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1. The GAPS Programme at TNG. LV. Multiple molecular species in the atmosphere of HAT-P-11 b and review of the HAT-P-11 planetary system

Author

Basilicata, M., primary, Giacobbe, P., additional, Bonomo, A.S., additional, Scandariato, G., additional, Brogi, M., additional, Singh, V., additional, Di Paola, A., additional, Mancini, L., additional, Sozzetti, A., additional, Lanza, A.F., additional, Cubillos, P.E., additional, Damasso, M., additional, Desidera, S., additional, Biazzo, K., additional, Bignamini, A., additional, Borsa, F., additional, Cabona, L., additional, Carleo, I., additional, Ghedina, A., additional, Guilluy, G., additional, Maggio, A., additional, Mainella, G., additional, Micela, G., additional, Molinari, E., additional, Molinaro, M., additional, Nardiello, D., additional, Pedani, M., additional, Pino, L., additional, Poretti, E., additional, Southworth, J., additional, Stangret, M., additional, and Turrini, D., additional

Published
2024
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2. Star-spot activity, orbital obliquity, transmission spectrum, physical properties, and transit time variations of the HATS-2 planetary system

Author

Biagiotti, F., primary, Mancini, L., additional, Southworth, J., additional, Tregloan-Reed, J., additional, Naponiello, L., additional, Jørgensen, U.G., additional, Bach-Møller, N., additional, Basilicata, M., additional, Bonavita, M., additional, Bozza, V., additional, Burgdorf, M.J., additional, Dominik, M., additional, Figuera Jaimes, R., additional, Henning, Th., additional, Hinse, T.C., additional, Hundertmark, M., additional, Khalouei, E., additional, Longa-Peña, P., additional, Peixinho, N., additional, Rabus, M., additional, Rahvar, S., additional, Sajadian, S., additional, Skottfelt, J., additional, Snodgrass, C., additional, Jongen, Y., additional, and Vignes, J.-P., additional

Published
2024
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3. Absolute dimensions of solar-type eclipsing binaries: NY Hya: A test for magnetic stellar evolution models.

Author

Hinse, T. C., Baştürk, Ö., Southworth, J., Feiden, G. A., Tregloan-Reed, J., Kostov, V. B., Livingston, J., Esmer, E. M., Yılmaz, M., Yalçınkaya, S., Torun, Ş., Vos, J., Evans, D. F., Morales, J. C., Wolf, J. C. A., Olsen, E. H., Clausen, J. V., Helt, B. E., Lý, C. T. K., and Stahl, O.

Subjects
ECLIPSING binaries, STELLAR mass, SPECTRAL energy distribution, TEMPERATURE of stars, TIME series analysis, STELLAR evolution
Abstract

Context. The binary star NY Hya is a bright, detached, double-lined eclipsing system with an orbital period of just under five days with two components each nearly identical to the Sun and located in the solar neighbourhood. Aims. The objective of this study is to test and confront various stellar evolution models for solar-type stars based on accurate measurements of stellar mass and radius. Methods. We present new ground-based spectroscopic and photometric as well as high-precision space-based photometric and astrometric data from which we derive orbital as well as physical properties of the components via the method of least-squares minimisation based on a standard binary model valid for two detached components. Classic statistical techniques were invoked to test the significance of model parameters. Additional empirical evidence was compiled from the public domain; the derived system properties were compared with archival broad-band photometry data enabling a measurement of the system's spectral energy distribution that allowed an independent estimate of stellar properties. We also utilised semi-empirical calibration methods to derive atmospheric properties from Strömgren photometry and related colour indices. Results. We measured (percentages are fractional uncertainties) masses, radii, and effective temperatures of the two stars in NY Hya and found them to be MA = 1.1605 ± 0.0090 M⊙ (0.78%), RA = 1.407 ± 0.015 R⊙ (1.1%), Teff, A = 5595 ± 61 K (1.09%), MB = 1.1678 ± 0.0096 M⊙ (0.82%), RB = 1.406 ± 0.017 R⊙ (1.2%), and Teff, B = 5607 ± 61 K (1.09%). The atmospheric properties from Strömgren photometry agree well with spectroscopic results. No evidence was found for nearby companions from high-resolution imaging. A detailed analysis of space-based data revealed a small but significant eccentricity (e cos ω) of the orbit. The spectroscopic and frequency analysis on photometric time series data reveal evidence of clear photospheric activity on both components likely in the form of star spots caused by magnetic activity. Conclusions. We confronted the observed physical properties with classic and magnetic stellar evolution models. Classic models yielded both young pre-main-sequence and old main-sequence turn-off solutions with the two components at super-solar metallicities, in disagreement with observations. Based on chromospheric activity and X-ray observations, we invoke magnetic models. While magnetic fields are likely to play an important role, we still encounter problems in explaining adequately the observed properties. To reconcile the observed tensions we also considered the effects of star spots known to mimic magnetic inhibition of convection. Encouraging results were obtained, although unrealistically large spots were required on each component. Overall we conclude that NY Hya proves to be complex in nature, and requires additional follow-up work aiming at a more accurate determination of stellar effective temperature and metallicity. [ABSTRACT FROM AUTHOR]

Published
2024
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4. TOI-2084 b and TOI-4184 b: Two new sub-Neptunes around M dwarf stars

Author

Barkaoui, K., primary, Timmermans, M., additional, Soubkiou, A., additional, Rackham, B. V., additional, Burgasser, A. J., additional, Chouqar, J., additional, Pozuelos, F. J., additional, Collins, K. A., additional, Howell, S. B., additional, Simcoe, R., additional, Melis, C., additional, Stassun, K. G., additional, Tregloan-Reed, J., additional, Cointepas, M., additional, Gillon, M., additional, Bonfils, X., additional, Furlan, E., additional, Gnilka, C. L., additional, Almenara, J. M., additional, Alonso, R., additional, Benkhaldoun, Z., additional, Bonavita, M., additional, Bouchy, F., additional, Burdanov, A., additional, Chinchilla, P., additional, Davoudi, F., additional, Delrez, L., additional, Demangeon, O., additional, Dominik, M., additional, Demory, B.-O., additional, de Wit, J., additional, Dransfield, G., additional, Ducrot, E., additional, Fukui, A., additional, Hinse, T. C., additional, Hooton, M. J., additional, Jehin, E., additional, Jenkins, J. M., additional, Jørgensen, U. G., additional, Latham, D. W., additional, Garcia, L., additional, Carrazco-Gaxiola, S., additional, Ghachoui, M., additional, Gómez Maqueo Chew, Y., additional, Günther, M. N., additional, McCormac, J., additional, Murgas, F., additional, Murray, C. A., additional, Narita, N., additional, Niraula, P., additional, Pedersen, P. P., additional, Queloz, D., additional, Rebolo-López, R., additional, Ricker, G., additional, Sabin, L., additional, Sajadian, S., additional, Schanche, N., additional, Schwarz, R. P., additional, Seager, S., additional, Sebastian, D., additional, Sefako, R., additional, Sohy, S., additional, Southworth, J., additional, Srdoc, G., additional, Thompson, S. J., additional, Triaud, A. H. M. J., additional, Vanderspek, R., additional, Wells, R. D., additional, Winn, J. N., additional, and Zúñiga-Fernández, S., additional

