cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.48577/jpl.v2f7au
title: Perseverance’s Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) Investigation

description: The Scanning Habitable Environments with Raman and Luminescence for Organics and Chemicals (SHERLOC) is an arm-mounted instrument on NASA’s Perseverance rover. SHERLOC has two primary boresights, the Spectroscopy boresight generates spatially resolved chemical maps using fluorescence and Raman spectroscopy coupled to microscopic images (10.1 microns/pixel) and the second boresight is a Wide Angle Topographic Sensor for Operations and eNgineering (WATSON); a reflight of the MAHLI camera on Mars Science Laboratory (MSL) which obtains color imaging from microscopic scales (~13 micron/pixel) to infinity. SHERLOC Spectroscopy focuses a deep UV, 248.6 nm, Neon-Copper, 40 µs pulsed laser source to a ~100 micron spot onto a target at a working distance of ~48 mm. Fluorescence emissions from organics and Raman scattered photons from organics and minerals are spectrally resolved with a single diffractive grating spectrograph with a spectral range from 250 to ~370 nm. Since the fluorescence and Raman regions are naturally separated with deep UV excitation (&lt;250 nm), the Raman region ~ 800 – 4000 cm-1 (250 to 273 nm) and the fluorescence region (274 to ~370 nm) are acquired simultaneously without time gating or additional mechanisms. SHERLOC science is enabled using an Autofocus Context Imager (ACI) to obtain focus and acquire 10.1 micron/pixel greyscale images. Chemical maps of organic and mineral signatures are enabled using an internal scanning mirror that moves the focused laser spot across the target surface. The high resolution images, and the &lt;100 micron chemical maps will enable the first in situ view of the distribution and interaction between organics, minerals, and chemicals to assess potential biogenicity. Single arm placement chemical maps can be up to 7x7 mm in area and with the &lt; 10 min acquisition time per map, larger mosaics are possible with arm movements. This microscopic view of the organic geochemistry of a sample at the Perseverance landing site, when combined with the other instruments, such as Mastcam-Z, PIXL and SuperCam, will enable unprecedented analysis of surface targets for both scientific research and for identifying samples that should be cached for sample return.
DOI: 10.48577/jpl.3eqbqw
title: Draft Genome Sequences of Enterobacteriales Isolated from the International Space Station

description: The whole-genome sequences (WGS) of 26 strains isolated from the International Space Station (ISS) were generated and identified as being part of the Order Enterobacteriales. Characterization of these WGS would enable the identification of potential pathogenic bacteria that have been adapting to the space environment.
DOI: 10.48577/jpl.qdsrqn
title: Future exploration of Ceres as an ocean world

description: After 2 years in orbit around Ceres, the Dawn spacecraft, in the last phase of its extended mission (June-October 2018), reached closer to Ceres’ surface, down to 35 km, and performed imaging, infrared spectroscopy, elemental spectroscopy, and gravity science at resolutions never achieved before at an icy body1. The focus was on Occator crater, a ~20-million-year old crater revealed earlier in the mission to be a site of recent evaporite exposure (faculae), primarily as sodium carbonate spread over &gt;100 km2 2. This discovery raised a debate in the community as to whether that activity could stem from a deep brine layer or from melt produced as a result of heat generated by the impact that created the crater, or both. Liquids from an impact melt chamber and evolve on different timescales than those from deeper (&gt;40 km) reservoirs: the former would start warm as a result of impact heat, up to 100oC, but freeze over a few million years because of its close proximity to the surface. On the other hand, a perennial brine layer could be maintained by the presence of salts at sub-zero temperature if it were deep enough for internal heat to slowly leak through a thick crust.
DOI: 10.48577/jpl.1lswax
title: Estimating and Removing the Sampling Biases of the AIRS Obs4MIPs V2 Data

