dataesr/scientific-paragraphs-categorization huggingface dataset:
From a single dataset, it allows to generate as many configurations as needed without requiring access to the scanner, which may be limited in terms of device and radiotracer availability. In addition, it can be applied directly to clinical data in order to evaluate impacts of acquisition and reconstruction parameter on patient examination  [14, 15]. We intend to employ this method to support the physical and clinical evaluation phase of a new PET-CT device as part of the collaborative research partnership with the manufacturer. Our final objective is to extend our simulation method to patient data in order to evaluate the impact of small lesions with low activity on clinical images while keeping control over the inserted object (location, size, activity, shape and pattern). Computation times for generating sinograms were significantly shorter than reconstruction times.
Similarly, the growth in data-driven decisionmaking has generated an array of governance-related management challenges and issues (Connolly-Barker 2020; Tooby 2019). Furthermore, in the field of logistics, new e-commerce infrastructures are simplifying and superseding extant systems hardware, software and networks, thereby reducing costs and shifting specialist capabilities away from centralised technologists to end users and managers via cloudbased software (Financial Times 2021a). Therefore, it should be noted that what already constituted a dynamic and rich socio-technical situation has now been rendered increasingly complex with the advent of the COVID-19 pandemic impacting all areas of the population. Nevertheless, it is important to underline the technological deterministic dimensions at play, namely, that it is not simply the implementation of a technological innovation that delivers performance but rather the interaction of human beings with technology that effectively (co-)creates such changes  (Boyd and Holton 2018).
2020). Citing evidence of workers being simultaneously empowered and enslaved by technology, scholars argue that the demarcation between work and domestic life is becoming increasingly blurred (Norgate and Cooper 2020;  Palm et al. 2020). Here again, the COVID-19 pandemic has acted as a catalyst and accelerated changes to the work-life balance  (Anwer 2020). This shift is underlined by, for example, the experience of Microsoft which estimates that the daily use of its MSTeams TM and 365 TM software collaboration tools increased from 20 million individuals in November 2019 to 115 million by November 2020 (Microsoft 2020). Microsoft believes that its contribution will lead to an Internet-enabled evolution requiring 'synchronous and asynchronous' 365 TM powered tools to underpin the notion of a digital portal for the workplace (Financial Times 2021b).
Data collection The researchers developed an exploratory semi-structured questionnaire intended to discover individual interpretations, attitudes and beliefs and to provide a more comprehensive view of social processes (McGuirk and O'Neill 2016). The inclusion of qualitative questioning enabled the researchers to undertake an interpretive individualism approach to reveal previously undiscovered phenomena and unique insights  (Eckerdal and Hagstr€ om 2017). The questionnaire was developed to explore the views of the respondents in alignment with the research constructs drawn from the literature review (De Vaus 2014). It incorporated five open questions to: elicit the views of the respondents concerning their experience of using technology for work during the pandemic; identify the perceived impact of remote working on well-being and resilience upon themselves and their staff; and, signal potential technological influences on future practice, career progression and work-life balance.
Drawing from the modelling of an urban project in Paris with ENVI-met software (Section 3), we simulate the various effects of UHI-oriented urban interventions adopted on that site (Section 4). We expand this first simulation beyond the already planned interventions and test a larger set of possible solutions to provide a hierarchy of possible interventions for healthy urban planning, whose aim is to lower UHI and thus enhance the liveability of some urban projects (Section 5). The various possibilities of urban interventions are then further discussed in terms of urban arbitrages (Section 6).
The LCZ method, developed by  Stewart and Oke (2012) , is used to identify the UHI intensity based on a defined set of properties on already existing territories. It rests on the idea that certain "types" of urban configurations display similar thermal behaviours. This approach is considered a fairly quick method that gives an idea of the UHI intensity without the use of computational simulations, and consequently informs urban decisionmaking processes  (Lensholzer, 2015). ENVI-met is a three-dimensional simulation software that forecasts the impact of urban interventions on the surrounding environment and takes into account an array of different indicators, which explains its growing use in academic articles  (Crank et al. , 2018; Simon et al. , 2018). In this project, ENVI-met is being used to quantify the cooling effect of different solutions that can be implemented in an urban setting.
