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24 results on '"Shadick, S."'

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. V392 Persei: a \gamma-ray bright nova eruption from a known dwarf nova

Author

Murphy-Glaysher, F. J., Darnley, M. J., Harvey, É. J., Newsam, A. M., Page, K. L., Starrfield, S., Wagner, R. M., Woodward, C. E., Terndrup, D. M., Kafka, S., Heras, T. Arranz, Berardi, P., Bertrand, E., Biernikowicz, R., Boussin, C., Boyd, D., Buchet, Y., Bundas, M., Coulter, D., Dejean, D., Diepvens, A., Dvorak, S., Edlin, J., Eenmae, T., Eggenstein, H., Fournier, R., Garde, O., Gout, J., Janzen, D., Jordanov, P., Kiiskinen, H., Lane, D., Larochelle, R., Leadbeater, R., Mankel, D., Martineau, G., Miller, I., Modic, R., Montier, J., Aimar, M. Morales, Muyllaert, E., Nogues, R. Naves, O'Keeffe, D., Oksanen, A., Pyatnytskyy, M., Rast, R., Rodgers, B., Perez, D. Rodriguez, Schorr, F., Schwendeman, E., Shadick, S., Sharpe, S., Alfaro, F. Soldán, Sove, T., Stone, G., Tordai, T., Venne, R., Vollmann, W., Vrastak, M., and Wenzel, K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

V392 Persei is a known dwarf nova (DN) that underwent a classical nova eruption in 2018. Here we report ground-based optical, Swift UV and X-ray, and Fermi-LAT \gamma-ray observations following the eruption for almost three years. V392 Per is one of the fastest evolving novae yet observed, with a $t_2$ decline time of 2 days. Early spectra present evidence for multiple and interacting mass ejections, with the associated shocks driving both the \gamma-ray and early optical luminosity. V392 Per entered Sun-constraint within days of eruption. Upon exit, the nova had evolved to the nebular phase, and we saw the tail of the super-soft X-ray phase. Subsequent optical emission captured the fading ejecta alongside a persistent narrow line emission spectrum from the accretion disk. Ongoing hard X-ray emission is characteristic of a standing accretion shock in an intermediate polar. Analysis of the optical data reveals an orbital period of 3.230 \pm 0.003 days, but we see no evidence for a white dwarf (WD) spin period. The optical and X-ray data suggest a high mass WD, the pre-nova spectral energy distribution (SED) indicates an evolved donor, and the post-nova SED points to a high mass accretion rate. Following eruption, the system has remained in a nova-like high mass transfer state, rather than returning to the pre-nova DN low mass transfer configuration. We suggest that this high state is driven by irradiation of the donor by the nova eruption. In many ways, V392 Per shows similarity to the well-studied nova and DN GK Persei., Comment: Accepted by MNRAS. 20 pages including references, with 37 pages of supplementary material

Published
2022
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3. 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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4. 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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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. 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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7. V392 Persei: A γ-ray bright nova eruption from a known dwarf nova

Author

Murphy-Glaysher, F J, primary, Darnley, M J, additional, Harvey, É J, additional, Newsam, A M, additional, Page, K L, additional, Starrfield, S, additional, Wagner, R M, additional, Woodward, C E, additional, Terndrup, D M, additional, Kafka, S, additional, Arranz Heras, T, additional, Berardi, P, additional, Bertrand, E, additional, Biernikowicz, R, additional, Boussin, C, additional, Boyd, D, additional, Buchet, Y, additional, Bundas, M, additional, Coulter, D, additional, Dejean, D, additional, Diepvens, A, additional, Dvorak, S, additional, Edlin, J, additional, Eenmae, T, additional, Eggenstein, H, additional, Fournier, R, additional, Garde, O, additional, Gout, J, additional, Janzen, D, additional, Jordanov, P, additional, Kiiskinen, H, additional, Lane, D, additional, Larochelle, R, additional, Leadbeater, R, additional, Mankel, D, additional, Martineau, G, additional, Miller, I, additional, Modic, R, additional, Montier, J, additional, Morales Aimar, M, additional, Muyllaert, E, additional, Naves Nogues, R, additional, O’Keeffe, D, additional, Oksanen, A, additional, Pyatnytskyy, M, additional, Rast, R, additional, Rodgers, B, additional, Rodriguez Perez, D, additional, Schorr, F, additional, Schwendeman, E, additional, Shadick, S, additional, Sharpe, S, additional, Soldán Alfaro, F, additional, Sove, T, additional, Stone, G, additional, Tordai, T, additional, Venne, R, additional, Vollmann, W, additional, Vrastak, M, additional, and Wenzel, K, additional

Published
2022
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8. 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

9. 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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10. 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, Fernandez-Lajus, E., Di Sisto, R. P., Basturk, O., Bretton, M., Wunsche, A., Hentunen, V-P, Shadick, S., Jongen, Y., Kang, W., Kim, T., and Pakstiene, E.