description: The Atmospheric Infrared Sounder (AIRS) Observations for Model Intercomparison Projects (Obs4MIPs) Version 2 (V2) monthly mean tropospheric air temperature, specific humidity and relative humidity data designed for climate model evaluation in the context of the Coupled Model Intercomparison Project (CMIP) have been publicly available at Earth System Grid Federation (ESGF) data centers since 2018. Due to the limitations of the Aqua satellite orbit and the AIRS retrieval algorithm, the AIRS Ob4MIPs V2 data are not sampled on the regular spatial and temporal grids like the climate model outputs. The resulting sampling biases of the AIRS Obs4MIPs V2 data from the sampling difference between the AIRS Ob4MIPs V2 data and climate model outputs can be large for certain cases and have to be considered when the AIRS Obs4MIPs V2 data are compared to the climate model outputs for climate model evaluation. We have estimated the sampling biases of the AIRS Obs4MIPs V2 data based on the fifth generation of the European Centre for Medium-Range Weather Forecasts (ECMWF) reanalysis (ERA5) and published them at the ESGF data centers. This sampling bias dataset is intended for users who wish to compare the AIRS Obs4MIPs V2 data with the climate model outputs for climate model evaluation to account the sampling difference between the AIRS and climate model data. This paper documents this sampling bias dataset in terms of its motivation, description, processing methodology, validation, and the issues to be considered for climate model evaluation.
DOI: 10.48577/jpl.5bdmiy
title: Phoebe's Differentiated Interior from Refined Shape Analysis

description: Context. Phoebe is an irregular satellite of Saturn and its origin, either between the orbits of the giant planets or from the Kuiper Belt, is still uncertain. The extent of dierentiation of its interior can potentially help inform its formation location because it is mainly determined by heat from 26-aluminum. The internal structure is reflected in the shape, assuming the body is relaxed to hydrostatic equilibrium. Although previous data analysis indicates Phoebe is close to hydrostatic equilibrium, heavily cratered surface makes it dicult to tease out the low-order shape characteristics. Aims. This paper aims to extract Phoebe’s global shape from the observations returned by the Cassini mission for comparison with uniform and stratified interior models under the assumption of hydrostatic equilibrium. Methods. The global shape is derived from fitting spherical harmonics and keeping only the low degree harmonics that represent the shape under the heavily crater surface. The hydrostatic theoretical model for shape interpretation is based on the Clairaut equation developed to order 3 (although 2 is sucient in this case). Results.We show that Phoebe is dierentiated with a mantle density between 1900 and 2400 kg/m3. The presence of a porous surface layer further restricts the fit with the observed shape. This result confirms the earlier suggestion that Phoebe accreted with sucient 26-aluminium to drive at least partial dierentiation, favoring an origin with C-type asteroids
DOI: 10.48577/jpl.93jfiw
title: Virtual IR Sensing for Planetary Rovers: Improved Terrain Classification and Thermal Inertia Estimation

description: Abstract—Terrain classification is critically important forMars rovers, which rely on it for planning and autonomous navigation.On-board terrain classification using visual informationhas limitations, and is sensitive to illumination conditions.Classification can be improved if one fuses visual imagery withadditional infrared (IR) imagery of the scene, yet unfortunatelythere are no IR image sensors on the current Mars rovers. Avirtual IR sensor, estimating IR from RGB imagery using deeplearning, was proposed in the context of a MU-Net architecture.However, virtual IR estimation was limited by the fact thatslope angle variations induce temperature differences within thesame terrain. This paper removes this limitation, giving good IRestimates and as a consequence improving terrain classificationby including the additional angle from the surface normal to theSun and the measurement of solar radiation. The estimates arealso useful when estimating thermal inertia, which can enhanceslip prediction and small rock density estimation. Our approachis demonstrated in two applications. We collected a new dataset to verify the effectiveness of the proposed approach andshow its benefit by applying to the two applications.
DOI: 10.48577/jpl.aepikj
title: Gas and dust dynamics in starlight-heated protoplanetary disks

