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International audience; The data provided features all light curves from the 5 October 2017 event. The names of the files are the same names, in lower caps and with no spaces, that are presented in Figures C.1 and C.2. The first column of all files is the time in seconds, starting on 5 October 2017 00:00:00 UTC. The second column of all files is the normalised flux, where the unocculted flux oscillates around 1. (2 data files).

Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range ∼8 km to ∼190 km, corresponding to pressure levels from 9 μbar down to a few nanobars. Results. (i) A pressure of 1.18 ± 0.03 μbar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 μbar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude. ©

We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, mb = 30.8 ± 1.5Mpdbl, Rb = 4.7 ± 0.3 Rpdbl) located in the "hot Neptune desert". Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST-South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TÜBITAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (Teff = 3950 ± 51 K) with a mass of 0.59 ± 0.02Mpdbl and a radius of 0.58 ± 0.02Rpdbl. From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained. © ESO 2020., CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. Based on data from the CARMENES data archive at CAB (INTA-CSIC). We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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. Some of the observations in the paper made use of the High-Resolution Imaging instrument Zorro. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Zorro was mounted on the Gemini South telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigacion y Desarrollo (Chile), Ministerio de Ciencia, Tecnologia e Innovacion (Argentina), Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work makes use of observations from the LCOGT network. This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sanchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This paper is also based on observations made in the Observatorios de Canarias del IAC with the Nordic Optical Telescope operated on the island of La Palma by NOTSA in the Observatorio del Roque de los Muchachos. Data were partly obtained with the MONET/South telescope of the MOnitoring NEtwork of Telescopes, funded by the Alfried Krupp von Bohlen und Halbach Foundation, Essen, and operated by the Georg-August-Universitat Gottingen, the McDonald Observatory of the University of Texas at Austin, and the South African Astronomical Observatory. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration 2018). We acknowledge financial support from the Spanish Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the European FEDER/ERF funds through projects AYA2015-69350-C3-2-P, PGC2018098153-B-C31/C33, AYA2016-79425-C3-1/2/3-P, AYA2018-84089, BES-2017080769, ESP2016-80435-C2-1/2-R, ESP2017-87676-C5-1/2/5-R, Instituto de Astrofisica de Andalucia (SEV-2017-0709), the Generalitat de Catalunya through CERCA programme, the UK Science and Technology Facilities Council through grant ST/P000592/1, the JSPS KAKENHI through grants 17H04574, JP18H01265, and 18H05439, and the JST PRESTO through grant JPMJPR1775, the "la Caixa" INPhINIT Fellowship Grant LCF/BQ/IN17/11620033 for Doctoral studies at Spanish Research Centres of Excellence, V.M.P. acknowledges support from NASA Grant NNX17AG24G, Support for this work was provided to J.K.T. by NASA through Hubble Fellowship grant HST-HF2-51399.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation (SNF). M.G. and E.J. are FNRS Senior Research Associates. S.D. acknowledges support from the Deutsche Forschungsgemeinschaft under Research Unit FOR2544 "Blue Planets around Red Stars", project no. RE 281/32-1. M.Z. acknowledges support from the Deutsche Forschungsgemeinschaft under DFG RE 1664/12-1 and Research Unit FOR2544 "Blue Planets around Red Stars", project no. RE 1664/14-1. M.S. was supported by the DFG Research Unit FOR2544 "Blue Planets around Red Stars", project no. RE 2694/4-1. I.J.M.C. and E.M. acknowledge support from the National Science Foundation through grant AST-1824644. B.B. thanks the European Research Council (ERC Starting Grant 757 448-PAMDORA) for their financial support. D.D. acknowledges support from NASA through Caltech/JPL grant RSA-1006130 and through the TESS Guest Investigator Program Grant 80NSSC19K1727. P.P. acknowledges support from NASA (16-APROBES16-0020 and the Exoplanet Exploration Program) and the National Science Foundation (Astronomy and Astrophysics grant 1716202), the Mt Cuba Astronomical Foundation, and George Mason University start-up and instructional equipment funds. The NASA Infrared Telescope Facility is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration. M.R.K is supported by the NSF Graduate Research Fellowship, grant No. DGE 1 339 067. M.Y. and H.V.S. thank to TUB.ITAK for a partial support in using T100 telescope with project number 19AT100-1474. J.N.W. thanks the Heising-Simons Foundation for support. D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379), and the National Science Foundation (AST-1 717 000). T.D. acknowledges support from MIT's Kavli Institute as a Kavli postdoctoral fellow. This work made use of tpfplotter (developed by J. Lillo-Box, which also made use of the python packages astropy, lightkurve, matplotlib and numpy. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Finally, we thank the referee for detailed and helpful comments.