Published
2023
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5. Power-2 limb-darkening coefficients for the uvby, UBVRIJHK, SDSS ugriz, Gaia, Kepler, TESS, and CHEOPS photometric systems II. PHOENIX spherically symmetric stellar atmosphere models

Author

Claret, A., Southworth, J., and CLARET

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Planetary systems, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, eclipsing [Binaries], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), close [Binaries], Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

The Spanish MEC (AYA2015-71718-R, ESP2017-87676-C5-2-R, PID2019-107061GB-C64, and PID2019-109522GB-C52) is gratefully acknowledged for its support during the development of this work. A.C. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France, of NASA’s Astrophysics Data System Abstract Service and of SVO Filter Profile supported from the Spanish MINECO through grant AYA2017-84089., Context. The phenomenon of limb-darkening is relevant to many topics in astrophysics, including the analysis of light curves of eclipsing binaries, optical interferometry, measurement of stellar diameters, line profiles of rotating stars, gravitational microlensing, and transits of extrasolar planets Aims. Multiple parametric limb-darkening laws have been presented, and there are many available sources of theoretical limb-darkening coefficients (LDCs) calculated using stellar model atmospheres. The power-2 limb-darkening law allows a very good representation of theoretically predicted intensity profiles, but few LDCs are available for this law from spherically symmetric model atmospheres. We therefore present such coefficients in this work. Methods. We computed LDCs for the space missions Gαiα, Kepler, TESS, and CHEOPS and for the passbands uνby, UBVRIJHK, and SDSS ugriz, using the PHOENIX-COND spherical models. We adopted two methods to characterise the truncation point, which sets the limb of the star: the first (M1) uses the point where the derivative dI(r)/dr is at its maximum - where I(r) is the specific intensity as a function of the normalised radius r - corresponding to μcri, and the second (M2) uses the midpoint between the point μcri and the point located at μcn-1. The LDCs were computed adopting the Levenberg-Marquardt least-squares minimisation method, with a resolution of 900 equally spaced μ points, and covering 823 model atmospheres for a solar metallicity, effective temperatures of 2300-12000 K, log g values from 0.0 to 6.0, and microturbulent velocities of 2 km s-1. As our previous calculations of LDCs using spherical models included only 100 μ points, we also updated the calculations for the four-parameter law for the passbands listed above, and compared them with those from the power-2 law. Results. Comparisons between the quality of the fits provided by the power-2 and four-parameter laws show that the latter presents a lower merit function, X2, than the former for both cases (M1 and M2). This is important when choosing the best approach for a particular science goal., The Spanish MEC (AYA2015-71718-R, ESP2017-87676-C5-2-R, PID2019-107061GB-C64, PID2019-109522GB-C52), MCIN/AEI/ 10.13039/501100011033 CEX2021-001131-S, CDS, NASA’s Astrophysics Data System Abstract Service, The Spanish MINECO AYA2017-84089

Published
2023

9. Power-2 limb-darkening coefficients for the uvby, UBVRIJHK, SDSS ugriz, Gaia, Kepler, and TESS photometric systems

Author

Claret, A. and Southworth, J.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - Solar and Stellar Astrophysics, QB460, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, QA, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB600, QC, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

Context. Limb darkening is an important stellar phenomenon and must be accounted for in the study of stellar spectra, eclipsing binaries, transiting planetary systems, and microlensing events. The power-2 limb-darkening law provides a good match to the specific intensities predicted by stellar atmosphere models: it is better than other two-parameter laws and is only surpassed by the four-parameter law.\ud \ud Aims. Predictions of the limb-darkening coefficients for the power-2 law are not widely available. We therefore compute them, using stellar atmosphere models generated by the ATLAS (plane-parallel) code.\ud \ud Methods. Limb-darkening coefficients were computed for the space missions Gαiα, Kepler, and TESS as well as for the photometric systems uvby, UBVRIJHK, and SDSS ugriz. The calculations were performed by adopting the Levenberg–Marquardt least-squares minimisation method and were computed with a resolution of 100 equally spaced viewing angles. We used 9586 model atmospheres covering 19 metallicities, effective temperatures of 3500–50 000 K, log g values from 0.0 to 5.0, and microturbulent velocities of 0, 1, 2, 4, and 8 km s-1.\ud \ud Results. We confirm the superiority of the power-2 law, in terms of the quality of the fits, over other two-parameter laws. This is particularly relevant for the quadratic law, which is widely used.\ud \ud Conclusions. We recommend the use of the power-2 law in cases where a two-parameter law is needed.

