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1. ExoClock Project III: 450 new exoplanet ephemerides from ground and space observations

Author: Kokori, A., Tsiaras, A., Edwards, B., Jones, A., Pantelidou, G., Tinetti, G., Bewersdorff, L., Iliadou, A., Jongen, Y., Lekkas, G., Nastasi, A., Poultourtzidis, E., Sidiropoulos, C., Walter, F., Wünsche, A., Abraham, R., Agnihotri, V. K., Albanesi, R., Arce-Mansego, E., Arnot, D., Audejean, M., Aumasson, C., Bachschmidt, M., Baj, G., Barroy, P. R., Belinski, A. A., Bennett, D., Benni, P., Bernacki, K., Betti, L., Biagini, A., Bosch, P., Brandebourg, P., Brát, L., Bretton, M., Brincat, S. M., Brouillard, S., Bruzas, A., Bruzzone, A., Buckland, R. A., Caló, M., Campos, F., Carreno, A., Rodrigo, J. -A. Carrion, Casali, R., Casalnuovo, G., Cataneo, M., Chang, C. -M., Changeat, L., Chowdhury, V., Ciantini, R., Cilluffo, M., Coliac, J. -F., Conzo, G., Correa, M., Coulon, G., Crouzet, N., Crow, M. V., Curtis, I., Daniel, D., Dawes, S., Dauchet, B., Deldem, M., Deligeorgopoulos, D., Dransfield, G., Dymock, R., Eenmäe, T., Evans, P., Esseiva, N., Falco, C., Farfán, R. G., Fernández-Lajús, E., Ferratfiat, S., Ferreira, S. L., Ferretti, A., Fiołka, J., Fowler, M., Futcher, S. R., Gabellini, D., Gainey, T., Gaitan, J., Gajdoš, P., García-Sánchez, A., Garlitz, J., Gillier, C., Gison, C., Horta, F. Grau, Grivas, G., Gonzales, J., Gorshanov, D., Guerra, P., Guillot, T., Haswell, C. A., Haymes, T., Hentunen, V. -P., Hills, K., Hose, K., Humbert, T., Hurter, F., Hynek, T., Irzyk, M., Jacobsen, J., Jannetta, A. L., Johnson, K., Jóźwik-Wabik, P., Kaeouach, A. E., Kang, W., Kiiskinen, H., Kim, T., Kivila, Ü., Koch, B., Kolb, U., Kučáková, H., Lai, S. -P., Laloum, D., Lasota, S., Lewis, L. A., Liakos, G. -I., Libotte, F., Lopresti, C., Lomoz, F., Majewski, R., Malcher, A., Mallonn, M., Mannucci, M., Marchini, A., Mari, J. -M., Marino, A., Marino, G., Mario, J. -C., Marquette, J. -B., Martínez-Bravo, F. A., Mašek, M., Matassa, P., Michel, P., Michelet, J., Miller, M., Miny, E., Mollier, T., Molina, D., Monteleone, B., Montigiani, N., Morales-Aimar, M., Mortari, F., Morvan, M., Mugnai, L. V., Murawski, G., Naponiello, L., Naves, R., Naudin, J. -L., Néel, D., Neito, R., Neveu, S., Noschese, A., Öğmen, Y., Ohshima, O., Orbanic, Z., Pace, E. P., Pantacchini, C., Paschalis, N. I., Pereira, C., Peretto, I., Perroud, V., Phillips, M., Pintr, P., Pioppa, J. -B., Plazas, J., Poelarends, A. J., Popowicz, A., Purcell, J., Quinn, N., Raetz, M., Rees, D., Regembal, F., Rocchetto, M., Rocci, P. -F., Rockenbauer, M., Roth, R., Rousselot, L., Rubia, X., Ruocco, N., Russo, E., Salisbury, M., Salvaggio, F., Santos, A., Savage, J., Scaggiante, F., Sedita, D., Shadick, S., Silva, A. F., Sioulas, N., Školník, V., Smith, M., Smolka, M., Solmaz, A., Stanbury, N., Stouraitis, D., Tan, T. -G., Theusner, M., Thurston, G., Tifner, F. -P., Tomacelli, A., Tomatis, A., Trnka, J., Tylšar, M., Valeau, P., Vignes, J. -P., Villa, A., Sureda, A. Vives, Vora, K., Vrašťák, M., Walliang, D., Wenzel, B., Wright, D. E., Zambelli, R., Zhang, M., and Zíbar, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: The ExoClock project has been created with the aim of increasing the efficiency of the Ariel mission. It will achieve this by continuously monitoring and updating the ephemerides of Ariel candidates over an extended period, in order to produce a consistent catalogue of reliable and precise ephemerides. This work presents a homogenous catalogue of updated ephemerides for 450 planets, generated by the integration of $\sim$18000 data points from multiple sources. These sources include observations from ground-based telescopes (ExoClock network and ETD), mid-time values from the literature and light-curves from space telescopes (Kepler/K2 and TESS). With all the above, we manage to collect observations for half of the post-discovery years (median), with data that have a median uncertainty less than one minute. In comparison with literature, the ephemerides generated by the project are more precise and less biased. More than 40\% of the initial literature ephemerides had to be updated to reach the goals of the project, as they were either of low precision or drifting. Moreover, the integrated approach of the project enables both the monitoring of the majority of the Ariel candidates (95\%), and also the identification of missing data. The dedicated ExoClock network effectively supports this task by contributing additional observations when a gap in the data is identified. These results highlight the need for continuous monitoring to increase the observing coverage of the candidate planets. Finally, the extended observing coverage of planets allows us to detect trends (TTVs - Transit Timing Variations) for a sample of 19 planets. All products, data, and codes used in this work are open and accessible to the wider scientific community., Comment: Recommended for publication to ApJS (reviewer's comments implemented). Main body: 13 pages, total: 77 pages, 7 figures, 7 tables. Data available at http://doi.org/10.17605/OSF.IO/P298N
Published: 2022
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2. Massive search of spot- and facula-crossing events in 1598 exoplanetary transit lightcurves

Author: Baluev, R. V., Sokov, E. N., Sokova, I. A., Shaidulin, V. Sh., Veselova, A. V., Aitov, V. N., Mitiani, G. Sh., Valeev, A. F., Gadelshin, D. R., Gutaev, A. G., Beskin, G. M., Valyavin, G. G., Antonyuk, K., Barkaoui, K., Gillon, M., Jehin, E., Delrez, L., Guðmundsson, S., Dale, H. A., Fernández-Lajús, E., Di Sisto, R. P., Bretton, M., Wunsche, A., Hentunen, V. -P., Shadick, S., Jongen, Y., Kang, W., Kim, T., Pakštienė, E., Qvam, J. K. T., Knight, C. R., Guerra, P., Marchini, A., Salvaggio, F., Papini, R., Evans, P., Salisbury, M., Garlitz, J., Esseiva, N., Ogmen, Y., Bosch-Cabot, P., Selezneva, A., and Hinse, T. C.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We developed a dedicated statistical test for a massive detection of spot- and facula-crossing anomalies in multiple exoplanetary transit lightcurves, based on the frequentist $p$-value thresholding. This test was used to augment our algorithmic pipeline for transit lightcurves analysis. It was applied to $1598$ amateur and professional transit observations of $26$ targets being monitored in the EXPANSION project. We detected $109$ statistically significant candidate events revealing a roughly $2:1$ asymmetry in favor of spots-crossings over faculae-crossings. Although some candidate anomalies likely appear non-physical and originate from systematic errors, such asymmetry between negative and positive events should indicate a physical difference between the frequency of star spots and faculae. Detected spot-crossing events also reveal positive correlation between their amplitude and width, possibly owed to spot size correlation. However, the frequency of all detectable crossing events appears just about a few per cent, so they cannot explain excessive transit timing noise observed for several targets., Comment: 30 pages, 9 figures, 1 table; accepted by Acta Astronomica
Published: 2021
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3. Discovery of a young low-mass brown dwarf transiting a fast-rotating F-type star by the Galactic Plane eXoplanet (GPX) survey

Author: Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštienė, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Horta, F. Grau, Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., and Henze, C. E.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of $19.7\pm 1.6$ $M_{\mathrm{Jup}}$ and a radius of $1.47\pm0.10$ $R_{\mathrm{Jup}}$, the first sub-stellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright ($V$ = 12.3 mag) fast-rotating F-type star with a projected rotational velocity $v\sin{ i_*}=40\pm10$ km/s. We use the isochrone placement algorithm to characterize the host star, which has effective temperature $7000\pm200$ K, mass $1.68\pm0.10$ $M_{\mathrm{Sun}}$, radius $1.56\pm0.10$ $R_{\mathrm{Sun}}$ and approximate age $0.27_{-0.15}^{+0.09}$ Gyr. GPX-1 b has an orbital period of $\sim$1.75 d, and a transit depth of $0.90\pm0.03$ %. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a sub-stellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data is affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of Doppler tomography., Comment: 13 pages, 13 figures, accepted to MNRAS in May 2021
Published: 2020
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4. A Magnetic White Dwarf with Five H$\alpha$ Components

Author: Kilic, Mukremin, Rolland, B., Bergeron, P., Vanderbosch, Z., Benni, P., and Garlitz, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: G183$-$35 is an unusual white dwarf that shows an H$\alpha$ line split into five components, instead of the usual three components seen in strongly magnetic white dwarfs. Potential explanations for the unusual set of lines includes a double degenerate system containing two magnetic white dwarfs and/or rotational modulation of a complex magnetic field structure. Here we present time-resolved spectroscopy of G183$-$35 obtained at the Gemini Observatory. These data reveal two sets of absorption lines that appear and disappear over a period of about 4 hours. We also detect low-level (0.2%) variability in optical photometry at the same period. We demonstrate that the spectroscopic and photometric variability can be explained by the presence of spots on the surface of the white dwarf and a change in the average field strength from about 4.6 MG to 6.2 MG. The observed variability is clearly due to G183$-$35's relatively short spin period. However, rotational modulation of a complex magnetic field by itself cannot explain the changes seen in the central H$\alpha$ component. An additional source of variability in the line profiles, most likely due to a chemically inhomogeneous surface composition, is also needed. We propose further observations of similar objects to test this scenario., Comment: MNRAS, in press
Published: 2019
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5. Homogeneously derived transit timings for 17 exoplanets and reassessed TTV trends for WASP-12 and WASP-4