Abstract

We homogeneously analyse similar to 3.2 x 10(5) photometric measurements for similar to 1100 transit light curves belonging to 17 exoplanet hosts. The photometric data cover 16 years (2004-2019) and include amateur and professional observations. Old archival light curves 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 non-linear transit timing variation (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 of about -7.5 +/- 2.2 ms(-1) yr(-1), 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 homogeneous TTV sample, including 10 ground-based EXPANSION light curves 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.

Published
2019

11. 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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12. KPS-1b: The first transiting exoplanet discovered using an amateur astronomerʼs wide-field CCD data

Author

Burdanov, A., Benni, P., Sokov, E., Krushinsky, V., Popov, A., Delrez, L., Gillon, M., Hébrard, G., Deleuil, M., Wilson, P. A., Demangeon, O., Baştürk, Ö., Pakštiene, E., Sokova, I., Rusov, S. A., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Marchini, A., Bretton, M., Shadick, S., Ivanov, K., Burdanov, A., Benni, P., Sokov, E., Krushinsky, V., Popov, A., Delrez, L., Gillon, M., Hébrard, G., Deleuil, M., Wilson, P. A., Demangeon, O., Baştürk, Ö., Pakštiene, E., Sokova, I., Rusov, S. A., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Marchini, A., Bretton, M., Shadick, S., and Ivanov, K.

Abstract

We report the discovery of the transiting hot Jupiter KPS-1b. This exoplanet orbits a V=13.0 K1-type main-sequence star every 1.7days, has a mass of 1.090+0.086-0.087 MJup and a radius of 1.03+0.13-0.12 RJup. The discovery was made by the prototype Kourovka Planet Search (KPS) project, which used wide-field CCD data gathered by an amateur astronomer using readily available and relatively affordable equipment. Here we describe the equipment and observing technique used for the discovery of KPS-1b, its characterization with spectroscopic observations by the SOPHIE spectrograph and with high-precision photometry obtained with 1 m class telescopes. We also outline the KPS project evolution into the Galactic Plane eXoplanet survey. The discovery of KPS-1b represents a new major step of the contribution of amateur astronomers to the burgeoning field of exoplanetology. © 2018. The Astronomical Society of the Pacific. All rights reserved. Printed in the U.S.A.

Published
2018

13. First results of the Kourovka Planet Search: Discovery of transiting exoplanet candidates in the first three target fields

Author

Burdanov, A. Y., Benni, P., Krushinsky, V. V., Popov, A. A., Sokov, E. N., Sokova, I. A., Rusov, S. A., Lyashenko, A. Y., Ivanov, K. I., Moiseev, A. V., Rastegaev, D. A., Dyachenko, V. V., Balega, Y. Y., Baştürk, O., Özavci, I., Puchalski, D., Marchini, A., Naves, R., Shadick, S., Bretton, M., Burdanov, A. Y., Benni, P., Krushinsky, V. V., Popov, A. A., Sokov, E. N., Sokova, I. A., Rusov, S. A., Lyashenko, A. Y., Ivanov, K. I., Moiseev, A. V., Rastegaev, D. A., Dyachenko, V. V., Balega, Y. Y., Baştürk, O., Özavci, I., Puchalski, D., Marchini, A., Naves, R., Shadick, S., and Bretton, M.

Abstract

We present the first results of our search for transiting exoplanet candidates as part of the Kourovka Planet Search (KPS) project. The primary objective of the project is to search for new hot Jupiters which transit their host stars, mainly in the Galactic plane, in the Rc magnitude range of 11-14 mag. Our observations were performed with the telescope of the MASTER robotic network, installed at the Kourovka astronomical observatory of the Ural Federal University (Russia), and the Rowe-Ackermann Schmidt Astrograph, installed at the private Acton Sky Portal Observatory (USA). As test observations, we observed three celestial fields of size 2 × 2deg2 during the period from 2012 to 2015. As a result, we discovered four transiting exoplanet candidates among the 39 000 stars of the input catalogue. In this paper, we provide the description of the project and analyse additional photometric, spectral, and speckle interferometric observations of the discovered transiting exoplanet candidates. Three of the four transiting exoplanet candidates are most likely astrophysical false positives, while the nature of the fourth (most promising) candidate remains to be ascertained. Also, we propose an alternative observing strategy that could increase the project's exoplanet haul. © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Published
2016

14. 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.

15. 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.

16. 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.

23. Book Reviews

Author

Fox, Glen A., primary, Shadick, S., additional, and Ransom, A. Brian, additional

Published
1970
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