dataesr/scientific-paragraphs-categorization huggingface dataset:
, 2020; Hossain et al. , 2022). The SWOT EA program has also been able to grow consistently because of the continuous support from the partnering space agency of France (CNES), NASA and their respective agency data archives of record for the SWOT mission. In other words, the SWOT EAP has been able to increase the user-readiness of SWOT data in anticipation of mission launch for the broader application community. This pro-active and sustained engagement approach is the hallmark of the EAP seeking to maximize the return in public investments of global satellite missions. Detailed information on the SWOT mission on application-related activities and SWOT Early Adopter projects can be found at http://swot. jpl. nasa. gov/applications. For a more comprehensive overview of SWOT application activities and EA projects, the reader is referred to http://depts.
Conclusion We are aware that the current stage of building user-readiness via the SWOT EAP and the anticipated scientific breakthroughs and societal applications during the initial years after launch may not be a sufficient guarantee for SWOT mission continuity demanded by end users. There are many other factors beyond the control of the scientific community for each satellite Earth mission. However, we are maximizing our chances for mission success through the Early Adopter program, inspired by age old adage-"By failing to prepare you are preparing to fail. " Planned Earth-observing satellite missions today require proactive and sustained engagement with a broad user community that spans the spectrum of scientific research and practitioner end-user needs if the mission is to hit the ground running when data becomes publicly available.
Doing so will also allow us to realize the full potential of SWOT observations in the longer-term. SWOT is a pathfinder mission, not officially an operational one-no other satellite has ever collected similar data globally on water. The sooner the community exploits and demonstrates the societal impact of such novel data, the better position the community will be to argue for future mission continuity beyond its nominal life span. Hence, the EA program can play a major role in describing and quantifying the societal benefits of new pathfinder missions such as SWOT to various governing bodies that decide the fate of future missions. The SWOT Early Adopter program represents the start of what is possible through sustained and continuous engagement with the stakeholder community through training, workshops, hackathons and collaborative learning in tandem with mission planning and development.
Experimental Section Thin film deposition: Polycrystalline La2NiO4+δ (L2NO4) thin films were synthesized by PI-MOCVD. [34, 42]   a(tmhd) Instrumentation: To identify the phase and evaluate the structural crystal quality of the samples, X-ray diffraction was performed in a 5-circle Rigaku Smartlab diffractometer. GI-XRD was used to enhance the diffraction signal from the polycrystalline films and minimize the signal of the silicon-based substrates. The study of surface morphology was carried out by SEM in a SEM FEG ZEISS GeminiSEM 300. To investigate the film roughness, AFM images were performed using AFM D3100 Veeco Instrument in tapping mode with a Si3N4 tip probe. The chemical film composition was analyzed by EPMA using a CAMECA SX100 spectrometer. Each film was measured at two different acceleration voltages: 12 keV and 16 keV and the data analysis was done by Strategem software.
Acknowledgements This work was partially supported by the  LabEx Minos   ANR-10-LABX-55-01  (for K. K. ) and by the  ANR  funded project " MICROSWITCH"  ( ANR-14-ACHN-0012 ). This research has benefited from characterization equipment of the Grenoble INP -CMTC platform supported by the  Centre of Excellence of Multifunctional Architectured Materials  " CEMAM" n°ANR-10-LABX-44-01  funded by the  "Investments for the Future" Program. The authors acknowledge  Rachel Martin  and  Florence Robault  ( CMTC-Consortium des Moyens Technologies Communs, Grenoble INP, France ) for the EPMA analysis. Part of this work, carried out on the Platform for Nanocharacterisation (PFNC), was supported by the " Recherches Technologiques de Base" program  of the  French National Research Agency (ANR). In addition, this work has been performed with the help of the " Plateforme Technologique Amont " in Grenoble, with the financial support of the " Nanosciences aux limites de la Nanoélectronique" Fundation" and CNRS Renatech network.