Author: Baluev, R. V., Sokov, E. N., Jones, H. R. A., Shaidulin, V. Sh., Sokova, I. A., Nielsen, L. D., Benni, P., Schneiter, E. M., D'Angelo, C. Villarreal, Fernández-Lajús, E., Di Sisto, R. P., Baştürk, Ö., Bretton, M., Wunsche, A., Hentunen, V. -P., Shadick, S., Jongen, Y., Kang, W., Kim, T., Pakštienė, E., Qvam, J. K. T., Knight, C. R., Guerra, P., Marchini, A., Salvaggio, F., Papini, R., Evans, P., Salisbury, M., Garcia, F., Molina, D., Garlitz, J., Esseiva, N., Ogmen, Y., Karavaev, Yu., Rusov, S., Ibrahimov, M. A., and Karimov, R. G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We homogeneously analyse $\sim 3.2\times 10^5$ photometric measurements for $\sim 1100$ transit lightcurves belonging to $17$ exoplanet hosts. The photometric data cover $16$ years 2004--2019 and include amateur and professional observations. Old archival lightcurves were reprocessed using up-to-date exoplanetary parameters and empirically debiased limb-darkening models. We also derive self-consistent transit and radial-velocity fits for $13$ targets. We confirm the nonlinear TTV trend in the WASP-12 data at a high significance, and with a consistent magnitude. However, Doppler data reveal hints of a radial acceleration about $(-7.5\pm 2.2)$~m/s/yr, indicating the presence of unseen distant companions, and suggesting that roughly $10$ per cent of the observed TTV was induced via the light-travel (or Roemer) effect. For WASP-4, a similar TTV trend suspected after the recent TESS observations appears controversial and model-dependent. It is not supported by our homogeneus TTV sample, including $10$ ground-based EXPANSION lightcurves obtained in 2018 simultaneously with TESS. Even if the TTV trend itself does exist in WASP-4, its magnitude and tidal nature are uncertain. Doppler data cannot entirely rule out the Roemer effect induced by possible distant companions., Comment: 19 pages, 4 figures, 6 tables; revised manuscript submitted to MNRAS; online-only supplements are in the download archive
Published: 2019
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6. Thermal properties of slowly rotating asteroids: Results from a targeted survey

Author: Marciniak, A., Alí-Lagoa, V., Müller, T. G., Szakáts, R., Molnár, L., Pál, A., Gaca, E. Podlewska, Parley, N., Antonini, P., Barbotin, E., Behrend, R., Bernasconi, L., Bąk, M. Butkiewicz, Crippa, R., Duffard, R., Ditteon, R., Feuerbach, M., Fauvaud, S., Garlitz, J., Geier, S., Goncalves, R., Grice, J., Grześkowiak, I., Hirsch, R., Horbowicz, J., Kamiński, K., Kamińska, M. K., Kim, D. -H., Kim, M. -J., Konstanciak, I., Kudak, V., Kulczak, P., Maestre, J. L., Manzini, F., Marks, S., Monteiro, F., Ogłoza, W., Oszkiewicz, D., Pilcher, F., Perig, V., Polakis, T., Polińska, M., Roy, R., Sanabria, J. J., Santana-Ros, T., Skiff, B., Skrzypek, J., Sobkowiak, K., Sonbas, E., Thizy, O., Trela, P., Urakawa, S., Żejmo, M., and Żukowski, K.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the sub-surface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 hours, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3$^{+33}_{-3}$ and 45$^{+60}_{-30}$ Jm$^{-2}$s$^{-1/2}$K$^{-1}$. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2019
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7. Discovery of XO-6b: a hot Jupiter transiting a fast rotating F5 star on an oblique orbit

Author: Crouzet, N., McCullough, P. R., Long, D., Rodriguez, P. Montanes, Etangs, A. Lecavelier des, Ribas, I., Bourrier, V., Hébrard, G., Vilardell, F., Deleuil, M., Herrero, E., Garcia-Melendo, E., Akhenak, L., Foote, J., Gary, B., Benni, P., Guillot, T., Conjat, M., Mékarnia, D., Garlitz, J., Burke, C. J., Courcol, B., and Demangeon, O.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Only a few hot Jupiters are known to orbit around fast rotating stars. These exoplanets are harder to detect and characterize and may be less common than around slow rotators. Here, we report the discovery of the transiting hot Jupiter XO-6b, which orbits a bright, hot, and fast rotating star: V = 10.25, Teff = 6720 +/- 100 K, v sin i = 48 +/- 3 km/s. We detected the planet from its transits using the XO instruments and conducted a follow-up campaign. Because of the fast stellar rotation, radial velocities taken along the orbit do not yield the planet's mass with a high confidence level, but we secure a 3-sigma upper limit Mp < 4.4 MJup. We also obtain high resolution spectroscopic observations of the transit with the SOPHIE spectrograph at the 193-cm telescope of the Observatoire de Haute-Provence and analyze the stellar lines profile by Doppler tomography. The transit is clearly detected in the spectra. The radii measured independently from the tomographic analysis and from the photometric lightcurves are consistent, showing that the object detected by both methods is the same and indeed transits in front of XO-6. We find that XO-6b lies on a prograde and misaligned orbit with a sky-projected obliquity lambda = -20.7 +/- 2.3 deg. The rotation period of the star is shorter than the orbital period of the planet: Prot < 2.12 days, Porb = 3.77 days. Thus, this system stands in a largely unexplored regime of dynamical interactions between close-in giant planets and their host stars., Comment: 12 pages, 11 figures, Accepted for publication in AJ
Published: 2016
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8. New and updated convex shape models of asteroids based on optical data from a large collaboration network

Author: Hanuš, J., Ďurech, J., Oszkiewicz, D. A., Behrend, R., Carry, B., Delbo', M., Adam, O., Afonina, V., Anquetin, R., Antonini, P., Arnold, L., Audejean, M., Aurard, P., Bachschmidt, M., Badue, B., Barbotin, E., Barroy, P., Baudouin, P., Berard, L., Berger, N., Bernasconi, L., Bosch, J-G., Bouley, S., Bozhinova, I., Brinsfield, J., Brunetto, L., Canaud, G., Caron, J., Carrier, F., Casalnuovo, G., Casulli, S., Cerda, M., Chalamet, L., Charbonnel, S., Chinaglia, B., Cikota, A., Colas, F., Coliac, J-F., Collet, A., Coloma, J., Conjat, M., Conseil, E., Costa, R., Crippa, R., Cristofanelli, M., Damerdji, Y., Debackere, A., Decock, A., Déhais, Q., Déléage, T., Delmelle, S., Demeautis, C., Dróżdż, M., Dubos, G., Dulcamara, T., Dumont, M., Durkee, R., Dymock, R., del Valle, A. Escalante, Esseiva, N., Esseiva, R., Esteban, M., Fauchez, T., Fauerbach, M., Fauvaud, M., Fauvaud, S., Forné, E., Fournel, C., Fradet, D., Garlitz, J., Gerteis, O., Gillier, C., Gillon, M., Giraud, R., Godard, J-P., Goncalves, R., Hamanowa, H., Hay, K., Hellmich, S., Heterier, S., Higgins, D., Hirsch, R., Hodosan, G., Hren, M., Hygate, A., Innocent, N., Jacquinot, H., Jawahar, S., Jehin, E., Jerosimic, L., Klotz, A., Koff, W., Korlevic, P., Kosturkiewicz, E., Krafft, P., Krugly, Y., Kugel, F., Labrevoir, O., Lecacheux, J., Lehký, M., Leroy, A., Lesquerbault, B., Lopez-Gonzales, M. J., Lutz, M., Mallecot, B., Manfroid, J., Manzini, F., Marciniak, A., Martin, A., Modave, B., Montaigut, R., Montier, J., Morelle, E., Morton, B., Mottola, S., Naves, R., Nomen, J., Oey, J., Ogłoza, W., Paiella, M., Pallares, H., Peyrot, A., Pilcher, F., Pirenne, J-F., Piron, P., Polinska, M., Polotto, M., Poncy, R., Previt, J. P., Reignier, F., Renauld, D., Ricci, D., Richard, F., Rinner, C., Risoldi, V., Robilliard, D., Romeuf, D., Rousseau, G., Roy, R., Ruthroff, J., Salom, P. A., Salvador, L., Sanchez, S., Santana-Ros, T., Scholz, A., Séné, G., Skiff, B., Sobkowiak, K., Sogorb, P., Soldán, F., Spiridakis, A., Splanska, E., Sposetti, S., Starkey, D., Stephens, R., Stiepen, A., Stoss, R., Strajnic, J., Teng, J-P., Tumolo, G., Vagnozzi, A., Vanoutryve, B., Vugnon, J. M., Warner, B. D., Waucomont, M., Wertz, O., Winiarski, M., and Wolf, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. This amount already provided a deep insight into physical properties of main-belt asteroids or large collisional families. We aim to increase the number of asteroid shape models and rotation states. Such results are an important input for various further studies such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides, in combination with known masses, bulk density estimates, but constrains also theoretical collisional and evolutional models of the Solar System. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as an input for the convex inversion method, and derive 3D shape models of asteroids, together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that one hundred observers who submit their optical data to publicly available databases. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature or their masses will be most likely determined from their gravitational influence on smaller bodies, which orbital deflection will be observed by the ESA Gaia astrometric mission. This was achieved by using additional optical data from recent apparitions for the shape optimization. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and 3 near-Earth asteroids., Comment: Accepted for publication in A&A
Published: 2015
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9. ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations

