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1. A controlled study on efficacy and egg reappearance period of Ivermectin in donkeys naturally infected with small strongyles

Author

Papini R. A., Orsetti C., and Sgorbini M.

Subjects
donkeys, small strongyles, ivermectin, efficacy, egg reappearance period, Microbiology, QR1-502
Abstract

The aim of the present study was to investigate the efficacy and the egg reappearance period (ERP) of ivermectin (IVM) in donkeys during a 13-week period. The study involved a total of 14 adult Amiata breed donkeys, 7 – 13 years of age, and naturally infected with small strongyles. A group of 10 donkeys was treated with IVM oral paste at a dose rate of 200 mcg/kg BW. Another group of 4 donkeys was kept as untreated control group. Faecal samples were collected and examined for strongyle eggs on day 0 before treatment. IVM efficacy was based on the faecal egg count reduction test (FECRT) on day 14 post-treatment. Then individual faecal samples were collected and examined by FECRT at weekly intervals. A FECRT of 100 % was found after treatment with IVM and its ERP, defined as the week when the mean FECRT decreased until to become lower than 90 %efficacy, was estimated to be 11 weeks without signs of developing anthelmintic resistance. No adverse reactions were observed during the study period. Our findings may be useful to veterinary practitioners and breeders as they show that IVM, at the recommended dose rate, can be still considered a highly effective and safe pharmacological tool for the treatment of small strongyles in donkeys. Therefore, it is strongly recommended that all possible strategies are undertaken to avoid the risk of emergence of anthelmintic resistance to IVM in donkeys.

Published
2020
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2. Evaluation of a marketed polyherbal dewormer against intestinal strongyles in naturally infected donkeys

Author

Papini R. A., Orsetti C., and Sgorbini M.

Subjects
donkeys, intestinal strongyles, herbal dewormer, phytotherapy, Microbiology, QR1-502
Abstract

The study evaluated the effectiveness of a commercially available polyherbal dewormer to control intestinal strongyles in naturally infected donkeys. The animals were allotted to two groups: treated with the herbal dewormer (n=8) according to manufacturer recommendations and untreated control group (n=6). Fecal samples were taken from each animal on days 0 (day of treatment), 14, 21 (day of second additional treatment), 35, and 42. Faecal egg count reduction tests showed very negligible or no reduction in number of strongyle eggs for donkeys in the phytotherapeutic treatment group compared to those in the control group. Thus, the herbal dewormer was mostly ineffective in reducing fecal egg counts in donkeys infected with intestinal strongyles. These findings can make equine practitioners aware of possible disadvantages of herbal dewormers.

Published
2020
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3. The young mini-Neptune HD 207496b that is either a naked core or on the verge of becoming one

Author

Barros, S. C. C., Demangeon, O. D. S., Armstrong, D. J., Mena, E. Delgado, Acuña, L., Fernández, Fernández, Deleuil, M., Collins, K. A., Howell, S. B., Ziegler, C., Adibekyan, V., Sousa, S. G., Stassun, K. G., Grieves, N., Lillo-Box, J., Hellier, C., Wheatley, P. J., Briceño, C., Collins, K. I., Hawthorn, F., Hoyer, S., Jenkins, J., Law, N., Mann, A. W., Matson, R. A., Mousis, O., Nielsen, L. D., Osborn, A., Osborn, H., Paegert, M., Papini, R., Ricker, G. R., Rudat, A. A., Santos, N. C., Seager, S., Stockdale, C., Strøm, P. A., Twicken, D., Udry, S., Wang, G., Vanderspek, R., and Winn, J. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery and characterisation of the transiting mini-Neptune HD~207496~b (TOI-1099) as part of a large programme that aims to characterise naked core planets. We obtained HARPS spectroscopic observations, one ground-based transit, and high-resolution imaging which we combined with the TESS photometry to confirm and characterise the TESS candidate and its host star. The host star is an active early K dwarf with a mass of $0.80 \pm 0.04\,$M$_\odot$, a radius of $0.769 \pm 0.026\,$R$_\odot$, and a G magnitude of 8. We found that the host star is young, $\sim 0.52\,$ Myr, allowing us to gain insight into planetary evolution. We derived a planetary mass of $6.1 \pm 1.6\,\mathrm{M}_E$,\, a planetary radius of $2.25 \pm 0.12\,\mathrm{R}_E$,\ and a planetary density of $\rho_p = 3.27_{-0.91}^{+0.97}\,\mathrm{g.cm^{-3}}$. From internal structure modelling of the planet, we conclude that the planet has either a water-rich envelope, a gas-rich envelope, or a mixture of both. We have performed evaporation modelling of the planet. If we assume the planet has a gas-rich envelope, we find that the planet has lost a significant fraction of its envelope and its radius has shrunk. Furthermore, we estimate it will lose all its remaining gaseous envelope in $\sim 0.52\,$ Gyr. Otherwise, the planet could have already lost all its primordial gas and is now a bare ocean planet. Further observations of its possible atmosphere and/or mass-loss rate would allow us to distinguish between these two hypotheses. Such observations would determine if the planet remains above the radius gap or if it will shrink and be below the gap., Comment: 20 pages, 18 figures, 4 tables, A&A accepted

