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204. The first view of delta Scuti and gamma Doradus stars with the TESS mission

Author

Antoci, V., Cunha, M.S., Bowman, D.M., Murphy, S. J., Kurtz, D.W., Bedding, T. R., Borre, C. C., Christophe, S., Daszynska-Daszkiewicz, J., Fox-Machado, L., García Hernández, Antonio, Ghasemi, H., Handberg, R., Hansen, H., Hasanzadeh, A., Houdek, G., Johnston, C., Justesen, A. B., Kahraman Alicavus, F., Kotysz, K., Latham, D., Matthews, J. M., Mønster, J., Niemczura, E., Paunzen, E., Sánchez Arias, J. P., Pigulski, A., Pepper, J., Richey-Yowell, T., Safari, H., Seager, S., Smalley, B., Shutt, T., Sódor, A., Suárez Yanes, Juan Carlos, Tkachenko, A., Wu, T., Zwintz, K., Barceló Forteza, S., Brunsden, E., Bognár, Z., Buzasi, D. L., Chowdhury, S., De Cat, P., Evans, J. A., Guo, Z., Guzik, J. A., Jevtic, N., Lampens, P., Lares Martiz, M., Lovekin, C., Li, G., Mirouh, G. M., Mkrtichian, D., Monteiro, M. J. P. F. G., Nemec, J. M., Ouazzani, R.-M., Pascual Granado, J., Reese, D. R., Rieutord, M., Rodón Ortiz, José Ramón, Skarka, M., Sowicka, P., Stateva, I., Szabó, R., Weiss, W. W., Danish National Research Foundation, European Space Agency, Aarhus University Research Foundation, Fundação para a Ciência e a Tecnologia (Portugal), Polish Academy of Sciences, European Commission, Ministerio de Ciencia e Innovación (España), Hungarian Academy of Sciences, European Research Council, Research Foundation - Flanders, Belgian Science Policy Office, Whitaker Foundation, Natural Sciences and Engineering Research Council of Canada, Ministry of Science and Technology (Thailand), Agence Nationale de la Recherche (France), National Natural Science Foundation of China, National Aeronautics and Space Administration (US), and National Science Foundation (US)

Subjects
photometric [techniques], interiors [stars], techniques: photometric, chemically peculiar [stars], Astrophysics - Solar and Stellar Astrophysics, stars: variables: delta Scuti, Asteroseismology, stars: interiors, variables: delta Scuti [stars], stars: chemically peculiar
Abstract