Published
2022

10. Surface brightness-colour relations of dwarf stars from detached eclipsing binaries

Author

Graczyk, D., primary, Pietrzyński, G., additional, Galan, C., additional, Southworth, J., additional, Gieren, W., additional, Kałuszyński, M., additional, Zgirski, B., additional, Gallenne, A., additional, Górski, M., additional, Hajdu, G., additional, Karczmarek, P., additional, Kervella, P., additional, Maxted, P. F. L., additional, Nardetto, N., additional, Narloch, W., additional, Pilecki, B., additional, Pych, W., additional, Rojas Garcia, G., additional, Storm, J., additional, Suchomska, K., additional, Taormina, M., additional, and Wielgórski, P., additional

Published
2022
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11. The GAPS Programme at TNG

Author

Mancini, L., primary, Esposito, M., additional, Covino, E., additional, Southworth, J., additional, Poretti, E., additional, Andreuzzi, G., additional, Barbato, D., additional, Biazzo, K., additional, Borsato, L., additional, Bruni, I., additional, Damasso, M., additional, Di Fabrizio, L., additional, Evans, D. F., additional, Granata, V., additional, Lanza, A. F., additional, Naponiello, L., additional, Nascimbeni, V., additional, Pinamonti, M., additional, Sozzetti, A., additional, Tregloan-Reed, J., additional, Basilicata, M., additional, Bignamini, A., additional, Bonomo, A. S., additional, Claudi, R., additional, Cosentino, R., additional, Desidera, S., additional, Fiorenzano, A. F. M., additional, Giacobbe, P., additional, Harutyunyan, A., additional, Henning, Th., additional, Knapic, C., additional, Maggio, A., additional, Micela, G., additional, Molinari, E., additional, Pagano, I., additional, Pedani, M., additional, and Piotto, G., additional

Published
2022
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14. The surface brightness–colour relations based on eclipsing binary stars and calibrated withGaiaEDR3

Author

Graczyk, D., primary, Pietrzyński, G., additional, Galan, C., additional, Gieren, W., additional, Tkachenko, A., additional, Anderson, R. I., additional, Gallenne, A., additional, Górski, M., additional, Hajdu, G., additional, Kałuszyński, M., additional, Karczmarek, P., additional, Kervella, P., additional, Maxted, P. F. L., additional, Nardetto, N., additional, Narloch, W., additional, Pavlovski, K., additional, Pilecki, B., additional, Pych, W., additional, Southworth, J., additional, Storm, J., additional, Suchomska, K., additional, Taormina, M., additional, Villanova, S., additional, Wielgórski, P., additional, Zgirski, B., additional, and Konorski, P., additional

Published
2021
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18. HD183648: a Kepler eclipsing binary with anomalous ellipsoidal variations and a pulsating component

Author

Derekas A., Borkovits T., Fuller J., Szabó Gy. M., Pavlovski K., Csák B., Dózsa Á., Kovács J., Szabó R., Hambleton K. M., Kinemuchi K., Kolbas V., Kurtz D. W., Maloney F., Prša A., Southworth J., Sztakovics J., Bíró I. B., and Jankovics I.

Subjects
Physics, QC1-999
Abstract

KIC 8560861 (HD 183648) is a marginally eccentric (e = 0.05) eclipsing binary with an orbital period of Porb = 31.973 d, exhibiting mmag amplitude pulsations on time scales of a few days. We present the results of the complex analysis of high and medium-resolution spectroscopic data and Kepler Q0 – Q16 long cadence photometry.

Published
2015
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19. KIC 7582608: a new Kepler roAp star with frequency variability

Author

Holdsworth D.L., Smalley B., Kurtz D.W., Southworth J., Cunha M.S., and Clubb K.I.

Subjects
Physics, QC1-999
Abstract

We analyse the fifth roAp star reported in the Kepler field, KIC 7582608, discovered with the SuperWASP project. The object shows a high frequency pulsation at 181.7324d−1 (P = 7.9 min) with an amplitude of 1.45 mmag, and low frequency rotational modulation corresponding to a period of 20.4339 d. Spectral analysis confirms the Ap nature of the target, with characteristic lines of rare earth elements present. From our spectral observations we derive a lower limit on the mean magnetic field modulus of 〈B〉 =3.05 ± 0.23 kG. Long Cadence Kepler observations show a frequency quintuplet split by the rotational period of the star, typical for an oblique pulsator. We suggest the star is a quadrupole pulsator with a geometry such that i ~ 66° and β ~ 33°. We detect frequency variations of the pulsation in both the WASP and Kepler data sets on many time scales. Linear, non-adiabatic stability modelling allows us to constrain a region on the HR diagram where the pulsations are unstable, an area consistent with observations.

Published
2015
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20. The highly inflated giant planet WASP-174b

Author

Mancini, L., primary, Sarkis, P., additional, Henning, Th., additional, Bakos, G. Á., additional, Bayliss, D., additional, Bento, J., additional, Bhatti, W., additional, Brahm, R., additional, Csubry, Z., additional, Espinoza, N., additional, Hartman, J., additional, Jordán, A., additional, Penev, K., additional, Rabus, M., additional, Suc, V., additional, de Val-Borro, M., additional, Zhou, G., additional, Chen, G., additional, Damasso, M., additional, Southworth, J., additional, and Tan, T. G., additional

Published
2020
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21. The EBLM project

Author

Gill, S., primary, Maxted, P. F. L., additional, Evans, J. A., additional, Evans, D. F., additional, Southworth, J., additional, Smalley, B., additional, Gary, B. L., additional, Anderson, D. R., additional, Bouchy, F., additional, Cameron, A. C., additional, Dominik, M., additional, Faedi, F., additional, Gillon, M., additional, Gomez Maqueo Chew, Y., additional, Hebb, L., additional, Hellier, C., additional, Jørgensen, U. G., additional, Longa-Peña, P., additional, Martin, D. V., additional, McCormac, J., additional, Pepe, F. V., additional, Pollaco, D., additional, Queloz, D., additional, Ségransan, D., additional, Snodgrass, C., additional, Turner, O. D., additional, Triaud, A. H. M., additional, Udry, S., additional, and West, R. G., additional

Published
2019
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22. Deciphering the atmosphere of HAT-P-12b: solving discrepant results

Author

Alexoudi, X., primary, Mallonn, M., additional, von Essen, C., additional, Turner, J. D., additional, Keles, E., additional, Southworth, J., additional, Mancini, L., additional, Ciceri, S., additional, Granzer, T., additional, Denker, C., additional, Dineva, E., additional, and Strassmeier, K. G., additional

Published
2018
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24. The GAPS programme with HARPS-N at TNG