Published
2023
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5. 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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6. 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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7. 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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8. Pluto's lower atmosphere and pressure evolution from ground-based stellar occultations, 1988-2016

Author

Meza, E., Sicardy, B., Assafin, M., Ortiz, J. L., Bertrand, T., Lellouch, E., Desmars, J., Forget, F., Bérard, D., Doressoundiram, A., Lecacheux, J., Oliveira, J. Marques, Roques, F., Widemann, T., Colas, F., Vachier, F., Renner, S., Leiva, R., Braga-Ribas, F., Benedetti-Rossi, G., Camargo, J. I. B., Dias-Oliveira, A., Morgado, B., Gomes-Júnior, A. R., Vieira-Martins, R., Behrend, R., Tirado, A. Castro, Duffard, R., Morales, N., Santos-Sanz, P., Jelínek, M., Cunniffe, R., Querel, R., Harnisch, M., Jansen, R., Pennell, A., Todd, S., Ivanov, V. D., Opitom, C., Gillon, M., Jehin, E., Manfroid, J., Pollock, J., Reichart, D. E., Haislip, J. B., Ivarsen, K. M., LaCluyze, A. P., Maury, A., Gil-Hutton, R., Dhillon, V., Littlefair, S., Marsh, T., Veillet, C., Bath, K. -L., Beisker, W., Bode, H. -J., Kretlow, M., Herald, D., Gault, D., Kerr, S., Pavlov, H., Faragó, O., Klös, O., Frappa, E., Lavayssière, M., Cole, A. A., Giles, A. B., Greenhill, J. G., Hill, K. M., Buie, M. W., Olkin, C. B., Young, E. F., Young, L. A., Wasserman, L. H., Devogèle, M., French, R. G., Bianco, F. B., Marchis, F., Brosch, N., Kaspi, S., Polishook, D., Manulis, I., Larbi, M. Ait Moulay, Benkhaldoun, Z., Daassou, A., Azhari, Y. El, Moulane, Y., Broughton, J., Milner, J., Dobosz, T., Bolt, G., Lade, B., Gilmore, A., Kilmartin, P., Allen, W. H., Graham, P. B., Loader, B., McKay, G., Talbot, J., Parker, S., Abe, L., Bendjoya, Ph., Rivet, J. -P., Vernet, D., Di Fabrizio, L., Lorenzi, V., Magazzù, A., Molinari, E., Gazeas, K., Tzouganatos, L., Carbognani, A., Bonnoli, G., Marchini, A., Leto, G., Sanchez, R. Zanmar, Mancini, L., Kattentidt, B., Dohrmann, M., Guhl, K., Rothe, W., Walzel, K., Wortmann, G., Eberle, A., Hampf, D., Ohlert, J., Krannich, G., Murawsky, G., Gährken, B., Gloistein, D., Alonso, S., Román, A., Communal, J. -E., Jabet, F., de Visscher, S., Sérot, J., Janik, T., Moravec, Z., Machado, P., Selva, A., Perelló, C., Rovira, J., Conti, M., Papini, R., Salvaggio, F., Noschese, A., Tsamis, V., Tigani, K., Barroy, P., Irzyk, M., Neel, D., Godard, J. P., Lanoiselée, D., Sogorb, P., Vérilhac, D., Bretton, M., Signoret, F., Ciabattari, F., Naves, R., Boutet, M., De Queiroz, J., Lindner, P., Lindner, K., Enskonatus, P., Dangl, G., Tordai, T., Eichler, H., Hattenbach, J., Peterson, C., Molnar, L. A., and Howell, R. R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Pluto's tenuous nitrogen (N2) atmosphere undergoes strong seasonal effects due to high obliquity and orbital eccentricity, and has been recently (July 2015) observed by the New Horizons spacecraft. Goals are (i) construct a well calibrated record of the seasonal evolution of surface pressure on Pluto and (ii) constrain the structure of the lower atmosphere using a central flash observed in 2015. Method: eleven stellar occultations by Pluto observed between 2002 and 2016 are used to retrieve atmospheric profiles (density, pressure, temperature) between $\sim$5 km and $\sim$380 km altitude levels (i.e. pressures from about 10 microbar to 10 nanobar). Results: (i) Pressure has suffered a monotonic increase from 1988 to 2016, that is compared to a seasonal volatile transport model, from which tight constraints on a combination of albedo and emissivity of N2 ice are derived; (ii) A central flash observed on 2015 June 29 is consistent with New Horizons REX profiles, provided that (a) large diurnal temperature variations (not expected by current models) occur over Sputnik Planitia and/or (b) hazes with tangential optical depth of about 0.3 are present at 4-7 km altitude levels and/or (c) the nominal REX density values are overestimated by an implausibly large factor of about 20% and/or (d) higher terrains block part of the flash in the Charon facing hemisphere., Comment: 21 pages, 11 figures