Introduction Reflectance spectroscopy is a nondestructive technique that is widely used to remotely investigate the mineralogical composition of rocks and, more generally, planetary surfaces. Spectral libraries are the main references used to interpret these spectra and assess the mineralogical composition of the analyzed surface. It is therefore crucial for databases to include: (a) well-documented samples, in particular through additional analyses with techniques complementary of reflectance spectroscopy and (b) samples that share characteristics with the rock samples of unknown composition being measured with reflectance spectroscopy. This includes the elemental and mineralogical composition of the sample, but also its physical properties such as grain size, surface roughness, and porosity, which are known to greatly affect the absolute reflectance values and band depths (e.
g. ,  Clark & Roush, 1984). Especially, it has been demonstrated that rocks have different spectral signatures compared to particulate surfaces (e. g. ,  Carli et al. , 2015; Harloff & Arnold, 2001; Pompilio et al. , 2007). While the spectra of a wide range of minerals of various compositions are well documented in the current databases, most of these measurements were performed on powders, with a majority of them being pure or nearly pure mineral phases (e. g. ,  Kokaly et al. , 2017). The complex effects of grain size, roughness, or impurities on natural rocks reflectance have been approached in the literature (e. g. ,  Carli & Sgavetti, 2011; Carli et al. , 2015; Clark & Roush, 1984; Harloff & Arnold, 2001) , but well-documented rock spectra are nonetheless needed for the planetary science community in order to fully understand the spectral behavior of planetary surfaces.
MANDON ET AL. 10. 1029/2021EA001871 2 of 14 rocks and soils, which are complex mixtures of various mineralogical phases: a comparison with well-documented rock spectra would improve the interpretation of these surface measurements. The main spectral libraries including measurements of intact rocks are the Reflectance Experiment Laboratory facility (RELAB;  Pieters & Hiroi, 2004)  and the database of the Centre for Terrestrial and Planetary Exploration (C-TAPE, formerly known as HoserLab;  Cloutis et al. , 2006). In particular, a fraction of the rocks measured at the C-TAPE facility is associated with mineralogical and elemental compositions, but at the time of writing of this manuscript, photographs showing the corresponding measurement spots were not provided in any of the databases. The Solid Spectroscopy Hosting Architecture of Databases and Expertise (SSHADE;  Schmitt et al.
, 2014 ) also provides some spectral measurements of intact rocks in the visible and infrared, but they comprise a minor fraction of the database. Finally, the more recent Planetary Terrestrial Analogs Library Project (PTAL) is being built with Martian whole-rock analogs characterized with various techniques already used on the Martian surface and including reflectance spectroscopy  (Dypvik et al. , 2021). However, all of the samples were ground prior to the reflectance measurements  (Lantz et al. , 2020). In this contribution, we present the ROMA (ROck reflectance for MArtian in situ exploration) database, which regroups a set of spectral measurements between 0. 4 and 3-4 μm on intact and particulate rocks-most of them have had their mineralogy characterized using X-ray diffraction (XRD) on ground samples.
This collection currently includes a set of terrestrial samples with various degrees of alteration, Martian meteorites, as well as synthetic mixtures of minerals detected over the landing sites and compacted into solid pellets. The latter are not perfect analogs to simulate rock textures, but expand the spectral library of nonparticulate materials that are relevant to planetary exploration. The reflectance spectra of these samples are provided, along with higher-level data, such as continuum-removed spectra and absorption band parameters, which are mostly influenced by rock composition, grain size, porosity, and roughness. Comparisons with this database will aid the interpretation of reflectance measurements performed on the Martian surface.
The ROMA Database The sample and spectral information in ROMA are regrouped into an SQLite database in which three tables are connected: a table that contains the sample information and two tables of reflectance and XRD data that either include VNIR spectra or diffractograms of these samples, measurement conditions, and higher-level data (Figure  1 ). In the following sections, each table is presented in details, along with the list of samples included in the database and the methodology employed to obtain the VNIR spectra and diffractograms of the samples.
Samples As of the beginning of 2021, the ROMA database documents the VNIR spectra of 27 Martian meteorites and 132 Mars analog samples: 64 terrestrial rocks and 68 unique synthetic pellets. When grinding was possible, reflectance spectra were acquired on powdered samples in addition to the ones acquired on unprocessed rocks. To ensure agreement between the powder (both used for XRD and reflectance observation) and the intact rock measurements, homogeneous areas of the rocks were considered, both for the reflectance acquisition on the chip and for sampling of the area to be crushed for powder preparation. A measurement area was considered representative of the rock when including all the apparent features used for a first-level description (e. g. , the presence of a groundmass, phenocrysts, vein, etc.
