cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.5066/p986b6hq
title: Phosphorus, nitrogen, and suspended-sediment loads measured at the Great Lakes Restoration Initiative tributary monitoring network: Water years 2011&amp;ndash;2020

description: Phosphorus, nitrogen, and suspended-sediment loads, in 24 U.S. tributaries of the Great Lakes, were calculated using U.S. Geological Survey (USGS) data from the Great Lakes Restoration Initiative (GLRI) monitoring program for the period Oct 2010 through Sept 2020 (USGS water years 2011?2020). Total phosphorus, orthophosphate, particulate phosphorus, total nitrogen, nitrate plus nitrite, ammonium plus ammonia, and suspended-sediment loads and changes in loads were determined by applying a weighted regression approach called WRTDS (Weighted Regression on Time, Discharge, and Season). The load results represent the total mass of nitrogen, phosphorus, and suspended sediment exported downstream at each tributary site. Daily loads were estimated using the WRTDS method with Kalman filtering. To determine the change in loads between the first and last water year in record, the annual load results were flow-normalized to standardize among years with varying flow dynamics. Three primary data tables are provided that describe phosphorus, nitrogen, and suspended-sediment conditions at 24 tributaries across the U.S. Great Lakes watershed: (1) annual results, (2) daily results, and (3) changes results. The annual table is organized by USGS water year (defined as Oct 1?Sept 30). The annual and daily tables also include time-weighted mean concentrations, mean discharge, and yield estimates, the latter being calculated by dividing loads by watershed areas. Descriptions for data tables are provided in the DataDictionary.csv file. Results are also displayed in an interactive web application (https://rconnect.usgs.gov/glritrends). This data release also contains a model archive. The ?model_code.zip? file contains the R code and input data to run the models, generate the results, and display the results on a shiny application. The README.md file includes instructions of how to run the model and descriptions of all inputs, model arguments, and outputs. Each model (saved as an eList) contains the input data (USGS station information (i.e., site information), daily discharge, and water sample data), model parameters, estimated values, and bootstrapped results. All eLists are archived in the ?model_archive? folder, which is organized by sample dataset (i.e., allsamples and midsamples) and are named with the parameter and station number (e.g., NH4_04024000.RData). The RData files used in the shiny application are archived in the ?shinydata? folder.
DOI: 10.6084/m9.figshare.24302629
title: DEM_Europe.tif

description: This dataset contains the Copernicus DEM project with a 25m spatial resolution
DOI: 10.6084/m9.figshare.24302629.v1
title: DEM_Europe.tif

description: This dataset contains the Copernicus DEM project with a 25m spatial resolution
DOI: 10.5066/p9vhfkdn
title: Black Bayou Hydrologic Restoration (CS-27): 2018 land-water classification

description: The Louisiana State Legislature created the Coastal Wetlands Planning, Protection and Restoration Act (CWPPRA) in order to conserve, restore, create and enhance Louisiana's coastal wetlands. The wetland restoration plans developed pursuant to these acts specifically require an evaluation of the effectiveness of each coastal wetlands restoration project in achieving long-term solutions to arresting coastal wetlands loss. This data set includes mosaicked aerial photographs for the Black Bayou Hydrologic Restoration (CS-27) project for 2018. This data is used as a basemap land-water classification. It also serves as a visual tool for project managers to help them identify any obvious problems or land loss within their project boundary. To better evaluate the effectiveness of restoration efforts, a land-water classification is performed on specific CWPPRA sites to help assess landscape changes.
DOI: 10.48324/dandi.000363/0.231012.2129
title: Mesoscale Activity Map Dataset

description: Mesoscale Activity Map Project. Map behavior-related activity in a multi-regional network supporting memory-guided movement in mice. Anatomy-guided recordings from multiple connected brain regions, from anterior lateral motor cortex to the medulla.

Supported by Simons Collaboration on the Global Brain, Janelia Visitor Project, NIH U19NS123714-01, R01NS112312, R01EB028171, McKnight foundation
DOI: 10.6084/m9.figshare.24302638
title: war_romance_main.zip

description: This study uses a machine learning technique to show that our collective memory of a war generally evolves into a more positive narrative over time.
DOI: 10.6084/m9.figshare.24302638.v1
title: war_romance_main.zip

description: This study uses a machine learning technique to show that our collective memory of a war generally evolves into a more positive narrative over time.
DOI: 10.48577/jpl.c92an1
title: High frequency study of FRB 20180916B using the 100-m Effelsberg radio telescope