We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V=11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 +/- 0.078 Mjup planet in a grazing transit configuration with an impact parameter of b = 1.17 +0.10/-0.08. As a result the radius is poorly constrained, 2.03 +0.61/-0.49 Rjup. The planet's distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Qs' = 10^7 - 10^9. We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 +/- 0.13 Mjup and a radius of 1.29 +/- 0.02 Rjup. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V=12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V=12.4 G-type star. It has a mass of 0.79 +/- 0.06 Mjup and a radius of 1.09 +0.08/-0.05 Rjup. Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe/H] ranging from 0.18 - 0.24., Published in A&A

We present the discovery and characterisation of two transiting planets observed by the Transiting Exoplanet Survey Satellite (TESS) orbiting the nearby (d∗ ≈ 22 pc), bright (J ≈ 9 mag) M3.5 dwarf LTT 3780 (TOI-732). We confirm both planets and their association with LTT 3780 via ground-based photometry and determine their masses using precise radial velocities measured with the CARMENES spectrograph. Precise stellar parameters determined from CARMENES high-resolution spectra confirm that LTT 3780 is a mid-M dwarf with an effective temperature of Teff = 3360 ± 51 K, a surface gravity of log g∗ = 4.81 ± 0.04 (cgs), and an iron abundance of [Fe/H] = 0.09 ± 0.16 dex, with an inferred mass of M∗ = 0.379 ± 0.016M· and a radius of R∗ = 0.382 ± 0.012R·. The ultra-short-period planet LTT 3780 b (Pb = 0.77 d) with a radius of 1.35-0.06+0.06 R·, a mass of 2.34-0.23+0.24 M·, and a bulk density of 5.24-0.81+0.94 g cm-3 joins the population of Earth-size planets with rocky, terrestrial composition. The outer planet, LTT 3780 c, with an orbital period of 12.25 d, radius of 2.42-0.10+0.10 R·, mass of 6.29-0.61+0.63 M·, and mean density of 2.45-0.37+0.44 g cm-3 belongs to the population of dense sub-Neptunes. With the two planets located on opposite sides of the radius gap, this planetary system is anexcellent target for testing planetary formation, evolution, and atmospheric models. In particular, LTT 3780 c is an ideal object for atmospheric studies with the James Webb Space Telescope (JWST).

Variants of the same process may be encountered in different organizations, e.g., any municipality will have a process to handle building permits. New paradigms such as Software-as-a-Service (SaaS) and Cloud Computing stimulate organizations to share a BPM infrastructure. The shared infrastructure has to support many processes and their variants. Dealing with such large collections of similar process models for multiple organizations is challenging. However, a shared BPM infrastructure also enables cross-organizational process mining. Since events are recorded in a unified way, it is possible to cross-correlate process models and the actual observed behavior in different organizations. This paper presents a novel approach to compare collections of process models and their events logs. The approach is used to compare processes in different Dutch municipalities. Keywords: cross-organizational process mining – software-as-a-service – process model collections – configurable process models

Streams of research are emerging that emphasize the advantages of using declarative process modeling languages over more traditional, imperative approaches. In particular, the declarative modeling approach is known for its ability to cope with the limited flexibility of the imperative approach. However, there is still not much empirical insight into the actual strengths and the applicability of each modeling paradigm. In this paper, we investigate in an experimental setting if either the imperative or the declarative process modeling approach is superior with respect to process model understanding. Even when task types are considered that should better match one or the other, our study finds that imperative process modeling languages appear to be connected with better understanding.