Martian Meteorites The reflectance spectra of 27 Martian meteorites are included in the database: 18 shergottites, five nakhlites, one chassignite, as well as the unique specimens of the augite-rich basalt NWA 8159, the polymict breccia NWA 7034 and the orthopyroxenite ALH 84 001. Most of these precious and rare samples are chips of rocks and were not ground to perform whole-rock XRD measurements; however, their mineralogical and chemical compositions are well documented in the literature (e. g. ,  Beck et al. , 2006; Herd et al. , 2017; Sautter et al. , 2002). A study dedicated to the investigation and interpretation of the spectral features of their reflectance spectra was performed by  Mandon et al. (2021a). MANDON ET AL.
Terrestrial Rocks The terrestrial rocks present in the database were collected in the geological collections of the Observatoire de Lyon or during field campaigns and come from various locations in France. Many geological units potentially of magmatic origin are identified at the Mars 2020 and ExoMars landing sites (e. g. ,  Goudge et al. , 2015; Quantin-Nataf et al. , 2021). Most of these units exhibit the spectral signatures of mafic minerals, such as pyroxene and olivine  (Goudge et al. , 2015; Hoefen et al. , 2003). More globally, spectral measurements on meteorites and from orbit indicate that the Martian crust is dominantly of basaltic composition (e. g. ,  McSween et al. , 2009). However, minerals enriched in silica are usually difficult to detect using VNIR spectroscopy  (Crown & Pieters, 1987 ) and evolved lithologies have been observed in situ while not being detected from orbit  (Sautter et al.
, 2015). Consequently, most of the igneous rocks present in the database are basaltic rocks, but in order to account for the potential presence of evolved rocks on the landing sites, a wider range of lithologies (e. g. , andesite, trachyte, dacite) has been investigated (Table  1 ). Both rocks that exhibit aphanitic and phaneritic textures are present in the suite, meaning that rocks with various grain sizes are included in the library. In addition to these igneous rocks, the library includes sedimentary samples, mineralized veins, or rocks in which the primary texture has been lost or strongly modified by alteration. The majority of these samples are paleosols (i. e. , rocks altered by pedogenesis processes). They were sampled during two field campaigns: 1. rocks with name starting with "SL" were sampled on various levels of altered basaltic flows in Loire and Velay, France.
For exact location of sampling and outcrop photographs, the reader is referred to  Mandon (2020)  and to the database website, which can be accessed at http://roma/univ-lyon1. fr 2. rocks with name starting with "R" or "S" were sampled in the "Ocres de Roussillon," France, on sedimentary rocks altered by pedogenesis  (Guennelon, 1962)  Figure  1. Current architecture of ROMA. The database is divided into three main tables: the "Sample," "Reflectance," and "X-ray diffraction (XRD)" tables. Each table includes a variety of fields that can either contain an integer, some text, or a binary object (e. g. , an image). The black key indicates an entry that is unique in the table, while the gray keys point to fields inherited from the "Name" field of the "Sample" table, meaning that each unique sample can be associated with multiple reflectance and XRD measurements.
Synthetic Pellets In addition to terrestrial and Martian rocks, our database also includes the reflectance spectra of synthetic samples of simplified composition and mineralogy that are directly comparable to those estimated on the Mars 2020 and ExoMars landing sites from orbit. As ROMA is a database focused on the reflectance of rocks (as opposed to powders), mixtures of pure minerals were compressed into solid pellets (Figure  3b ). These samples are not perfect analogs to mimic rock textures, but are here used to evaluate the spectral properties of mixtures in a medium with reduced porosity and compacted grains. The mixed samples were selected based on their relevance for the Martian sites explored (see Section 3) and their mineralogical purity, estimated with XRD (see Section 2. 3). Three types of mixtures analog to the landing sites were produced (Table  1 ):   (Mandon et al.