description: Theoretical models of the ionization state in protoplanetary disks suggest the existence of large areas with low ionization and weak coupling between the gas and magnetic fields. In this regime hydrodynamical instabilities may become important. In this work we investigate the gas and dust structure and dynamics for a typical T Tauri system under the influence of the vertical shear instability (VSI). We use global 3D radiation hydrodynamics simulations covering all 360◦ of azimuth with embedded particles of 0.1 and 1 mm size, evolved for 400 orbits. Stellar irradiation heating is included with opacities for 0.1- to 10-μm-sized dust. Saturated VSI turbulence produces a stress-to-pressure ratio of α ≃ 10^−4. The value of α is lowest within 30 au of the star, where thermal relaxation is slower relative to the orbital period and approaches the rate below which VSI is cut off. The rise in α from 20 to 30 au causes a dip in the surface density near 35 au, leading to Rossby wave instability and the generation of a stationary, long-lived vortex spanning about 4 au in radius and 40 au in azimuth. Our results confirm previous findings that mm size grains are strongly vertically mixed by the VSI. The scale height aspect ratio for 1 mm grains is determined to be 0.037, much higher than the value H/r = 0.007 obtained from millimeter-wave observations of the HL Tau system. The measured aspect ratio is better fit by non-ideal MHD models. In our VSI turbulence model, the mm grains drift radially inwards and many are trapped and concentrated inside the vortex. The turbulence induces a velocity dispersion of ∼ 12 m/s for the mm grains, indicating that grain-grain collisions could lead to fragmentation.
DOI: 10.48577/jpl.fzbls4
title: Teleportation Systems Towards a Quantum Internet

description: Quantum teleportation is essential for many quantum information technologies including long-distance quantum networks. Using fiber-coupled devices, including off-the-shelf optics and state-of-the-art low-noise superconducting nanowire single photon detectors, we achieve quantum teleportation of time-bin qubits at the telecommunication wavelength of 1536.5 nm. We measure teleportation fidelities of $\geq90$\% that are consistent with an analytical model of our system, which includes realistic imperfections. To demonstrate the compatibility of our setup with deployed quantum networks, we teleport qubits over 22 km of single-mode fiber while transmitting qubits over an additional 22 km of fiber. Our system, which is compatible with emerging solid-state quantum devices, is a foundation for a high-fidelity quantum internet with practical devices.
DOI: 10.48577/jpl.4s2wug
title: Numerical investigation of mechanisms underlying oceanic internal gravity wave power-law spectra

description: We consider the power-law spectra of internal gravity waves in a rotating and stratified ocean. Field measurements have shown considerable variability of spectral slopes compared to the high-wavenumber high-frequency portion of the Garrett-Munk (GM) spectrum. Theoretical explanations have been developed through wave turbulence theory (WTT), where different power-law solutions of the kinetic equation can be found depending on the mechanisms underlying the nonlinear interactions. Mathematically, these are reflected by the convergence properties of the so-called collision integral (CL) at low and high frequency limits. In this work, we study the mechanisms in the formation of the power-law spectra of internal gravity waves, utilizing numerical data from the high-resolution modeling of internal waves (HRMIW) in a region northwest of Hawaii. The model captures the power-law spectra in broad ranges of space and time scales, with scalings w^-2.05+/-0.2 in frequency and m^-2.58+/-0.4 in vertical wavenumber. The latter clearly deviates from the GM76 spectrum but is closer to a family of induced-diffusion-dominated solutions predicted by WTT. Our analysis of nonlinear interactions is performed directly on these model outputs, which is fundamentally different from previous work assuming a GM76 spectrum. By applying a bi-coherence analysis and evaluations of modal energy transfer, we show that the CL is dominated by non-local interactions between modes in the power-law range and low-frequency inertial motions. We further identify induced diffusion and the near-resonances at its spectral vicinity as dominating the formation of power-law spectrum.
DOI: 10.48577/jpl.l8ytev
title: Observed temperature changes in the troposphere and stratosphere from 1979 to 2018