8. In the eighth area, asphalt is replaced by deactivated concrete with stone inlay. The methodological protocol followed a two-step approach. First, the case study (as is and with the planned interventions) was simulated with meteorological data that depicts a heat wave that previously hit Paris in 2018. The simulated period spans three days, with a maximum temperature of 37. 3 °C, a minimum temperature of 21 °C, and a mean temperature of 29. 3 °C. ENVI-met was used to model, simulate, and analyse the gathered data. The mean radiant temperature (MRT) and potential air temperature (PAT) indicators were chosen to measure the intensity of UHI. The MRT is a heuristic indicator, as it highlights thermal radiant exchanges of surfaces in the thermal environment  (Kántor & Unger, 2011). Second, we expanded simulations to other types of interventions that were not planned for this site, regardless of their potential financial constraints.
2018 ) and Kepler-644 b  (Berger et al. 2018). This paper presents the discovery and characterisation of the intermediate-sized planet TOI-2196 b (TIC 372172128. 01) in the hot Neptune desert discovered by The Transiting Exoplanet Survey Satellite (TESS;  Ricker et al. 2015)  in 2020. Following the discovery, our international KESPRINT 2  collaboration performed follow-up radial velocity observations of this planet candidate to confirm the planetary nature and determine its mass. The star's equatorial coordinates together with other basic parameters are listed in Table  1. We present the observations in Sect. 2 and the data analysis in Sect. 3. In Sect. 4, we discuss the hot Neptune desert,  (a) (mas yr -1 ) -20. 168 ± 0. 013 T eff (b) (K) 5634 ± 31 M ⋆ (b) (M ⊙ ) 1. 032 ± 0. 038 R ⋆ (b) (R ⊙ ) 1.
TESS photometry Figure  1  shows a 3 ′ × 3 ′ image from the Digitized Sky Survey 2 (DSS2) centered on TIC 372172128 (TOI-2196), marked with a cyan circle. TOI-2196 was observed by TESS 3  in sector 13, during the primary mission, and in sector 27 in the first set of observations of the TESS extended mission. The outline of the Science Processing Operations Center (SPOC) photometric aperture of sector 27 is overplotted in black in Fig. 1 , while the red circles mark the positions of Gaia DR2 sources within 2 ′ from the target. The photometric dilution from other sources is negligible and adjusted for by the pipeline. TOI-2196 was observed in sector 13 with camera 2 in full-frame images at a cadence of 30 min from 19 June to 17 July 2019. The observations of sector 27 spanned the interval 5 July through 30 July 2020, with a gap in the middle of approximately one day, when the data were being downloaded.
This produced 23. 35 days of science data at 2-min cadence, including 14 transits of TIC 372172128 monitored with camera 2, CCD 1. Due to the combination of the short period of the planet (1. 2 days) and the long cadence in sector 13, the planet candidate TOI-2196. 01 was not discovered orbiting its G-type host star until it was observed in sector 27 at a 2-min cadence and processed by SPOC at NASA Ames Research Center  (Jenkins et al. 2016). A search of the sector 27 data with an adaptive, wavelet-based matched filter  (Jenkins 2002; Jenkins et al. 2010 Jenkins et al. , 2020a) )  identified the transit signature of TOI-2196 b just above the detection threshold at 7. 2 σ. The data validation reports (DVR;  Twicken et al. 2018; Li et al. 2019 ) process fit a limbdarkened transit model with a signal-to-noise ratio (S/N) of 9.
2, a period of 1. 1954 days, a duration of 1. 6 h, and a transit depth of 1127 ppm, corresponding to a preliminary planet radius of ∼3. 5 R ⊕. We independently detected the transit signal using the DST  (Cabrera et al. 2012 ) pipeline and found a planet candidate with an orbital period of 1. 19387 ± 0. 00043 days and a transit depth of 1359 ± 147 ppm. We downloaded the light curves processed by the SPOC pipeline from the Mikulski Archive for Space Telescopes (MAST 4  ) and used the Pre-search Data Conditioning Simple Aperture Photometry (PDCSAP) data. This was generated by the pipeline by identifying and correcting the SAP flux for instrumental signatures using cotrending basis vectors drawn from the light curves of an ensemble of quiet and highly temporally correlated stars long-term trends, thus resulting in a cleaner data set with fewer systematics  (Stumpe et al.