We present the first asteroseismic results for δ Scuti and γ Doradus stars observed in Sectors 1 and 2 of the TESS mission. We utilize the 2-min cadence TESS data for a sample of 117 stars to classify their behaviour regarding variability and place them in the Hertzsprung-Russell diagram using Gaia DR2 data. Included within our sample are the eponymous members of two pulsator classes, γ Doradus and SX Phoenicis. Our sample of pulsating intermediate-mass stars observed by TESS also allows us to confront theoretical models of pulsation driving in the classical instability strip for the first time and show that mixing processes in the outer envelope play an important role. We derive an empirical estimate of 74 per cent for the relative amplitude suppression factor as a result of the redder TESS passband compared to the Kepler mission using a pulsating eclipsing binary system. Furthermore, our sample contains many high-frequency pulsators, allowing us to probe the frequency variability of hot young δ Scuti stars, which were lacking in the Kepler mission data set, and identify promising targets for future asteroseismic modelling. The TESS data also allow us to refine the stellar parameters of SX Phoenicis, which is believed to be a blue straggler. © 2019 The Author(s), We thank the referee for useful comments and discussions. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Re-search Foundation (Grant agreement no.: DNRF106), ESA PRODEX (PEA 4000119301), and Stellar Astrophysics Centre (SAC) at Aarhus University. We thank the TESS and TASC/TASOC teams for their support of this work. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-2655. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). MC was supported by FCT -Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2019, PTDC/FIS-AST/30389/2017, and POCI-01-0145-FEDER-030389. MC is supported in the form of work contract funded by national funds through FCT (CEECIND/02619/2017). JDD acknowledges support from the Polish National Science Center (NCN), grant no. 2018/29/B/ST9/02803. AGH acknowledges funding support from Spanish public funds for research under projects ESP201787676-2-2 and ESP2015-65712-C5-5-R of the Spanish Ministry of Science and Education. FKA gratefully acknowledges funding through grant 2015/18/A/ST9/00578 of the Polish National Science Centre (NCN). JPe acknowledges funding support from the NSF REU program under grant number PHY-1359195. APi and KK acknowledge support provided by the Polish National Science Center (NCN) grant No. 2016/21/B/ST9/01126. This project has been supported by the Lendulet Program of the Hungarian Academy of Sciences, project No. LP2018-7/2018, and by the support provided from the National Research, Development and Innovation Fund of Hungary, financed under the K16 funding scheme, project No. 115709. JCS acknowledges funding support from Spanish public funds for research under projects ESP2017-87676-2-2 and ESP2015-65712-C5-5-R, and from project RYC2012-09913 under the 'Ramon y Cajal' program of the Spanish Ministry of Science and Education. The research leading to these results has (partially) received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement N.670519: MAMSIE), from the KULeuven Research Council (grant C16/18/005: PARADISE), from the Research Foundation Flanders (FWO) under grant agreement G0H5416N (ERC Runner Up Project), as well as from the BELgian federal Science Policy Office (BELSPO) through PRODEX grant PLATO. SBF acknowledges support by the Spanish State Research Agency (AEI) through project No. 'ESP2017-87676-C5-1-R' and No MDM-2017-0737 Unidad de Excelencia `Maria de Maeztu'-Centro de Astrobiolog ' ia (CSICINTA). ZsB acknowledges the support provided from the National Research, Development and Innovation Fund of Hungary, financed under the PD1717 funding scheme, project no. PD-123910. DLB acknowledges support from the Whitaker Foundation. SC gratefully acknowledges funding through grant 2015/18/A/ST9/00578 of the Polish National Science Centre (NCN). CCL gratefully acknowledges support from the Natural Sciences and Engineering Research Council of Canada. GMM acknowledges funding by the STFC consolidated grant ST/R000603/1. RMO, SC, and DR were supported in this work by the 'Programme National de Physique Stellaire' (PNPS) of CNRS/INSU co-funded by CEA and CNES. IS acknowledges the partial support of projects DN 08-1/2016 and DN 18/13-12.12.2017. PS acknowledges financial support by the Polish NCN grant 2015/18/A/ST9/00578. MS acknowledges the Postdoc@MUNI project CZ.02.2.69/0.0/0.0/16-027/0008360. JPG, JRR, and MLM acknowledge funding support from Spanish public funds for research under project ESP2017-87676-C5-5-R and from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). JAE acknowledges STFC for funding support (reference ST/N504348/1). LFM acknowledges the financial support from the DGAPA-UNAM under grant PAPIIT IN100918. DMk acknowledges his work as part of the research activity of the National Astronomical Research Institute of Thailand (NARIT), which is supported by the Ministry of Science and Technology of Thailand. MR acknowledges the support of the French Agence Nationale de la Recherche (ANR), under grant ESRR (ANR-16-CE31-0007-01). We acknowledge the International Space Science Institute (ISSI) for supporting the SoFAR international team http://www.issi.unibe.ch/teams/sofar/.TW acknowledges the NSFC of China (Grant Nos. 11873084 and 11521303) and YunnanApplied Basic Research Projects (GrantNo. 2017B008). IS acknowledges for a partial support of DN 08-1/2016 funded by the Bulgarian NSF. This work hasmade use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, ht tps://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 670519: MAMSIE) and from the Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO) under the grant agreement G0H5416N (ERC Opvangproject). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in A&AS 143, 23. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.

