Search

Citizen science is a powerful analysis tool, capable of processing large amounts of data in a very short time. To bridge the gap between classification data products from web-based citizen science platforms to statistically robust signal significance scores, we present the Search Algorithm for Transits in the Citizen science Hunt for Exoplanets in Lightcurves (SATCHEL) pipeline. This open source, customizable pipeline was constructed to identify and assign significance estimates to one-dimensional features marked by volunteers. We describe the functional capabilities of the SATCHEL pipeline through application to features in photometric time-series data from the Kepler Space Telescope, classified by volunteers as part of the Planet Hunters citizen science project hosted on the Zooniverse platform. We evaluate the SATCHEL pipeline's overall performance based on recovery of known signals (both simulations and signals corresponding to official Kepler Objects of Interest) and relative contamination by spurious features. We find that, for a range of pipeline hyperparameters and with a reasonable score cutoff, SATCHEL is able to recover volunteer identifications of over 98% of signals from simulations corresponding to exoplanets $>2~R_\oplus$ in radius and about 85% of signals corresponding to the same size range of KOIs. SATCHEL is transparently adaptable to other citizen science classification datasets, and available on GitHub., 20 pages, 23 figures. Accepted for publication in MNRAS

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.--Full list of authors: Barragan, O.; Armstrong, D. J.; Gandolfi, D.; Carleo, I; Vidotto, A. A.; D'Angelo, C. Villarreal; Oklopcic, A.; Isaacson, H.; Oddo, D.; Collins, K.; Fridlund, M.; Sousa, S. G.; Persson, C. M.; Hellier, C.; Howell, S.; Howard, A.; Redfield, S.; Eisner, N.; Georgieva, I. Y.; Dragomir, D.; Bayliss, D.; Nielsen, L. D.; Klein, B.; Aigrain, S.; Zhang, M.; Teske, J.; Twicken, J. D.; Jenkins, J.; Esposito, M.; Van Eylen, V.; Rodler, F.; Adibekyan, V; Alarcon, J.; Anderson, D. R.; Murphy, J. M. Akana; Barrado, D.; Barros, S. C. C.; Benneke, B.; Bouchy, F.; Bryant, E. M.; Butler, R. P.; Burt, J.; Cabrera, J.; Casewell, S.; Chaturvedi, P.; Cloutier, R.; Cochran, W. D.; Crane, J.; Crossfield, I; Crouzet, N.; Collins, K., I; Dai, F.; Deeg, H. J.; Deline, A.; Demangeon, O. D. S.; Dumusque, X.; Figueira, P.; Furlan, E.; Gnilka, C.; Goad, M. R.; Goffo, E.; Gutierrez-Canales, F.; Hadjigeorghiou, A.; Hartman, Z.; Hatzes, A. P.; Harris, M.; Henderson, B.; Hirano, T.; Hojjatpanah, S.; Hoyer, S.; Kabath, P.; Korth, J.; Lillo-Box, J.; Luque, R.; Marmier, M.; Mocnik, T.; Muresan, A.; Murgas, F.; Nagel, E.; Osborne, H. L. M.; Osborn, A.; Osborn, H. P.; Palle, E.; Raimbault, M.; Ricker, G. R.; Rubenzahl, R. A.; Stockdale, C.; Santos, N. C.; Scott, N.; Schwarz, R. P.; Shectman, S.; Seager, S.; Segransan, D.; Serrano, L. M.; Skarka, M.; Smith, A. M. S.; Subjak, J.; Tan, T. G.; Udry, S.; Watson, C.; Wheatley, P. J.; West, R.; Winn, J. N.; Wang, S. X.; Wolfgang, A.; Ziegler, C.; KESPRINT Team., We present the discovery and characterization of two transiting planets observed by TESS in the light curves of the young and bright (V = 9.67) star HD73583 (TOI-560). We perform an intensive spectroscopic and photometric space- and ground-based follow-up in order to confirm and characterize the system. We found that HD73583 is a young (∼500 Myr) active star with a rotational period of 12.08 ± 0.11 d, and a mass and radius of 0.73 ± 0.02 M⊙ and 0.65 ± 0.02 R⊙, respectively. HD 73583 b (Pb = 6.3980420+0.0000067−0.0000062 d) has a mass and radius of 10.2+3.4−3.1 M⊕ and 2.79 ± 0.10 R⊕, respectively, which gives a density of 2.58+0.95−0.81 gcm−3⁠. HD 73583 c (Pc = 18.87974+0.00086−0.00074 d) has a mass and radius of 9.7+1.8−1.7 M⊕ and 2.39+0.10−0.09 R⊕, respectively, which translates to a density of 3.88+0.91−0.80 gcm−3⁠. Both planets are consistent with worlds made of a solid core surrounded by a volatile envelope. Because of their youth and host star brightness, they both are excellent candidates to perform transmission spectroscopy studies. We expect ongoing atmospheric mass-loss for both planets caused by stellar irradiation. We estimate that the detection of evaporating signatures on H and He would be challenging, but doable with present and future instruments. © The Author(s) 2022. Published by Oxford University Press on behalf of Royal Astronomical Society., This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions (http://www.kesprint.science). We thank the referee for their helpful comments and suggestions that improved the quality of this manuscript. 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 uses observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper is in part based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities Council (STFC) projects ST/M001962/1 and ST/S002642/1. This research has used 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. Some of the observations in the paper used the High-Resolution Imaging instrument Zorro obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. 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 North (and/or 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 Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). OB, BK, and SA acknowledge that this publication is part of a project that has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 865624). DG and LMS gratefully acknowledge financial support from the Cassa di Risparmio di Torino foundation under Grant No. 2018.2323 ‘Gaseous or rocky? Unveiling the nature of small worlds’. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). APH and ME acknowledges grant HA 3279/12-1 within the DFG Schwerpunkt SPP 1992, ‘Exploring the Diversity of Extrasolar Planets’. JS and PK would like to acknowledge support from MSMT grant LTT-20015. We acknowledges the support by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FISAST /28953/2017 & POCI-01-0145-FEDER-028953. AD acknowledges the financial support of the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). AD also acknowledges financial support of the the Swiss National Science Foundation (SNSF) through the National Centre for Competence in Research ‘PlanetS’. MF, IYG, JK, and CMP gratefully acknowledge the support of the Swedish National Space Agency (DNR 177/19, 174/18, 2020-00104, 65/19). FGC thanks the Mexican national council for science and technology (CONACYT, CVU-1005374). MS acknowledge financial support of the Inter-transfer grant no LTT-20015. JL-B acknowledges financial support received from ‘la Caixa’ Foundation (ID 100010434) and from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 847648, with fellowship code LCF/BQ/PI20/11760023. AAV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 817540, ASTROFLOW). JMAM is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1842400. JMAM acknowledges the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant No. 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. RAR is supported by the NSF Graduate Research Fellowship, grant No. DGE 1745301. RL acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52, and the Centre of Excellence ‘Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). PC acknowledges the generous support from Deutsche Forschungsgemeinschaft (DFG) of the grant CH 2636/1-1. SH acknowledges CNES funding through the grant 837319. VA acknowledges the support from Fundação para a Ciência e Tecnologia (FCT) through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). AO is supported by an STFC studentship. XD would like to acknowledge the funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement SCORE No 851555). HJD acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under the grant ‘Contribution of the IAC to the PLATO Space Mission’ with reference PID2019-107061GB-C66, DOI: 10.13039/501100011033. DD acknowledges support from the TESS Guest Investigator Program grant 80NSSC19K1727 and NASA Exoplanet Research Program grant 18-2XRP18_2-0136. AO gratefully acknowledges support from the Dutch Research Council NWO Veni grant.