Published
2019
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9. Rapid quasi-periodic oscillations in the relativistic jet of BL Lacertae

Author

Jorstad, S. G., Marscher, A. P., Raiteri, C. M., Villata, M., Weaver, Z. R., Zhang, H., Dong, L., Gómez, J. L., Perel, M. V., Savchenko, S. S., Larionov, V. M., Carosati, D., Chen, W. P., Kurtanidze, O. M., Marchini, A., Matsumoto, K., Mortari, F., Aceti, P., Acosta-Pulido, J. A., Andreeva, T., Apolonio, G., Arena, C., Arkharov, A., Bachev, R., Banfi, M., Bonnoli, G., Borman, G. A., Bozhilov, V., Carnerero, M. I., Damljanovic, G., Ehgamberdiev, S. A., Elsässer, D., Frasca, A., Gabellini, D., Grishina, T. S., Gupta, A. C., Hagen-Thorn, V. A., Hallum, M. K., Hart, M., Hasuda, K., Hemrich, F., Hsiao, H. Y., Ibryamov, S., Irsmambetova, T. R., Ivanov, D. V., Joner, M. D., Kimeridze, G. N., Klimanov, S. A., Knött, J., Kopatskaya, E. N., Kurtanidze, S. O., Kurtenkov, A., Kuutma, T., Larionova, E. G., Leonini, S., Lin, H. C., Lorey, C., Mannheim, K., Marino, G., Minev, M., Mirzaqulov, D. O., Morozova, D. A., Nikiforova, A. A., Nikolashvili, M. G., Ovcharov, E., Papini, R., Pursimo, T., Rahimov, I., Reinhart, D., Sakamoto, T., Salvaggio, F., Semkov, E., Shakhovskoy, D. N., Sigua, L. A., Steineke, R., Stojanovic, M., Strigachev, A., Troitskaya, Y. V., Troitskiy, I. S., Tsai, A., Valcheva, A., Vasilyev, A. A., Vince, O., Waller, L., Zaharieva, E., and Chatterjee, R.

Published
2022
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14. The young mini-Neptune HD 207496b that is either a naked core or on the verge of becoming one

Author

Barros, S. C. C., primary, Demangeon, O. D. S., additional, Armstrong, D. J., additional, Delgado Mena, E., additional, Acuña, L., additional, Fernández Fernández, J., additional, Deleuil, M., additional, Collins, K. A., additional, Howell, S. B., additional, Ziegler, C., additional, Adibekyan, V., additional, Sousa, S. G., additional, Stassun, K. G., additional, Grieves, N., additional, Lillo-Box, J., additional, Hellier, C., additional, Wheatley, P. J., additional, Briceño, C., additional, Collins, K. I., additional, Hawthorn, F., additional, Hoyer, S., additional, Jenkins, J., additional, Law, N., additional, Mann, A. W., additional, Matson, R. A., additional, Mousis, O., additional, Nielsen, L. D., additional, Osborn, A., additional, Osborn, H., additional, Paegert, M., additional, Papini, R., additional, Ricker, G. R., additional, Rudat, A. A., additional, Santos, N. C., additional, Seager, S., additional, Stockdale, C., additional, Strøm, P. A., additional, Twicken, J. D., additional, Udry, S., additional, Wang, G., additional, Vanderspek, R., additional, and Winn, J. N., additional

Published
2023
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15. The optical behaviour of BL Lacertae at its maximum brightness levels: a blend of geometry and energetics

