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Additional file 1. Clinical and sleep evaluation and supporting Table 1. Details about clinical and sleep evaluation.

La pandemia originada por la COVID-19, ha provocado una crisis mundial sin precedentes en la cual se manifiestan, adem��s de la crisis sanitaria, importantes efectos psicosociales y econ��micos. Sin embargo, representa grandes oportunidades si se considera la importancia del esp��ritu emprendedor durante una etapa de crisis. Por ello, el objetivo de este trabajo consisti�� en determinar la producci��n cient��fica sobre el fen��meno emprendedor desde el inicio de la COVID-19 hasta la actualidad. La metodolog��a empleada fue la revisi��n bibliom��trica de la literatura, siendo analizados 31 trabajos publicados en la base de datos Web of Science durante ese per��odo. Los resultados obtenidos evidencian que casi el 50% de la producci��n cient��fica se ha concentrado en cuatro publicaciones, que dos son los pa��ses con mayor producci��n, Estados Unidos y Australia, y que la presencia de mujeres es relevante respecto al total de autores, siendo en concreto dos autoras las que mayor n��mero de trabajos relacionados han publicado en este periodo. Como conclusiones de este trabajo puede establecerse que es un t��pico feminizado, donde destacan las publicaciones que hacen referencia al papel importante que puede desempe��ar la opci��n del emprendimiento en momentos de incertidumbre como el que se vive.

The study of adornments found in the necropolis at Valle de las Higueras (Huecas, Toledo) has determined the morphotypology and mineral composition of one quadrangular pendant and 341 stone beads. Most of the beads are short (length ≤ 5 mm), but within this regularity series can be differentiated that might be the result of standardised fabrication processes and different times of acquisition. Portable X-ray fluorescence (p-XRF) and X-ray diffraction (XRD) analysis identified the use of phyllosilicates as sepiolite and clinochlore, and above all variscite, a mineral that became especially important for adornments in the Iberian Peninsula in the 3rd millennium BC. The inland location of the necropolis, distant from source areas, certifies its remote origin, as far away as northwest Zamora according to the chronological framework. It is still not possible to determine for sure the source of the variscite at Valle de las Higueras. However, the inland location of the necropolis, distant from source areas, certifies its remote origin. The chronology suggests that it might have come from the north-west, in the area of Zamora. Archaeological and chronological data obtained in tombs in the necropolis, together with other inland sites, contribute to understanding variscite circulation in the Iberian Peninsula in the Chalcolithic. It was restricted to a few individuals, both adults and children, who wore necklaces and bracelets. Distance did not condition the arrival of variscite, but the small amounts suggest it was traded together with other ostentation elements, such as sea shells, cinnabar and amber. The heterogeneous regional panorama displays differences in the demand, use and acquisition of variscite depending on the socioeconomic organisation and connection to exchange networks.

This letter presents a combined measurement of the energy spectra of atmospheric $��_e$ and $��_��$ in the energy range between $\sim$100 GeV and $\sim$50 TeV with the ANTARES neutrino telescope. The analysis uses 3012 days of detector livetime in the period 2007--2017, and selects 1016 neutrinos interacting in (or close to) the instrumented volume of the detector, yielding shower-like events (mainly from $��_e+\overline ��_e$ charged current plus all neutrino neutral current interactions) and starting track events (mainly from $��_��+ \overline ��_��$ charged current interactions). The contamination by atmospheric muons in the final sample is suppressed at the level of a few per mill by different steps in the selection analysis, including a Boosted Decision Tree classifier. The distribution of reconstructed events is unfolded in terms of electron and muon neutrino fluxes. The derived energy spectra are compared with previous measurements that, above 100 GeV, are limited to experiments in polar ice and, for $��_��$, to Super-Kamiokande., Accepted to PLB

Our goal is to estimate the star formation main sequence (SFMS) and the star formation rate density (SFRD) at z 8 and it is clearly defined by the blue galaxies, with the red galaxies located below them. The SFMS is described as log SFR = 0.83 log M - 8.44. We find a good agreement with previous estimations of the SFMS, especially those based on integral field spectroscopy. The Halpha luminosity function of the AGN-free sample is well described by a Schechter function with log L* = 41.34, log phi* = -2.43, and alpha = -1.25. Our measurements provide a lower characteristic luminosity than several previous studies in the literature. The derived star formation rate density at d < 75 Mpc is log rho_SFR = -2.10 +- 0.11, with red galaxies accounting for 15% of the SFRD. Our value is lower than previous estimations at similar redshift, and provides a local reference for evolutionary studies regarding the star formation history of the Universe., 26 pages. Accepted for publication in Astronomy and Astrophysics