description: Temperature observations of the upper-air atmosphere are now available for more than 40 years for both ground- and satellite-based observation systems. Recent years have seen substantial improvements in long-standing discrepancies between data sets through major reprocessing efforts. The advent of GNSS radio occultation observations in 2001 has led to further improvements in vertically-resolved temperature measurements, enabling a detailed analysis of upper troposphere/lower stratosphere trends. This paper presents the current state of atmospheric temperature trends from the latest available observation records. We analyze observations from merged operational satellite measurements, radiosondes, lidars, and GNSS radio occultation, spanning a vertical range from the lower troposphere to the upper stratosphere. The focus is on assessing climate trends and their significance, and on identifying the degree of consistency between the different observational systems. Results show a robust cooling of the stratosphere of about 2–3 K, and a robust warming in the troposphere of about 0.6–0.8 K over the last four decades. Consistent results are found between the analyzed satellite-based layer average temperatures and vertically-resolved radiosonde records. The overall latitude-altitude trend patterns are found to be consistent between GNSS RO and radiosonde records. Significant warming of the troposphere is clearly revealed in the GNSS RO measurements with trends of 0.25–0.35 K per decade in this shorter time period. The enhanced consistency of the latest upper-air data sets will help to improve our understanding of climate changes and their drivers and underlines the need for sustaining long term climate data records of essential climate variables
DOI: 10.48577/jpl.vsqovj
title: Accelerating Applications for Planned NASA Satellite Missions: A New Paradigm of Virtual Hackathons during a Pandemic and in the Post-Pandemic Era

description: While the primary mission of NASA’s Earth Science Division (ESD) is to develop a scientific understanding of the Earth System and how it is responding to human and natural drivers of change, an implicit need is also to understand how best to promote the use of NASA satellite mission products and information for application activities that directly benefit society and our environment. In fact, the 2018 National Academies on Science, Engineering and Medicine Decadal Survey for NASA, “Thriving on Our Changing Planet: A Decadal Strategy for Earth Observations from Space,” clearly underscores the tremendous value of satellite mission data, which “enabled societal applications that provide tremendous value to individuals, businesses, the nation, and the world. Such applications are growing in breadth and depth, becoming an essential information infrastructure element for society as they are integrated into people’s daily lives (NASEM, 2018).”The NASA Applied Sciences Program (ASP) was set up to empower people around the world to use NASA satellite data to solve relevant problems by providing support and funding to institutions and individuals to make better decisions. To maximize the value of satellite data for planned missions, NASA ASP has developed a pre-launch protocol called the Early Adopter Program (EAP) for engaging with the broader user community (Brown and Escobar, 2019). In the vision of the EAP, each selected EA proposes an activity for the use of planned satellite data using either proxy datasets or simulated data that mimics the anticipated mission during the post-launch era. EAs are defined as those groups and individuals who will have a potential or clearly defined need for data from the planned mission, and who are planning to apply their own resources to demonstrate the utility of planned satellite mission data for their application, system, or model. Experience from recently-launched satellite missions such as Soil Moisture Active and Passive (SMAP) has shown that the sooner this pre-launch engagement begins and is sustained, the better are the outcomes on the use of mission data beyond the declared goals of scientific query and data generation (Escobar et al., 2016).
DOI: 10.48577/jpl.zcrljo
title: Starshade Rendezvous: Exoplanet Sensitivity and Observing Strategy

description: Launching a starshade to rendezvous with the Roman Space Telescope would provide the first opportunity to directly image the habitable zones of nearby sunlike stars in the coming decade. A report on the science and feasibility of such a mission was recently submitted to NASA as a probe study concept (Seager et al. 2019). The driving objective of the concept is to determine whether Earth-like exoplanets exist in the habitable zones of the nearest sunlike stars and have biosignature gases in their atmospheres. With the sensitivity provided by this telescope, it is possible to measure the brightness of zodiacal dust disks around the nearest sunlike stars and establish how their population compares to our own. In addition, known gas-giant exoplanets can be targeted to measure their atmospheric metallicity to determine if the correlation with planet mass follows the trend observed in the Solar System and hinted at by exoplanet transit spectroscopy data. In this paper we provide the details of the calculations used to estimate the sensitivity of Roman with a starshade and provide the Python-based source code. Given the fixed capability of Roman and the constrained observing windows inherent for the starshade, we calculate the sensitivity of the combined observatory to detect these three types of targets and we present an overall observing strategy that enables us to achieve the objectives.
DOI: 10.48577/jpl.absm5d
title: Characteristics of Pluto’s haze and surface from an analytic radiative transfer model