description: FRB 20180916B is a repeating fast radio burst (FRB) with an activity period of 16.33 days. In previous observations ranging from ∼ 150 − 1400 MHz, the activity window was found to be frequency dependent, with lower frequency bursts occurring later. In this work, we present the highest-frequency detections of bursts from this FRB, using the 100-m Effelsberg Radio Telescope at 4-8 GHz. We present the results from two observing campaigns. We performed the first campaign over an entire activity period which resulted in no detections. The second campaign was in an active window at 4-8 GHz which we predicted from our modelling of chromaticity, resulting in eight burst detections. The bursts were detected in a window of 1.35 days, 3.6 days preceding the activity peak seen by CHIME, suggesting the chromaticity extends to higher frequency. The detected bursts have narrower temporal widths and larger spectral widths compared to lower frequencies. All of them have flat polarization position angle sweeps and high polarization fractions. The bursts also exhibit diffractive scintillation due to the Milky Way, following a freq^3.90+/-0.05 scaling, and vary significantly over time. We find that burst rate across frequency scales as freq^−2.6+/-0.2. Lastly, we examine implications of the frequency dependency on the source models.
DOI: 10.48577/jpl.bn5alz
title: Low–Temperature Specific Heat Capacity of Water–Ammonia Mixtures Down to the Eutectic

description: Robust thermodynamic data are essential for the development of geodynamic andgeochemical models of ocean worlds. The water–ammonia system is of interest inthe study of ocean worlds due to its purported abundance in the outer solar system,geological implications and potential importance for origins of life. In support of thedevelopment of a new equation of state, we conducted 1 bar specific heat capacitymeasurements (Cp) using a differential scanning calorimeter (DSC) at low temperatures(184 − 314 K) and low mass fractions of ammonia (5.2 − 26.912 wt%) to provide noveldata in the parameter space most relevant for planetary studies. This is the first knownset of data with sufficient fidelity to investigate the trend of specific heat capacity with respect to temperature. The obtained Cp in the liquid phase domain abovethe liquidus generally increasing with temperature. Deviations of our data from thecurrently adopted equation of state by Tillner-Roth and Friend is generally negativeand ranges from of +1% to −10 %, where deviations are larger at lower temperatures.This suggests that suppression of the critical behavior of super-cooled water (rapidincrease in specific heat with decreasing temperature) by ammonia starts at a smallerconcentration than that arbitrarily set by Tillner-Roth and Friend. Cp measurementsof the liquid were also obtained from the partial melting domain between the eutecticand liquidus. This novel set of data will be useful in future investigations in conditionswhere such partial melt may exist, such as the ice shell–ocean boundary.
DOI: 10.48577/jpl.casvv2
title: Deep learning denoising by dimension reduction: Application to the ORION-B line cubes

description: Context. The availability of large bandwidth receivers for millimeter radio-telescopes allows the acquisition of position-position-frequency data cubes over a wide field of view and a broad frequency coverage. These cubes contain much information on the physical, chemical, and kinematical properties of the emitting gas. But their large size coupled with inhomogenous signal-to-noise ratio (SNR) are major challenges for consistent analysis and interpretation. Aims. We search for a denoising method of the low SNR regions of the studied data cubes that would allow to recover the low SNR emission without distorting the signals with high SNR. Methods. We perform an in-depth data analysis the 13CO and C17O (1 − 0) data cubes obtained as part of the ORION-B large program performed at the IRAM 30m telescope. We analyse the statistical properties of the noise and the evolution of the correlation of the signal in a given frequency channel with that of the adjacent channels. This allows us to propose significant improvements of typical autoassociative neural networks, also called autoencoders, often used to denoise hyperspectral Earth remote sensing data. Applying this method to the 13CO (1 − 0) cube, we compare the denoised data with those derived with the multiple Gaussian fitting algorithm ROHSA, considered as the state of the art procedure for data line cubes. Results. The nature of astronomical spectral datacubes is distinct from that of the hyperspectral data usually studied in the Earth remote sensing literature because the observed intensities become statistically independent beyond a short channel separation. This lack of redundancy in data has led us to adapt the method, notably by taking into account the sparsity of the signal along the spectral axis. The application of the proposed algorithm leads to an increase of the SNR in voxels with weak signal, while preserving the spectral shape of the data in high SNR voxels. Conclusions. The proposed algorithm that combines a detailed analysis of the noise statistics with an innovative autoencoder architecture is a promising path to denoise radio-astronomy line data cubes. In the future, exploring whether a better use of the spatial correlations of the noise may further improve the denoising performances seems a promising avenue. In addition, dealing with the multiplicative noise associated with the calibration uncertainty at high SNR would also be beneficial for such large data cubes.
DOI: 10.48577/jpl.mkbs3r
title: Molecular Outgassing in Centaur 29P/Schwassmann-Wachmann 1 During Its Exceptional 2021 Outburst: Coordinated Multi-Wavelength Observations Using nFLASH at APEX and iSHELL at the NASA-IRTF