Author: Kokori, A., primary, Tsiaras, A., additional, Edwards, B., additional, Jones, A., additional, Pantelidou, G., additional, Tinetti, G., additional, Bewersdorff, L., additional, Iliadou, A., additional, Jongen, Y., additional, Lekkas, G., additional, Nastasi, A., additional, Poultourtzidis, E., additional, Sidiropoulos, C., additional, Walter, F., additional, Wünsche, A., additional, Abraham, R., additional, Agnihotri, V. K., additional, Albanesi, R., additional, Arce-Mansego, E., additional, Arnot, D., additional, Audejean, M., additional, Aumasson, C., additional, Bachschmidt, M., additional, Baj, G., additional, Barroy, P. R., additional, Belinski, A. A., additional, Bennett, D., additional, Benni, P., additional, Bernacki, K., additional, Betti, L., additional, Biagini, A., additional, Bosch, P., additional, Brandebourg, P., additional, Brát, L., additional, Bretton, M., additional, Brincat, S. M., additional, Brouillard, S., additional, Bruzas, A., additional, Bruzzone, A., additional, Buckland, R. A., additional, Caló, M., additional, Campos, F., additional, Carreño, A., additional, Carrion Rodrigo, J. A., additional, Casali, R., additional, Casalnuovo, G., additional, Cataneo, M., additional, Chang, C.-M., additional, Changeat, L., additional, Chowdhury, V., additional, Ciantini, R., additional, Cilluffo, M., additional, Coliac, J.-F., additional, Conzo, G., additional, Correa, M., additional, Coulon, G., additional, Crouzet, N., additional, Crow, M. V., additional, Curtis, I. A., additional, Daniel, D., additional, Dauchet, B., additional, Dawes, S., additional, Deldem, M., additional, Deligeorgopoulos, D., additional, Dransfield, G., additional, Dymock, R., additional, Eenmäe, T., additional, Esseiva, N., additional, Evans, P., additional, Falco, C., additional, Farfán, R. G., additional, Fernández-Lajús, E., additional, Ferratfiat, S., additional, Ferreira, S. L., additional, Ferretti, A., additional, Fiołka, J., additional, Fowler, M., additional, Futcher, S. R., additional, Gabellini, D., additional, Gainey, T., additional, Gaitan, J., additional, Gajdoš, P., additional, García-Sánchez, A., additional, Garlitz, J., additional, Gillier, C., additional, Gison, C., additional, Gonzales, J., additional, Gorshanov, D., additional, Grau Horta, F., additional, Grivas, G., additional, Guerra, P., additional, Guillot, T., additional, Haswell, C. A., additional, Haymes, T., additional, Hentunen, V.-P., additional, Hills, K., additional, Hose, K., additional, Humbert, T., additional, Hurter, F., additional, Hynek, T., additional, Irzyk, M., additional, Jacobsen, J., additional, Jannetta, A. L., additional, Johnson, K., additional, Jóźwik-Wabik, P., additional, Kaeouach, A. E., additional, Kang, W., additional, Kiiskinen, H., additional, Kim, T., additional, Kivila, Ü., additional, Koch, B., additional, Kolb, U., additional, Kučáková, H., additional, Lai, S.-P., additional, Laloum, D., additional, Lasota, S., additional, Lewis, L. A., additional, Liakos, G.-I., additional, Libotte, F., additional, Lomoz, F., additional, Lopresti, C., additional, Majewski, R., additional, Malcher, A., additional, Mallonn, M., additional, Mannucci, M., additional, Marchini, A., additional, Mari, J.-M., additional, Marino, A., additional, Marino, G., additional, Mario, J.-C., additional, Marquette, J.-B., additional, Martínez-Bravo, F. A., additional, Mašek, M., additional, Matassa, P., additional, Michel, P., additional, Michelet, J., additional, Miller, M., additional, Miny, E., additional, Molina, D., additional, Mollier, T., additional, Monteleone, B., additional, Montigiani, N., additional, Morales-Aimar, M., additional, Mortari, F., additional, Morvan, M., additional, Mugnai, L. V., additional, Murawski, G., additional, Naponiello, L., additional, Naudin, J.-L., additional, Naves, R., additional, Néel, D., additional, Neito, R., additional, Neveu, S., additional, Noschese, A., additional, Öğmen, Y., additional, Ohshima, O., additional, Orbanic, Z., additional, Pace, E. P., additional, Pantacchini, C., additional, Paschalis, N. I., additional, Pereira, C., additional, Peretto, I., additional, Perroud, V., additional, Phillips, M., additional, Pintr, P., additional, Pioppa, J.-B., additional, Plazas, J., additional, Poelarends, A. J., additional, Popowicz, A., additional, Purcell, J., additional, Quinn, N., additional, Raetz, M., additional, Rees, D., additional, Regembal, F., additional, Rocchetto, M., additional, Rocci, P.-F., additional, Rockenbauer, M., additional, Roth, R., additional, Rousselot, L., additional, Rubia, X., additional, Ruocco, N., additional, Russo, E., additional, Salisbury, M., additional, Salvaggio, F., additional, Santos, A., additional, Savage, J., additional, Scaggiante, F., additional, Sedita, D., additional, Shadick, S., additional, Silva, A. F., additional, Sioulas, N., additional, Školník, V., additional, Smith, M., additional, Smolka, M., additional, Solmaz, A., additional, Stanbury, N., additional, Stouraitis, D., additional, Tan, T.-G., additional, Theusner, M., additional, Thurston, G., additional, Tifner, F. P., additional, Tomacelli, A., additional, Tomatis, A., additional, Trnka, J., additional, Tylšar, M., additional, Valeau, P., additional, Vignes, J.-P., additional, Villa, A., additional, Sureda, A. Vives, additional, Vora, K., additional, Vrašt’ák, M., additional, Walliang, D., additional, Wenzel, B., additional, Wright, D. E., additional, Zambelli, R., additional, Zhang, M., additional, and Zíbar, M., additional
Published: 2023
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10. Discovery of a Young Low-Mass Brown Dwarf Transiting a Fast-Rotating F-Type Star by the Galactic Plane eXoplanet (GPX) Survey

Author: Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštiene, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Grau Horta, F., Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., Henze, C. E., Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštiene, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Grau Horta, F., Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., and Henze, C. E.
Abstract: We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of 19.7 ± 1.6 MJup and a radius of 1.47 ± 0.10 RJup, the first substellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright (V = 12.3 mag) fast-rotating F-type star with a projected rotational velocity v sin i∗ = 40 ± 10 km s−1. We use the isochrone placement algorithm to characterize the host star, which has effective temperature 7000 ± 200 K, mass 1.68 ± 0.10 M☉, radius 1.56 ± 0.10 R☉, and approximate age 0.27-0.15+0.09 Gyr. GPX-1 b has an orbital period of -1.75 d and a transit depth of 0.90 ± 0.03 per cent. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a substellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data are affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of the Doppler tomography. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
Published: 2021

11. Discovery of a young low-mass brown dwarf transiting a fast-rotating F-type star by the Galactic Plane eXoplanet (GPX) survey

Author: Benni, P, primary, Burdanov, A Y, additional, Krushinsky, V V, additional, Bonfanti, A, additional, Hébrard, G, additional, Almenara, J M, additional, Dalal, S, additional, Demangeon, O D S, additional, Tsantaki, M, additional, Pepper, J, additional, Stassun, K G, additional, Vanderburg, A, additional, Belinski, A, additional, Kashaev, F, additional, Barkaoui, K, additional, Kim, T, additional, Kang, W, additional, Antonyuk, K, additional, Dyachenko, V V, additional, Rastegaev, D A, additional, Beskakotov, A, additional, Mitrofanova, A A, additional, Pozuelos, F J, additional, Kuznetsov, E D, additional, Popov, A, additional, Kiefer, F, additional, Wilson, P A, additional, Ricker, G, additional, Vanderspek, R, additional, Latham, D W, additional, Seager, S, additional, Jenkins, J M, additional, Sokov, E, additional, Sokova, I, additional, Marchini, A, additional, Papini, R, additional, Salvaggio, F, additional, Banfi, M, additional, Baştürk, Ö, additional, Torun, Ş, additional, Yalçınkaya, S, additional, Ivanov, K, additional, Valyavin, G, additional, Jehin, E, additional, Gillon, M, additional, Pakštienė, E, additional, Hentunen, V-P, additional, Shadick, S, additional, Bretton, M, additional, Wünsche, A, additional, Garlitz, J, additional, Jongen, Y, additional, Molina, D, additional, Girardin, E, additional, Grau Horta, F, additional, Naves, R, additional, Benkhaldoun, Z, additional, Joner, M D, additional, Spencer, M, additional, Bieryla, A, additional, Stevens, D J, additional, Jensen, E L N, additional, Collins, K A, additional, Charbonneau, D, additional, Quintana, E V, additional, Mullally, S E, additional, and Henze, C E, additional
Published: 2021
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12. Thermal properties of slowly rotating asteroids: results from a targeted survey

Author: National Science Centre (Poland), European Commission, Ministry of Education (Slovak Republic), Ministerio de Ciencia, Innovación y Universidades (España), Hungarian Academy of Sciences, Marciniak, A., Ali-Lagoa, Victor, Mueller, T.G., Szakáts, R., Molnár, L., Pal, A., Podlewska-Gaca, E., Parley, N., Antonini, P., Barbotin, E., Behrend, R., Bernasconi, L., Butkiewicz-Bąk, M., Crippa, R., Duffard, René D., Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S., Goncalves, R, Grice, J., Grzeskowiak, I, Hirsch, R., Horbowicz, J, Kaminski, K., Kamińska, M. K., Kim, D. H., Kim, M. J., Konstanciak, I., Kudak, V., Kulczak, P, Maestre, J.L., Manzini, F., Marks, S, Monteiro, F, Ogloza, W, Oszkiewicz, D., Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R., Sanabria, JJ, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, Zukowski, K, National Science Centre (Poland), European Commission, Ministry of Education (Slovak Republic), Ministerio de Ciencia, Innovación y Universidades (España), Hungarian Academy of Sciences, Marciniak, A., Ali-Lagoa, Victor, Mueller, T.G., Szakáts, R., Molnár, L., Pal, A., Podlewska-Gaca, E., Parley, N., Antonini, P., Barbotin, E., Behrend, R., Bernasconi, L., Butkiewicz-Bąk, M., Crippa, R., Duffard, René D., Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S., Goncalves, R, Grice, J., Grzeskowiak, I, Hirsch, R., Horbowicz, J, Kaminski, K., Kamińska, M. K., Kim, D. H., Kim, M. J., Konstanciak, I., Kudak, V., Kulczak, P, Maestre, J.L., Manzini, F., Marks, S, Monteiro, F, Ogloza, W, Oszkiewicz, D., Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R., Sanabria, JJ, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, and Zukowski, K
Abstract: Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the subsurface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 h, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3(-3)(+33) and 45(-30)(+60) Jm(-2) s(-1/2) K-1. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.© ESO 2019
Published: 2019

13. The PHEMU15 catalogue and astrometric results of the Jupiter's Galilean satellite mutual occultation and eclipse observations made in 2014-2015

Author: Saquet, E. Emelyanov, N. Robert, V. Arlot, J.-E. Anbazhagan, P. Baillié, K. Bardecker, J. Berezhnoy, A.A. Bretton, M. Campos, F. Capannoli, L. Carry, B. Castet, M. Charbonnier, Y. Chernikov, M.M. Christou, A. Colas, F. Coliac, J.-F. Dangl, G. Dechambre, O. Delcroix, M. Dias-Oliveira, A. Drillaud, C. Duchemin, Y. Dunford, R. Dupouy, P. Ellington, C. Fabre, P. Filippov, V.A. Finnegan, J. Foglia, S. Font, D. Gaillard, B. Galli, G. Garlitz, J. Gasmi, A. Gaspar, H.S. Gault, D. Gazeas, K. George, T. Gorda, S.Y. Gorshanov, D.L. Gualdoni, C. Guhl, K. Halir, K. Hanna, W. Henry, X. Herald, D. Houdin, G. Ito, Y. Izmailov, I.S. Jacobsen, J. Jones, A. Kamoun, S. Kardasis, E. Karimov, A.M. Khovritchev, M.Y. Kulikova, A.M. Laborde, J. Lainey, V. Lavayssiere, M. Le Guen, P. Leroy, A. Loader, B. Lopez, O.C. Lyashenko, A.Y. Lyssenko, P.G. Machado, D.I. Maigurova, N. Manek, J. Marchini, A. Midavaine, T. Montier, J. Morgado, B.E. Naumov, K.N. Nedelcu, A. Newman, J. Ohlert, J.M. Oksanen, A. Pavlov, H. Petrescu, E. Pomazan, A. Popescu, M. Pratt, A. Raskhozhev, V.N. Resch, J.-M. Robilliard, D. Roschina, E. Rothenberg, E. Rottenborn, M. Rusov, S.A. Saby, F. Saya, L.F. Selvakumar, G. Signoret, F. Slesarenko, V.Y. Sokov, E.N. Soldateschi, J. Sonka, A. Soulie, G. Talbot, J. Tejfel, V.G. Thuillot, W. Timerson, B. Toma, R. Torsellini, S. Trabuco, L.L. Traverse, P. Tsamis, V. Unwin, M. Van Den Abbeel, F. Vandenbruaene, H. Vasundhara, R. Velikodsky, Y.I. Vienne, A. Vilar, J. Vugnon, J.-M. Wuensche, N. Zeleny, P.
Subjects: Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: During the 2014-2015 mutual events season, the Institut de Mécanique Céleste et de Calcul des Éphémérides (IMCCE), Paris, France, and the Sternberg Astronomical Institute (SAI), Moscow, Russia, led an international observation campaign to record ground-based photometric observations of Galilean moon mutual occultations and eclipses.We focused on processing the complete photometric observations data base to compute new accurate astrometric positions. We used our method to derive astrometric positions from the light curves of the events. We developed an accurate photometric model of mutual occultations and eclipses, while correcting for the satellite albedos, Hapke's light scattering law, the phase effect, and the limb darkening. We processed 609 light curves, and we compared the observed positions of the satellites with the theoretical positions from IMCCE NOE-5-2010-GAL satellite ephemerides and INPOP13c planetary ephemeris. The standard deviation after fitting the light curve in equatorial positions is ±24 mas, or 75 km at Jupiter. The rms (O-C) in equatorial positions is ±50 mas, or 150 km at Jupiter. © 2017 The Author(s).
Published: 2018