, 2021c ) 2. olivine (forsterite) mixed with Mg-carbonate (magnesite) and serpentine (antigorite), assemblage likely present in the region of the Mars 2020 landing site  (Ehlmann et al. , 2008 (Ehlmann et al. , , 2009;; Hoefen et al. , 2003)  3. montmorillonite mixed with kaolinite, assemblage likely present in the region of the Mars 2020 and ExoMars landing sites  (Carter et al. , 2016; Ehlmann et al. , 2009). These two samples are well characterized natural standards from the Clay Minerals Society (e. g. ,  Chipera & Bish, 2001; Moll, 2001)  Diffractograms acquired on powders of the samples used in the mixtures are available in the database (see Section 2. 3). Reflectance measurements on mineral mixtures have already been performed for similar species (e. g. ,  Bishop et al. , 2013; McKeown et al.
VNIR Reflectance Spectra The ROMA database includes the calibrated reflectance spectra of the samples ("calibrated spectrum" field) along with measurement information and associated errors (Figure  1 ; see  Potin et al. , 2018 on errors). Higher-level data are also provided: smoothed spectra corrected from recurring artifacts ("corrected spectrum" field), continuum-removed spectra and quantitative parameters of the main absorption bands (Figure  1 ).
Spectral Acquisition The VNIR reflectance of every sample in the ROMA database was measured between 0. 4 and 3-4 μm at a spectral sampling of 10 or 20 nm and with a varying spectral resolution (on the order of 10 nm) by the Spectrophotometer with cHanging Angles for the Detection Of Weak Signals (SHADOWS;  Potin et al. , 2018). This setup provides the possibility of varying the geometry of illumination and observation, whose parameters are the incidence, emergence, and azimuth angles, following the convention described by  Potin et al. (2018). The incidence angle is the angle between the normal to the surface and the incident beam and the emergence angle is the angle between the normal to the surface and the direction of observation. The azimuth is the angle between the plane defined by the normal to the surface and the incident beam, and the plane defined by the normal to the surface and the direction of observation.
SNR and Main Artifacts The SHADOWS point spectro-goniometer is able to measure the reflectance of a sample in the VNIR down to 0. 005% in reflectance, with 1% accuracy and with varying illumination and emergence angles  (Potin et al. , 2018). This high sensitivity allows excellent signal-to-noise ratio (SNR), usually exceeding 100-1,000 in the VNIR range for most of the rocks measured, which hence permits the detection of absorption bands at a 0. 1-1% precision relative to the spectral continuum. While, the SNR values are usually higher than 100-1,000 over the whole spectral range, they can be lower in the case of dark samples. The near-infrared detector produces data with SNR one to three orders lower than in the case of the visible detector and an SNR drop corresponding to the detector switch is observed at 1 μm.
XRD Characterization of the Samples In order to estimate the mineralogical assemblages of the samples, whole-rock X-ray diffraction (XRD) analyses were performed at the Centre de Diffractométrie Henri Longchambon. The XRD technique requires grinding of a few tens of grams for each sample. Diffractograms were acquired in the 3-70° 2θ range using a Bruker D8 Advance Bragg-Brentano diffractometer (40 kV/40 mA Cu tube) with variable divergence slits and using the Cu K α radiation, at 0. 0205° 2θ step and 0. 4-s time step. The diffractograms analysis was carried out using the DIFFRAC. EVA software suite. A peak comparison with the PDF-4 database allowed phase identification and semiquantification with the Reference Intensity Ratio (RIR) method  (Hubbard & Snyder, 1988). Semiquantification on whole-rock analysis is time-efficient and allows the investigation of a large collection of samples, but can lead to large uncertainties in the quantification results, especially if phyllosilicate peaks are present.
Potential Applications to Martian Measurements ROMA aims at providing an additional framework for future comparisons with in situ measurements performed on the Martian surface by VNIR spectrometers. The specificity of the database is to provide spectra measured on whole-rocks, both intact and ground to powder, as well as synthetic mixtures of Martian analogs, and to include XRD measurements as well as absorption band parameters (e. g. , position, depth), which are information that are meaningful in terms of mineralogical assemblage. A comparison with the band parameters values might be helpful for estimating the composition of a Martian target of unknown nature. MANDON ET AL. 10. 1029/2021EA001871 10 of 14 Figure  4  illustrates how particulate and intact rock samples of the same material can behave very differently.