Author

Raiteri, C M, primary, Villata, M, additional, Jorstad, S G, additional, Marscher, A P, additional, Acosta Pulido, J A, additional, Carosati, D, additional, Chen, W P, additional, Joner, M D, additional, Kurtanidze, S O, additional, Lorey, C, additional, Marchini, A, additional, Matsumoto, K, additional, Mirzaqulov, D O, additional, Savchenko, S S, additional, Strigachev, A, additional, Vince, O, additional, Aceti, P, additional, Apolonio, G, additional, Arena, C, additional, Arkharov, A, additional, Bachev, R, additional, Bader, N, additional, Banfi, M, additional, Bonnoli, G, additional, Borman, G A, additional, Bozhilov, V, additional, Brown, L F, additional, Carbonell, W, additional, Carnerero, M I, additional, Damljanovic, G, additional, Dhiman, V, additional, Ehgamberdiev, S A, additional, Elsaesser, D, additional, Feige, M, additional, Gabellini, D, additional, Galán, D, additional, Galli, G, additional, Gaur, H, additional, Gazeas, K, additional, Grishina, T S, additional, Gupta, A C, additional, Hagen-Thorn, V A, additional, Hallum, M K, additional, Hart, M, additional, Hasuda, K, additional, Heidemann, K, additional, Horst, B, additional, Hou, W-J, additional, Ibryamov, S, additional, Ivanidze, R Z, additional, Jovanovic, M D, additional, Kimeridze, G N, additional, Kishore, S, additional, Klimanov, S, additional, Kopatskaya, E N, additional, Kurtanidze, O M, additional, Kushwaha, P, additional, Lane, D J, additional, Larionova, E G, additional, Leonini, S, additional, Lin, H C, additional, Mannheim, K, additional, Marino, G, additional, Minev, M, additional, Modaressi, A, additional, Morozova, D A, additional, Mortari, F, additional, Nazarov, S V, additional, Nikolashvili, M G, additional, Otero Santos, J, additional, Ovcharov, E, additional, Papini, R, additional, Pinter, V, additional, Privitera, C A, additional, Pursimo, T, additional, Reinhart, D, additional, Roberts, J, additional, Romanov, F D, additional, Rosenlehner, K, additional, Sakamoto, T, additional, Salvaggio, F, additional, Schoch, K, additional, Semkov, E, additional, Seufert, J, additional, Shakhovskoy, D, additional, Sigua, L A, additional, Singh, C, additional, Steineke, R, additional, Stojanovic, M, additional, Tripathi, T, additional, Troitskaya, Y V, additional, Troitskiy, I S, additional, Tsai, A, additional, Valcheva, A, additional, Vasilyev, A A, additional, Vrontaki, K, additional, Weaver, Z R, additional, Wooley, J H F, additional, Zaharieva, E, additional, and Zhovtan, A V, additional

Published
2023
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24. 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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26. 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

30. B.R.N.O. CONTRIBUTIONS #41 - TIMES OF MINIMA

Author

Hoňková, Lehký M., primary, Šmelcer, L., additional, Souza de Joode, M., additional, Jílek, F., additional, Mašek, M., additional, Urbaník, M., additional, Walter, F., additional, Dienstbier, V., additional, Bragagnolo, U., additional, Nosáĺ, P., additional, Červinka, L., additional, Mazanec, J., additional, Vrašťák, M., additional, Lomoz, F., additional, Hanžl, D., additional, Sergey, I., additional, Gudmundsson, S., additional, Jacobsen, J., additional, Ehrenberger, R., additional, Hladík, B., additional, Magris, M., additional, Tylšar, M., additional, Persha, G., additional, Školník, V., additional, Smolka, M., additional, Audejean, M., additional, Trnka, J., additional, Medulka, T., additional, Šuchaň, J., additional, Salvaggio, F., additional, Papini, R., additional, Marchini, A., additional, Colaco, C., additional, Vala, J., additional, Starck, M., additional, Quiňones, C., additional, Auer, R. F., additional, Melia, R., additional, Ruocco, N., additional, Kalášek, J., additional, Jíra, S., additional, Versari, L., additional, Girardici, C., additional, Tornatore, M., additional, Boková, S., additional, Malinak, J., additional, Novotný, P., additional, Mokrý, A., additional, Banfi, M., additional, Castillo, M., additional, Durantini, L., additional, Hrádek, L., additional, Kubica, T., additional, Lamberská, I., additional, López, O., additional, Lyachová, K., additional, Mrňák, P., additional, Pavlíková, E., additional, Vilchis, E., additional, and Začal, M., additional

Published
2021
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38. Pluto's lower atmosphere and pressure evolution from ground-based stellar occultations, 1988-2016