Published
2019

205. A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS

Author

Huber, D. Chaplin, W.J. Chontos, A. Kjeldsen, H. Christensen-Dalsgaard, J. Bedding, T.R. Ball, W. Brahm, R. Espinoza, N. Henning, T. Jordán, A. Sarkis, P. Knudstrup, E. Albrecht, S. Grundahl, F. Andersen, M.F. Pallé, P.L. Crossfield, I. Fulton, B. Howard, A.W. Isaacson, H.T. Weiss, L.M. Handberg, R. Lund, M.N. Serenelli, A.M. Rørsted Mosumgaard, J. Stokholm, A. Bieryla, A. Buchhave, L.A. Latham, D.W. Quinn, S.N. Gaidos, E. Hirano, T. Ricker, G.R. Vanderspek, R.K. Seager, S. Jenkins, J.M. Winn, J.N. Antia, H.M. Appourchaux, T. Basu, S. Bell, K.J. Benomar, O. Bonanno, A. Buzasi, D.L. Campante, T.L. Çelik Orhan, Z. Corsaro, E. Cunha, M.S. Davies, G.R. Deheuvels, S. Grunblatt, S.K. Hasanzadeh, A. Di Mauro, M.P. A. García, R. Gaulme, P. Girardi, L. Guzik, J.A. Hon, M. Jiang, C. Kallinger, T. Kawaler, S.D. Kuszlewicz, J.S. Lebreton, Y. Li, T. Lucas, M. Lundkvist, M.S. Mann, A.W. Mathis, S. Mathur, S. Mazumdar, A. Metcalfe, T.S. Miglio, A. F. G. Monteiro, M.J.P. Mosser, B. Noll, A. Nsamba, B. Joel Ong, J.M. Örtel, S. Pereira, F. Ranadive, P. Régulo, C. Rodrigues, T.S. Roxburgh, I.W. Aguirre, V.S. Smalley, B. Schofield, M. Sousa, S.G. Stassun, K.G. Stello, D. Tayar, J. White, T.R. Verma, K. Vrard, M. Yildiz, M. Baker, D. Bazot, M. Beichmann, C. Bergmann, C. Bugnet, L. Cale, B. Carlino, R. Cartwright, S.M. Christiansen, J.L. Ciardi, D.R. Creevey, O. Dittmann, J.A. Nascimento, J.-D.D. Eylen, V.V. Fürész, G. Gagné, J. Gao, P. Gazeas, K. Giddens, F. Hall, O.J. Hekker, S. Ireland, M.J. Latouf, N. Lebrun, D. Levine, A.M. Matzko, W. Natinsky, E. Page, E. Plavchan, P. Mansouri-Samani, M. McCauliff, S. Mullally, S.E. Orenstein, B. Soto, A.G. Paegert, M. Van Saders, J.L. Schnaible, C. Soderblom, D.R. Szabó, R. Tanner, A. Tinney, C.G. Teske, J. Thomas, A. Trampedach, R. Wright, D. Yuan, T.T. Zohrabi, F.

Abstract

We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R∗ = 2.943 ± 0.064 Ro), mass (M∗ = 1.212 ± 0.074 Mo), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a "hot Saturn" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm-3). The properties of HD 221416 b show that the host-star metallicity-planet mass correlation found in sub-Saturns (4-8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology. © 2019. The American Astronomical Society. All rights reserved..