[EN] The first gamma-ray burst detections by Imaging Atmospheric Cherenkov Telescopes have been recently announced: GRB 190114C, detected by MAGIC, GRB 180720B and GRB 190829A, observed by H.E.S.S. A dedicated search for neutrinos in space and time coincidence with the gamma-ray emission observed by IACTs has been performed using ANTARES data. The search covers both the prompt and afterglow phases, yielding no neutrinos in coincidence with the three GRBs studied. Upper limits on the energetics of the neutrino emission are inferred. The resulting upper limits are several orders of magnitude above the observed gamma-ray emission, and they do not allow to constrain the available models., The authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), LabEx UnivEarthS (ANR-10-LABX-0023 and ANR18-IDEX-0001), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; Executive Unit for Financing Higher Education, Research, Development and Innovation (UEFISCDI), Romania; Ministerio de Ciencia e Innovacion (MCI) and Agencia Estatal de Investigacion: Programa Estatal de Generacion de Conocimiento (refs. PGC2018-096663-B-C41, -A-C42, -B-C43, -BC44) (MCI/FEDER), Severo Ochoa Centre of Excellence and MultiDark Consolider, Junta de Andalucia (ref. SOMM17/6104/UGR and A-FQM-053-UGR18), Generalitat Valenciana: Grisolia (ref. GRISOLIA/2018/119), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities.

The Transiting Exoplanet Survey Satellite (TESS) is observing bright known planet-host stars across almost the entire sky. These stars have been subject to extensive ground-based observations, providing a large number of radial velocity (RV) measurements. In this work we use the new TESS photometric observations to characterize the star $��^2$ Fornacis, and following this to update the parameters of the orbiting planet $��^2$ For b. We measure the p-mode oscillation frequencies in $��^2$ For, and in combination with non-seismic parameters estimate the stellar fundamental properties using stellar models. Using the revised stellar properties and a time series of archival RV data from the UCLES, HIRES and HARPS instruments spanning almost 20 years, we refit the orbit of $��^2$ For b and search the RV residuals for remaining variability. We find that $��^2$ For has a mass of $1.16\pm0.03$M$_\odot$ and a radius of $1.63\pm0.04$R$_\odot$, with an age of $6.3\pm0.9$Gyr. This and the updated RV measurements suggest a mass of $��^2$ For b of $16.8^{+1.2}_{-1.3}$M$_\oplus$, which is $\sim5$M$_\oplus$ less than literature estimates. We also detect a periodicity at 33 days in the RV measurements, which is likely due to the rotation of the host star. While previous literature estimates of the properties of $��^2$ are ambiguous, the asteroseismic measurements place the star firmly at the early stage of its subgiant evolutionary phase. Typically only short time series of photometric data are available from TESS, but by using asteroseismology it is still possible to provide tight constraints on the properties of bright stars that until now have only been observed from the ground. This prompts a reexamination of archival RV data from the past few decades to update the characteristics of the planet hosting systems observed by TESS for which asteroseismology is possible., Accepted for publication in A&A. 12 pages, 11 figures

Aims The aim of this paper is to stablish de position of the Ibero-American Society of Neurourology and Urogynecology (SINUG) in relation to the use of suburethral meshes for the surgical treatment of female stress incontinence. Methods Tension-free mid-urethral slings (MUS) have become the most popular procedure for the treatment of stress urinary incontinence (SUI). In July 2018, the British government announced a pause in the use of meshes for both pelvic organ prolapse (POP) and urinary incontinence (UI) treatment without differentiating whether the meshes were used for treating UI or POP. The decision was taken to stop their use until the publication of the updated UI and POP guidelines of the British National Health Service, which is available from April 2019. SINUG has reviewed the evidence and official position of different societies in relation to the safety and efficacy of MUS in the surgical treatment of incontinence differentiating them from meshes used to repair POP. Results Data from synthetic mesh manufacturers indicate that in 2010, 300 000 women underwent surgical procedures to repair POP and approximately 260 000 were operated on for SUI. According to these estimates, approximately more than 80% of the surgical techniques for UI treatment were performed transvaginally with meshes. Conclusions Once reviewed evidence and position of different societies, the SINUG presents its vision in this communication, which is a summary of the document analysing the state of topic prepared by the society.

The LAGO (Latin American Giant Observatory) observatory is an experiment that spans over Latin America in a wide range of latitudes that gives different rigidity cut offs for the enter of cosmic rays in the atmosphere. The motivation of the Observatory is to study atmospheric radiation and space weather through the measurement of the secondary emission of low energy cosmic rays at ground level using Water Cherenkov Detectors (WCD). This work presents the contributions of the LAGO collaboration to the 2019 36th ICRC., International Cosmic Ray Conference 2019

Acute promyelocytic leukemia is infrequent among patients aged >= 75 years old, a population that is rarely eligible for clinical protocols. This study aims to analyze the treatment strategies and clinical outcomes of very old APL patients reported to the international PETHEMA registry. Between 1997 and 2017, among 2501 APL cases registered 120 were >= 75 years old. Treatment approaches were: AIDA regimen, 79 patients; ATRA alone, 23; 16, supportive care (SC) and 2, other strategies. Patients treated with AIDA were younger, had better ECOG and lower leukocytes. Complete remission (CR) was achieved in 65% of AIDA-group vs. 45% in the ATRA-group, being infections followed by bleeding the most frequent causes of induction death. Patients in CR after AIDA showed 3-year DFS of 73%. Our real-life series of very old APL patients provides a reference basis for future treatment strategies aiming to improve clinical outcomes in this challenging population.

