    190    00    30    BS    I     2004    190    04    13    BS    O   2004    190    10    56    BS    I     2004    190    11    54    BS    O   2004    190    11    54    DG    S_SW  2004    194    05    12    DG    E_SH   2004    194    05    12    BS    O     2004    196    03    11    BS    I     2004    196    06    59    BS    O   Change #2: Change 2004    348    05    27    MP    I     to 2004    348    05    00    MP    I     Change #3: Added some crossings on 2004 day 345 2004 345 11 52 BS I 2004 345 11 58 BS O 2004 345 12 20 BS I 2004 345 12 26 BS O 2004 345 23 06 BS I 2004 345 23 13 BS O Change #4:  Changed 2004 day 345 13 24 BS I  to 2004 day 345 12 57 BS I Change #5:  Remove 2014    322    6    8    BS    I     2014    326    1    23    BS    O     _________________________________________________________________________________________ Additional changes made through discussion with Matthew Cheng, August 13th 2021 Original list: Master_BS_MP_Crossing_List_04_16_incCMJcorr_published 1st Revised list: Master_BS_MP_Crossing_List_04_16_incCMJcorr_revised 2nd Revised list: Master_BS_MP_Crossing_List_04_16_incCMJcorr_revised_120821 Since 1st revised list: Total #MP crossings: 2122 (2 new pairs, some times changed) Total #BS crossings: 1249 (1 new pair, some times changed) Change #6 Changed typo 2016    068    12    19    DG    E_MP         to 2016    068    12    19    DG    E_SP         Change #7 Change  2016    242    12    00    MP    O         To: 2016    242    11    15    MP    O     Change #8 Change  2016    152    16    33    BS    O to  2016    152    15    22    BS    O Change #9 Change  2016    153    02    24    BS    O     to     2016    153    02    08    BS    O         Change #10 Change  2016    153    12    00    BS    I         to 2016    153    11    45    BS    I         Change #11 Add new MP pair 2016    155    11    05    MP    O     2016    155    12    52    MP    I     Change #12 Change 2011    2    03    14    MP    O     to 2011    2    01    48    MP    O     Change #13 Change: 2012    145    15    11    MP    O     To 2012    145    14    36    MP    O Change #14 Changed 2007    33    16    25    MP    I     to  2007    33    15    25    MP    I     Change #15 Add new MP pair 2005    45    11    55    MP    O     2005    45    12    36    MP    I    Change #16 Add new BS pair 2012    277    00    15    BS    I     2012    277    01    36    BS    O Change #17 Add new MP pair 2008    85    14    31    MP    I   2008    85    15    38    MP    O

opencc-by-4.0Oct 2022View details →

Lid-Driven Cavity Re=400 flow solution computed using LUMA and Code_Saturne coupled to each other

This dataset is the result of running the Code_Saturne and LUMA codes coupled to each other to simulate a standard Re=400 Lid-Driven Cavity problemon ARCHER2.  This is a test case for the coupling of the two codes. The domain is a unit cube.  LUMA evolved the portion $x \le 0.6$, and Code\_Saturne evolved the portion $x \ge 0.4$.  The boundary $x=0$ was driven with a velocity $u_y = 1$.  Boundary data at the coupling boundaries is obtained from the other code using the PLE library. See https://github.com/cfdemons/cs-luma-archer/blob/main/tutorial.md for details to reproduce this dataset.

zenodo36/100

The Plasma Distribution in Saturn's Inner Magnetosphere from 2.4 to 10 Rs: A Diffusive Equilibrium Model

This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, <a href="https://doi.org/10.1029/2019JA027545">10.1029/2019JA027545</a> Abstract: Electron density measurements have been obtained by the Cassini Radio and Plasma Wave Science (RPWS) instrument covering the period from 30 June, 2004 to 19 April, 2017, spanning latitudes up to ~30o and L values from 2.4 to 10. Near the F ring, electron densities are derived from RPWS measurements of electron plasma oscillations at high latitudes and from the Langmuir Probe (RPWS/LP) sweep data at low latitudes. The electron density measurements from the ring-grazing orbits, beginning in December 2016, have made it possible to extend the work of a previous diffusive equilibrium model to include the distribution of the ring plasma. Beyond the ring-grazing orbits, the densities are derived from RPWS measurements of the upper hybrid resonance frequency. These density measurements are used to anchor the fit of an expanded diffusive equilibrium density model for a two-species plasma consisting of water group and hydrogen ions in Saturn’s inner magnetosphere. Density contour plots for the two ion species and the electrons are presented. The distribution of the derived plasma densities is consistent with two primary sources, the Enceladus plumes and the extended ring atmosphere. There is also an indication of a weaker plasma source at Dione. In the region just outside the A Ring and in the region including the Enceladus orbit, the diffusive equilibrium model also clearly shows the expansion of lighter ions and electrons to higher latitudes along the magnetic field lines with evidence of a weaker plasma expansion between the orbits of Tethys and Dione.