Published
2019

206. K2 Observations of SN 2018oh Reveal a Two-component Rising Light Curve for a Type Ia Supernova

Author

Dimitriadis, G, Foley, RJ, Rest, A, Kasen, D, Piro, AL, Polin, A, Jones, DO, Villar, A, Narayan, G, A. Coulter, D, Kilpatrick, CD, Pan, Y-C, Rojas-Bravo, C, Fox, OD, Jha, SW, Nugent, PE, Riess, AG, Scolnic, D, Drout, MR, Barentsen, G, Dotson, J, Gully-Santiago, M, Hedges, C, Cody, AM, Barclay, T, Howell, S, Garnavich, P, Tucker, BE, Shaya, E, Mushotzky, R, Olling, RP, Margheim, S, Zenteno, A, Coughlin, J, Cleve, JE Van, de Miranda Cardoso, J Vinícius, Larson, KA, McCalmont-Everton, KM, Peterson, CA, Ross, SE, Reedy, LH, Osborne, D, McGinn, C, Kohnert, L, Migliorini, L, Wheaton, A, Spencer, B, Labonde, C, Castillo, G, Beerman, G, Steward, K, Hanley, M, Larsen, R, Gangopadhyay, R, Kloetzel, R, Weschler, T, Nystrom, V, Moffatt, J, Redick, M, Griest, K, Packard, M, Muszynski, M, Kampmeier, J, Bjella, R, Flynn, S, Elsaesser, B, Chambers, KC, Flewelling, HA, Huber, ME, Magnier, EA, Waters, CZ, Schultz, ASB, Bulger, J, Lowe, TB, Willman, M, Smartt, SJ, Smith, KW, Points, S, Strampelli, GM, Brimacombe, J, Chen, P, Muñoz, JA, Mutel, RL, Shields, J, Vallely, PJ, Villanueva, S, Li, W, Wang, X, Zhang, J, Lin, H, Mo, J, Zhao, X, Sai, H, Zhang, X, Zhang, K, Zhang, T, Wang, L, Baron, E, DerKacy, JM, Li, L, Chen, Z, Xiang, D, Rui, L, Huang, F, Li, X, Hosseinzadeh, G, Howell, DA, Arcavi, I, Hiramatsu, D, Burke, J, Valenti, S, Tonry, JL, Denneau, L, Heinze, AN, Weiland, H, Stalder, B, Vinkó, J, Sárneczky, K, Pál, A, Bódi, A, Bognár, Zs, Csák, B, Cseh, B, Csörnyei, G, Hanyecz, O, Ignácz, B, Kalup, Cs, Könyves-Tóth, R, Kriskovics, L, Ordasi, A, Rajmon, I, Sódor, A, Szabó, R, Szakáts, R, Zsidi, G, Williams, SC, Nordin, J, Cartier, R, Frohmaier, C, Galbany, L, Gutiérrez, CP, Hook, I, Inserra, C, Smith, M, Sand, DJ, Andrews, JE, Smith, N, and Bilinski, C

Subjects
Brightness, FOS: Physical sciences, Flux, Astrophysics, Type (model theory), Astronomy & Astrophysics, 01 natural sciences, Luminosity, individual (SN 2018oh) [supernovae], individual [supernovae], 0103 physical sciences, Black-body radiation, Astronomical And Space Sciences, 010306 general physics, 010303 astronomy & astrophysics, STFC, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, RCUK, Astronomy and Astrophysics, Light curve, Supernova, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, general [supernovae], Energy (signal processing)
Abstract

We present an exquisite, 30-min cadence Kepler (K2) light curve of the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks before explosion, covering the moment of explosion and the subsequent rise, and continuing past peak brightness. These data are supplemented by multi-color Pan-STARRS1 and CTIO 4-m DECam observations obtained within hours of explosion. The K2 light curve has an unusual two-component shape, where the flux rises with a steep linear gradient for the first few days, followed by a quadratic rise as seen for typical SNe Ia. This "flux excess" relative to canonical SN Ia behavior is confirmed in our $i$-band light curve, and furthermore, SN 2018oh is especially blue during the early epochs. The flux excess peaks 2.14$\pm0.04$ days after explosion, has a FWHM of 3.12$\pm0.04$ days, a blackbody temperature of $T=17,500^{+11,500}_{-9,000}$ K, a peak luminosity of $4.3\pm0.2\times10^{37}\,{\rm erg\,s^{-1}}$, and a total integrated energy of $1.27\pm0.01\times10^{43}\,{\rm erg}$. We compare SN 2018oh to several models that may provide additional heating at early times, including collision with a companion and a shallow concentration of radioactive nickel. While all of these models generally reproduce the early K2 light curve shape, we slightly favor a companion interaction, at a distance of $\sim$$2\times10^{12}\,{\rm cm}$ based on our early color measurements, although the exact distance depends on the uncertain viewing angle. Additional confirmation of a companion interaction in future modeling and observations of SN 2018oh would provide strong support for a single-degenerate progenitor system., 20 pages, 9 figures, 2 tables. Submitted to APJ Letters on 31 Jul 2018, Accepted for publication on 31 Aug 2018