Depression and anxiety currently rank as the second and fifth most common causes worldwide of years lived with disability-a reality that has intensified the search for new treatments. There are many studies of herbal extracts and secondary metabolites from plants used in traditional medicine due to their antidepressant and anxiolytic properties. Clinical and preclinical studies about some of the mechanisms of action of metabolites like alkaloids, terpenes, flavonoids, and sterols, among others, have documented effects similar to those produced by clinically effective drugs. These metabolites have shown anxiolytic and antidepressant effects in various experimental models of anxiety by interacting with γ-aminobutyric acid subtype A receptors (GABAA-receptors) and by stimulating the serotonergic, noradrenergic, and dopaminergic neurotransmitter systems. These pharmacological effects can be attributed to plant metabolites that share structural similarities with monoamines, which allow them to bind to receptors. The objective of this chapter is to summarize the various mechanisms of action that have been identified in secondary metabolites with anxiolytic and antidepressant properties. Terpenes, alkaloids, flavonoids, and sterols can interact at different levels of the neurotransmission systems involved in the neurobiology of anxiety and depression, suggesting their potential for treating these mental illnesses.

The recently launched NASA Transiting Exoplanet Survey Satellite (TESS) mission is going to collect lightcurves for a few hundred million of stars and we expect to increase the number of pulsating stars to analyze compared to the few thousand stars observed by the CoRoT, $\textit{Kepler}$ and K2 missions. However, most of the TESS targets have not yet been properly classified and characterized. In order to improve the analysis of the TESS data, it is crucial to determine the type of stellar pulsations in a timely manner. We propose an automatic method to classify stars attending to their pulsation properties, in particular, to identify solar-like pulsators among all TESS targets. It relies on the use of the global amount of power contained in the power spectrum (already known as the FliPer method) as a key parameter, along with the effective temperature, to feed into a machine learning classifier. Our study, based on TESS simulated datasets, shows that we are able to classify pulsators with a $98\%$ accuracy., 4 pages, 1 figure, Proceeding of the 2018 SF2A conference

An indirect measurement of the antiproton flux in cosmic rays is possible as the particles undergo deflection by the geomagnetic field. This effect can be measured by studying the deficit in the flux, or shadow, created by the Moon as it absorbs cosmic rays that are headed towards the Earth. The shadow is displaced from the actual position of the Moon due to geomagnetic deflection, which is a function of the energy and charge of the cosmic rays. The displacement provides a natural tool for momentum/charge discrimination that can be used to study the composition of cosmic rays. Using 33 months of data comprising more than 80 billion cosmic rays measured by the High Altitude Water Cherenkov (HAWC) observatory, we have analyzed the Moon shadow to search for TeV antiprotons in cosmic rays. We present our first upper limits on the $\bar{p}/p$ fraction, which in the absence of any direct measurements, provide the tightest available constraints of $\sim1\%$ on the antiproton fraction for energies between 1 and 10 TeV., 10 pages, 5 figures. Accepted by Physical Review D

CoRoT and Kepler high-precision photometric data allowed the detection and characterization of the oscillation parameters in stars other than the Sun. Moreover, thanks to the scaling relations, it is possible to estimate masses and radii for thousands of solar-type oscillating stars. Recently, a ����- ��relation has been found for ��Scuti stars. Now, analyzing several hundreds of this kind of stars observed with CoRoT and Kepler, we present an empiric relation between their frequency at maximum power of their oscillation spectra and their effective temperature. Such a relation can be explained with the help of the ��-mechanism and the observed dispersion of the residuals is compatible with they being caused by the gravity-darkening effect.

Motivated by the construction of Bach flat neutral signature Riemannian extensions, we study the space of parallel trace free tensors of type $(1,1)$ on an affine surface. It is shown that the existence of such a parallel tensor field is characterized by the recurrence of the symmetric part of the Ricci tensor.

In cases where both components of a binary system show oscillations, asteroseismology has been proposed as a method to identify the system. For KIC 2568888, observed with $Kepler$, we detect oscillation modes for two red giants in a single power density spectrum. Through an asteroseismic study we investigate if the stars have similar properties, which could be an indication that they are physically bound into a binary system. While one star lies on the red giant branch (RGB), the other, more evolved star, is either a RGB or asymptotic-giant-branch star. We found similar ages for the red giants and a mass ratio close to 1. Based on these asteroseismic results we propose KIC 2568888 as a rare candidate binary system ($\sim 0.1\%$ chance). However, when combining the asteroseismic data with ground-based $BVI$ photometry we estimated different distances for the stars, which we cross-checked with $Gaia$ DR2. From $Gaia$ we obtained for one object a distance between and broadly consistent with the distances from $BVI$ photometry. For the other object we have a negative parallax with a not yet reliable $Gaia$ distance solution. The derived distances challenge a binary interpretation and may either point to a triple system, which could explain the visible magnitudes, or, to a rare chance alignment ($\sim 0.05\%$ chance based on stellar magnitudes). This probability would even be smaller, if calculated for close pairs of stars with a mass ratio close to unity in addition to similar magnitudes, which may indeed indicate that a binary scenario is more favourable., 12 pages, 5 figures, 4 tables; accepted for publication in ApJ