Author

Mancini, L., primary, Esposito, M., additional, Covino, E., additional, Southworth, J., additional, Biazzo, K., additional, Bruni, I., additional, Ciceri, S., additional, Evans, D., additional, Lanza, A. F., additional, Poretti, E., additional, Sarkis, P., additional, Smith, A. M. S., additional, Brogi, M., additional, Affer, L., additional, Benatti, S., additional, Bignamini, A., additional, Boccato, C., additional, Bonomo, A. S., additional, Borsa, F., additional, Carleo, I., additional, Claudi, R., additional, Cosentino, R., additional, Damasso, M., additional, Desidera, S., additional, Giacobbe, P., additional, González-Álvarez, E., additional, Gratton, R., additional, Harutyunyan, A., additional, Leto, G., additional, Maggio, A., additional, Malavolta, L., additional, Maldonado, J., additional, Martinez-Fiorenzano, A., additional, Masiero, S., additional, Micela, G., additional, Molinari, E., additional, Nascimbeni, V., additional, Pagano, I., additional, Pedani, M., additional, Piotto, G., additional, Rainer, M., additional, Scandariato, G., additional, Smareglia, R., additional, Sozzetti, A., additional, Andreuzzi, G., additional, and Henning, Th., additional

Published
2018
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25. High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Author

Evans, D. F., primary, Southworth, J., additional, Smalley, B., additional, Jørgensen, U. G., additional, Dominik, M., additional, Andersen, M. I., additional, Bozza, V., additional, Bramich, D. M., additional, Burgdorf, M. J., additional, Ciceri, S., additional, D’Ago, G., additional, Figuera Jaimes, R., additional, Gu, S.-H., additional, Hinse, T. C., additional, Henning, Th., additional, Hundertmark, M., additional, Kains, N., additional, Kerins, E., additional, Korhonen, H., additional, Kokotanekova, R., additional, Kuffmeier, M., additional, Longa-Peña, P., additional, Mancini, L., additional, MacKenzie, J., additional, Popovas, A., additional, Rabus, M., additional, Rahvar, S., additional, Sajadian, S., additional, Snodgrass, C., additional, Skottfelt, J., additional, Surdej, J., additional, Tronsgaard, R., additional, Unda-Sanzana, E., additional, von Essen, C., additional, Wang, Yi-Bo, additional, and Wertz, O., additional

Published
2018
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26. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (vol 555, pg A36, 2013)

Author

Kains, N, Bramich, DM, Ferro, AA, Jaimes, RF, Jorgensen, UG, Giridhar, S, Penny, MT, Alsubai, KA, Andersen, JM, Bozza, V, Browne, P, Burgdorf', M, Novati, SC, Damerdji, Y, Diehl, C, Dodds, P, Dominik, M, Elyiv, A, Fang, X-S, Giannini, E, Hardis, S, Harpsoe, K, Hinse, TC, Hornstrup, A, Hundertmark, M, Jessen-Hansen, J, Juncher, D, Kerins, E, Kjeldsen, H, Korhonen, H, Liebig, C, Lund, MN, Lundkvist, M, Mancini, L, Martin, R, Mathiasen, M, Rabus, M, Rahvar, S, Ricci, D, Sahu, K, Scarpetta, G, Skottfelt, J, Snodgrass, C, Southworth, J, Surdej, J, Tregloan-Reed, J, Vilela, C, Wertz, O, Williams, A, and Consortium, M

Subjects
QC, QB
Abstract

Aims. We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We\ud used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to\ud derive values for the cluster’s parameters.\ud Methods. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster\ud parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also\ud derived an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD).\ud Results. Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables,\ud and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler\ud system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of\ud the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]ZW = −2.01±0.04,\ud or [Fe/H]UVES = −2.11 ± 0.06, and a distance of 8.32 ± 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 ± 0.42 kpc\ud (using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 ± 1.0 Gyr for M 30.

Published
2016

27. Erratum: Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (Astronomy and Astrophysics (2013) 555 (A36))

Author

Kains, N, Bramich, Dm, Arellano Ferro, A, Figuera Jaimes, R, Jorgensen, Ug, Giridhar, S, Penny, Mt, Alsubai, Ka, Andersen, Jm, Bozza, V, Browne, P, Burgdorf, M, Calchi Novati, S, Damerdji, Y, Diehl, C, Dodds, P, Dominik, M, Elyiv, A, Fang, X, Giannini, E, S. -H., G, Hardis, S, Harpsoe, K, Hinse, Tc, Hornstrup, A, Hundertmark, M, Jessen-Hansen, J, Juncher, D, Kerins, E, Kjeldsen, H, Korhonen, H, Liebig, C, Lund, Mn, Lundkvist, M, Mancini, L, Martin, R, Mathiasen, M, Rabus, M, Rahvar, S, Ricci, D, Sahu, K, Scarpetta, G, Skottfelt, J, Snodgrass, C, Southworth, J, Surdej, J, Tregloan-Reed, J, Vilela, C, Wertz, O, and Williams, A

Subjects
Settore FIS/05 - Astronomia e Astrofisica
Published
2016

28. The GAPS Programme with HARPS-N at TNG

Author

Esposito, M., primary, Covino, E., additional, Desidera, S., additional, Mancini, L., additional, Nascimbeni, V., additional, Zanmar Sanchez, R., additional, Biazzo, K., additional, Lanza, A. F., additional, Leto, G., additional, Southworth, J., additional, Bonomo, A. S., additional, Suárez Mascareño, A., additional, Boccato, C., additional, Cosentino, R., additional, Claudi, R. U., additional, Gratton, R., additional, Maggio, A., additional, Micela, G., additional, Molinari, E., additional, Pagano, I., additional, Piotto, G., additional, Poretti, E., additional, Smareglia, R., additional, Sozzetti, A., additional, Affer, L., additional, Anderson, D. R., additional, Andreuzzi, G., additional, Benatti, S., additional, Bignamini, A., additional, Borsa, F., additional, Borsato, L., additional, Ciceri, S., additional, Damasso, M., additional, di Fabrizio, L., additional, Giacobbe, P., additional, Granata, V., additional, Harutyunyan, A., additional, Henning, T., additional, Malavolta, L., additional, Maldonado, J., additional, Martinez Fiorenzano, A., additional, Masiero, S., additional, Molaro, P., additional, Molinaro, M., additional, Pedani, M., additional, Rainer, M., additional, Scandariato, G., additional, and Turner, O. D., additional

Published
2017
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29. From dense hot Jupiter to low-density Neptune: The discovery of WASP-127b, WASP-136b, and WASP-138b