Introduction - Satisfying the growing demand for agricultural products while improving N input efficiency in Mediterranean cereal systems (Hochman et al., 2013) will require significant change in cropping systems structure and management. Our hypothesis, developed from the concepts of eco-efficiency (Keating et al., 2010) is that it is possible to obtain a better compromise between production and resource efficiency by adopting transformational technologies, such as changing genotype or by temporal and/or spatial diversification of crops. In this study, the hypothesis is tested on rotation as a temporal complexification of a cereal system structure. We addressed the following question: does crop rotation allow for a better trade-off between nitrogen efficiency and yield of Durum wheat in farmers conditions and how far can it compensate for the reduction of area allocated to wheat? Materials and Methods - We introduced in the efficiency analysis two intermediate variables between nitrogen supply and grain yield in order to establish a four-quadrant diagram (Fig 1). Nitrogen uptake was used, on the right of this diagram, to separate the efficiencies of resource capture and resource conversion (De Wit, 1992). On the left, N-efficiency was introduced as intermediate variable, in order to visualize trade-offs between efficiencies and production or input. In each quadrant we established boundary curves which represent the maximum achievable performances (yield, N uptake, N efficiency) when the input (here N fertilizer) is the only limiting factor. This framework has been tested on 432 “agronomic situations” (climatic year, previous crop and N rate) of Durum wheat in farmers' fields representative of the diversity of farmers practices in four regions of Tunisia. Results and Discussion - Nitrogen capture by Durum wheat is benchmarked against boundary curves that represent achievable nitrogen uptake when nitrogen supply is the only limiting factor (Fig 1.A).These boundary curves were significantly different according to the preceding crop. The highest achievable N absorbed was found for irrigated wheat grown after vegetables (CM_Dwi), followed by rainfed wheat grown after legumes (LG_Dwr). In contrast, the lowest achievable N absorbed was found for rainfed wheat in a cereal-wheat rotation (CE_Dwr), revealing the poor N-capture potential of rotation sequences based on cereals only. Our method of estimation of N absorbed (Fig 1.B) does not allow discussion of the effect of the preceding crop on the efficiency of N conversion into grain but experimental data showed that this factor does not break the proportionality of yield to N absorbed. The equations of boundary curves of quadrants A and B allowed us to establish the trade-off curves between N efficiency and an objective of grain production (Fig 1.C) or of N fertilizer use (Fig 1.D). They show that in cereal-based systems of Tunisia high N efficiency can be obtained but only with low level of fertilization and grain yield. Changing the preceding crop into legume does not change this tendency but creates a new efficiency frontier which allows both an increase in Yield and N efficiency (Fig 1.C), especially if the level of N fertilizer used on this area has to be limited for environmental purposes (Fig 1.D). In irrigated systems, where wheat is grown after vegetable, these shifts in the efficiency frontiers are sufficiently high to compensate for the reduction of Durum wheat area in a 3 years rotation, especially at low level of N fertilization. Conclusions - This four quadrant framework allows to combine process-based (right part) and design oriented (left part) analysis of food production vs. resource use in cropping systems, making use of easy to access data in farmers fields. It showed the breakthrough which can be obtained in high production-low N input cereal-based systems through crop diversification and irrigation. Nevertheless the level and frequency of N absorption efficiency gaps for each preceding crop suggest that there are other crop management factors to be taken into account in farmers' fields.

Conference of 9th Workshop on Verification and Evaluation of Computer and Communication Systems, VECoS 2015 ; Conference Date: 10 September 2015 Through 11 September 2015; Conference Code:115655; International audience; Model checking is an effective technique for uncovering subtle errors in concurrent systems. Unfortunately, the state space explosion is the main bottleneck in model checking tools. Here we propose a state space reduction technique for model checking concurrent programs written in C. The reduction technique consists in an analysis phase, which defines an approximate agglomeration predicate. This latter states whether a statement can be agglomerated or not. We implement this predicate using a syntactic analysis, as well as a semantic analysis based on abstract interpretation. We show the usefulness of using agglomeration technique to reduce the state space, as well as to generate an abstract TLA+ specification from a C program.