In the present paper we aim to validate a methodology designed to extract the Halpha emission line flux from J-PLUS photometric data. J-PLUS is a multi narrow-band filter survey carried out with the 2 deg2 field of view T80Cam camera, mounted on the JAST/T80 telescope in the OAJ, Teruel, Spain. The information of the twelve J-PLUS bands, including the J0660 narrow-band filter located at rest-frame Halpha, is used over 42 deg2 to extract de-reddened and [NII] decontaminated Halpha emission line fluxes of 46 star-forming regions with previous SDSS and/or CALIFA spectroscopic information. The agreement of the inferred J-PLUS photometric Halpha fluxes and those obtained with spectroscopic data is remarkable, with a median comparison ratio R = 1.05 +- 0.25. This demonstrates that it is possible to retrieve reliable Halpha emission line fluxes from J-PLUS photometric data. With an expected area of thousands of square degrees upon completion, the J-PLUS dataset will allow the study of several star formation science cases in the nearby universe, as the spatially resolved star formation rate of nearby galaxies at z < 0.015, and how it is influenced by the environment, morphology or nuclear activity. As an illustrative example, the close pair of interacting galaxies NGC3994 and NGC3995 is analyzed, finding an enhancement of the star formation rate not only in the center, but also in outer parts of the disk of NGC3994., 13 pages, 8 figures, 3 tables. Submitted to Astronomy and Astrophysics. Comments are welcome

List of proceedings from the HAWC Collaboration presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands., List of proceedings from the HAWC Collaboration presented at ICRC2015. Follow the "HTML" link to access the list

We provide classification results for and examples of half conformally flat generalized quasi Einstein manifolds of signature $(2,2)$. This analysis leads to a natural equation in affine geometry called the affine quasi-Einstein equation that we explore in further detail.