Author

Lam, K. W. F., primary, Faedi, F., additional, Brown, D. J. A., additional, Anderson, D. R., additional, Delrez, L., additional, Gillon, M., additional, Hébrard, G., additional, Lendl, M., additional, Mancini, L., additional, Southworth, J., additional, Smalley, B., additional, Triaud, A. H. M., additional, Turner, O. D., additional, Hay, K. L., additional, Armstrong, D. J., additional, Barros, S. C. C., additional, Bonomo, A. S., additional, Bouchy, F., additional, Boumis, P., additional, Collier Cameron, A., additional, Doyle, A. P., additional, Hellier, C., additional, Henning, T., additional, Jehin, E., additional, King, G., additional, Kirk, J., additional, Louden, T., additional, Maxted, P. F. L., additional, McCormac, J. J., additional, Osborn, H. P., additional, Palle, E., additional, Pepe, F., additional, Pollacco, D., additional, Prieto-Arranz, J., additional, Queloz, D., additional, Rey, J., additional, Ségransan, D., additional, Udry, S., additional, Walker, S., additional, West, R. G., additional, and Wheatley, P. J., additional

Published
2017
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31. KIC 9533489: a genuine gamma Doradus - delta Scuti Kepler hybrid pulsator with transit events

Author

Bogn��r, Zs., Lampens, P., Fr��mat, Y., Southworth, J., S��dor, ��., De Cat, P., Isaacson, H. T., Marcy, G. W., Ciardi, D. R., Gilliland, R. L., and Mart��n-Fern��ndez, P.

Subjects
Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QC, QB
Abstract

Context: Several hundred candidate hybrid pulsators of type A-F have been identified from space-based observations. Their large number allows both statistical analyses and detailed investigations of individual stars. This offers the opportunity to study the full interior of the genuine hybrids, in which both low-radial-order p- and high-order g-modes are self-excited at the same time. However, a few other physical processes can also be responsible for the observed hybrid nature, related to binarity or to surface inhomogeneities. The finding that most delta Scuti stars also show long-period light variations represents a real challenge for theory. Methods: Fourier analysis of all the available Kepler light curves. Investigation of the frequency and period spacings. Determination of the stellar physical parameters from spectroscopic observations. Modelling of the transit events. Results: The Fourier analysis of the Kepler light curves revealed 55 significant frequencies clustered into two groups, which are separated by a gap between 15 and 27 c/d. The light variations are dominated by the beating of two dominant frequencies located at around 4 c/d. The amplitudes of these two frequencies show a monotonic long-term trend. The frequency spacing analysis revealed two possibilities: the pulsator is either a highly inclined moderate rotator (v~70 km/s, i > 70 deg) or a fast rotator (v~200 km/s) with i~20 deg. The transit analysis disclosed that the transit events which occur with a ~197 c/d period may be caused by a 1.6 R_Jup body orbiting a fainter star, which would be spatially coincident with KIC 9533489., 13 pages, 13 figures, accepted for publication in Astronomy & Astrophysics

Published
2015

32. KIC 9533489: a genuine γ Doradus – δ Scuti Kepler hybrid pulsator with transit events

Author

Bognár, Zs., Lampens, P., Frémat, Y., Southworth, J., Sódor, Á., De Cat, P., Isaacson, H. T., Marcy, G. W., Ciardi, D. R., Gilliland, R. L., and Martín-Fernández, P.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

Context. Several hundred candidate hybrid pulsators of type A–F have been identified from space-based observations. Their large number allows both statistical analyses and detailed investigations of individual stars. This offers the opportunity to study the full interior of the genuine hybrids, in which both low radial order p- and high-order g-modes are self-excited at the same time. However, a few other physical processes can also be responsible for the observed hybrid nature, related to binarity or to surface inhomogeneities. The finding that most δ Scuti stars also show long-period light variations represents a real challenge for theory. Aims. We aim at determining the pulsation frequencies of KIC 9533489, to search for regular patterns and spacings among them, and to investigate the stability of the frequencies and the amplitudes. An additional goal is to study the serendipitously detected transit events: is KIC 9533489 the host star? What are the limitations on the physical parameters of the involved bodies? Methods. We performed a Fourier analysis of all the available Kepler light curves. We investigated the frequency and period spacings and determined the stellar physical parameters from spectroscopic observations. We also modelled the transit events. Results. The Fourier analysis of the Kepler light curves revealed 55 significant frequencies clustered into two groups, which are separated by a gap between 15 and 27 d^(1). The light variations are dominated by the beating of two dominant frequencies located at around 4 d^(-1). The amplitudes of these two frequencies show a monotonic long-term trend. The frequency spacing analysis revealed two possibilities: the pulsator is either a highly inclined moderate rotator (v ≈ 70 km s^(-1), i> 70°) or a fast rotator (v ≈ 200 km s^(-1)) with i ≈ 20°. The transit analysis disclosed that the transit events that occur with a ≈197 d period may be caused by a 1.6 R_(Jup) body orbiting a fainter star, which would be spatially coincident with KIC 9533489.

Published
2015

33. The EBLM project: VI. Mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey.

Author

Gill, S., Maxted, P. F. L., Evans, J. A., Evans, D. F., Southworth, J., Smalley, B., Gary, B. L., Anderson, D. R., Bouchy, F., Cameron, A. C., Dominik, M., Faedi, F., Gillon, M., Gomez Maqueo Chew, Y., Hebb, L., Hellier, C., Jørgensen, U. G., Longa-Peña, P., Martin, D. V., and McCormac, J.

Subjects
BINARY stars, PHYSICAL measurements, VELOCITY measurements, RADIUS (Geometry), STELLAR evolution, AGE of stars
Abstract

Some M-dwarfs around F-/G-type stars have been measured to be hotter and larger than predicted by stellar evolution models. Inconsistencies between observations and models need to be addressed with more mass, radius, and luminosity measurements of low-mass stars to test and refine evolutionary models. Our aim is to measure the masses, radii and ages of the stars in five low-mass eclipsing binary systems discovered by the WASP survey. We used WASP photometry to establish eclipse-time ephemerides and to obtain initial estimates for the transit depth and width. Radial velocity measurements were simultaneously fitted with follow-up photometry to find the best-fitting orbital solution. This solution was combined with measurements of atmospheric parameters to interpolate evolutionary models and estimate the mass of the primary star, and the mass and radius of the M-dwarf companion. We assess how the best fitting orbital solution changes if an alternative limb-darkening law is used and quantify the systematic effects of unresolved companions. We also gauge how the best-fitting evolutionary model changes if different values are used for the mixing length parameter and helium enhancement. We report the mass and radius of five M-dwarfs and find little evidence of inflation with respect to evolutionary models. The primary stars in two systems are near the "blue hook" stage of their post sequence evolution, resulting in two possible solutions for mass and age. We find that choices in helium enhancement and mixing-length parameter can introduce an additional 3−5% uncertainty in measured M-dwarf mass. Unresolved companions can introduce an additional 3−8% uncertainty in the radius of an M-dwarf, while the choice of limb-darkening law can introduce up to an additional 2% uncertainty. The choices in orbital fitting and evolutionary models can introduce significant uncertainties in measurements of physical properties of such systems. [ABSTRACT FROM AUTHOR]