Author

Meza, E, Sicardy, B, Assafin, M, Ortiz, JL, Bertrand, T, Lellouch, E, Desmars, J, Forget, F, Bérard, D, Doressoundiram, A, Lecacheux, J, Oliveira, JM, Roques, F, Widemann, T, Colas, F, Vachier, F, Renner, S, Leiva, R, Braga-Ribas, F, Benedetti-Rossi, G, Camargo, JIB, Dias-Oliveira, A, Morgado, B, Gomes-Júnior, AR, Vieira-Martins, R, Behrend, R, Tirado, AC, Duffard, R, Morales, N, Santos-Sanz, P, Jelínek, M, Cunniffe, R, Querel, R, Harnisch, M, Jansen, R, Pennell, A, Todd, S, Ivanov, VD, Opitom, C, Gillon, M, Jehin, E, Manfroid, J, Pollock, J, Reichart, DE, Haislip, JB, Ivarsen, KM, LaCluyze, AP, Maury, A, Gil-Hutton, R, Dhillon, V, Littlefair, S, Marsh, T, Veillet, C, Bath, K-L, Beisker, W, Bode, H-J, Kretlow, M, Herald, D, Gault, D, Kerr, S, Pavlov, H, Faragó, O, Klös, O, Frappa, E, Lavayssière, M, Cole, AA, Giles, AB, Greenhill, JG, Hill, KM, Buie, MW, Olkin, CB, Young, EF, Young, LA, Wasserman, LH, Devogèle, M, French, RG, Bianco, FB, Marchis, F, Brosch, N, Kaspi, S, Polishook, D, Manulis, I, Larbi, MAM, Benkhaldoun, Z, Daassou, A, Azhari, YE, Moulane, Y, Broughton, J, Milner, J, Dobosz, T, Bolt, G, Lade, B, Gilmore, A, Kilmartin, P, Allen, WH, Graham, PB, Loader, B, McKay, G, Talbot, J, Parker, S, Abe, L, Bendjoya, P, Rivet, J-P, Vernet, D, Fabrizio, LD, Lorenzi, V, Magazzù, A, Molinari, E, Gazeas, K, Tzouganatos, L, Carbognani, A, Bonnoli, G, Marchini, A, Leto, G, Sanchez, RZ, Mancini, L, Kattentidt, B, Dohrmann, M, Guhl, K, Rothe, W, Walzel, K, Wortmann, G, Eberle, A, Hampf, D, Ohlert, J, Krannich, G, Murawsky, G, Gährken, B, Gloistein, D, Alonso, S, Román, A, Communal, J-E, Jabet, F, Visscher, SD, Sérot, J, Janik, T, Moravec, Z, Machado, P, Selva, A, Perelló, C, Rovira, J, Conti, M, Papini, R, Salvaggio, F, Noschese, A, Tsamis, V, Tigani, K, Barroy, P, Irzyk, M, Neel, D, Godard, JP, Lanoiselée, D, Sogorb, P, Vérilhac, D, Bretton, M, Signoret, F, Ciabattari, F, Naves, R, Boutet, M, Queiroz, JD, Lindner, P, Lindner, K, Enskonatus, P, Dangl, G, Tordai, T, Eichler, H, Hattenbach, J, Peterson, C, Molnar, LA, and Howell, RR

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Pluto's tenuous nitrogen (N2) atmosphere undergoes strong seasonal effects due to high obliquity and orbital eccentricity, and has been recently (July 2015) observed by the New Horizons spacecraft. Goals are (i) construct a well calibrated record of the seasonal evolution of surface pressure on Pluto and (ii) constrain the structure of the lower atmosphere using a central flash observed in 2015. Method: eleven stellar occultations by Pluto observed between 2002 and 2016 are used to retrieve atmospheric profiles (density, pressure, temperature) between $\sim$5 km and $\sim$380 km altitude levels (i.e. pressures from about 10 microbar to 10 nanobar). Results: (i) Pressure has suffered a monotonic increase from 1988 to 2016, that is compared to a seasonal volatile transport model, from which tight constraints on a combination of albedo and emissivity of N2 ice are derived; (ii) A central flash observed on 2015 June 29 is consistent with New Horizons REX profiles, provided that (a) large diurnal temperature variations (not expected by current models) occur over Sputnik Planitia and/or (b) hazes with tangential optical depth of about 0.3 are present at 4-7 km altitude levels and/or (c) the nominal REX density values are overestimated by an implausibly large factor of about 20% and/or (d) higher terrains block part of the flash in the Charon facing hemisphere., 21 pages, 11 figures

Published
2019

44. Discovery of a pre-cataclysmic binary with unusual chromaticity of the eclipsed white dwarf by the GPX survey

Author

Krushinsky, V., Benni, P., Burdanov, A., Antokhin, I., Antokhina, E., Jehin, E., Barkaoui, K., Fitzsimmons, A., Gibson, C., Gillon, M., Popov, A., Baştürk, Ö., Benkhaldoun, Z., Marchini, A., Papini, R., Salvaggio, F., Brazhko, V., Krushinsky, V., Benni, P., Burdanov, A., Antokhin, I., Antokhina, E., Jehin, E., Barkaoui, K., Fitzsimmons, A., Gibson, C., Gillon, M., Popov, A., Baştürk, Ö., Benkhaldoun, Z., Marchini, A., Papini, R., Salvaggio, F., and Brazhko, V.