opencc-by-4.0Dec 2019View details →

zenodo36/100

Triple shadow phenomena on Jupiter, Saturn and Uranus from 1000 CE to 3000 CE

I computed all triple shadow phenomena of the major moons with their planet from 1000 CE to 3000 CE. I found 315 of such phenomena occurring on Jupiter, 303 on Saturn and 151 on Uranus. During the 2001 year period Saturn experiences 1 quadruple shadow phenomena meanwhile Uranus experiences 3 of such. I computed all shadow events of the Galilean moons with Jupiter, their mutual eclipses and the planet’s elongation from 1000 CE to 3000 CE with Occult 4.10.1.0 (files updated: 2020 March 20). I repeated the same procedure for Tethys, Dione, Rhea, Titan and Iapetus with Saturn and Miranda, Ariel, Umbriel, Titania and Oberon with Uranus. I then filtered the results to find triple and quadruple shadow events within the satellites and their respective primaries. Finally, I added the planet’s elongation for the event’s date above found and mutual eclipses only occurring during a triple or quadruple shadow event on the planet. I assumed that the Gregorian calendar commenced in 1582 October 4. Before that date, I used the Julian calendar.  All times are in Universal Time. Minutes are rounded to the nearest tenth of a minute. For convenience, I used Arabic numbers to designate all satellites instead of Roman ones.

opencc-by-4.0Sep 2021View details →

zenodo36/100

Model of the planet saturn

The presented object is a model of Saturn, which was used for educational purposes. The model shows the planet with two rings and the moon - Titan. It was used to demonstrate the tilt of Saturn's rings and the position of its moon in relation to the observer. Henryk Niemetz 1869, Kraków Jagiellonian University Museum Collegium Maius Inventory number: 4081; 81/V https://muzea.malopolska.pl/en/objects-list/2782 Source: Objaverse 1.0 / Sketchfab

opencc-zeroDec 2020View details →

ClinicalTrials.gov36/100

Investigation of H01 in Adults With Pulmonary Hypertension Including Interstitial Lung Disease (The SATURN Study).

ClinicalTrials.gov study NCT05128929. IPD Sharing: Not stated. Countries: 1. Publications: 2.

restrictedIPD-UNDECIDEDFeb 2026View details →

dryad36/100

Retrospective data collected on SATURN, a public domain self-administered cognitive screening test

Open the record for dataset details and reuse information.

publicApr 2025View details →

dryad32/100

Comet fading begins beyond Saturn

The discovery probability of long-period comets (LPCs) passing near the Sun is highest during their first passage and then declines, or fades, during subsequent return passages. Comet fading is largely attributed to devolatilization and fragmentation via thermal processing within 2-3 AU of the Sun (1 AU being the Earth-Sun distance). Here our numerical simulations show that comet observing campaigns miss vast numbers of LPCs making returning passages through the Saturn region (near 10 AU) because these comets fade during prior, even more distant passages exterior to Saturn and thus elude detection. Consequently, comet properties significantly evolve at solar distances much larger than previously considered, and this offers new insights into the physical and dynamical properties of LPCs, both near and far from Earth.

opencc-zeroFeb 2022View details →

opencc-by-4.0Jun 2024View details →

STIM model output for "Aurorally-driven Supersonic Gravity Waves in Saturn's Atmosphere"

Saturn Thermosphere-Ionosphere Model (STIM) output corresponding to the figures shown in the paper "Aurorally-driven Supersonic Gravity Waves in Saturn's Atmosphere".

opencc-by-4.0Jul 2024View details →

Smoothed VLT/MUSE observations of Jupiter and Saturn

Data are those used for the JGR submission: "Clouds and ammonia in the atmospheres of Jupiter and Saturn determined from a band-depth analysis of VLT/MUSE observations". Observation dates are 23rd March 2020 for Jupiter, and 6th April 2017 for Saturn.

opencc-by-4.0Mar 2023View details →

Data products associated with: Tamburo, Withers, Dalba, Moore, and Koskinen (2023) Cassini radio occultation observations of Saturn's ionosphere: Electron density profiles from 2005 to 2013, Journal of Geophysical Research, doi:10.1029/2023JA031310

These data products are associated with Tamburo, Withers, Dalba, Moore, and Koskinen (2023) Cassini radio occultation observations of Saturn’s ionosphere: Electron density profiles from 2005 to 2013, Journal of Geophysical Research, doi:10.1029/2023JA031310. At the time of writing, this manuscript is under review. In the future, these data products will be submitted for archiving at the NASA Planetary Data System (PDS).