Published
2019
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34. A census of variability in globular cluster M 68 (NGC 4590)

Author

Kains, N, Arellano Ferro, A, Jaimes, RF, Bramich, DM, Skottfelt, J, Jorgensen, UG, Tsapras, Y, Street, RA, Browne, P, Dominik, M, Horne, K, Hundertmark, M, Ipatov, S, Snodgrass, C, Steele, IA, Alsubai, KA, Bozza, V, Novati, SC, Ciceri, S, D'Ago, G, Galianni, P, Gu, S-H, Harpsoe, K, Hinse, TC, Juncher, D, Korhonen, H, Mancini, L, Popovas, A, Rabus, M, Rahvar, S, Southworth, J, Surdej, J, Vilela, C, Wang, X-B, Wertz, O, Consortium, LCOGTR, Consortium, M, The Royal Society, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy

Subjects
Metallicity, Globular clusters: individual: M 68, Stars: variables: general, NDAS, FOS: Physical sciences, Astrophysics, variables: RR Lyrae [Stars], RR Lyrae variable, variables: general [Stars], Stars: variables: RR Lyrae, Astronomy and Astrophysics, Space and Planetary Science, Photometry (optics), Settore FIS/05 - Astronomia e Astrofisica, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Light curve, individual: M 68 [Globular clusters], Distance modulus, Stars, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Globular cluster, Variable star
Abstract

We analyse 20 nights of CCD observations in the V and I bands of the globular cluster M68 (NGC 4590), using these to detect variable objects. We also obtained electron-multiplying CCD (EMCCD) observations for this cluster in order to explore its core with unprecedented spatial resolution from the ground. We reduced our data using difference image analysis, in order to achieve the best possible photometry in the crowded field of the cluster. In doing so, we showed that when dealing with identical networked telescopes, a reference image from any telescope may be used to reduce data from any other telescope, which facilitates the analysis significantly. We then used our light curves to estimate the properties of the RR Lyrae (RRL) stars in M68 through Fourier decomposition and empirical relations. The variable star properties then allowed us to derive the cluster's metallicity and distance. We determine new periods for the variable stars, and search for new variables, especially in the core of the cluster where our method performs particularly well. We detect an additional 4 SX Phe stars, and confirm the variability of another star, bringing the total number of confirmed variable stars in this cluster to 50. We also used archival data stretching back to 1951 in order to derive period changes for some of the single-mode RRL stars, and analyse the significant number of double-mode RRL stars in M68. Furthermore, we find evidence for double-mode pulsation in one of the SX Phe stars in this cluster. Using the different types of variables, we derived an estimate of the metallicity, [Fe/H]=$-2.07 \pm 0.06$ on the ZW scale, and 4 independent estimates of the distance modulus ($\mu_0 \sim$ 15.00 mag) for this cluster. Thanks to the first use of difference image analysis on time-series observations of M68, we are now confident that we have a complete census of the RRL stars in this cluster., Comment: 25 pages, 18 figures, A&A in press

Published
2015

35. Transiting planets from WASP-South, Euler, and TRAPPIST

Author

Delrez, L., Van Grootel, V., Anderson, D. R., Collier-Cameron, A., Doyle, A. P., Fumel, A., Gillon, M., Hellier, C., Jehin, E., Lendl, M., Neveu-VanMalle, M., Maxted, P. F. L., Pepe, F., Pollacco, Don, Queloz, D., Ségransan, D., Smalley, B., Smith, A. M. S., Southworth, J. (John), Triaud, A. H. M. J., Udry, S., and West, Richard G.

Subjects
QB
Abstract

Using the WASP transit survey, we report the discovery of three new hot Jupiters, WASP-68 b, WASP-73 b and WASP-88 b. The planet WASP-68 bhas a mass of 0.95 ± 0.03 MJup, a radius of 1.24-0.06+0.10 RJup, and orbits a V = 10.7 G0-type star (1.24 ± 0.03 M⊙ 1.69-0.06+0.11 R⊙, Teff = 5911 ± 60 K) with a period of 5.084298 ± 0.000015 days. Its size is typical of hot Jupiters with similar masses. The planet WASP-73 bis significantly more massive (1.88-0.06+0.07 MJup) and slightly larger (1.16-0.08+0.12 RJup) than Jupiter. It orbits a V = 10.5 F9-type star (1.34-0.04+0.05 M⊙, 2.07-0.08+0.19 R⊙, Teff = 6036 ± 120 K) every 4.08722 ± 0.00022 days. Despite its high irradiation (~2.3 × 109 erg s-1 cm-2), WASP-73 b has a high mean density (1.20-0.30+0.26 ρJup) that suggests an enrichment of the planet in heavy elements. The planet WASP-88 bis a 0.56 ± 0.08 MJuphot Jupiter orbiting a V = 11.4 F6-type star (1.45 ± 0.05 M⊙, 2.08-0.06+0.12 R⊙, Teff = 6431 ± 130 K) with a period of 4.954000 ± 0.000019 days. With a radius of 1.70-0.07+0.13 RJup, it joins the handful of planets with super-inflated radii. The ranges of ages we determine through stellar evolution modeling are 4.5–7.0 Gyr for WASP-68, 2.8-5.7 Gyr for WASP-73 and 1.8–4.3 Gyr for WASP-88. The star WASP-73 appears to be significantly evolved, close to or already in the subgiant phase. The stars WASP-68 and WASP-88 are less evolved, although in an advanced stage of core H-burning.