14. Homogeneously derived transit timings for 17 exoplanets and reassessed TTV trends for WASP-12 and WASP-4

Author: Baluev, R V, primary, Sokov, E N, additional, Jones, H R A, additional, Shaidulin, V Sh, additional, Sokova, I A, additional, Nielsen, L D, additional, Benni, P, additional, Schneiter, E M, additional, Villarreal D’Angelo, C, additional, Fernández-Lajús, E, additional, Di Sisto, R P, additional, Baştürk, Ö, additional, Bretton, M, additional, Wunsche, A, additional, Hentunen, V-P, additional, Shadick, S, additional, Jongen, Y, additional, Kang, W, additional, Kim, T, additional, Pakštienė, E, additional, Qvam, J K T, additional, Knight, C R, additional, Guerra, P, additional, Marchini, A, additional, Salvaggio, F, additional, Papini, R, additional, Evans, P, additional, Salisbury, M, additional, Garcia, F, additional, Molina, D, additional, Garlitz, J, additional, Esseiva, N, additional, Ogmen, Y, additional, Karavaev, Yu, additional, Rusov, S, additional, Ibrahimov, M A, additional, and Karimov, R G, additional
Published: 2019
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15. A magnetic white dwarf with five H α components

Author: Kilic, Mukremin, primary, Rolland, B, additional, Bergeron, P, additional, Vanderbosch, Z, additional, Benni, P, additional, and Garlitz, J, additional
Published: 2019
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16. Thermal properties of slowly rotating asteroids: results from a targeted survey

Author: Marciniak, A., primary, Alí-Lagoa, V., additional, Müller, T. G., additional, Szakáts, R., additional, Molnár, L., additional, Pál, A., additional, Podlewska-Gaca, E., additional, Parley, N., additional, Antonini, P., additional, Barbotin, E., additional, Behrend, R., additional, Bernasconi, L., additional, Butkiewicz-Bąk, M., additional, Crippa, R., additional, Duffard, R., additional, Ditteon, R., additional, Feuerbach, M., additional, Fauvaud, S., additional, Garlitz, J., additional, Geier, S., additional, Goncalves, R., additional, Grice, J., additional, Grześkowiak, I., additional, Hirsch, R., additional, Horbowicz, J., additional, Kamiński, K., additional, Kamińska, M. K., additional, Kim, D.-H., additional, Kim, M.-J., additional, Konstanciak, I., additional, Kudak, V., additional, Kulczak, P., additional, Maestre, J. L., additional, Manzini, F., additional, Marks, S., additional, Monteiro, F., additional, Ogłoza, W., additional, Oszkiewicz, D., additional, Pilcher, F., additional, Perig, V., additional, Polakis, T., additional, Polińska, M., additional, Roy, R., additional, Sanabria, J. J., additional, Santana-Ros, T., additional, Skiff, B., additional, Skrzypek, J., additional, Sobkowiak, K., additional, Sonbas, E., additional, Thizy, O., additional, Trela, P., additional, Urakawa, S., additional, Żejmo, M., additional, and Żukowski, K., additional
Published: 2019
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17. Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit

Author: Universitat Politècnica de Catalunya. Departament de Física, Crouzet, N., McCullough, Peter, Long, D., Montañes Rodriguez, Pilar, Lecavelier des Etangs, A, Ribas, Ignasi, Bourrier, V., Hébrard, G., Vilardell, Francesc, Deleuil, M., Herrero, Enrique, García Melendo, Enrique José, Akhenak, L., Foote, Cindy, Gary, B., Benny, P., Guillot, T., Conjat, M., Mékarnia, D., Garlitz, J., Burke, C. J., Courcol, B., Demangeon, O, Universitat Politècnica de Catalunya. Departament de Física, Crouzet, N., McCullough, Peter, Long, D., Montañes Rodriguez, Pilar, Lecavelier des Etangs, A, Ribas, Ignasi, Bourrier, V., Hébrard, G., Vilardell, Francesc, Deleuil, M., Herrero, Enrique, García Melendo, Enrique José, Akhenak, L., Foote, Cindy, Gary, B., Benny, P., Guillot, T., Conjat, M., Mékarnia, D., Garlitz, J., Burke, C. J., Courcol, B., and Demangeon, O
Abstract: © 2017. The American Astronomical Society. All rights reserved., Only a few hot Jupiters are known to orbit around fast rotating stars. These exoplanets are harder to detect and characterize and may be less common than around slow rotators. Here, we report the discovery of the transiting hot Jupiter XO-6b, which orbits a bright, hot, and fast rotating star: V = 10.25, T effsstarf = 6720 ± 100 K, v sin i sstarf = 48 ± 3 km s-1. We detected the planet from its transits using the XO instruments and conducted a follow-up campaign. Because of the fast stellar rotation, radial velocities taken along the orbit do not yield the planet's mass with a high confidence level, but we secure a 3s upper limit M p < 4.4 M Jup. We also obtain high-resolution spectroscopic observations of the transit with the SOPHIE spectrograph at the 193-cm telescope of the Observatoire de Haute-Provence and analyze the stellar lines profile by Doppler tomography. The transit is clearly detected in the spectra. The radii measured independently from the tomographic analysis and from the photometric light curves are consistent, showing that the object detected by both methods is the same and indeed transits in front of XO-6. We find that XO-6b lies on a prograde and misaligned orbit with a sky-projected obliquity ${\boldsymbol{\lambda }}=-20\buildrel{\circ}\over{.} 7\pm 2\buildrel{\circ}\over{.} 3$. The rotation period of the star is shorter than the orbital period of the planet: P rot < 2.12 days, P orb = 3.77 days. Thus, this system stands in a largely unexplored regime of dynamical interactions between close-in giant planets and their host stars., Peer Reviewed, Postprint (published version)
Published: 2017

18. The PHEMU15 catalogue and astrometric results of the Jupiter's Galilean satellite mutual occultation and eclipse observations made in 2014–2015

Author: Saquet, E, primary, Emelyanov, N, additional, Robert, V, additional, Arlot, J-E, additional, Anbazhagan, P, additional, Baillié, K, additional, Bardecker, J, additional, Berezhnoy, A A, additional, Bretton, M, additional, Campos, F, additional, Capannoli, L, additional, Carry, B, additional, Castet, M, additional, Charbonnier, Y, additional, Chernikov, M M, additional, Christou, A, additional, Colas, F, additional, Coliac, J-F, additional, Dangl, G, additional, Dechambre, O, additional, Delcroix, M, additional, Dias-Oliveira, A, additional, Drillaud, C, additional, Duchemin, Y, additional, Dunford, R, additional, Dupouy, P, additional, Ellington, C, additional, Fabre, P, additional, Filippov, V A, additional, Finnegan, J, additional, Foglia, S, additional, Font, D, additional, Gaillard, B, additional, Galli, G, additional, Garlitz, J, additional, Gasmi, A, additional, Gaspar, H S, additional, Gault, D, additional, Gazeas, K, additional, George, T, additional, Gorda, S Y, additional, Gorshanov, D L, additional, Gualdoni, C, additional, Guhl, K, additional, Halir, K, additional, Hanna, W, additional, Henry, X, additional, Herald, D, additional, Houdin, G, additional, Ito, Y, additional, Izmailov, I S, additional, Jacobsen, J, additional, Jones, A, additional, Kamoun, S, additional, Kardasis, E, additional, Karimov, A M, additional, Khovritchev, M Y, additional, Kulikova, A M, additional, Laborde, J, additional, Lainey, V, additional, Lavayssiere, M, additional, Le Guen, P, additional, Leroy, A, additional, Loader, B, additional, Lopez, O C, additional, Lyashenko, A Y, additional, Lyssenko, P G, additional, Machado, D I, additional, Maigurova, N, additional, Manek, J, additional, Marchini, A, additional, Midavaine, T, additional, Montier, J, additional, Morgado, B E, additional, Naumov, K N, additional, Nedelcu, A, additional, Newman, J, additional, Ohlert, J M, additional, Oksanen, A, additional, Pavlov, H, additional, Petrescu, E, additional, Pomazan, A, additional, Popescu, M, additional, Pratt, A, additional, Raskhozhev, V N, additional, Resch, J-M, additional, Robilliard, D, additional, Roschina, E, additional, Rothenberg, E, additional, Rottenborn, M, additional, Rusov, S A, additional, Saby, F, additional, Saya, L F, additional, Selvakumar, G, additional, Signoret, F, additional, Slesarenko, V Y, additional, Sokov, E N, additional, Soldateschi, J, additional, Sonka, A, additional, Soulie, G, additional, Talbot, J, additional, Tejfel, V G, additional, Thuillot, W, additional, Timerson, B, additional, Toma, R, additional, Torsellini, S, additional, Trabuco, L L, additional, Traverse, P, additional, Tsamis, V, additional, Unwin, M, additional, Abbeel, F Van Den, additional, Vandenbruaene, H, additional, Vasundhara, R, additional, Velikodsky, Y I, additional, Vienne, A, additional, Vilar, J, additional, Vugnon, J-M, additional, Wuensche, N, additional, and Zeleny, P, additional
Published: 2017
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19. Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit

Author: Crouzet, N., primary, McCullough, P. R., additional, Long, D., additional, Rodriguez, P. Montanes, additional, Etangs, A. Lecavelier des, additional, Ribas, I., additional, Bourrier, V., additional, Hébrard, G., additional, Vilardell, F., additional, Deleuil, M., additional, Herrero, E., additional, Garcia-Melendo, E., additional, Akhenak, L., additional, Foote, J., additional, Gary, B., additional, Benni, P., additional, Guillot, T., additional, Conjat, M., additional, Mékarnia, D., additional, Garlitz, J., additional, Burke, C. J., additional, Courcol, B., additional, and Demangeon, O., additional
Published: 2017
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20. New and updated convex shape models of asteroids based on optical data from a large collaboration network