Analogy to the Mars 2020 and ExoMars Landing Sites The Mars 2020 and ExoMars rovers both carry near-infrared reflectance spectrometers that operate or will operate on the surface of Mars. In terrestrial laboratories, samples to be analyzed by VNIR spectrometers are usually ground into fine powders to homogenize the sample and increase the signal values. This step will not be achieved on the surface of Mars by the two rovers, where natural, unprocessed surfaces will be observed-or roughly crushed rocks in the case of ExoMars' MicrOmega imaging spectrometer  (Bibring et al. , 2017). Our database is focused on compact rock spectra, providing a physical state analogy between terrestrial and Martian samples to be analyzed. The Perseverance rover of the Mars 2020 mission has landed on Mars in 2021 and will investigate for the upcoming years Jezero crater and the Nili Planum region, which from orbit exhibit very diverse mineralogical assemblages  (Ehlmann et al.
, 2008 (Ehlmann et al. , , 2009;; Goudge et al. , 2015; Mustard et al. , 2007; Scheller & Ehlmann, 2020; Tarnas et al. , 2019). Various samples from the ROMA database exhibit similarities with Jezero crater and Nili Planum, either spectrally or based on the rock type inferred to be present on the sites. In particular, the olivine-bearing bedrock which widely outcrops in the region  (Hoefen et al. , 2003; Mandon et al. , 2020)  shows evidence of alteration into Mg-carbonate and serpentine  (Ehlmann et al. , 2008 (Ehlmann et al. , , 2009)). The ROMA spectra of olivine, magnesite, and serpentine mixtures would allow the investigation of the first-order relative proportion of these minerals in the field of view. The various dark and crater-retaining units possibly interpreted as volcanic in Jezero crater and Nili Planum might be analogous to some volcanic rocks of the database.
In particular, of interest for the comparison with the Jezero floor unit, multiple samples from our database exhibit the strong absorption bands typical of pyroxene-bearing rocks (mostly Martian meteorites), which have been detected from orbit over this unit  (Goudge et al. , 2015; Horgan et al. , 2020). Most of the other unaltered igneous rocks included in ROMA show less prominent spectral absorptions, and could be relevant for a comparison with the other potential volcanic units of the region from which no spectral features could be clearly identified from orbit  (Mustard et al. , 2007; Quantin-Nataf et al. , 2018). The ExoMars landing site Oxia Planum is a hundred of kilometers-wide plateau, where the main geological units identified from orbit are a stratified and fractured basement enriched in Fe/Mg-clay minerals (vermiculite or iron-saponite being the best spectral match), some deltaic deposits with a signature of opaline silica, as well as a spectrally muted dark resistant unit whose origin has been interpreted as potentially volcanic  (Carter et al.
, 2016; Quantin-Nataf et al. , 2021). In particular,  Mandon, Parkes Bowen, et al. (2021)  showed that the clay-bearing unit exhibits a spectral signature consistent with a mixture of olivine in addition to the clay minerals. The mixtures of vermiculite and olivine from the ROMA database provide an analogy with these clay-bearing deposits at Oxia Planum, which are the main targets of the mission and are the most common types of exposures at the site  (Quantin-Nataf et al. , 2021). The various mixing ratios included in the database would provide a framework for the estimation of the olivine versus clay mineral proportions. In addition, pedogenesis was proposed by  Carter et al. (2016)  as one of the main mechanisms of basement alteration to explain the widespread occurrence of clay minerals at Oxia Planum.
Phase Detectability and Band Depth/Mineralogical Proportion Relationship The spectra of natural rocks included in ROMA can be used to study the complex effects of mineralogical mixtures and surface state and their implications on the interpretation of planetary surfaces reflectance spectra. In particular, the following effects are observed: 1. in the igneous rock data set, a considerable amount of rocks are estimated as relatively fresh: XRD analysis might reveal the presence of minor secondary minerals, but these rocks do not exhibit a visible/evident physical or chemical alteration and rather display an undisturbed texture with the prevalence of igneous minerals. However, these rocks often exhibit reflectance spectra dominated by the spectral features of alteration minerals (e. g. , UCB18), similarly to highly altered samples.