Published
2014

36. Erratum: Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (Astronomy and Astrophysics (2013) 555 (A36))

Author

Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsøe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, Andrew, Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsøe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, Andrew

Published
2016

37. MiNDSTEp differential photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756: microlensing and a new time delay

Author

Giannini, E., primary, Schmidt, R. W., additional, Wambsganss, J., additional, Alsubai, K., additional, Andersen, J. M., additional, Anguita, T., additional, Bozza, V., additional, Bramich, D. M., additional, Browne, P., additional, Calchi Novati, S., additional, Damerdji, Y., additional, Diehl, C., additional, Dodds, P., additional, Dominik, M., additional, Elyiv, A., additional, Fang, X., additional, Figuera Jaimes, R., additional, Finet, F., additional, Gerner, T., additional, Gu, S., additional, Hardis, S., additional, Harpsøe, K., additional, Hinse, T. C., additional, Hornstrup, A., additional, Hundertmark, M., additional, Jessen-Hansen, J., additional, Jørgensen, U. G., additional, Juncher, D., additional, Kains, N., additional, Kerins, E., additional, Korhonen, H., additional, Liebig, C., additional, Lund, M. N., additional, Lundkvist, M. S., additional, Maier, G., additional, Mancini, L., additional, Masi, G., additional, Mathiasen, M., additional, Penny, M., additional, Proft, S., additional, Rabus, M., additional, Rahvar, S., additional, Ricci, D., additional, Scarpetta, G., additional, Sahu, K., additional, Schäfer, S., additional, Schönebeck, F., additional, Skottfelt, J., additional, Snodgrass, C., additional, Southworth, J., additional, Surdej, J., additional, Tregloan-Reed, J., additional, Vilela, C., additional, Wertz, O., additional, and Zimmer, F., additional

Published
2016
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38. A solar twin in the eclipsing binary LL Aquarii

Author

Graczyk, D., primary, Smolec, R., additional, Pavlovski, K., additional, Southworth, J., additional, Pietrzyński, G., additional, Maxted, P. F. L., additional, Konorski, P., additional, Gieren, W., additional, Pilecki, B., additional, Taormina, M., additional, Suchomska, K., additional, Karczmarek, P., additional, Górski, M., additional, Wielgórski, P., additional, and Anderson, R. I., additional

Published
2016
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39. Five transiting hot Jupiters discovered using WASP-South,Euler, and TRAPPIST: WASP-119 b, WASP-124 b, WASP-126 b, WASP-129 b, and WASP-133 b

Author

Maxted, P. F. L., primary, Anderson, D. R., additional, Collier Cameron, A., additional, Delrez, L., additional, Gillon, M., additional, Hellier, C., additional, Jehin, E., additional, Lendl, M., additional, Neveu-VanMalle, M., additional, Pepe, F., additional, Pollacco, D., additional, Queloz, D., additional, Ségransan, D., additional, Smalley, B., additional, Smith, A. M. S., additional, Southworth, J., additional, Triaud, A. H. M. J., additional, Udry, S., additional, Wagg, T., additional, and West, R. G., additional

Published
2016
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41. High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Author

Evans, D. F., primary, Southworth, J., additional, Maxted, P. F. L., additional, Skottfelt, J., additional, Hundertmark, M., additional, Jørgensen, U. G., additional, Dominik, M., additional, Alsubai, K. A., additional, Andersen, M. I., additional, Bozza, V., additional, Bramich, D. M., additional, Burgdorf, M. J., additional, Ciceri, S., additional, D’Ago, G., additional, Figuera Jaimes, R., additional, Gu, S.-H., additional, Haugbølle, T., additional, Hinse, T. C., additional, Juncher, D., additional, Kains, N., additional, Kerins, E., additional, Korhonen, H., additional, Kuffmeier, M., additional, Mancini, L., additional, Peixinho, N., additional, Popovas, A., additional, Rabus, M., additional, Rahvar, S., additional, Schmidt, R. W., additional, Snodgrass, C., additional, Starkey, D., additional, Surdej, J., additional, Tronsgaard, R., additional, von Essen, C., additional, Wang, Yi-Bo, additional, and Wertz, O., additional

Published
2016
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42. Exploring the crowded central region of ten Galactic globular clusters using EMCCDs

Author

Figuera Jaimes, R., primary, Bramich, D. M., additional, Skottfelt, J., additional, Kains, N., additional, Jørgensen, U. G., additional, Horne, K., additional, Dominik, M., additional, Alsubai, K. A., additional, Bozza, V., additional, Calchi Novati, S., additional, Ciceri, S., additional, D’Ago, G., additional, Galianni, P., additional, Gu, S.-H., additional, W Harpsøe, K. B., additional, Haugbølle, T., additional, Hinse, T. C., additional, Hundertmark, M., additional, Juncher, D., additional, Korhonen, H., additional, Mancini, L., additional, Popovas, A., additional, Rabus, M., additional, Rahvar, S., additional, Scarpetta, G., additional, Schmidt, R. W., additional, Snodgrass, C., additional, Southworth, J., additional, Starkey, D., additional, Street, R. A., additional, Surdej, J., additional, Wang, X.-B., additional, and Wertz, O., additional

Published
2016
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43. Multi-site campaign for transit timing variations of WASP-12 b: Possible detection of a long-period signal of planetary origin a long-period signal of planetary origin

Author

Maciejewski, G, Dimitrov, D, Seeliger, M, Raetz, S, Bukowiecki, L, Kitze, M, Errmann, R, Nowak, G, Niedzielski, A, Popov, V, Marka, C, Gozdziewski, K, Neuhauser, R, Ohlert, J, Hinse, Tc, Lee, Jw, Lee, C, Yoon, J, Berndt, A, Gilbert, H, Ginski, C, Hohle, Mm, Mugrauer, M, Roll, T, Schmidt, Tob, Tetzlaff, N, Mancini, L, Southworth, J, Dall'Ora, M, Ciceri, S, Zambelli, R, Corfini, G, Takahashi, H, Tachihara, K, Benko, Jm, Sarneczky, K, Szabo, Gm, Varga, Tn, Vanko, M, Joshi, Yc, and Chen, Wp

Subjects
Settore FIS/05 - Astronomia e Astrofisica
Published
2013

44. A much lower density for the transiting extrasolar planet WASP-7: (Research Note)

Author

Southworth, J, Dominik, M, Jorgensen, Ug, Rahvar, S, Snodgrass, C, Alsubai, K, Bozza, V, Browne, P, Burgdorf, M, Novati, Sc, Dodds, P, Dreizler, S, Finet, F, Gerner, T, Hardis, S, Harpsoe, K, Hellier, C, Hinse, Tc, Hundertmark, M, Kains, N, Kerins, E, Liebig, C, Mancini, L, Mathiasen, M, Penny, Mt, Proft, S, Ricci, D, Sahu, K, Scarpetta, G, Schafer, S, Schonebeck, F, and Surdej, J