Full list of authors: Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Al Samarai, I.; Altmann, D.; Andeen, K.; Anderson, T.; Ansseau, I.; Anton, G.; Archinger, M.; Argüelles, C.; Auffenberg, J.; Axani, S.; Bai, X.; Barwick, S. W.; Baum, V. Bay, R.; Beatty, J. J.; Tjus, J. Becker; Becker, K. -H.; Benzvi, S.; Berley, D.; Bernardini, E.; Bernhard, A.; Besson, D. Z.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, S.; Bohm, C.; Börner, M.; Bos, F.; Bose, D.; Böser, S.; Botner, O.; Braun, J.; Brayeur, L.; Bretz, H. -P.; Bron, S.; Burgman, A.; Carver, T.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Clark, K.; Classen, L.; Coenders, S.; Collin, G. H.; Conrad, J. M.; Cowen, D. F.; Cross, R.; Day, M.; de André, J. P. A. M.; de Clercq, C.; Del Pino Rosendo, E.; Dembinski, H.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; Deyoung, T.; di Lorenzo, V.; Dujmovic, H.; Dumm, J. P.; Dunkman, M.; Eberhardt, B.; Ehrhardt, T.; Eichmann, B.; Eller, P.; Euler, S.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Feintzeig, J.; Felde, J.; Filimonov, K.; Finley, C.; Flis, S.; Fösig, C. -C.; Franckowiak, A.; Friedman, E.; Fuchs, T.; Gaisser, T. K.; Gallagher, J.; Gerhardt, L.; Ghorbani, K.; Giang, W.; Gladstone, L.; Glauch, T.; Glüsenkamp, T.; Goldschmidt, A.; Gonzalez, J. G.; Grant, D.; Griffith, Z.; Haack, C.; Hallgren, A.; Halzen, F.; Hansen, E.; Hansmann, T.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoshina, K.; Huang, F.; Huber, M.; Hultqvist, K.; in, S.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jeong, M.; Jero, K.; Jones, B. J. P.; Kang, W.; Kappes, A.; Karg, T.; Karle, A.; Katz, U.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, A.; Kim, J.; Kim, M.; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Kohnen, G.; Koirala, R.; Kolanoski, H.; Konietz, R.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, M.; Krückl, G.; Krüger, C.; Kunnen, J.; Kunwar, S.; Kurahashi, N.; Kuwabara, T.; Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber, F.; Lesiak-Bzdak, M.; Leuermann, M.; Lu, L.; Lünemann, J.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Mancina, S.; Mandelartz, M.; Maruyama, R.; Mase, K.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meier, M.; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Micallef, J.; Momenté, G.; Montaruli, T.; Moulai, M.; Nahnhauer, R.; Naumann, U.; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke Pollmann, A.; Olivas, A.; O'Murchadha, A.; Palczewski, T.; Pandya, H.; Pankova, D. V.; Peiffer, P.; Penek, Ö.; Pepper, J. A.; Pérez de Los Heros, C.; Pieloth, D.; Pinat, E.; Price, P. B.; Przybylski, G. T.; Quinnan, M.; Raab, C.; Rädel, L.; Rameez, M.; Rawlins, K.; Reimann, R.; Relethford, B.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Riedel, B.; Robertson, S.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk, D.; Sabbatini, L.; Sanchez Herrera, S. E.; Sandrock, A.; Sandroos, J.; Sarkar, S.; Satalecka, K.; Schlunder, P.; Schmidt, T.; Schoenen, S.; Schöneberg, S.; Schumacher, L.; Seckel, D.; Seunarine, S.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stachurska, J.; Stanev, T.; Stasik, A.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Ström, R.; Strotjohann, N. L.; Sullivan, G. W.; Sutherland, M.; Taavola, H.; Taboada, I.; Tatar, J.; Tenholt, F.; Ter-Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Toscano, S.; Tosi, D.; Tselengidou, M.; Tung, C. F.; Turcati, A.; Unger, E.; Usner, M.; Vandenbroucke, J.; van Eijndhoven, N.; Vanheule, S.; van Rossem, M.; van Santen, J.; Vehring, M.; Voge, M.; Vogel, E.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandkowsky, N.; Waza, A.; Weaver, Ch.; Weiss, M. J.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Wickmann, S.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wolf, M.; Wood, T. R.; Woolsey, E.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Zoll, M.; Asas-Sn Collaboration; Stanek, K. Z.; Shappee, B. J.; Kochanek, C. S.; Holoien, T. W. -S.; Prieto, J. L.; Astrophysical Multimessenger Observatory Network; Fox, D. B.; Delaunay, J. J.; Turley, C. F.; Barthelmy, S. D.; Lien, A. Y.; Mészáros, P.; Murase, K.; Fermi Collaboration; Kocevski, D.; Buehler, R.; Giomi, M.; Racusin, J. L.; Hawc Collaboration; Albert, A.; Alfaro, R.; Alvarez, C.; Álvarez, J. D.; Arceo, R.; Arteaga-Velázquez, J. C.; Ayala Solares, H. A.; Barber, A. S.; Baustista-Elivar, N.; Becerril, A.; Belmont-Moreno, E.; Bernal, A.; Brisbois, C.; Caballero-Mora, K. S.; Capistrán, T.; Carramiñana, A.; Casanova, S.; Castillo, M.; Cotti, U.; Coutiño de León, S.; de La Fuente, E.; de León, C.; Diaz Hernandez, R.; Díaz-Vélez, J. C.; Dingus, B. L.; Duvernois, M. A.; Ellsworth, R. W.; Engel, K.; Fiorino, D. W.; Fraija, N.; García-González, J. A.; Gerhardt, M.; González Muñoz, A.; González, M. M.; Goodman, J. A.; Hampel-Arias, Z.; Harding, J. P.; Hernandez, S.; Hui, C. M.; Hüntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Joshi, V.; Kaufmann, S.; Lara, A.; Lauer, R. J.; Lee, W. H.; Lennarz, D.; León Vargas, H.; Linnemann, J. T.; Luis Raya, G.; Luna-García, R.; López-Coto, R.; Malone, K.; Marinelli, S. S.; Martinez, O.; Martinez-Castellanos, I.; Martínez-Castro, J.; Martínez-Huerta, H.; Matthews, J. A.; Miranda-Romagnoli, P.; Moreno, E.; Mostafá, M.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Pelayo, R.; Pretz, J.; Pérez-Pérez, E. G.; Ren, Z.; Rho, C. D.; Rivière, C.; Rosa-González, D.; Rosenberg, M.; Salesa Greus, F.; Sandoval, A.; Schneider, M.; Schoorlemmer, H.; Sinnis, G.; Smith, A. J.; Springer, R. W.; Surajbali, P.; Tibolla, O.; Tollefson, K.; Torres, I.; Ukwatta, T. N.; Villaseñor, L.; Weisgarber, T.; Wisher, I. G.; Wood, J.; Yapici, T.; Zepeda, A.; Zhou, H.; Lco Collaboration; Arcavi, I.; Hosseinzadeh, G.; Howell, D. A.; Valenti, S.; McCully, C.; Master Collaboration; Lipunov, V. M.; Gorbovskoy, E. S.; Tiurina, N. V.; Balanutsa, P. V.; Kuznetsov, A. S.; Kornilov, V. G.; Chazov, V.; Budnev, N. M.; Gress, O. A.; Ivanov, K. I.; Tlatov, A. G.; Rebolo Lopez, R.; Serra-Ricart, M.; Swift Collaboration; Evans, P. A.; Kennea, J. A.; Gehrels, N.; Osborne, J. P.; Page, K. L.; VERITAS Collaboration; Abeysekara, A. U.; Archer, A.; Benbow, W.; Bird, R.; Brantseg, T.; Bugaev, V.; v Cardenzana, J.; Connolly, M. P.; Cui, W.; Falcone, A.; Feng, Q.; Finley, J. P.; Fleischhack, H.; Fortson, L.; Furniss, A.; Griffin, S.; Grube, J.; Hütten, M.; Hervet, O.; Holder, J.; Hughes, G.; Humensky, T. B.; Johnson, C. A.; Kaaret, P.; Kar, P.; Kelley-Hoskins, N.; Kertzman, M.; Krause, M.; Kumar, S.; Lang, M. J.; Lin, T. T. Y.; McArthur, S.; Moriarty, P.; Mukherjee, R.; Nieto, D.; Ong, R. A.; Otte, A. N.; Pohl, M.; Popkow, A.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Richards, G. T.; Roache, E.; Rulten, C.; Sadeh, I.; Santander, M.; Sembroski, G. H.; Staszak, D.; Trépanier, S.; Tyler, J.; Wakely, S. P.; Weinstein, A.; Wilcox, P.; Wilhelm, A.; Williams, D. A.; Zitzer, B.; Bellm, E.; Cano, Z.; Gal-Yam, A.; Kann, D. A.; Ofek, E. O.; Rigault, M.; Soumagnac, M., On February 17, 2016, the IceCube real-time neutrino search identified, for the first time, three muon neutrino candidates arriving within 100 s of one another, consistent with coming from the same point in the sky. Such a triplet is expected once every 13.7 years as a random coincidence of background events. However, considering the lifetime of the follow-up program the probability of detecting at least one triplet from atmospheric background is 32%. Follow-up observatories were notified in order to search for an electromagnetic counterpart. Observations were obtained by Swift's X-ray telescope, by ASAS-SN, LCO and MASTER at optical wavelengths, and by VERITAS in the very-high-energy gamma-ray regime. Moreover, the Swift BAT serendipitously observed the location 100 s after the first neutrino was detected, and data from the Fermi LAT and HAWC observatory were analyzed. We present details of the neutrino triplet and the follow-up observations. No likely electromagnetic counterpart was detected, and we discuss the implications of these constraints on candidate neutrino sources such as gamma-ray bursts, core-collapse supernovae and active galactic nucleus flares. This study illustrates the potential of and challenges for future follow-up campaigns. © ESO, 2017. © ESO, 2017., The IceCube Collaboration acknowledges the support from the following agencies: US National Science Foundation-Office of Polar Programs, US National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin – Madison, the Open Science Grid (OSG) grid infrastructure; US Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Villum Fonden, Danish National Research Foundation (DNRF), Denmark This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. Funding for the Swift project in the UK is provided by the UK Space Agency. Part of this work was facilitated by the GROWTH project, a partnership in international research and education, NSF PIRE Grant No. 1545949. ASAS-SN is supported by NSF grant AST-1515927. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Mt. Cuba Astronomical Foundation, and by George Skestos. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), high-energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. The HAWC Collaboration acknowledges the support from: the US National Science Foundation (NSF); the US Department of Energy Office of High-Energy Physics; the Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnología (CONACyT), México (grants 271051, 232656, 260378, 179588, 239762, 254964, 271737, 258865, 243290, 132197), Laboratorio Nacional HAWC de rayos gamma; L’OREAL Fellowship for Women in Science 2014; Red HAWC, México; DGAPA-UNAM (grants IG100317, IN111315, IN111716-3, IA102715, 109916, IA102917); VIEP-BUAP; PIFI 2012, 2013, PROFOCIE 2014, 2015;the University of Wisconsin Alumni Research Foundation; the Institute of Geophysics, Planetary Physics, andSignatures at Los Alamos National Laboratory; Polish Science Centre grant DEC-2014/13/B/ST9/945; Coordinación de la Investigación Científica de la Universidad Michoacana. We thank Luciano Díaz and Eduardo Murrieta for technical support of the HAWC detector. Support for I. Arcavi was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. D. A. Howell, C. McCully, and G. Hosseinzadeh are supported by NSF-1313484. This work makes use of observations from the LCO network. VERITAS research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, and by NSERC in Canada. VERITAS acknowledges the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. E. O. Ofek and A. Gal-Yam acknowledge a Minerva grant.