2014; Jenkins et al. 2020a). In order to remove any remaining low-frequency signals in preparation for the modelling described in Sect. 3. 3, we further detrended the light curve by applying a Gaussian Process (GP). This was achieved using the package citlalicue 5 (e. g. Georgieva et al. 2021; Barragán et al. 2022a ), a PYTHON wrapper of george (Foreman-Mackey et al. 2014) and pytransit  (Parviainen 2015). We masked out the transits of the planet and applied a squared exponential covariance function as well as a 5 σ clipping algorithm to remove outliers. Figure  2  displays both the PDCSAP data in sector 27 with the GP model overplotted, and the detrended normalised light curve. The latter is subsequently used in the joint transit and RV analysis in Sect. 3. 3.
Radial velocity follow-up with HARPS We performed high-resolution (R ≈ 115 000) spectroscopic observations of TOI-2196 using the High Accuracy Radial velocity Planet Searcher (HARPS;  Mayor et al. 2003 ) spectrograph mounted at the ESO 3. 6 m telescope (La Silla observatory, Chile). We obtained a total of 41 spectra between 24 July 2021 and 12 November 2021 UT as part of our HARPS large program (ID: 106. 21TJ. 001, PI: Gandolfi). All RVs and activity indicators are listed in Table  A. 1 along with BJD TBD , exposure time, and S/N. We reduced the data with the dedicated HARPS data reduction software (DRS) available at the observatory  (Lovis & Pepe 2007 ) and extracted the radial velocity (RV) measurements using the code HARPS-TERRA (Anglada-Escudé & Butler 2012), which employs a template-matching algorithm to derive precise relative velocities.
We also extracted a variety of stellar activity and line profile variation indicators: the Hα and S-index were extracted using TERRA; the FWHM and the bisector inverse slope (BIS) were derived by cross-correlating the HARPS spectra with a G2 numerical mask  (Baranne et al. 1996; Pepe et al. 2002) ; and the differential line width (dLW) was extracted using the code SERVAL  (Zechmeister et al. 2018 ). A184, page 4 of 15 Method T eff log(g) [Fe/H] [Ca/H] [Mg/H] [Na/H] [Si/H] V sin i ⋆ (K) (dex) (cgs) (km s -1 ) SME (a) 5552 ± 85 4. 42 ± 0. 05 0. 14 ± 0. 05 0. 15 ± 0. 06 0. 18 ± 0. 09 0. 20 ± 0. 08 0. 15 ± 0. 08 2. 0 ± 0. 4 SpecMatch-Emp  5623 ± 110 4. 22 ± 0. 12 0. 18 ± 0.
Frequency analysis of HARPS data In order to search for the Doppler reflex motion induced by the transiting planet and unveil the presence of additional RV signals, we performed a frequency analysis of the HARPS RV measurements and activity indicators. To this aim, we computed the generalised Lomb-Scargle (GLS; Zechmeister & Kürster 2009) periodograms of the HARPS time series (shown in Fig. 4 ) and estimated the false alarm probabilities (FAPs) using the bootstrap technique described in  Kuerster et al. (1997). We considered a peak to be significant if its FAP is less than 0. 1%. The GLS periodogram of the HARPS RVs displays a significant peak at ν b = 0. 837 day -1 which is the transit frequency of TOI-2196 b (Fig. 4 , upper panel, thick vertical yellow line). This peak is not significantly detected in any of the activity indicators confirming the planetary nature of the transit signal found in the TESS light curve.
Stellar properties In order to derive the fundamental parameters of the host star, we analysed our co-added high-resolution HARPS spectra with two methods, the SpecMatch-Emp code  (Yee et al. 2017 ) and SME 7 (Spectroscopy Made Easy;  Valenti & Piskunov 1996; Piskunov & Valenti 2017). In particular, SpecMatch-Emp is an empirical code that compares observations of optical spectra to a dense library of well-characterised FGKM stars, while SME fits observed spectra to computed synthetic spectra for a chosen set of parameters based on atomic and molecular line data from VALD 8  (Ryabchikova et al. 2015 ) and a stellar atmosphere grid. We chose Atlas12  (Kurucz 2013 ) and derived the stellar effective temperature, T eff , the surface gravity, log g ⋆ , abundances, and the projected rotational velocity, V sin i ⋆.