Abstract

We report the discovery of a relatively bright eclipsing binary system, which consists of a white dwarf (WD) and a main-sequence K7 star with clear signs of chromospheric and spot activity. The light curve of this system shows ∼0.2 mag ellipsoidal variability with a period of 0.297549 d and a short total eclipse of the WD. Based on our analysis of the spectral and photometric data, we estimated the parameters of the system. The K7V star is tidally deformed but does not fill its Roche lobe (the filling factor is about 0.86). The orbital inclination is i = 73◦.1 ± 0◦.2, and the mass ratio is q = M2/M1 ≈ 0.88. The parameters of the K7V star are M2 ≈ 0.64 M☉, R2 = 0.645 ± 0.012R☉, and T2 ≈ 4070 K. The parameters of the WD are M1 ≈ 0.72 M☉, R1 = 0.013 ± 0.003R☉, and T1 = 8700 ± 1100 K. Photometric observations in different bands revealed that the maximum depth of the eclipse is in the SDSS r filter, which is unusual for a system of a WD and a late main-sequence star. We suspect that this system is a product of the evolution of a common-envelope binary star, and that the WD accretes the stellar wind from the secondary star (the so-called low-accretion-rate polar, hereafter LARP). © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Published
2020

45. Lower atmosphere and pressure evolution on Pluto from ground-based stellar occultations, 1988-2016

Author

Meza, E. Sicardy, B. Assafin, M. Ortiz, J.L. Bertrand, T. Lellouch, E. Desmars, J. Forget, F. Bérard, D. Doressoundiram, A. Lecacheux, J. Marques Oliveira, J. Roques, F. Widemann, T. Colas, F. Vachier, F. Renner, S. Leiva, R. Braga-Ribas, F. Benedetti-Rossi, G. Camargo, J.I.B. Dias-Oliveira, A. Morgado, B. Gomes-Júnior, A.R. Vieira-Martins, R. Behrend, R. Castro Tirado, A. Duffard, R. Morales, N. Santos-Sanz, P. Jelínek, M. Cunniffe, R. Querel, R. Harnisch, M. Jansen, R. Pennell, A. Todd, S. Ivanov, V.D. Opitom, C. Gillon, M. Jehin, E. Manfroid, J. Pollock, J. Reichart, D.E. Haislip, J.B. Ivarsen, K.M. LaCluyze, A.P. Maury, A. Gil-Hutton, R. Dhillon, V. Littlefair, S. Marsh, T. Veillet, C. Bath, K.-L. Beisker, W. Bode, H.-J. Kretlow, M. Herald, D. Gault, D. Kerr, S. Pavlov, H. Faragó, O. Klös, O. Frappa, E. Lavayssière, M. Cole, A.A. Giles, A.B. Greenhill, J.G. Hill, K.M. Buie, M.W. Olkin, C.B. Young, E.F. Young, L.A. Wasserman, L.H. Devogèle, M. French, R.G. Bianco, F.B. Marchis, F. Brosch, N. Kaspi, S. Polishook, D. Manulis, I. Ait Moulay Larbi, M. Benkhaldoun, Z. Daassou, A. El Azhari, Y. Moulane, Y. Broughton, J. Milner, J. Dobosz, T. Bolt, G. Lade, B. Gilmore, A. Kilmartin, P. Allen, W.H. Graham, P.B. Loader, B. McKay, G. Talbot, J. Parker, S. Abe, L. Bendjoya, P. Rivet, J.-P. Vernet, D. Di Fabrizio, L. Lorenzi, V. Magazzú, A. Molinari, E. Gazeas, K. Tzouganatos, L. Carbognani, A. Bonnoli, G. Marchini, A. Leto, G. Zanmar Sanchez, R. Mancini, L. Kattentidt, B. Dohrmann, M. Guhl, K. Rothe, W. Walzel, K. Wortmann, G. Eberle, A. Hampf, D. Ohlert, J. Krannich, G. Murawsky, G. Gährken, B. Gloistein, D. Alonso, S. Román, A. Communal, J.-E. Jabet, F. DeVisscher, S. Sérot, J. Janik, T. Moravec, Z. MacHado, P. Selva, A. Perelló, C. Rovira, J. Conti, M. Papini, R. Salvaggio, F. Noschese, A. Tsamis, V. Tigani, K. Barroy, P. Irzyk, M. Neel, D. Godard, J.P. Lanoiselée, D. Sogorb, P. Vérilhac, D. Bretton, M. Signoret, F. Ciabattari, F. Naves, R. Boutet, M. De Queiroz, J. Lindner, P. Lindner, K. Enskonatus, P. Dangl, G. Tordai, T. Eichler, H. Hattenbach, J. Peterson, C. Molnar, L.A. Howell, R.R.