Published
2019

207. The first view of δ Scuti and γ Doradus stars with the TESS mission

Author

Antoci, V, Cunha, M S, Bowman, D M, Murphy, S J, Kurtz, Donald Wayne, Bedding, T R, Borre, C C, Christophe, S, Daszyńska-Daszkiewicz, J, Fox-Machado, L, Hernández, A García, Ghasemi, H, Handberg, R, Hansen, H, Hasanzadeh, A, Houdek, G, Johnston, C, Justesen, A B, Alicavus, F Kahraman, Kotysz, K, Latham, D, Matthews, J M, Mønster, J, Niemczura, E, Paunzen, E, Arias, J P Sánchez, Pigulski, A, Pepper, J, Richey-Yowell, T, Safari, H, Seager, S, Smalley, B, Shutt, T, Sódor, A, Suárez, J-C, Tkachenko, A, Wu, T, Zwintz, K, Forteza, S Barceló, Brunsden, E, Bognár, Z, Buzasi, D L, Chowdhury, S, De Cat, P, Evans, J A, Guo, Z, Guzik, J A, Jevtic, N, Lampens, P, Martiz, M Lares, Lovekin, C, Li, G, Mirouh, G M, Mkrtichian, D, Monteiro, M J P F G, Nemec, J M, Ouazzani, R-M, Pascual-Granado, J, Reese, D R, Rieutord, M, Rodon, J R, Skarka, M, Sowicka, P, Stateva, I, Szabó, R, Weiss, W W, Antoci, V, Cunha, M S, Bowman, D M, Murphy, S J, Kurtz, Donald Wayne, Bedding, T R, Borre, C C, Christophe, S, Daszyńska-Daszkiewicz, J, Fox-Machado, L, Hernández, A García, Ghasemi, H, Handberg, R, Hansen, H, Hasanzadeh, A, Houdek, G, Johnston, C, Justesen, A B, Alicavus, F Kahraman, Kotysz, K, Latham, D, Matthews, J M, Mønster, J, Niemczura, E, Paunzen, E, Arias, J P Sánchez, Pigulski, A, Pepper, J, Richey-Yowell, T, Safari, H, Seager, S, Smalley, B, Shutt, T, Sódor, A, Suárez, J-C, Tkachenko, A, Wu, T, Zwintz, K, Forteza, S Barceló, Brunsden, E, Bognár, Z, Buzasi, D L, Chowdhury, S, De Cat, P, Evans, J A, Guo, Z, Guzik, J A, Jevtic, N, Lampens, P, Martiz, M Lares, Lovekin, C, Li, G, Mirouh, G M, Mkrtichian, D, Monteiro, M J P F G, Nemec, J M, Ouazzani, R-M, Pascual-Granado, J, Reese, D R, Rieutord, M, Rodon, J R, Skarka, M, Sowicka, P, Stateva, I, Szabó, R, and Weiss, W W

Abstract

We present the first asteroseismic results for δ Scuti and γ Doradus stars observed in Sectors 1 and 2 of the TESS mission. We utilise the 2-min cadence TESS data for a sample of 117 stars to classify their behaviour regarding variability and place them in the Hertzsprung-Russell diagram using Gaia DR2 data. Included within our sample are the eponymous members of two pulsator classes, γ Doradus and SX Phoenicis. Our sample of pulsating intermediate-mass stars observed by TESS also allows us to confront theoretical models of pulsation driving in the classical instability strip for the first time and show that mixing processes in the outer envelope play an important role. We derive an empirical estimate of 74% for the relative amplitude suppression factor as a result of the redder TESS passband compared to the Kepler mission using a pulsating eclipsing binary system. Furthermore, our sample contains many high-frequency pulsators, allowing us to probe the frequency variability of hot young δ Scuti stars, which were lacking in the Kepler mission data set, and identify promising targets for future asteroseismic modelling. The TESS data also allow us to refine the stellar parameters of SX Phoenicis, which is believed to be a blue straggler.