Subjects
Settore FIS/05 - Astronomia e Astrofisica
Published
2011

45. Three irradiated and bloated hot Jupiters

Author

West, R. G., primary, Hellier, C., additional, Almenara, J.-M., additional, Anderson, D. R., additional, Barros, S. C. C., additional, Bouchy, F., additional, Brown, D. J. A., additional, Collier Cameron, A., additional, Deleuil, M., additional, Delrez, L., additional, Doyle, A. P., additional, Faedi, F., additional, Fumel, A., additional, Gillon, M., additional, Gómez Maqueo Chew, Y., additional, Hébrard, G., additional, Jehin, E., additional, Lendl, M., additional, Maxted, P. F. L., additional, Pepe, F., additional, Pollacco, D., additional, Queloz, D., additional, Ségransan, D., additional, Smalley, B., additional, Smith, A. M. S., additional, Southworth, J., additional, Triaud, A. H. M. J., additional, and Udry, S., additional

Published
2016
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46. KIC 7582608: a newKeplerroAp star with frequency variability

Author

Holdsworth, Daniel Luke, Smalley, B., Kurtz, D.W., Southworth, J., Cunha, M.S., Clubb, K.I., Ballot, J., Holdsworth, Daniel Luke, Smalley, B., Kurtz, D.W., Southworth, J., Cunha, M.S., Clubb, K.I., and Ballot, J.

Abstract

We analyse the fifth roAp star reported in the Kepler field, KIC 7582608, discovered with the SuperWASP project. The object shows a high frequency pulsation at 181.7324 d−1 (P = 7.9 min) with an amplitude of 1.45 mmag, and low frequency rotational modulation corresponding to a period of 20.4339 d. Spectral analysis confirms the Ap nature of the target, with characteristic lines of rare earth elements present. From our spectral observations we derive a lower limit on the mean magnetic field modulus of (B) = 3.05 ± 0.23 kG. Long Cadence Kepler observations show a frequency quintuplet split by the rotational period of the star, typical for an oblique pulsator. We suggest the star is a quadrupole pulsator with a geometry such that i ∼ 66◦ and β ∼ 33◦. We detect frequency variations of the pulsation in both the WASP and Kepler data sets on many time scales. Linear, non-adiabatic stability modelling allows us to constrain a region on the HR diagram where the pulsations are unstable, an area consistent with observations.

Published
2015

47. HD183648: a Kepler eclipsing binary with anomalous ellipsoidal variations and a pulsating component

Author

García, R.A., Derekas, A., Borkovits, T., Fuller, J., Szabó, Gy. M., Pavlovski, K., Csák, B., Dózsa, Á., Kovács, J., Szabó, R., Hambleton, Kelly, Kinemuchi, K., Kolbas, V., Kurtz, D. W., Maloney, F., Prša, A., Southworth, J., Sztakovics, J., Bíró, I. B., Jankovics, I., Ballot, J., García, R.A., Derekas, A., Borkovits, T., Fuller, J., Szabó, Gy. M., Pavlovski, K., Csák, B., Dózsa, Á., Kovács, J., Szabó, R., Hambleton, Kelly, Kinemuchi, K., Kolbas, V., Kurtz, D. W., Maloney, F., Prša, A., Southworth, J., Sztakovics, J., Bíró, I. B., Jankovics, I., and Ballot, J.

Abstract

KIC 8560861 (HD 183648) is a marginally eccentric (e = 0.05) eclipsing binary with an orbital period of Porb = 31.973 d, exhibiting mmag amplitude pulsations on time scales of a few days. We present the results of the complex analysis of high and medium-resolution spectroscopic data and Kepler Q0 – Q16 long cadence photometry.

Published
2015

48. Rotation periods and astrometric motions of the Luhman 16AB brown dwarfs by high-resolution lucky-imaging monitoring

Author

Mancini, L., primary, Giacobbe, P., additional, Littlefair, S. P., additional, Southworth, J., additional, Bozza, V., additional, Damasso, M., additional, Dominik, M., additional, Hundertmark, M., additional, Jørgensen, U. G., additional, Juncher, D., additional, Popovas, A., additional, Rabus, M., additional, Rahvar, S., additional, Schmidt, R. W., additional, Skottfelt, J., additional, Snodgrass, C., additional, Sozzetti, A., additional, Alsubai, K., additional, Bramich, D. M., additional, Calchi Novati, S., additional, Ciceri, S., additional, D’Ago, G., additional, Figuera Jaimes, R., additional, Galianni, P., additional, Gu, S.-H., additional, Harpsøe, K., additional, Haugbølle, T., additional, Henning, Th., additional, Hinse, T. C., additional, Kains, N., additional, Korhonen, H., additional, Scarpetta, G., additional, Starkey, D., additional, Surdej, J., additional, Wang, X.-B., additional, and Wertz, O., additional

Published
2015
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50. The GAPS programme with HARPS-N at TNG

Author

Damasso, M., primary, Esposito, M., additional, Nascimbeni, V., additional, Desidera, S., additional, Bonomo, A. S., additional, Bieryla, A., additional, Malavolta, L., additional, Biazzo, K., additional, Sozzetti, A., additional, Covino, E., additional, Latham, D. W., additional, Gandolfi, D., additional, Rainer, M., additional, Petrovich, C., additional, Collins, K. A., additional, Boccato, C., additional, Claudi, R. U., additional, Cosentino, R., additional, Gratton, R., additional, Lanza, A. F., additional, Maggio, A., additional, Micela, G., additional, Molinari, E., additional, Pagano, I., additional, Piotto, G., additional, Poretti, E., additional, Smareglia, R., additional, Di Fabrizio, L., additional, Giacobbe, P., additional, Gomez-Jimenez, M., additional, Murabito, S., additional, Molinaro, M., additional, Affer, L., additional, Barbieri, M., additional, Bedin, L. R., additional, Benatti, S., additional, Borsa, F., additional, Maldonado, J., additional, Mancini, L., additional, Scandariato, G., additional, Southworth, J., additional, and Zanmar Sanchez, R., additional

Published
2015
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