Author: Hanuš, J., primary, Ďurech, J., additional, Oszkiewicz, D. A., additional, Behrend, R., additional, Carry, B., additional, Delbo, M., additional, Adam, O., additional, Afonina, V., additional, Anquetin, R., additional, Antonini, P., additional, Arnold, L., additional, Audejean, M., additional, Aurard, P., additional, Bachschmidt, M., additional, Baduel, B., additional, Barbotin, E., additional, Barroy, P., additional, Baudouin, P., additional, Berard, L., additional, Berger, N., additional, Bernasconi, L., additional, Bosch, J-G., additional, Bouley, S., additional, Bozhinova, I., additional, Brinsfield, J., additional, Brunetto, L., additional, Canaud, G., additional, Caron, J., additional, Carrier, F., additional, Casalnuovo, G., additional, Casulli, S., additional, Cerda, M., additional, Chalamet, L., additional, Charbonnel, S., additional, Chinaglia, B., additional, Cikota, A., additional, Colas, F., additional, Coliac, J.-F., additional, Collet, A., additional, Coloma, J., additional, Conjat, M., additional, Conseil, E., additional, Costa, R., additional, Crippa, R., additional, Cristofanelli, M., additional, Damerdji, Y., additional, Debackère, A., additional, Decock, A., additional, Déhais, Q., additional, Déléage, T., additional, Delmelle, S., additional, Demeautis, C., additional, Dróżdż, M., additional, Dubos, G., additional, Dulcamara, T., additional, Dumont, M., additional, Durkee, R., additional, Dymock, R., additional, Escalante del Valle, A., additional, Esseiva, N., additional, Esseiva, R., additional, Esteban, M., additional, Fauchez, T., additional, Fauerbach, M., additional, Fauvaud, M., additional, Fauvaud, S., additional, Forné, E., additional, Fournel, C., additional, Fradet, D., additional, Garlitz, J., additional, Gerteis, O., additional, Gillier, C., additional, Gillon, M., additional, Giraud, R., additional, Godard, J.-P., additional, Goncalves, R., additional, Hamanowa, Hiroko, additional, Hamanowa, Hiromi, additional, Hay, K., additional, Hellmich, S., additional, Heterier, S., additional, Higgins, D., additional, Hirsch, R., additional, Hodosan, G., additional, Hren, M., additional, Hygate, A., additional, Innocent, N., additional, Jacquinot, H., additional, Jawahar, S., additional, Jehin, E., additional, Jerosimic, L., additional, Klotz, A., additional, Koff, W., additional, Korlevic, P., additional, Kosturkiewicz, E., additional, Krafft, P., additional, Krugly, Y., additional, Kugel, F., additional, Labrevoir, O., additional, Lecacheux, J., additional, Lehký, M., additional, Leroy, A., additional, Lesquerbault, B., additional, Lopez-Gonzales, M. J., additional, Lutz, M., additional, Mallecot, B., additional, Manfroid, J., additional, Manzini, F., additional, Marciniak, A., additional, Martin, A., additional, Modave, B., additional, Montaigut, R., additional, Montier, J., additional, Morelle, E., additional, Morton, B., additional, Mottola, S., additional, Naves, R., additional, Nomen, J., additional, Oey, J., additional, Ogłoza, W., additional, Paiella, M., additional, Pallares, H., additional, Peyrot, A., additional, Pilcher, F., additional, Pirenne, J.-F., additional, Piron, P., additional, Polińska, M., additional, Polotto, M., additional, Poncy, R., additional, Previt, J. P., additional, Reignier, F., additional, Renauld, D., additional, Ricci, D., additional, Richard, F., additional, Rinner, C., additional, Risoldi, V., additional, Robilliard, D., additional, Romeuf, D., additional, Rousseau, G., additional, Roy, R., additional, Ruthroff, J., additional, Salom, P. A., additional, Salvador, L., additional, Sanchez, S., additional, Santana-Ros, T., additional, Scholz, A., additional, Séné, G., additional, Skiff, B., additional, Sobkowiak, K., additional, Sogorb, P., additional, Soldán, F., additional, Spiridakis, A., additional, Splanska, E., additional, Sposetti, S., additional, Starkey, D., additional, Stephens, R., additional, Stiepen, A., additional, Stoss, R., additional, Strajnic, J., additional, Teng, J.-P., additional, Tumolo, G., additional, Vagnozzi, A., additional, Vanoutryve, B., additional, Vugnon, J. M., additional, Warner, B. D., additional, Waucomont, M., additional, Wertz, O., additional, Winiarski, M., additional, and Wolf, M., additional
Published: 2016
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21. The PHEMU09 catalogue and astrometric results of the observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made in 2009

Author: Arlot, J. -E., Emelyanov, N., Varfolomeev, M. I., Amossé, A., Arena, C., Assafin, M., Barbieri, L., Bolzoni, S., Bragas-Ribas, F., Camargo, J. I. B., Casarramona, F., Casas, R., Christou, A., Colas, F., Collard, A., Combe, S., Constantinescu, M., Dangl, G., De, Cat, P., Degenhardt, S., Delcroix, M., Dias-Oliveira, A., Dourneau, G., Douvris, A., Druon, C., Ellington, C. K., Estraviz, G., Farissier, P., Farmakopoulos, A., Garlitz, J., Gault, D., George, T., Gorda, S. Y., Grismore, J., Guo, D. F., Herald, D., Ida, M., Ishida, M., Ivanov, A. V., Klemt, B., Koshkin, N., Le, Campion, J. F., Liakos, A., Liao, S. L., Li, S. N., Loader, B., Lopresti, C., Lo, Savio, E., Marchini, A., Marino, G., Masi, G., Massallé, A., Maulella, R., Mcfarland, J., Miyashita, K., Napoli, C., Noyelles, B., Pauwels, T., Pavlov, H., Peng, Q. Y., Perelló, C., Priban, V., Prost, J., Razemon, S., Rousselle, J. P., Rovira, J., Ruisi, R., Ruocco, N., Salvaggio, F., Sbarufatti, G., Shakun, L., Scheck, A., Sciuto, C., Da, Silva, Neto, D. N., V, Sinyaeva, N., Sofia, A., Sonka, A., Talbot, J., Tang, Z. H., Tejfel, V. G., Thuillot, W., Tigani, K., Timerson, B., Tontodonati, E., Tsamis, V., Unwin, M., Venable, R., Vieira-Martins, R., Vilar, J., Vingerhoets, P., Watanabe, H., Yin, H. X., Yu, Y., Zambelli, R., Arlot, J. -E., Emelyanov, N., Varfolomeev, M. I., Amossé, A., Arena, C., Assafin, M., Barbieri, L., Bolzoni, S., Bragas-Ribas, F., Camargo, J. I. B., Casarramona, F., Casas, R., Christou, A., Colas, F., Collard, A., Combe, S., Constantinescu, M., Dangl, G., De, Cat, P., Degenhardt, S., Delcroix, M., Dias-Oliveira, A., Dourneau, G., Douvris, A., Druon, C., Ellington, C. K., Estraviz, G., Farissier, P., Farmakopoulos, A., Garlitz, J., Gault, D., George, T., Gorda, S. Y., Grismore, J., Guo, D. F., Herald, D., Ida, M., Ishida, M., Ivanov, A. V., Klemt, B., Koshkin, N., Le, Campion, J. F., Liakos, A., Liao, S. L., Li, S. N., Loader, B., Lopresti, C., Lo, Savio, E., Marchini, A., Marino, G., Masi, G., Massallé, A., Maulella, R., Mcfarland, J., Miyashita, K., Napoli, C., Noyelles, B., Pauwels, T., Pavlov, H., Peng, Q. Y., Perelló, C., Priban, V., Prost, J., Razemon, S., Rousselle, J. P., Rovira, J., Ruisi, R., Ruocco, N., Salvaggio, F., Sbarufatti, G., Shakun, L., Scheck, A., Sciuto, C., Da, Silva, Neto, D. N., V, Sinyaeva, N., Sofia, A., Sonka, A., Talbot, J., Tang, Z. H., Tejfel, V. G., Thuillot, W., Tigani, K., Timerson, B., Tontodonati, E., Tsamis, V., Unwin, M., Venable, R., Vieira-Martins, R., Vilar, J., Vingerhoets, P., Watanabe, H., Yin, H. X., Yu, Y., and Zambelli, R.
Abstract: Context. In 2009, the Sun and the Earth passed through the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. It was the equinox on Jupiter. This occurrence made mutual occultations and eclipses between the satellites possible. Experience has shown that the observations of such events provide accurate astrometric data able to bring new information on the dynamics of the Galilean satellites. Observations are made under the form of photometric measurements, but need to be made through the organization of a worldwide observation campaign maximizing the number and the quality of the data obtained. Aims. This work focuses on processing the complete database of photometric observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made during the international campaign in 2009. The final goal is to derive new accurate astrometric data. Methods. We used an accurate photometric model of mutual events adequate with the accuracy of the observation. Our original method was applied to derive astrometric data from photometric observations of mutual occultations and eclipses of the Galilean satellites of Jupiter. Results. We processed the 457 lightcurves obtained during the international campaign of photometric observations of the Galilean satellites of Jupiter in 2009. Compared with the theory, for successful observations, the r.m.s. of O-C residuals are equal to 45.8 mas and 81.1 mas in right ascension and declination, respectively; the mean O-C residuals are equal to -2 mas and -9 mas in right ascension and declination, respectively, for mutual occultations; and -6 mas and +1 mas in right ascension and declination, respectively, for mutual eclipses. © ESO, 2014.
Published: 2014

22. The PHEMU09 catalogue and astrometric results of the observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made in 2009

Author: Arlot, J.-E., primary, Emelyanov, N., additional, Varfolomeev, M. I., additional, Amossé, A., additional, Arena, C., additional, Assafin, M., additional, Barbieri, L., additional, Bolzoni, S., additional, Bragas-Ribas, F., additional, Camargo, J. I. B., additional, Casarramona, F., additional, Casas, R., additional, Christou, A., additional, Colas, F., additional, Collard, A., additional, Combe, S., additional, Constantinescu, M., additional, Dangl, G., additional, De Cat, P., additional, Degenhardt, S., additional, Delcroix, M., additional, Dias-Oliveira, A., additional, Dourneau, G., additional, Douvris, A., additional, Druon, C., additional, Ellington, C. K., additional, Estraviz, G., additional, Farissier, P., additional, Farmakopoulos, A., additional, Garlitz, J., additional, Gault, D., additional, George, T., additional, Gorda, S. Yu., additional, Grismore, J., additional, Guo, D. F., additional, Herald, D., additional, Ida, M., additional, Ishida, M., additional, Ivanov, A. V., additional, Klemt, B., additional, Koshkin, N., additional, Le Campion, J. F., additional, Liakos, A., additional, Liao, S. L., additional, Li, S. N., additional, Loader, B., additional, Lopresti, C., additional, Lo Savio, E., additional, Marchini, A., additional, Marino, G., additional, Masi, G., additional, Massallé, A., additional, Maulella, R., additional, McFarland, J., additional, Miyashita, K., additional, Napoli, C., additional, Noyelles, B., additional, Pauwels, T., additional, Pavlov, H., additional, Peng, Q. Y., additional, Perelló, C., additional, Priban, V., additional, Prost, J., additional, Razemon, S., additional, Rousselle, J. P., additional, Rovira, J., additional, Ruisi, R., additional, Ruocco, N., additional, Salvaggio, F., additional, Sbarufatti, G., additional, Shakun, L., additional, Scheck, A., additional, Sciuto, C., additional, da Silva Neto, D. N., additional, V Sinyaeva, N., additional, Sofia, A., additional, Sonka, A., additional, Talbot, J., additional, Tang, Z. H., additional, Tejfel, V. G., additional, Thuillot, W., additional, Tigani, K., additional, Timerson, B., additional, Tontodonati, E., additional, Tsamis, V., additional, Unwin, M., additional, Venable, R., additional, Vieira-Martins, R., additional, Vilar, J., additional, Vingerhoets, P., additional, Watanabe, H., additional, Yin, H. X., additional, Yu, Y., additional, and Zambelli, R., additional
Published: 2014
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23. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author: Arlot, J. -E., Thuillot, W., Ruatti, C., Ahmad, A., Amosse, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G. D., Christou, A. A., Coquerel, J. -P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T. N., Dorokhov, N. I., Dourneau, G., Duenas, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R. M. D., Gonzales, D., Gorda, S. Yu., Gorshanov, D. L., Hansen, M. W., Harrington, M., Irsmambetova, T. R., Ito, Y., Ivanova, V., Izmailov, I. S., Khovritchev, M. Yu., Khrutskaya, E. V., Kieken, J., Kiseleva, T. P., Kuppuswamy, K., Lainey, V., Lavayssiere, M., Lazzarotti, P., Le Campion, J. -F., Lellouch, E., Li, Z. L., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J. P., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J. M., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q. Y., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacre, J. -J., Sada, P. V., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S. A., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A. K., Vidal-Sainz, J., Vienne, A., Vilar, J., Vingerhoets, P., Vollman, W., Arlot, J. -E., Thuillot, W., Ruatti, C., Ahmad, A., Amosse, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G. D., Christou, A. A., Coquerel, J. -P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T. N., Dorokhov, N. I., Dourneau, G., Duenas, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R. M. D., Gonzales, D., Gorda, S. Yu., Gorshanov, D. L., Hansen, M. W., Harrington, M., Irsmambetova, T. R., Ito, Y., Ivanova, V., Izmailov, I. S., Khovritchev, M. Yu., Khrutskaya, E. V., Kieken, J., Kiseleva, T. P., Kuppuswamy, K., Lainey, V., Lavayssiere, M., Lazzarotti, P., Le Campion, J. -F., Lellouch, E., Li, Z. L., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J. P., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J. M., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q. Y., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacre, J. -J., Sada, P. V., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S. A., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A. K., Vidal-Sainz, J., Vienne, A., Vilar, J., Vingerhoets, P., and Vollman, W.
Published: 2009

24. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author: Arlot, J.-E., primary, Thuillot, W., additional, Ruatti, C., additional, Ahmad, A., additional, Amossé, A., additional, Anbazhagan, P., additional, Andreyev, M., additional, Antov, A., additional, Appakutty, M., additional, Asher, D., additional, Aubry, S., additional, Baron, N., additional, Bassiere, N., additional, Berthe, M., additional, Bogdanovski, R., additional, Bosq, F., additional, Bredner, E., additional, Buettner, D., additional, Buromsky, M., additional, Cammarata, S., additional, Casas, R., additional, Chis, G. D., additional, Christou, A. A., additional, Coquerel, J.-P., additional, Corlan, R., additional, Cremaschini, C., additional, Crussaire, D., additional, Cuypers, J., additional, Dennefeld, M., additional, Descamps, P., additional, Devyatkin, A., additional, Dimitrov, D., additional, Dorokhova, T. N., additional, Dorokhov, N. I., additional, Dourneau, G., additional, Dueñas, M., additional, Dumitrescu, A., additional, Emelianov, N., additional, Ferrara, D., additional, Fiel, D., additional, Fienga, A., additional, Flatres, T., additional, Foglia, S., additional, Garlitz, J., additional, Gerbos, J., additional, Gilbert, R., additional, Goncalves, R. M. D., additional, Gonzãles, D., additional, Gorda, S. Yu., additional, Gorshanov, D. L., additional, Hansen, M. W., additional, Harrington, M., additional, Irsmambetova, T. R., additional, Ito, Y., additional, Ivanova, V., additional, Izmailov, I. S., additional, Khovritchev, M. Yu., additional, Khrutskaya, E. V., additional, Kieken, J., additional, Kiseleva, T. P., additional, Kuppuswamy, K., additional, Lainey, V., additional, Lavayssiére, M., additional, Lazzarotti, P., additional, Le Campion, J.-F., additional, Lellouch, E., additional, Li, Z. L., additional, Lo Savio, E., additional, Lou, M., additional, Magny, E., additional, Manek, J., additional, Marinello, W., additional, Marino, G., additional, McAuliffe, J. P., additional, Michelli, M., additional, Moldovan, D., additional, Montagnac, S., additional, Moorthy, V., additional, Nickel, O., additional, Nier, J. M., additional, Noel, T., additional, Noyelles, B., additional, Oksanen, A., additional, Parrat, D., additional, Pauwels, T., additional, Peng, Q. Y., additional, Pizzetti, G., additional, Priban, V., additional, Ramachandran, B., additional, Rambaux, N., additional, Rapaport, M., additional, Rapavy, P., additional, Rau, G., additional, Sacré, J.-J., additional, Sada, P. V., additional, Salvaggio, F., additional, Sarlin, P., additional, Sciuto, C., additional, Selvakumar, G., additional, Sergeyev, A., additional, Sidorov, M., additional, Sorescu, S., additional, Spampinato, S. A., additional, Stellmacher, I., additional, Trunkovsky, E., additional, Tejfel, V., additional, Tudose, V., additional, Turcu, V., additional, Ugarte, I., additional, Vantyghem, P., additional, Vasundhara, R., additional, Vaubaillon, J., additional, Velu, C., additional, Venkataramana, A. K., additional, Vidal-Sãinz, J., additional, Vienne, A., additional, Vilar, J., additional, Vingerhoets, P., additional, and Vollman, W., additional
Published: 2008
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25. The use of recombinant activated factor VII in trauma-associated hemorrhage with crush injury.

Author: Christians K, Brasel K, Garlitz J, Abu-Hajir M, and Gottschall J
Published: 2005

26. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author: Arlot, J.-E., Thuillot, W., Ruatti, C., Ahmad, A., Amoss?, A., Anbazhagan, P., Andreyev, M., Antov, A., Appakutty, M., Asher, D., Aubry, S., Baron, N., Bassiere, N., Berthe, M., Bogdanovski, R., Bosq, F., Bredner, E., Buettner, D., Buromsky, M., Cammarata, S., Casas, R., Chis, G., Christou, A., Coquerel, J.-P., Corlan, R., Cremaschini, C., Crussaire, D., Cuypers, J., Dennefeld, M., Descamps, P., Devyatkin, A., Dimitrov, D., Dorokhova, T., Dorokhov, N., Dourneau, G., Due?as, M., Dumitrescu, A., Emelianov, N., Ferrara, D., Fiel, D., Fienga, A., Flatres, T., Foglia, S., Garlitz, J., Gerbos, J., Gilbert, R., Goncalves, R., Gonz?les, D., Gorda, S., Gorshanov, D., Hansen, M., Harrington, M., Irsmambetova, T., Ito, Y., Ivanova, V., Izmailov, I., Khovritchev, M., Khrutskaya, E., Kieken, J., Kiseleva, T., Kuppuswamy, K., Lainey, V., Lavayssi?re, M., Lazzarotti, P., Le Campion, J.-F., Lellouch, E., Li, Z., Lo Savio, E., Lou, M., Magny, E., Manek, J., Marinello, W., Marino, G., McAuliffe, J., Michelli, M., Moldovan, D., Montagnac, S., Moorthy, V., Nickel, O., Nier, J., Noel, T., Noyelles, B., Oksanen, A., Parrat, D., Pauwels, T., Peng, Q., Pizzetti, G., Priban, V., Ramachandran, B., Rambaux, N., Rapaport, M., Rapavy, P., Rau, G., Sacr?, J.-J., Sada, P., Salvaggio, F., Sarlin, P., Sciuto, C., Selvakumar, G., Sergeyev, A., Sidorov, M., Sorescu, S., Spampinato, S., Stellmacher, I., Trunkovsky, E., Tejfel, V., Tudose, V., Turcu, V., Ugarte, I., Vantyghem, P., Vasundhara, R., Vaubaillon, J., Velu, C., Venkataramana, A., Vidal-S?inz, J., Vienne, A., Vilar, J., Vingerhoets, P., and Vollman, W.
Abstract: Context. In 2003, the Sun and the Earth passed through both the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. Aims. During this period, mutual eclipses and occultations were observed and we present the data collected.Methods. Light curves of mutual eclipses and occultations were recorded by the observers of the international campaign PHEMU03 organized by the Institut de m?canique c?leste, Paris, France. Results. We completed 377?observations of 118?mutual events from 42?sites and the corresponding data are presented in this paper. For each observation, information about the telescope, receptor, site, and observational conditions are provided.Conclusions. This paper gathers all data and indicates a first estimate of its precision. This catalogue of these rare events should constitute an improved basis for accurate astrometric data useful in the development of dynamical models.
Published: 2009

27. U.S. Coast Guard Equipment Deployment Requirements for Hazardous Chemical Spill Response.

Author: TRANSPORTATION SYSTEMS CENTER CAMBRIDGE MA, Bellantoni,J, Frenkel,L, Litant,I, Fang,P, Garlitz,J, TRANSPORTATION SYSTEMS CENTER CAMBRIDGE MA, Bellantoni,J, Frenkel,L, Litant,I, Fang,P, and Garlitz,J
Abstract: The objective of the study was to determine the types, quantities and locations of equipment required by the U.S. Coast Guard to respond to spills of hazardous chemicals into U.S. waters and adjacent shorelines, over and above the resources of private industry, contractors and other government agencies. The methodology was to (1) assess equipment availability outside the Coast Guard, (2) determine the distribution of hazardous chemical spills in time and location, and (3) determine the Coast Guard equipment deployment, allowing for the results of (1) and (2).
Published: 1982

28. Deployment Requirements for U.S. Coast Guard Pollution Response Equipment. Volume II. Appendixes.

Author: TRANSPORTATION SYSTEMS CENTER CAMBRIDGE MA, Bellantoni,J, Garlitz,J, Kodis,R, O'Brien,A , Jr, Passera,A, TRANSPORTATION SYSTEMS CENTER CAMBRIDGE MA, Bellantoni,J, Garlitz,J, Kodis,R, O'Brien,A , Jr, and Passera,A
Abstract: The volume contains 13 technical appendixes dealing with: The Major Oil Spill Information System (data base); Outflow rates from seven massive tanker oil spills; Distribution of US coastal tanker traffic in 1985; Narratives of 17 selected oil spills, 1967-1978; A list of debarkation ports, with figures, in the U.S.; Load/Range tradeoff curves for the USCG HH3-F and C130 aircraft; An analysis of availability of USCG towing vessels; Maps of USCG installations and DOD air bases; The spill potential data base employed in Volume I; A model for distribution of equipment; An analysis of the probabilities of large and simultaneous spills; A list of non-USCG pollution response capabilities; and A brief review of the behavior of surface oil slicks., See also Volume 1, AD-A070 815. Supersedes AD-B030 518L.
Published: 1979

29. Thermal properties of slowly rotating asteroids: Results from a targeted survey

Author: Marciniak, A, Ali-Lagoa, V, Muller, T.G, Szakáts, R, Molnár, L, Pál, A, Antonini, P, Barbotin, E, Behrend, R, Bernasconi, L, Butkiewicz-Bak, M, Crippa, R, Duffard, R, Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S, Goncalves, R, Grice, J, Grzeskowiak, I, Hirsch, R, Horbowicz, J, Kaminski, K, Kaminska, M.K, Kim, D.H, Kim, M.J, Konstanciak, I, Kudak, V, Kulczak, P, Maestre, J.L, Manzini, F, Marks, S, Monteiro, F, Ogłoza, W, Oszkiewicz, D, Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R, Sanabria, J.J, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, Zukowski, K, Marciniak, A, Ali-Lagoa, V, Muller, T.G, Szakáts, R, Molnár, L, Pál, A, Antonini, P, Barbotin, E, Behrend, R, Bernasconi, L, Butkiewicz-Bak, M, Crippa, R, Duffard, R, Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S, Goncalves, R, Grice, J, Grzeskowiak, I, Hirsch, R, Horbowicz, J, Kaminski, K, Kaminska, M.K, Kim, D.H, Kim, M.J, Konstanciak, I, Kudak, V, Kulczak, P, Maestre, J.L, Manzini, F, Marks, S, Monteiro, F, Ogłoza, W, Oszkiewicz, D, Pilcher, F, Perig, V, Polakis, T, Polinska, M, Roy, R, Sanabria, J.J, Santana-Ros, T, Skiff, B, Skrzypek, J, Sobkowiak, K, Sonbas, E, Thizy, O, Trela, P, Urakawa, S, Zejmo, M, and Zukowski, K
Abstract: Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the subsurface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 h, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3−3 and 3+−333 and 45+−6030 J m−2 s−1/2 K−1. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.