Abstract

Context. The tenuous nitrogen (N2) atmosphere on Pluto undergoes strong seasonal effects due to high obliquity and orbital eccentricity, and has recently (July 2015) been observed by the New Horizons spacecraft. Aims. The main goals of this study are (i) to construct a well calibrated record of the seasonal evolution of surface pressure on Pluto and (ii) to constrain the structure of the lower atmosphere using a central flash observed in 2015. Methods. Eleven stellar occultations by Pluto observed between 2002 and 2016 are used to retrieve atmospheric profiles (density, pressure, temperature) between altitude levels of ∼5 and ∼380 km (i.e. pressures from ∼10 μbar to 10 nbar). Results. (i) Pressure has suffered a monotonic increase from 1988 to 2016, that is compared to a seasonal volatile transport model, from which tight constraints on a combination of albedo and emissivity of N2 ice are derived. (ii) A central flash observed on 2015 June 29 is consistent with New Horizons REX profiles, provided that (a) large diurnal temperature variations (not expected by current models) occur over Sputnik Planitia; and/or (b) hazes with tangential optical depth of ∼0.3 are present at 4-7 km altitude levels; and/or (c) the nominal REX density values are overestimated by an implausibly large factor of ∼20%; and/or (d) higher terrains block part of the flash in the Charon facing hemisphere. © E. Meza et al. 2019.

Published
2019

46. 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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47. Lower atmosphere and pressure evolution on Pluto from ground-based stellar occultations, 1988–2016

Author

Meza, E., primary, Sicardy, B., additional, Assafin, M., additional, Ortiz, J. L., additional, Bertrand, T., additional, Lellouch, E., additional, Desmars, J., additional, Forget, F., additional, Bérard, D., additional, Doressoundiram, A., additional, Lecacheux, J., additional, Oliveira, J. Marques, additional, Roques, F., additional, Widemann, T., additional, Colas, F., additional, Vachier, F., additional, Renner, S., additional, Leiva, R., additional, Braga-Ribas, F., additional, Benedetti-Rossi, G., additional, Camargo, J. I. B., additional, Dias-Oliveira, A., additional, Morgado, B., additional, Gomes-Júnior, A. R., additional, Vieira-Martins, R., additional, Behrend, R., additional, Tirado, A. Castro, additional, Duffard, R., additional, Morales, N., additional, Santos-Sanz, P., additional, Jelínek, M., additional, Cunniffe, R., additional, Querel, R., additional, Harnisch, M., additional, Jansen, R., additional, Pennell, A., additional, Todd, S., additional, Ivanov, V. D., additional, Opitom, C., additional, Gillon, M., additional, Jehin, E., additional, Manfroid, J., additional, Pollock, J., additional, Reichart, D. E., additional, Haislip, J. B., additional, Ivarsen, K. M., additional, LaCluyze, A. P., additional, Maury, A., additional, Gil-Hutton, R., additional, Dhillon, V., additional, Littlefair, S., additional, Marsh, T., additional, Veillet, C., additional, Bath, K.-L., additional, Beisker, W., additional, Bode, H.-J., additional, Kretlow, M., additional, Herald, D., additional, Gault, D., additional, Kerr, S., additional, Pavlov, H., additional, Faragó, O., additional, Klös, O., additional, Frappa, E., additional, Lavayssière, M., additional, Cole, A. A., additional, Giles, A. B., additional, Greenhill, J. G., additional, Hill, K. M., additional, Buie, M. W., additional, Olkin, C. B., additional, Young, E. F., additional, Young, L. A., additional, Wasserman, L. H., additional, Devogèle, M., additional, French, R. G., additional, Bianco, F. B., additional, Marchis, F., additional, Brosch, N., additional, Kaspi, S., additional, Polishook, D., additional, Manulis, I., additional, Ait Moulay Larbi, M., additional, Benkhaldoun, Z., additional, Daassou, A., additional, El Azhari, Y., additional, Moulane, Y., additional, Broughton, J., additional, Milner, J., additional, Dobosz, T., additional, Bolt, G., additional, Lade, B., additional, Gilmore, A., additional, Kilmartin, P., additional, Allen, W. H., additional, Graham, P. B., additional, Loader, B., additional, McKay, G., additional, Talbot, J., additional, Parker, S., additional, Abe, L., additional, Bendjoya, Ph., additional, Rivet, J.-P., additional, Vernet, D., additional, Di Fabrizio, L., additional, Lorenzi, V., additional, Magazzú, A., additional, Molinari, E., additional, Gazeas, K., additional, Tzouganatos, L., additional, Carbognani, A., additional, Bonnoli, G., additional, Marchini, A., additional, Leto, G., additional, Sanchez, R. Zanmar, additional, Mancini, L., additional, Kattentidt, B., additional, Dohrmann, M., additional, Guhl, K., additional, Rothe, W., additional, Walzel, K., additional, Wortmann, G., additional, Eberle, A., additional, Hampf, D., additional, Ohlert, J., additional, Krannich, G., additional, Murawsky, G., additional, Gährken, B., additional, Gloistein, D., additional, Alonso, S., additional, Román, A., additional, Communal, J.-E., additional, Jabet, F., additional, deVisscher, S., additional, Sérot, J., additional, Janik, T., additional, Moravec, Z., additional, Machado, P., additional, Selva, A., additional, Perelló, C., additional, Rovira, J., additional, Conti, M., additional, Papini, R., additional, Salvaggio, F., additional, Noschese, A., additional, Tsamis, V., additional, Tigani, K., additional, Barroy, P., additional, Irzyk, M., additional, Neel, D., additional, Godard, J. P., additional, Lanoiselée, D., additional, Sogorb, P., additional, Vérilhac, D., additional, Bretton, M., additional, Signoret, F., additional, Ciabattari, F., additional, Naves, R., additional, Boutet, M., additional, De Queiroz, J., additional, Lindner, P., additional, Lindner, K., additional, Enskonatus, P., additional, Dangl, G., additional, Tordai, T., additional, Eichler, H., additional, Hattenbach, J., additional, Peterson, C., additional, Molnar, L. A., additional, and Howell, R. R., additional