T3. Crop modeling and yield gap analysis for agricultural systems analysis and design; International audience; In most Mediterranean regions, durum wheat yield is variable with time and location, depending on several factors, primarily water and nitrogen supply (Boussen et al., 2005). Nitrogen (N) is one of the most important nutrients applied as a fertilizer and responsible to a great extent for the large yields obtained from high input agriculture (Latiri, 1998). However, the increased use of N fertilizer can affect farmers' margins, causes excessive losses to the environment and make agriculture dependent of non-renewable energy. The simultaneous increase in both yield and N-efficiency is at the core of eco-efficient agriculture which targets efficient and sustainable use of resources in agricultural production and land management (Keating et al., 2010). It adds to the concept of ecological intensification (Cassman, 1999), the hypothesis of eco-efficiency frontiers that are determined by the genetic nature or by the agrobiodiversity of the cropping systems. This study aims to analyze the efficiency of nitrogen supply on durum wheat and its drivers in different regions in Tunisia and try to identify eco-efficiency frontiers, associated with constrasting rotation sequences. We addressed the following question: Can higher yields and greater N-efficiency be expected in wheat-based cropping systems by diversifying rotation sequences?

Substitution is fundamental to computer science, underlying for example quantifiers in predicate logic and beta-reduction in the lambda-calculus. So is substitution something we define on syntax on a case-by-case basis, or can we turn the idea of ‘substitution’ into a mathematical object? We exploit the new framework of Nominal Algebra to axiomatise substitution. We prove our axioms sound and complete with respect to a canonical model; this turns out to be quite hard, involving subtle use of results of rewriting and algebra.

The paper deals with automatic reconfiguration problems of distributed control systems that are composed of a group/set of networked reconfigurable devices. A multi-agent architecture is proposed such that each device of a distributed control system has a special self-governed agent named reconfiguration sub controller agent to manage its local reconfiguration. Accordingly a communication protocol is developed to handle interaction style among these agents for the purpose of consistency.The proposed architecture is modeled by RECATNets and the distributed reconfiguration process is modeled by an ECATNet. Furthermore, in order to check the correctness of the proposed approach, the model checker Maude is applied, where required properties are specified by Linear Temporal Logic. Finally, a virtual distributed control system contains two reconfigurable devices is applied to illustrate this work.

When multiple similar business processes must be designed, a trade-off is necessary between designing a single, standardized, process or designing multiple, specific, processes. Standardization, on the one hand, helps to benefit from re-use of resources and to reduce redundancy. Specificity, on the other hand, helps to tailor the processes to specific needs. The activity of deciding on this trade-off is called harmonization. This paper operationalizes the notion of process harmonization, identifies aspects that determine harmonization and defines metrics to determine the level of harmonization. Furthermore, it presents the factors that influence the level of harmonization that can be achieved in a company. The harmonization aspects and factors are extracted from case studies in practice. Together the metrics, aspects and factors can be used to determine the current and optimal level of harmonization for a company.

A real-life event log, taken from a Dutch Academic Hospital, provided for the BPI challenge is analyzed using process mining techniques. The log contains events related to treatment and diagnosis steps for patients diagnosed with cancer. Given the heterogeneous nature of these cases, we first demonstrate that it is possible to create more homogeneous subsets of cases (e.g., patients having a particular type of cancer that need to be treated urgently). Such preprocessing is crucial given the variation and variability found in the event log. The discovered homogeneous subsets are analyzed using state-of-the-art process mining approaches. More specifically, we report on the findings discovered using enhanced fuzzy mining and trace alignment. A dedicated preprocessing ProM plug-in was developed for this challenge. The analysis was done using recent, but pre-existing, ProM plug-ins. The high-level view of our approach is depicted in Fig. 1. [Figure omitted] Using this approach we are able to uncover many interesting findings that could be used to improve the underlying care processes.