Each parameter is modelled, one at a time, from specific spectral lines: the broad line wings of H α are particularly sensitive to T eff , and the line wings of the Ca I triplet 6102, 6122, and 6162 Å are sensitive to the surface gravity. Abundances and the projected stellar rotational velocity, V sin i ⋆ , were modelled from narrow and unblended lines between 6000 and 6600 Å. We held the micro-  (Bruntt et al. 2008 ) and macro-turbulent  (Doyle et al. 2014 ) velocities fixed to 1. 0 km s -1 , and 2. 8 km s -1 , respectively. Further details on the modelling can be found in  Fridlund et al. (2017)  and  Persson et al. (2018). Results from both models listed in Table  2  are in good agreement within the uncertainties and with the effective temperature from Gaia 9 DR2. We used the spectral parameters from SME as priors to model the stellar radius and mass with the python code ARIADNE 10 (Vines & Jenkins 2022).
The hot Neptune desert TOI-2196 b is one of very few planets found in the hot Neptune desert (shown in Fig. 9 ). In this figure, we plot in grey 14 https://gea. esac. esa. int/archive/documentation/GDR2/ Gaia_archive/chap_datamodel/sec_dm_main_tables/ssec_ dm_ruwe. html the radius of all known planets with radius measurements from transit surveys with a precision of 10% or better as a function of equilibrium temperature. About a third of the planets in Fig. 9  also have masses from RV measurements with a precision of 30% or better and are colour-coded with mass. The data were downloaded from the NASA Exoplanet archive 15  Notes. Table  5. Known sub-Neptune and Neptune planets in the hot Neptune desert (T eq > 1800 K) with a precision in radius of 10% or better. In addition to TOI-2196 b, three of the planets have RV measurements with a precision of 30% or better.
Acknowledgements. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the  NASA   Explorer Program. We acknowledge the use of public TESS data from pipelines at the  TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the  NASA   High-End Computing (HEC) Program  through the  NASA Advanced Supercomputing (NAS) Division at Ames Research Center  for the production of the SPOC data products. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by  NOIRLab through the Mid-Scale Innovations Program (MSIP). This work uses observations made with ESO 3. 6-m telescope at  La Silla Observatory  under programme ID  106. 21TJ. 001. We are grateful to the  ESO  staff members for their support during the observations, and to  François Bouchy  and  Xavier Dumusque  for coordinating the HARPS time sharing agreement.
This work has made use of SME package, which benefits from the continuing development work by  J. Valenti  and  N. Piskunov  and we gratefully acknowledge their continued support. (Kupka et al. 2000;Ryabchikova et al. 2015). to page 5 C. M. P. , M. F. , I. G. , and J. K. gratefully acknowledges the support of the  Swedish National Space Agency  ( DNR 65/19 ,  174/18 ,  177/19 ,  2020-00104 ). L. M. S and D. G. gratefully acknowledge financial support from the  CRT foundation  under Grant No. 2018. 2323"Gaseous or rocky?Unveiling the nature of small worlds". P. K. acknowledges support from grant  LTT-20015. E. G. acknowledges the support of the  Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale Gesellschaft. J. S. J. greatfully acknowledges support by  FONDECYT  grant  1201371  and from the  ANID BASAL  projects  ACE210002  and  FB210003.
H. J. D. acknowledges support from the  Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN)  under grant  PID2019-107061GB-C66 ,  DOI: 10. 13039/501100011033. D. D. acknowledges support from the  TESS Guest Investigator Program  grants  80NSSC21K0108  and  80NSSC22K0185. M. E. acknowledges the support of the  DFG priority program SPP 1992 "Exploring the Diversity of Extrasolar Planets " ( HA 3279/12-1 ). K. W. F. L. was supported by  Deutsche Forschungsgemeinschaft  grants  RA714/14-1  within the  DFG Schwerpunkt SPP 1992 , Exploring the  Diversity of Extrasolar Planets. N. N. acknowledges support from  JSPS KAKENHI  Grant Number  JP18H05439 ,  JST CREST  Grant Number  JPMJCR1761. M. S. I. P. is funded by  NSF.
I. INTRODUCTION V ISUAL Simultaneous Localization And Mapping (SLAM)   is an important problem for robotics that has been heavily studied in the past decade. Its goal is to estimate the pose of a camera moving in a scene while building a map of the environment. Some algorithms such as  [1] ,  [2]  can efficiently solve this problem, however they rely on the static scene assumption. This hypothesis assumes that the world is a single rigid body and thus that no object can move within it. This assumption, which is rarely met in most real world scenes, as they can contain moving objects (e. g. cars, bikes, pedestrians for urban scenes of the KITTI dataset), limits the scenarios in which a SLAM algorithm can be used. Classical SLAM systems such as  [1]  try to alleviate this assumption using robust estimators, allowing them to flag moving parts as outliers.