Stars similar to the Sun, known as solar analogues, provide an excellent opportunity to study the preceding and following evolutionary phases of our host star. The unprecedented quality of photometric data collected by the \Kepler NASA mission allows us to characterise solar-like stars through asteroseismology and study diagnostics of stellar evolution, such as variation of magnetic activity, rotation and the surface lithium abundance. In this project, presented in a series of papers by Salabert et al. (2016a,b) and Beck et al (2016a,b), we investigate the link between stellar activity, rotation, lithium abundance and oscillations in a group of 18 solar-analogue stars through space photometry, obtained with the NASA Kepler space telescope and from currently 50+ hours of ground-based, high-resolution spectroscopy with the Hermes instrument. In these proceedings, we first discuss the selection of the stars in the sample, observations and calibrations and then summarise the main results of the project. By investigating the chromospheric and photospheric activity of the solar analogues in this sample, it was shown that for a large fraction of these stars the measured activity levels are compatible to levels of the 11-year solar activity cycle 23. A clear correlation between the lithium abundance and surface rotation was found for rotation periods shorter than the solar value. Comparing the lithium abundance measured in the solar analogues to evolutionary models with the Toulouse-Geneva Evolutionary Code (TGEC), we found that the solar models calibrated to the Sun also correctly describe the set of solar/stellar analogs showing that they share the same internal mixing physics. Finally, the star KIC 3241581 and KIC 10644353 are discussed in more detail., Proceedings of "The 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun"; 8 pages, 4 Figures