International audience; La gestion pérenne des déchets issus de l'assainissement passe par des solutions adaptées au contexte des territoires. Elle doit notamment respecter les principes de proximité dans les circuits de collecte et traitement et permettre au mieux la valorisation des déchets. L'unité de traitement des matières de vidange de Nègrepelisse répond à ces impératifs avec une solution écologique qui offre plusieurs avantages : - sobriété énergétique dans les transports induits avec un site proche des déchets à éliminer, et dans la consommation énergétique de la filière extensive de traitement mise en ½uvre - valorisation énergétique vers une filière bois-énergie locale, - intégration paysagère avec une filière qui se fond dans le paysage environnant. - durabilité du système technique et agronomique. Le travail a consisté à suivre les performances de la filière dans son ensemble : traitements des effluents, distribution sur la parcelle et son homogénéité et valorisation des eaux usées traitées par la croissance des arbres sur une période de trois saisons d'irrigation. L'objectif était de valider la filière de traitement ainsi que de tester plusieurs modalités de conduite des irrigations afin de montrer que cette filière est très performante tant en terme de finalisation du traitement de l'effluent que de valorisation par la production de bois sans impacter le milieu.

Decubitus ulcers are a significant source of morbidity and mortality in those populations affected 1–3 : the elderly, the neurologically impaired, and paraplegics. Health care expenditures rise because of the increased length of hospital stay for patients with pressure ulcers. Treatment modalities and staffing time are increased considerably with the management of pressure ulcers both in the United States 1,4 and abroad. 5 The magnitude of the decubitus ulcer problem has been compared to an epidemic in the British literature, 5 and it is considered a serious public health concern by authorities in the United States. 4,6 The literature abounds with reviews focusing on the epidemiology, etiology, pathophysiology, risk factors, prevention, and treatment of decubitus ulcers. 5–12 These aspects are addressed in this article to provide a clear understanding of the populations at risk for developing decubitus ulcers and of those pathophysiologic factors responsible for their development. Subsequently, preventive measures, management, and treatment modalities are discussed.