Our contributions presented in this paper are: • A semantic SLAM system that can robustly estimate the pose of a camera in static as well as dynamic scenes. • A stereo SLAM framework that can track multiple moving objects in the scene. • A new formulation for both the tracking and bundle adjustment that takes into account the characteristics of mechanical joints between objects in the scene to constrain their movements. We also evaluate our approach on several sequences from the public KITTI dataset and compare our approach quantitatively with respect to ORB-SLAM2  [1] , DynaSLAM  [3] , VDO-SLAM  [6]  and DynaSLAM II  [5] , which demonstrates the benefits of our method in terms of object poses and velocities and camera pose estimation accuracy. The rest of the paper is described as follows.
A. Experiments details Datasets. We evaluate our approach on the KITTI  [27]  tracking dataset which consists in multiple sequences recorded from a camera mounted on a car. This dataset is particularly interesting for our approach as it contains the ground truth for both the camera pose and for some objects poses such as vehicles. It should be noted that the segmentation network can yield an "unknown" class which we consider to be static, as the dynamic classes in the KITTI dataset (cars, bikes and pedestrians) are correctly segmented by the network. Metrics. The metrics for the evaluation of SLAM systems are usually the absolute translation error (ATE)  [28]  and the relative pose error (RPE)  [29]. For each sequence we report the translation and rotation parts of the RPE, as it is done by both VDO-SLAM and DynaSLAM2.
System under study The HPS under study is composed of different sources of energy, the solar PV power plant, and the wind farm, with pre-identified production profile. The battery stack and the static load are connected to the grid to form an RES-based HPS considered. The system model is developed in Matlab TM/Simulink allowing the visualization of the power flow and its overall dynamic behaviour of the voltage and current. The strategy of energy management allows the battery to either absorb or supply power. As shown in Figure  2 , the HPS under study is composed of: 1. Wind Power source: It is a plentiful, renewable, widely distributed energy having no emissions of green-house gas during the generation of electricity. However, the variability of wind power through hours, days and seasons remains a barrier to wider applications of such energy source.
To assist in the sustainable management of water resources, a groundwater model of the shallow groundwater in the Plaine du Nord-Massacre transboundary aquifer system was developed. The Plaine du Nord-Massacre Aquifer is one of the largest aquifer systems of Haiti, supposedly bearing a high potential for water supply and irrigation. The shallower part is already tapped by hundreds of domestic wells and hand-pumped public and private boreholes. In the framework of the AVANSE project (Appui à la Valorisation du Potentiel Agricole du Nord, pour la Sécurité Économique et Environnementale), a USAID funded project aiming at developing sustainable agriculture in the region, a groundwater model was built to assist in decision making. The finitedifference-based MARTHE software was used for the model.
This can represent complex multi-layer aquifer systems, with pinchouts and the occurrence of free surfaces in any layer. MARTHE addresses modelling of regional multi-layer systems covering several thousand square kilometres, as well as local-scale modelling of porous media systems down to a few cubic centimetres, with millimetre-size cells. It is especially designed to evaluate and manage groundwater resources. Finally, the MARTHE software presents all the functions necessary for modelling of the alluvial groundwater of the North Plain. In the MARTHE code, there is no concept of "confined layer", "unconfined layer" or "convertible layer". At any time, any cell can become confined, unconfined or dewatered, depending upon the current hydraulic head. The transmissivity is calculated from the hydraulic conductivity assigned to each mesh and the water height.
In the transient mode, MARTHE uses two storage coefficients: the storage coefficient in an unconfined state (equivalent to the effective porosity) when the cell is not fully saturated with water, and the confined storage coefficient when the cell is saturated with water. The MARTHE software includes a package that fully couples the groundwater flow calculation with the river network, as well as lakes and wetlands. Depending upon the relative position of the water level in the river and of the aquifer's groundwater level, water flows can be simulated from the river reach to the aquifer, or, inversely, from the aquifer to the river network. Such flow exchanges are controlled, in a nonlinear manner, by linking riverbed and banks proportionally to their surface area, thickness and hydraulic conductivity.