30. Homogeneously derived transit timings for 17 exoplanets and reassessed TTV trends for WASP-12 and WASP-4

Author: Baluev, R V, Sokov, E N, Jones, H R A, Shaidulin, V Sh, Sokova, I A, Nielsen, L D, Benni, P, Schneiter, E M, D’Angelo, C Villarreal, Fernández-Lajús, E, Di Sisto, R P, Baştürk, Ö, Bretton, M, Wunsche, A, Hentunen, V-P, Shadick, S, Jongen, Y, Kang, W, Kim, T, Pakštienė, E, Qvam, J K T, Knight, C R, Guerra, P, Marchini, A, Salvaggio, F, Papini, R, Evans, P, Salisbury, M., Garcia, F, Molina, D, Garlitz, J, Esseiva, N, Ogmen, Y, Karavaev, Yu, Rusov, S, Ibrahimov, M A, Karimov, R G, Baluev, R V, Sokov, E N, Jones, H R A, Shaidulin, V Sh, Sokova, I A, Nielsen, L D, Benni, P, Schneiter, E M, D’Angelo, C Villarreal, Fernández-Lajús, E, Di Sisto, R P, Baştürk, Ö, Bretton, M, Wunsche, A, Hentunen, V-P, Shadick, S, Jongen, Y, Kang, W, Kim, T, Pakštienė, E, Qvam, J K T, Knight, C R, Guerra, P, Marchini, A, Salvaggio, F, Papini, R, Evans, P, Salisbury, M., Garcia, F, Molina, D, Garlitz, J, Esseiva, N, Ogmen, Y, Karavaev, Yu, Rusov, S, Ibrahimov, M A, and Karimov, R G
Abstract: We homogeneously analyse ∼3.2 × 105 photometric measurements for ∼1100 transit lightcurves belonging to 17 exoplanet hosts. The photometric data cover 16 years 2004–2019 and include amateur and professional observations. Old archival lightcurves were reprocessed using up-to-date exoplanetary parameters and empirically debiased limb-darkening models. We also derive self-consistent transit and radial-velocity fits for 13 targets. We confirm the nonlinear TTV trend in the WASP-12 data at a high significance, and with a consistent magnitude. However, Doppler data reveal hints of a radial acceleration about ( − 7.5 ± 2.2) m/s/yr, indicating the presence of unseen distant companions, and suggesting that roughly 10 per cent of the observed TTV was induced via the light-travel (or Roemer) effect. For WASP-4, a similar TTV trend suspected after the recent TESS observations appears controversial and model-dependent. It is not supported by our homogeneus TTV sample, including 10 ground-based EXPANSION lightcurves obtained in 2018 simultaneously with TESS. Even if the TTV trend itself does exist in WASP-4, its magnitude and tidal nature are uncertain. Doppler data cannot entirely rule out the Roemer effect induced by possible distant companions.

31. ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations

Author: Kokori, A., Tsiaras, A., Edwards, B., Jones, A., Pantelidou, G., Tinetti, G., Bewersdorff, L., Iliadou, A., Jongen, Y., Lekkas, G., Nastasi, A., Poultourtzidis, E., Sidiropoulos, C., Walter, F., Wünsche, A., Abraham, R., Agnihotri, V. K., Albanesi, R., Arce-Mansego, E., Arnot, D., Audejean, M., Aumasson, C., Bachschmidt, M., Baj, G., Barroy, P. R., Belinski, A. A., Bennett, D., Benni, P., Bernacki, K., Betti, L., Biagini, A., Bosch, P., Brandebourg, P., Brát, L., Bretton, M., Brincat, S. M., Brouillard, S., Bruzas, A., Bruzzone, A., Buckland, R. A., Caló, M., Campos, F., Carreño, A., Carrion Rodrigo, J. A., Casali, R., Casalnuovo, G., Cataneo, M., Chang, C.-M., Changeat, L., Chowdhury, V., Ciantini, R., Cilluffo, M., Coliac, J.-F., Conzo, G., Correa, M., Coulon, G., Crouzet, N., Crow, M. V., Curtis, I. A., Daniel, D., Dauchet, B., Dawes, S., Deldem, M., Deligeorgopoulos, D., Dransfield, G., Dymock, R., Eenmäe, T., Esseiva, N., Evans, P., Falco, C., Farfán, R. G., Fernández-Lajús, E., Ferratfiat, S., Ferreira, S. L., Ferretti, A., Fiołka, J., Fowler, M., Futcher, S. R., Gabellini, D., Gainey, T., Gaitan, J., Gajdoš, P., García-Sánchez, A., Garlitz, J., Gillier, C., Gison, C., Gonzales, J., Gorshanov, D., Grau Horta, F., Grivas, G., Guerra, P., Guillot, T., Haswell, C. A., Haymes, T., Hentunen, V.-P., Hills, K., Hose, K., Humbert, T., Hurter, F., Hynek, T., Irzyk, M., Jacobsen, J., Jannetta, A. L., Johnson, K., Jóźwik-Wabik, P., Kaeouach, A. E., Kang, W., Kiiskinen, H., Kim, T., Kivila, Ü., Koch, B., Kolb, U., Kučáková, H., Lai, S.-P., Laloum, D., Lasota, S., Lewis, L. A., Liakos, G.-I., Libotte, F., Lomoz, F., Lopresti, C., Majewski, R., Malcher, A., Mallonn, M., Mannucci, M., Marchini, A., Mari, J.-M., Marino, A., Marino, G., Mario, J.-C., Marquette, J.-B., Martínez-Bravo, F. A., Mašek, M., Matassa, P., Michel, P., Michelet, J., Miller, M., Miny, E., Molina, D., Mollier, T., Monteleone, B., Montigiani, N., Morales-Aimar, M., Mortari, F., Morvan, M., Mugnai, L. V., Murawski, G., Naponiello, L., Naudin, J.-L., Naves, R., Néel, D., Neito, R., Neveu, S., Noschese, A., Öğmen, Y., Ohshima, O., Orbanic, Z., Pace, E. P., Pantacchini, C., Paschalis, N. I., Pereira, C., Peretto, I., Perroud, V., Phillips, M., Pintr, P., Pioppa, J.-B., Plazas, J., Poelarends, A. J., Popowicz, A., Purcell, J., Quinn, N., Raetz, M., Rees, D., Regembal, F., Rocchetto, M., Rocci, P.-F., Rockenbauer, M., Roth, R., Rousselot, L., Rubia, X., Ruocco, N., Russo, E., Salisbury, M., Salvaggio, F., Santos, A., Savage, J., Scaggiante, F., Sedita, D., Shadick, S., Silva, A. F., Sioulas, N., Školník, V., Smith, M., Smolka, M., Solmaz, A., Stanbury, N., Stouraitis, D., Tan, T.-G., Theusner, M., Thurston, G., Tifner, F. P., Tomacelli, A., Tomatis, A., Trnka, J., Tylšar, M., Valeau, P., Vignes, J.-P., Villa, A., Sureda, A. Vives, Vora, K., Vrašt’ák, M., Walliang, D., Wenzel, B., Wright, D. E., Zambelli, R., Zhang, M., Zíbar, M., Kokori, A., Tsiaras, A., Edwards, B., Jones, A., Pantelidou, G., Tinetti, G., Bewersdorff, L., Iliadou, A., Jongen, Y., Lekkas, G., Nastasi, A., Poultourtzidis, E., Sidiropoulos, C., Walter, F., Wünsche, A., Abraham, R., Agnihotri, V. K., Albanesi, R., Arce-Mansego, E., Arnot, D., Audejean, M., Aumasson, C., Bachschmidt, M., Baj, G., Barroy, P. R., Belinski, A. A., Bennett, D., Benni, P., Bernacki, K., Betti, L., Biagini, A., Bosch, P., Brandebourg, P., Brát, L., Bretton, M., Brincat, S. M., Brouillard, S., Bruzas, A., Bruzzone, A., Buckland, R. A., Caló, M., Campos, F., Carreño, A., Carrion Rodrigo, J. A., Casali, R., Casalnuovo, G., Cataneo, M., Chang, C.-M., Changeat, L., Chowdhury, V., Ciantini, R., Cilluffo, M., Coliac, J.-F., Conzo, G., Correa, M., Coulon, G., Crouzet, N., Crow, M. V., Curtis, I. A., Daniel, D., Dauchet, B., Dawes, S., Deldem, M., Deligeorgopoulos, D., Dransfield, G., Dymock, R., Eenmäe, T., Esseiva, N., Evans, P., Falco, C., Farfán, R. G., Fernández-Lajús, E., Ferratfiat, S., Ferreira, S. L., Ferretti, A., Fiołka, J., Fowler, M., Futcher, S. R., Gabellini, D., Gainey, T., Gaitan, J., Gajdoš, P., García-Sánchez, A., Garlitz, J., Gillier, C., Gison, C., Gonzales, J., Gorshanov, D., Grau Horta, F., Grivas, G., Guerra, P., Guillot, T., Haswell, C. A., Haymes, T., Hentunen, V.-P., Hills, K., Hose, K., Humbert, T., Hurter, F., Hynek, T., Irzyk, M., Jacobsen, J., Jannetta, A. L., Johnson, K., Jóźwik-Wabik, P., Kaeouach, A. E., Kang, W., Kiiskinen, H., Kim, T., Kivila, Ü., Koch, B., Kolb, U., Kučáková, H., Lai, S.-P., Laloum, D., Lasota, S., Lewis, L. A., Liakos, G.-I., Libotte, F., Lomoz, F., Lopresti, C., Majewski, R., Malcher, A., Mallonn, M., Mannucci, M., Marchini, A., Mari, J.-M., Marino, A., Marino, G., Mario, J.-C., Marquette, J.-B., Martínez-Bravo, F. A., Mašek, M., Matassa, P., Michel, P., Michelet, J., Miller, M., Miny, E., Molina, D., Mollier, T., Monteleone, B., Montigiani, N., Morales-Aimar, M., Mortari, F., Morvan, M., Mugnai, L. V., Murawski, G., Naponiello, L., Naudin, J.-L., Naves, R., Néel, D., Neito, R., Neveu, S., Noschese, A., Öğmen, Y., Ohshima, O., Orbanic, Z., Pace, E. P., Pantacchini, C., Paschalis, N. I., Pereira, C., Peretto, I., Perroud, V., Phillips, M., Pintr, P., Pioppa, J.-B., Plazas, J., Poelarends, A. J., Popowicz, A., Purcell, J., Quinn, N., Raetz, M., Rees, D., Regembal, F., Rocchetto, M., Rocci, P.-F., Rockenbauer, M., Roth, R., Rousselot, L., Rubia, X., Ruocco, N., Russo, E., Salisbury, M., Salvaggio, F., Santos, A., Savage, J., Scaggiante, F., Sedita, D., Shadick, S., Silva, A. F., Sioulas, N., Školník, V., Smith, M., Smolka, M., Solmaz, A., Stanbury, N., Stouraitis, D., Tan, T.-G., Theusner, M., Thurston, G., Tifner, F. P., Tomacelli, A., Tomatis, A., Trnka, J., Tylšar, M., Valeau, P., Vignes, J.-P., Villa, A., Sureda, A. Vives, Vora, K., Vrašt’ák, M., Walliang, D., Wenzel, B., Wright, D. E., Zambelli, R., Zhang, M., and Zíbar, M.
Abstract: The ExoClock project has been created to increase the efficiency of the Ariel mission. It will achieve this by continuously monitoring and updating the ephemerides of Ariel candidates, in order to produce a consistent catalog of reliable and precise ephemerides. This work presents a homogenous catalog of updated ephemerides for 450 planets, generated by the integration of ∼18,000 data points from multiple sources. These sources include observations from ground-based telescopes (the ExoClock network and the Exoplanet Transit Database), midtime values from the literature, and light curves from space telescopes (Kepler, K2, and TESS). With all the above, we manage to collect observations for half of the postdiscovery years (median), with data that have a median uncertainty less than 1 minute. In comparison with the literature, the ephemerides generated by the project are more precise and less biased. More than 40% of the initial literature ephemerides had to be updated to reach the goals of the project, as they were either of low precision or drifting. Moreover, the integrated approach of the project enables both the monitoring of the majority of the Ariel candidates (95%), and also the identification of missing data. These results highlight the need for continuous monitoring to increase the observing coverage of the candidate planets. Finally, the extended observing coverage of planets allows us to detect trends (transit-timing variations) for a sample of 19 planets. All the products, data, and codes used in this work are open and accessible to the wider scientific community.