A motional Stark effect (MSE) instrument to measure q(r) using the Torus Experiment for Technology (TEXT) neutral beam on the Alcator C-Mod tokamak has been designed and installed. The neutral beam is on the midplane, aimed radially, and designed to operate in hydrogen at 50 keV. The MSE optics view the outer half of the plasma −0.3

The Trinidad Ultra-deepwater (UDW) area lies on today’s continental slope off the eastern coast of Trinidad; it overlies oceanic crust and is part the Barbados Fold Belt, an active accretionary prism. See Figure 1 for location. Sedimentation has been rapid due to the constant feeding of clastic material from the Orinoco River. Figure 2 is a cross section that shows the relationship between the Columbus Basin extension and the active thrusting. In the area, deepwater turbidite sands are interbedded with shales, possibly providing both reservoir and seals. Deepwater channels and lobes have been identified and mapped in the existing 2D seismic. There are 13 wells that reached up to the lowest Pliocene, immediately to the west of the UDW area, providing a direct tie to the seismic stratigraphy interpretation. Figure 3 shows an E-W oriented seismic section showing the active thrusting and shale dome interaction. Priority for reservoir investigation was given to the late Middle Miocene to Pliocene, if only because deeper sections are increasingly overpressured and therefore difficult and risky to drill. Clastic composition and texture are interpreted to be mature, with mainly quartzose sands of continental affinity, consisting of amalgamated sand in the lobes and fine sand/silt interbedded with silty shales, in predominantly distal turbidites or overbank deposits. Minibasin deposition shown in Figure 4 is comparable in general terms with deepwater Gulf of Mexico lows created by salt tectonics. Most of the structures identified in the UDW area were active during the Upper Miocene and Plio-Pleistocene, so no areas are expected to show sheet like, unconfined basin floor fans. The ongoing development of the accretionary wedge will have focused sediments in a NNE-direction, in contrast to the SW-NE basinal axis trends which would dominate slightly older sediments. The growth of mud diapirs, probably initiated in the Plio-Pleistocene as increased amount of sediments were deposited further complicated the depositional pattern. Turbidite deposition of Upper and Middle Miocene age is interpreted to be of distal fans facies, while in the Plio-Pleistocene, they respond more to a minibasin setting and channellevee facies.

This paper describes techniques employed in the laboratory investigation of charged and neutral particle reactions of importance in the ionosphere. Atmospheric gases at densities appropriate to the D region, contained in a large reaction chamber, are irradiated by a spatially uniform flux of 1.5 MeV electrons. The resulting reactions are studied by a combination of resonant cavity measurements of electron density, mass analysis of positive and negative ions, and optical emission spectroscopy, both during continuous beam irradiation of the gas and in the radiation afterglow. Mechanisms and rates for molecular production and loss processes have been investigated using this apparatus under conditions resembling those in the ionosphere, with negligible competition from diffusion losses to the container walls. In addition to descriptions of the techniques, the paper includes examples of measurements made with the experimental system.

A versatile low energy electron gun suitable for electron‐atom scattering experiments has been designed utilizing photoetched grids and precision ceramic spacers which stack onto ceramic rods. Diagnostic techniques are described which determine the absolute electron energy to within ±0.1 eV. Electron guns which operate over the energy range 0.1–25 eV with currents up to 10 mA and energy spreads as low as 0.2 eV have been built using the design presented here.

We present experimental results from a partial simulation of the disturbed nighttime ionosphere at 300°K. N2:O2 mixtures at pressures from 0.1 to 30 torr are contained in a 700-liter chamber and irradiated by a diffuse beam of megavolt electrons. In dry gas, only the ions O2−, O2+, and NO+ are seen with the mass spectrometer at the onset of irradiation. As the electron bombardment continues, these ions interact with beam-generated neutral species to produce a spectrum eventually dominated by NO+, NO2−, and NO3−. From measurements of O2+ production and loss rates as a function of irradiation time, the dominant NO production mechanism is shown to be O2+ + N2 → NO+ + NO with a rate constant ≤1×10−16 cm3/sec, followed by ionic recombination to neutralize the NO+. We measure the following thermal-energy two-body ionic recombination coefficients, in units of 10−8 cm3/sec: α(NO+, NO−3) = (3.4±1.2); α(NO+, NO−2) = (17.5±6.0); and α(O2+, O2−) ≤ (14±5). With water added to the gas, the sequence H3O+(H2O)n (n = 0, 1, 2, 3) becomes important in the positive-ion spectrum.

The present report covers work performed during the period 1 January to 31 March 1963. It begins with a description of modifications made to the experimental equipment to permit the measurement of time-dependent ionization phenomena. The results of transient measurements in oxygen and N sub 2 - O sub 2 mixtures using these techniques is then presented. A detailed calculation of the role of diffusion in transient ionization phenomena has been started and is discussed in the report. The report closes with a description of the proposed work for the next quarter.