We introduce a simple model of deterministic particles in weakly disordered media which exhibits a transition from normal to anomalous diffusion. The model consists of a set of non-interacting overdamped particles moving on a disordered potential. The disordered potential can be thought as a substrate having some "defects" scattered along a one-dimensional line. The distance between two contiguous defects is assumed to have a heavy-tailed distribution with a given exponent $\alpha$, which means that the defects along the substrate are scarce if $\alpha$ is small. We prove that this system exhibits a transition from normal to anomalous diffusion when the distribution exponent $\alpha$ decreases, i.e., when the defects become scarcer. Thus we identify three distinct scenarios: a normal diffusive phase for $\alpha>2$, a superdiffusive phase for $1/2, Comment: 9 pages, 6 figures

We classify non-reductive four-dimensional homogeneous conformally Einstein manifolds., New version correcting some inaccuracies in the original paper

Paragallinula gen. nov. urn:lsid:zoobank.org:act: 909AC100-559E-4CA3-BC7E-E6FD87002E30 Type species Gallinula angulata Sundevall, 1850. Monotypic. Differential diagnosis Paragallinula gen. nov. differs from Gallinula, Pareudiastes, Tribonyx and Porphyriops in that (i) the orange suffusion on the frontal shield does not encompass the entire shield (in Gallinula encompassing entire frontal shield (Fig. 2); in Pareudiastes, Tribonyx and Porphyriops no suffusion of orange). In addition, Paragallinula gen. nov. differs from most species in the Fulica -clade (except T. ventralis) in (ii) showing marked sexual plumage dimorphism (Taylor 1996; Taylor & van Perlo 1998). Paragallinula gen. nov. further differs from Gallinula in (iii) the lack of a contrasting reddish band (���garter���) on the legs immediately proximal to the ankle joint (present in Gallinula) (Fig. 2). Paragallinula gen. nov. differs from Fulica in (ii) gradual change in colouration on hindneck from dark grey head to paler lower neck and back (abrupt change in Fulica); (iii) absence of broad cutaneous lobes on digits II���IV of feet (present in Fulica); and (iv) presence of narrow cutaneous folds on lateral and medial sides of digits I���IV of feet (absent in Fulica). Paragallinula also differs from Fulica in at least 12 diagnostic osteological characters (characters 120, 124, 125, 127, 139, 216, 274, 298, 311, 312, 316, 343 in Livezey 1998, to which is referred for descriptions of characters and their states). Paragallinula gen. nov. further differs from the two species of Pareudiastes in (iii) frontal shield with acuminate posterior margin (squared margin in Pareudiastes); (iv) ventroanterior position of nasal depression (ventromedial in Pareudiastes); (v) fully feathered lores (in Pareudiastes, lores with sparsely feathered, yellow-orange area from base of maxilla to orbit); (vi) gradual change in colouration on hindneck from dark grey head to paler lower neck and back (very dark without noticeable change in colour from head to back in Pareudiastes); (vii) flank feathers with large white streaks (no streaks in Pareudiastes); (viii) undertail-coverts white dorsolaterally, black ventromedially (entirely black or brownish-black in Pareudiastes); (ix) six pairs of rectrices (four in Pareudiastes); (x) rectrices forming normally-shaped tail (in Pareudiastes, rectrices very short barely protruding beyond uppertail- and undertail-coverts); (xi) leading edge of distalmost primary with narrow white margin (absent in Pareudiastes); (xii) underwing-coverts with white bars (not barred in Pareudiastes); (xiii) bend of wing whitish (no white colouration in Pareudiastes); and (xiv) presence of narrow cutaneous folds on lateral and medial sides of digits I���IV of feet (absent in Pareudiastes). Paragallinula gen. nov. further differs from Tribonyx in (ii) broad naked area on crown in downy plumage (absent in Tribonyx); (iii) long, filamentous white filoplumes in downy plumage (absent in Tribonyx); (iv) frontal shield with acuminate posterior margin (rounded in Tribonyx); (v) undertail-coverts white dorsolaterally, black ventromedially (entirely blackish in Tribonyx); (vi) six pairs of rectrices (eight in Tribonyx); (vii) underwing-coverts dark grey, blackish or black (medium brown in Tribonyx); and (viii) . bend of wing whitish (no white colouration in Tribonyx). Paragallinula also differs from Tribonyx in a single osteological character: (ix) ossa digitorum pedis, digiti tertius, phalanx intermedialis (secundi) is equal to or longer than phalanx quartus (in Tribonyx modally shorter than phalanx distalis (tertius). Paragallinula gen. nov. further differs from Porphyriops (P. melanops) in (iii) broad naked area on crown in downy plumage (absent in Porphyriops); (iv) long, filamentous white filoplumes in downy plumage (absent in Porphyriops); (v) ventroanterior position of nasal depression (ventromedial in Porphyriops); (vi) feathers at base of bill, lores and crown not contrasting with rest of head (in Porphyriops contrastingly black); (vii) flank feathers mostly plain but with large white streaks at tips (flank feathers brown-grey, spotted white in Porphyriops); (viii) central belly dark slate-grey (whitish in Porphyriops); (xi) undertailcoverts white dorsolaterally, black ventromedially (white in Porphyriops); and (x) rectrices dark grey or black (brown in Porphyriops). In addition, there are two diagnostic osteological differences between Paragallinula and Porphyriops: (xi) os frontale, facies dorsalis moderately convex (flat or slightly concave in Porphyriops), and (xii) os squamosum, fossa temporalis distinct, separated medially from each other by significantly broad, elevated expanse of os frontale (in Porphyriops, indistinct, shallow, limited to region immediately ventral to processus postorbitalis). Etymology The generic name is derived from the Greek para (beside) and the Latin gallinula (a little hen or chicken). It denotes the resemblance of P. angulata to species of Gallinula but highlights that they are independent evolutionary lineages. The gender of the name is feminine. Distribution Paragallinula angulata is found in most of the African continent from Senegal and Gambia to Ethiopia, Namibia, Botswana and South Africa., Published as part of Sangster, George, Garc��a-R, Juan Carlos & Trewick, Steve A., 2015, A new genus for the Lesser Moorhen Gallinula angulata Sundevall, 1850 (Aves, Rallidae), pp. 1-8 in European Journal of Taxonomy 153 on pages 4-6, DOI: 10.5852/ejt.2015.153, http://zenodo.org/record/3787992, {"references":["Taylor P. B. 1996. Family Rallidae (rails, gallinules and coots). In: del Hoyo J., Elliot A. & Sargatal J. (eds) Handbook of the Birds of the World. Vol. 3. Hoatzin to auks: 108 - 209. Lynx Edicions, Barcelona.","Taylor P. B. & van Perlo B. 1998. Rails, a Guide to the Rails, Crakes, Gallinules and Coots of the World. Pica Press, Sussex.","Livezey B. C. 1998. A phylogenetic analysis of the Gruiformes (Aves) based on morphological characters, with an emphasis on the rails (Rallidae). Philosophical Transactions of the Royal Society of London B 353: 2077 - 2151. http: // dx. doi. org / 10.1098 / rstb. 1998.0353"]}

PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 sec readout cadence and 2 with 2.5 sec candence) providing a wide field-of-view (2232 deg2) and a large photometric magnitude range (4-16 mag). It focusses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2%, 4-10% and 10% for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50% of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0., Comment: 63 pages, 17 figures, submitted to Experimental Astronomy (ExA)

We examine the difference between several notions of curvature homogeneity and show that the notions introduced by Kowalski and Van\v{z}urov\'a are genuine generalizations of the ordinary notion of $k$-curvature homogeneity. The homothety group plays an essential role in the analysis.

Thanks to the asteroseimic study of the red giant star KIC 7341231 observed by Kepler, it has been possible to infer its radial differential rotation profile (Deheuvels et al. 2012). This opens new ways to constrain the physical mechanisms responsible of the angular momentum transport in stellar interiors by directly comparing this radial rotation profile with the ones computed using stellar evolution codes including dynamical processes. In this preliminary work, we computed different models of KIC 7341231 with the Geneva stellar evolution code that includes transport mechanisms due to a shellular rotation and the associated large-scale meridional circulation and shear-induced turbulence. Once the global parameters of the star had been established, we modified some of the model's input parameters in order to understand their effects on the predicted rotation profile of the modeled star. As a result, we find a discrepancy between the rotation profile deduced from asteroseismic measurements and the profiles predicted from models including shellular rotation and related meridional flows and turbulence. This indicates that a most powerful mechanism is in action to extract angular momentum from the core of this star., 4 pages, 2 figures, Proceedings of the ESF Conference The Modern Era of Helio- and Asteroseismology

The present note relies on the recently published conceptual design report of the LHeC and extends the first contribution to the European strategy debate in emphasising the role of the LHeC to complement and complete the high luminosity LHC programme. The brief discussion therefore focuses on the importance of high precision PDF and $\alpha_s$ determinations for the physics beyond the Standard Model (GUTs, SUSY, Higgs). Emphasis is also given to the importance of high parton density phenomena in nuclei and their relevance to the heavy ion physics programme at the LHC. The present note relies on the recently published conceptual design report of the LHeC and extends the first contribution to the European strategy debate in emphasising the role of the LHeC to complement and complete the high luminosity LHC programme. The brief discussion therefore focuses on the importance of high precision PDF and $\alpha_s$ determinations for the physics beyond the Standard Model (GUTs, SUSY, Higgs). Emphasis is also given to the importance of high parton density phenomena in nuclei and their relevance to the heavy ion physics programme at the LHC.

The covariant derivative of the K��hler form of an almost pseudo-Hermitian or of an almost para-Hermitian manifold satisfies certain algebraic relations. We show, conversely, that any 3-tensor which satisfies these algebraic relations can be realized geometrically.