32. Homogeneously derived transit timings for 17 exoplanets and reassessed TTV trends for WASP-12 and WASP-4

Author: Baluev, R V, Sokov, E N, Jones, H R A, Shaidulin, V Sh, Sokova, I A, Nielsen, L D, Benni, P, Schneiter, E M, D’Angelo, C Villarreal, Fernández-Lajús, E, Di Sisto, R P, Baştürk, Ö, Bretton, M, Wunsche, A, Hentunen, V-P, Shadick, S, Jongen, Y, Kang, W, Kim, T, Pakštienė, E, Qvam, J K T, Knight, C R, Guerra, P, Marchini, A, Salvaggio, F, Papini, R, Evans, P, Salisbury, M., Garcia, F, Molina, D, Garlitz, J, Esseiva, N, Ogmen, Y, Karavaev, Yu, Rusov, S, Ibrahimov, M A, Karimov, R G, Baluev, R V, Sokov, E N, Jones, H R A, Shaidulin, V Sh, Sokova, I A, Nielsen, L D, Benni, P, Schneiter, E M, D’Angelo, C Villarreal, Fernández-Lajús, E, Di Sisto, R P, Baştürk, Ö, Bretton, M, Wunsche, A, Hentunen, V-P, Shadick, S, Jongen, Y, Kang, W, Kim, T, Pakštienė, E, Qvam, J K T, Knight, C R, Guerra, P, Marchini, A, Salvaggio, F, Papini, R, Evans, P, Salisbury, M., Garcia, F, Molina, D, Garlitz, J, Esseiva, N, Ogmen, Y, Karavaev, Yu, Rusov, S, Ibrahimov, M A, and Karimov, R G
Abstract: We homogeneously analyse ∼3.2 × 105 photometric measurements for ∼1100 transit lightcurves belonging to 17 exoplanet hosts. The photometric data cover 16 years 2004–2019 and include amateur and professional observations. Old archival lightcurves were reprocessed using up-to-date exoplanetary parameters and empirically debiased limb-darkening models. We also derive self-consistent transit and radial-velocity fits for 13 targets. We confirm the nonlinear TTV trend in the WASP-12 data at a high significance, and with a consistent magnitude. However, Doppler data reveal hints of a radial acceleration about ( − 7.5 ± 2.2) m/s/yr, indicating the presence of unseen distant companions, and suggesting that roughly 10 per cent of the observed TTV was induced via the light-travel (or Roemer) effect. For WASP-4, a similar TTV trend suspected after the recent TESS observations appears controversial and model-dependent. It is not supported by our homogeneus TTV sample, including 10 ground-based EXPANSION lightcurves obtained in 2018 simultaneously with TESS. Even if the TTV trend itself does exist in WASP-4, its magnitude and tidal nature are uncertain. Doppler data cannot entirely rule out the Roemer effect induced by possible distant companions.

33. Thermal properties of slowly rotating asteroids: Results from a targeted survey

Author: Marciniak, A, Ali-Lagoa, V, Muller, T.G, Szakáts, R, Molnár, L, Pál, A, Antonini, P, Barbotin, E, Behrend, R, Bernasconi, L, Butkiewicz-Bak, M, Crippa, R, Duffard, R, Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, Geier, S, Marciniak, A, Ali-Lagoa, V, Muller, T.G, Szakáts, R, Molnár, L, Pál, A, Antonini, P, Barbotin, E, Behrend, R, Bernasconi, L, Butkiewicz-Bak, M, Crippa, R, Duffard, R, Ditteon, R, Feuerbach, M, Fauvaud, S, Garlitz, J, and Geier, S
Abstract: Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the subsurface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 h, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3−3 and 3+−333 and 45+−6030 J m−2 s−1/2 K−1. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.

34. Pollution Response Systems Analysis

Author: United States. Coast Guard, Bellantoni, Juan F., Garlitz, J., Kodis, Ralph D., O'Brien, A., Jr., John A. Volpe National Transportation Systems Center (U.S.), United States. Coast Guard, Bellantoni, Juan F., Garlitz, J., Kodis, Ralph D., O'Brien, A., Jr., and John A. Volpe National Transportation Systems Center (U.S.)
Abstract: This study was initiated as part of the U.S. Coast Guard effort to provide adequate response within six hours for a spill of up to 100,000 ton of oil in U.S. waters. The guidelines and assumptions for the study are described, and partial results are reported on. A data base of spills over 50,000 gallons in U.S. waters has been compiled from the Pollution Incident Reporting System and Nation Response Center files of the USCG. Spill rates are derived and applied for the U.S. as a whole and for four major sub-ageas. a set of baseline pollution response equipment is adopted, and four equipment site configurations covering the U.S. are evaluated on the basis of six-hour coverage, historic spills encompassed and oil throughput. Relative levels of equipment capability for the sites are derived from a simpole optimization model.

35. Deployment Requirements for U.S. Coast Guard Pollution Response Equipment: Volume I. Analysis

Author: U.S. Coast Guard Research & Development Center, Bellantoni, Juan F., Garlitz, J., Kodis, Ralph D., O'Brien, A., Jr., Passera, Anthony, John A. Volpe National Transportation Systems Center (U.S.), U.S. Coast Guard Research & Development Center, Bellantoni, Juan F., Garlitz, J., Kodis, Ralph D., O'Brien, A., Jr., Passera, Anthony, and John A. Volpe National Transportation Systems Center (U.S.)
Abstract: This report presents the results of a study to examine the siting and equipment requirements that would have to be met by the U.S. Coast Guard to provide an adequate response within six hours for spills of up to 10,000 tons (28,000,000 gals.) of oil in U.S. waters. A data base of spills over 50,000 gallons in U.S. waters has been compiled from the Pollution Incident Reporting System and National Response Center files of the USCG. Spill rates are derived and applied for the U.S. as a whole and for four major sub-areas. A set of baseline pollution response equipment is adopted, and several equipment site configurations covering the U.S. are evaluated on the basis of six-hour coverage, historic spills encompassed and spill potential. Relative levels of equipment capability for the sites are derived from a simple optimization model. These relative levels are converted to specific equipment requirements on the basis of reasonable forecasts of oil movements in U.S. coastal waters, including oceanic tankers, coastal tank vessels, deepwater ports, and outer continental shelf production. The additional needs of the U.S. Coast Guard are estimated by subtracting the response capacity of equipment available from other response organizations. Finally, worldwide experience of oil spills larger than 1,000,000 gallons is examined for the decade 1968-1978, and three massive spill scenarios are present for the U.S. Atlantic and Pacific coasts. Corresponding response scenarios are evaluated, and site locations, equipment levels and logistic requirements are re-examined. System adjustments are noted, where indicated.

36. U.S. Coast Guard Equipment Deployment Requirements for Hazardous Chemical Spill Response

Author: United States. Coast Guard, Bellantoni, Juan F., Frankel, L., Litant, Irving, Fang, P., Garlitz, J., John A. Volpe National Transportation Systems Center (U.S.), United States. Coast Guard, Bellantoni, Juan F., Frankel, L., Litant, Irving, Fang, P., Garlitz, J., and John A. Volpe National Transportation Systems Center (U.S.)
Abstract: The objective of the study was to determine the types, quantities and locations of equipment required by the U.S. Coast Guard to respond to spills of hazardous chemicals into U.S. waters and adjacent shorelines, over and above the resources of private industry, contractors and other government agencies. The methodology was to (1) assess equipment availability outside the Coast Guard, (2) determine the distribution of hazardous chemical spills in time and location, and (3) determine the Coast Guard equipment deployment, allowing for the results of (1) and (2).

37. Computer modeling of transportation-generated air pollution. State-of-the-art survey, II. Final report, July 1976--June 1977

Author: Garlitz, J
Published: 1978

38. Ethylammonium nitrate: a protein crystallization reagent.

Author: Garlitz JA, Summers CA, Flowers RA 2nd, and Borgstahl GE
Subjects: Animals, Chemical Precipitation, Muramidase isolation & purification, Nitrates, Quaternary Ammonium Compounds, Crystallization, Indicators and Reagents, Proteins isolation & purification
Abstract: Ethylammonium nitrate (EAN) is a liquid organic salt that has many potential applications in protein chemistry. Because this solvent has hydrophobic and ionic character as well as the ability to hydrogen bond, it is especially well suited for broad use in protein crystallography. For example, EAN may be used as an additive, a detergent, a precipitating agent or to deliver ligands into protein crystals. A discussion of the crystallization of lysozyme using EAN as a precipitating agent is given here.
Published: 1999
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