description: The extraordinary 2021 September–October outburst of Centaur 29P/Schwassmann–Wachmann 1 afforded an opportunity to test the composition of primitive Kuiper disk material at high sensitivity. We conducted nearly simultaneous multi-wavelength spectroscopic observations of 29P/Schwassmann–Wachmann 1 using iSHELL at the NASA Infrared Telescope Facility and nFLASH at the Atacama Pathfinder EXperiment (APEX) on 2021 October 6, with follow-up APEX/nFLASH observations on 2021 October 7 and 2022 April 3. This coordinated campaign between near-infrared and radio wavelengths enabled us to sample molecular emission from a wealth of coma molecules and to perform measurements that cannot be accomplished at either wavelength alone. We securely de- tected CO emission on all dates with both facilities, including velocity-resolved spectra of the CO (J=2–1) transition with APEX/nFLASH and multiple CO (v=1–0) rovibrational transitions with IRTF/iSHELL. We report rotational temperatures, coma kinematics, and production rates for CO and stringent (3σ) upper limits on abundance ratios relative to CO for CH4, C2H6, CH3OH, H2CO, CS, and OCS. Our upper limits for CS/CO and OCS/CO represent their first values in the literature for this Centaur. Upper limits for CH4, C2H6, CH3OH, and H2CO are the most stringent reported to date, and are most similar to values found in ultra CO-rich Oort cloud comet C/2016 R2 (PanSTARRS), which may have implications for how ices are preserved in cometary nuclei. We demonstrate the su- perb synergy of coordinated radio and near-infrared measurements, and advocate for future small body studies that jointly leverage the capabilities of each wavelength.
DOI: 10.48577/jpl.u5daph
title: Secondary gas in debris discs released by the decay of long-lived radioactive nuclides, catastrophic and resurfacing collisions

description: Kuiper-like belts of planetesimals orbiting stars other than the Sun are most com- monly detected from the thermal emission of small dust produced in collisions. Emis- sion from gas, most notably CO, highlights the cometary nature of these planetesimals. Here we present models for the release of gas from comet-like bodies in these belts, both due to their thermophysical evolution, most notably the decay of long-lived radioac- tive nuclides and collisions, including catastrophic and gentler resurfacing collisions. We show that the rate of gas release is not proportional to the rate of dust release, if non-catastrophic collisions or thermal evolution dominate the release of CO gas. In this case, care must be taken in inferring the composition of comets. Non-catastrophic collisions dominate the gas production at earlier times than catastrophic collisions, depending on the properties of the planetesimal belt. We highlight the importance of the thermal evolution of comets, including crucially the decay of long-lived radioactive nuclides, as a source of CO gas around young (&lt; 50Myr) planetary systems, if large (10-100s kms) planetesimals are present.
DOI: 10.48577/jpl.zxv5q7
title: Rotation measure variations in Galactic Centre pulsars

description: We report the results of an observational campaign using the Effelsberg 100-m telescope of the pulsars J1746−2849, J1746−2850, J1746−2856 and J1745−2912 located in the Central Molecular Zone (CMZ) close to the Galactic centre in order to study rotation measure (RM) variations. We report for the first time the RM value of PSR J1746−2850 to be −12300 ± 160 rad m^-2. All pulsars show significant variations of RM of 300 − 400 rad m^-2 over the course of months to years that suggest a strongly magnetized environment. The structure function analysis of the RM of PSR J1746−2850 revealed a shallow power-law index of 0.43 ± 0.07 comparable to the value expected for two dimensional turbulence. This pulsar also showed large dispersion measure (DM) variation of ∼ 50 pc cm−3 in an event lasting a few months where the RM increased by ∼ 200 rad m−2. The large difference in RM between PSR J1746−2849 and PSR J1746−2850 despite the small angular separation reveals the presence of a magnetic field of at least 70 𝜇G in the CMZ and can explain the lack of polarization in the radio images of the region. These results contribute to our understanding of the magnetic field in the CMZ and show similarities between the RM behaviours of these pulsars and some fast radio bursts (FRBs).
DOI: 10.48577/jpl.1nid5y
title: Investigating Europa’s Radiation Environment with the Radiation Monitor