Published
2019
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50. The PDS 110 observing campaign - photometric and spectroscopic observations reveal eclipses are aperiodic

Author

Osborn, H. P., Kenworthy, M., Rodriguez, J. E., de Mooij, E. J. W., Kennedy, G. M., Relles, H., Gomez, E., Hippke, M., Banfi, M., Barbieri, L., Becker, I. S., Benni, P., Berlind, P., Bieryla, A., Bonnoli, G., Boussier, H., Brincat, S. M., Briol, J., Burleigh, M. R., Butterley, T., Calkins, M. L., Chote, P., Ciceri, Simona, Deldem, M., Dhillon, V. S., Dose, E., Dubois, F., Dvorak, S., Esquerdo, G. A., Evans, D. F., Ferratfiat, S., Fossey, S. J., Günther, M. N., Hall, J., Hambsch, F.-J., Herrero, E., Hills, K., James, R., Jayawardhana, R., Kafka, S., Killestein, T. L., Kotnik, C., Latham, D. W., Lemay, D., Lewin, P., Littlefair, S., Lopresti, C., Mallonn, M., Mancini, L., Marchini, A., McCormac, J. J., Murawski, G., Myers, G., Papini, R., Popov, V., Quadri, U., Quinn, S. N., Raynard, L., Rizzuti, L., Robertson, J., Salvaggio, F., Scholz, A., Sfair, R., Smith, A. M. S., Southworth, J., Tan, T. G., Vanaverbeke, S., Waagen, E. O., Watson, C. A., West, R. G., Winter, O. C., Wheatley, P. J., Wilson, R. W., Zhou, G., Osborn, H. P., Kenworthy, M., Rodriguez, J. E., de Mooij, E. J. W., Kennedy, G. M., Relles, H., Gomez, E., Hippke, M., Banfi, M., Barbieri, L., Becker, I. S., Benni, P., Berlind, P., Bieryla, A., Bonnoli, G., Boussier, H., Brincat, S. M., Briol, J., Burleigh, M. R., Butterley, T., Calkins, M. L., Chote, P., Ciceri, Simona, Deldem, M., Dhillon, V. S., Dose, E., Dubois, F., Dvorak, S., Esquerdo, G. A., Evans, D. F., Ferratfiat, S., Fossey, S. J., Günther, M. N., Hall, J., Hambsch, F.-J., Herrero, E., Hills, K., James, R., Jayawardhana, R., Kafka, S., Killestein, T. L., Kotnik, C., Latham, D. W., Lemay, D., Lewin, P., Littlefair, S., Lopresti, C., Mallonn, M., Mancini, L., Marchini, A., McCormac, J. J., Murawski, G., Myers, G., Papini, R., Popov, V., Quadri, U., Quinn, S. N., Raynard, L., Rizzuti, L., Robertson, J., Salvaggio, F., Scholz, A., Sfair, R., Smith, A. M. S., Southworth, J., Tan, T. G., Vanaverbeke, S., Waagen, E. O., Watson, C. A., West, R. G., Winter, O. C., Wheatley, P. J., Wilson, R. W., and Zhou, G.

Abstract

PDS 110 is a young disc-hosting star in the Orion OB1A association. Two dimming events of similar depth and duration were seen in 2008 (WASP) and 2011 (KELT), consistent with an object in a closed periodic orbit. In this paper, we present data from a ground-based observing campaign designed to measure the star both photometrically and spectroscopically during the time of predicted eclipse in 2017 September. Despite high-quality photometry, the predicted eclipse did not occur, although coherent structure is present suggesting variable amounts of stellar flux or dust obscuration. We also searched for radial velocity (RV) oscillations caused by any hypothetical companion and can rule out close binaries to 0.1Ms. Asearch of Sonneberg plate archive data also enabled us to extend the photometric baseline of this star back more than 50 yr, and similarly does not re-detect any deep eclipses. Taken together, they suggest that the eclipses seen in WASP and KELT photometry were due to aperiodic events. It would seem that PDS 110 undergoes stochastic dimmings that are shallower and of shorter duration than those of UX Ori variables, but may have a similar mechanism.

Published
2019
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