description: Observations of Pluto from New Horizons have been combined with previous ground-based observations and fit to a radiative transfer model to derive the physical properties of the dwarf planet’s surface and atmosphere. We derive the macroscopic roughness, single scattering albedo, and directional scattering properties of the surface, and the single scattering albedo, optical depth, and single scattering phase function of Pluto’s haze. The haze particles are small, and some constraints can be put on their size. We find that Pluto’s haze is similar to that of Titan, rich in organic compounds, and unlike that of Triton. With organic compounds and a likely subsurface water ocean, Pluto may harbor sustainable habitable environments. Our model, which includes the coherent backscatter effect, fits the anomalously large opposition surge recently discovered on Pluto (Buratti et al. 2019b).
DOI: 10.48577/jpl.lll2t6
title: The CatWISE2020 Catalog

description: The CatWISE2020 Catalog consists of 1,890,715,640 sources over the entire sky selected from WISE and NEOWISE survey data at 3.4 and 4.6 μm (W1 and W2) collected from 2010 Jan. 7 to 2018 Dec. 13. This dataset adds two years to that used for the CatWISE Preliminary Catalog (Eisenhardt et al. 2020), bringing the total to six times as many exposures spanning over sixteen times as large a time baseline as the AllWISE catalog. The other major change from the CatWISE Preliminary Catalog is that the detection list for the CatWISE2020 Catalog was generated using crowdsource (Schlafly et al. 2019), while the CatWISE Preliminary Catalog used the detection software used for AllWISE. These two factors result in roughly twice as many sources in the CatWISE2020 Catalog. The scatter with respect to Spitzer photometry at faint magnitudes in the COSMOS field, which is out of the Galactic plane and at low ecliptic latitude (corresponding to lower WISE coverage depth) is similar to that for the CatWISE Preliminary Catalog. The 90% completeness depth for the CatWISE2020 Catalog is at W1=17.7mag and W2=17.5mag, 1.7mag deeper than in the CatWISE Preliminary Catalog. From comparison to Gaia, CatWISE2020 motions are accurate at the 20 mas yr−1 level for W1∼15 mag sources, and at the ∼ 100masyr−1 level for W1∼17mag sources. This level of precision represents a 12× improvement over AllWISE. The CatWISE catalogs are available in the WISE/NEOWISE Enhanced and Contributed Products area of the NASA/IPAC Infrared Science Archive.
DOI: 10.48577/jpl.03auap
title: Habitability Models for Astrobiology

description: Abstract: Habitability has been generally defined as the capability of an environment to supportlife. Ecologists have been using Habitat Suitability Models (HSMs) for more than four decades tostudy the habitability of Earth from local to global scales. Astrobiologists have been proposingdifferent habitability models for some time, with little integration and consistency betweenthem and different in function to those used by ecologists. Here we review and compare thedifferent models used by ecologists and astrobiologists and suggest how they might beintegrated into new standards. Such standards will help to improve the comparison andcharacterization of potentially habitable environments, prioritize target selections, and studycorrelations between habitability and biosignatures. Habitability models are the foundation ofplanetary habitability science and the synergy between ecologists and astrobiologists isnecessary to expand our understanding of the habitability of Earth, the Solar System, and extrasolar planets.
DOI: 10.48577/jpl.o2yiaa
title: NASA’s starshade technology development activity

description: NASA is developing starshade technology to Technology Readiness Level 5 within a directed activity called S5. The objective of S5 is to mature starshade technology to the level that exoplanet imaging missions such as Starshade Rendezvous and HabEx can begin the formulation phase. This article outlines the S5 activity as whole, to show how it closes all starshade technology gaps in a mutually consistent way. It serves as a companion article to several other articles in this special issue that report progress in specific starshade technologies.
DOI: 10.48577/jpl.vo5zbt
title: A Decade with VAMDC: Results and Ambitions

description: The paper is an overview of the current status of the VAMDC e-infrastructure that is addressed through the description of the latest updates of the VAMDC connected (or to be connected) databases, through an update on the latest technological developments within the infrastructure, through a visibility on some application tools that make use of the VAMDC e-infrastructure. We analyse the past and current impact of the VAMDC initiative not only in the field of atomic and molecular physics, but also in the field of data management at the international level. Finally we address various issues not currently solved by VAMDC, but that will be investigated in the future.