description: We present an overview of the radiation environment monitoring program planned for the Europa Clipper mission. The harsh radiation environment of Jupiter will be measured by a dedicated Radiation Monitor (RadMon) subsystem, yielding mission accumulative Total Ionizing Dose (TID) and instantaneous electron flux measurements with a 1-Hz cadence. The radiation monitoring subsystem is comprised of a stand-alone sensor assembly along with distributed TID assemblies at various locations on the spacecraft. The sensor assembly itself is made of a TID sensor stack using the Metal-Oxide Semiconducting Field-Effect Transistor (MOSFET) and a Charging Rate Monitor (CRM) that uses a stack of bulk charge collection plates. The TID measurements will provide the critical information about the overall radiation levels relevant to the degradation of electronics over time and the electron flux data can serve as a proxy for the Internal ElectroStatic Discharge (IESD) environment by measuring the &gt;~1 MeV electron environment. In addition, the radiation monitoring subsystem data will be augmented by serendipitous radiation data from science instruments onboard. This will be made possible by careful modeling and analysis of opportunistic background data from the following instruments (as we envision now): Europa Imaging System (EIS), Europa-Ultraviolet Spectrograph (Europa-UVS), Mapping Imaging Spectrometer for Europa (MISE), MAss Spectrometer for Planetary EXploration (MASPEX), Plasma Instrument for Magnetic Sounding (PIMS), and SUrface Dust Analyzer (SUDA). Based on the current analysis, these instruments will be most sensitive to &gt; 1 MeV electrons. As such, the high-energy electron data obtained by the radiation monitoring subsystem will be qualitatively and quantitatively enhanced by the high-energy electron data acquired by the instruments. The holistic radiation monitoring program for the mission will be an extensive collaboration among many teams across the flight and payload systems. Although the radiation monitoring subsystem itself is an engineering resource for the mission, the collective data from the mission can be also used to improve the scientific understanding of the Jovian magnetosphere and the high-energy electron environment near Europa, where the motion of charged particles is perturbed by the local electromagnetic environment. The data will also help in understanding of the radiation modification of Europa surface compounds, which will subsequently help guide lab experiments to aid in understanding the origin and evolution of surface materials and in constraining the interpretation of observational data.
DOI: 10.48577/jpl.dztylp
title: A planetary collision afterglow and transit of the resultant debris cloud

description: Planets grow in rotating disks of dust and gas around forming stars, some of which can subsequently collide in giant impacts after the gas component is removed from the disk1–3. Monitoring programmes with the warm Spitzer mission have recorded substantial and rapid changes in mid-infrared output for several stars, interpreted as variations in the surface area of warm, dusty material ejected by planetary-scale collisions and heated by the central star: for example, NGC 2354–ID8 (refs. 4,5), HD 166191 (ref. 6) and V488 Persei7. Here we report combined observations of the young (about 300 Myr), solar-like star ASASSN-21qj: an infrared brightening consistent with a blackbody temperature of 1,000 K and a luminosity 4% of that of the star lasting for about 1,000 days, partially overlapping in time with a complex and deep, wavelength- dependent optical eclipse that lasted for about 500 days. The optical eclipse started 2.5 years after the infrared brightening, implying an orbital period of at least that duration. These observations are consistent with a collision between two exoplanets of several to tens of Earth masses at 2–16 au from the central star. Such an impact produces a hot, highly extended post-impact remnant with sufficient luminosity to explain the infrared observations. Transit of the impact debris, sheared by orbital motion into a long cloud, causes the subsequent complex eclipse of the host star.
DOI: 10.48577/jpl.lhvhwq
title: The second International Asteroid Warning Network Timing Campaign: 2005 LW3

description: The Earth close approach of near-Earth asteroid 2005 LW3 on 2022 November 23 represented a good93opportunity for a second observing campaign to test the timing accuracy of astrometric observation.94With 82 participating stations, the International Asteroid Warning Network collected 1046 observations95of 2005 LW3 around the time of the close approach. Compared to the previous timing campaign96targeting 2019 XS, some individual observers were able to significantly improve the accuracy of their97reported observation times. However, no broad, systematic improvement was achieved compared98to the previous campaign, with an overall negative bias persisting among the different observers.99The calibration of observing times and the mitigation of timing errors should be important future100considerations for observers and orbit computers, respectively.
DOI: 10.48577/jpl.vcflr5
title: Planetary Protection Knowledge Gap Closure Enabling Crewed Missions to Mars

description: As focus for exploration of Mars transitions from current robotic explorers to development of crewed missions, it remains important to protect the integrity of scientific investigations at Mars, as well as protecting the Earth’s biosphere from harmful effects. This is the discipline of planetary protection, and COSPAR (the Committee on Space Research) maintains the consensus international policy and guidelines on how this is implemented. In the early 2010s, COSPAR identified that, despite guidelines for crewed missions being in place, gaps in knowledge meant that a spacecraft designer could not design a crewed Mars exploration mission, based on current information, that would demonstrate compatibility with the intent of the Outer Space Treaty. Beginning in 2016, COSPAR then sponsored a multi-year interdisciplinary meeting series to address these planetary protection “knowledge gaps” (KGs) with the intent of refining the current robotic-focused Planetary Protection Policy to more adequately support the implementation of crewed exploration missions. This paper describes the outcome of the interdisciplinary COSPAR meeting series, to describe and address these KGs, as well as identify potential paths to gap closure. It includes the background scientific basis for each topic and knowledge updates since the meeting series. The paper includes a KG data table intended to be a point of departure for making future progress in developing an end-to-end planetary protection requirements implementation solution for a crewed mission to Mars.