Published
2019

208. Rotation and pulsation in Ap stars: first light results from TESS sectors 1 and 2

Author

Cunha, M S, Antoci, V, Holdsworth, Daniel Luke, Kurtz, Donald Wayne, Balona, L A, Bognár, Zs, Bowman, D M, Guo, Z, Kołaczek-Szymański, P A, Lares-Martiz, M, Paunzen, E, Skarka, M, Smalley, B, Sódor, Á, Kochukhov, O, Pepper, J, Richey-Yowell, T, Ricker, G R, Seager, S, Buzasi, D L, Fox-Machado, L, Hasanzadeh, A, Niemczura, E, Quitral-Manosalva, P, Monteiro, M J P F G, Stateva, I, De Cat, P, Hernández, A García, Ghasemi, H, Handler, G, Hey, D, Matthews, J M, Nemec, J M, Pascual-Granado, J, Safari, H, Suárez, J C, Szabó, R, Tkachenko, A, Weiss, W W, Cunha, M S, Antoci, V, Holdsworth, Daniel Luke, Kurtz, Donald Wayne, Balona, L A, Bognár, Zs, Bowman, D M, Guo, Z, Kołaczek-Szymański, P A, Lares-Martiz, M, Paunzen, E, Skarka, M, Smalley, B, Sódor, Á, Kochukhov, O, Pepper, J, Richey-Yowell, T, Ricker, G R, Seager, S, Buzasi, D L, Fox-Machado, L, Hasanzadeh, A, Niemczura, E, Quitral-Manosalva, P, Monteiro, M J P F G, Stateva, I, De Cat, P, Hernández, A García, Ghasemi, H, Handler, G, Hey, D, Matthews, J M, Nemec, J M, Pascual-Granado, J, Safari, H, Suárez, J C, Szabó, R, Tkachenko, A, and Weiss, W W

Abstract

We present the first results from the Transiting Exoplanet Survey Satellite (TESS) on the ro- tational and pulsational variability of magnetic chemically peculiar A-type stars. We analyse TESS 2-min cadence data from sectors 1 and 2 on a sample of 83 stars. Five new rapidly oscillating Ap (roAp) stars are announced. One of these pulsates with periods around 4.7 min, making it the shortest period roAp star known to date. Four out of the five new roAp stars are multiperiodic. Three of these, and the singly-periodic one show the presence of rotational mode splitting. Individual frequencies are provided in all cases. In addition, seven previously known roAp stars are analysed. Additional modes of oscillation are found in some stars, while in others we are able to distinguish the true pulsations from possible aliases present in the ground-based data. We find that the pulsation amplitude in the TESS filter is typically a factor 6 smaller than that in the B filter which is usually used for ground-based observations. For four roAp stars we set constraints on the inclination angle and magnetic obliquity, through the application of the oblique pulsator model. We also confirm the absence of roAp-type pulsa- tions down to amplitude limits of 6 and 13 µmag, respectively, in two of the best characterised non-oscillating Ap (noAp) stars. We announce 27 new rotational variables along with their ro- tation periods, and provide different rotation periods for seven other stars. Finally, we discuss how these results challenge state-of-the-art pulsation models for roAp stars.

Published
2019

209. Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the $Kepler$ 2 Observations

Author

Li, W., Wang, X., Vinkó, J., Mo, J., Hosseinzadeh, G., Sand, D. J., Zhang, J., Lin, H., Zhang, T., Wang, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Zhang, X., Li, L., Baron, E., Derkacy, J. M., Zhao, X., Sai, H., Zhang, K., Howell, D. A., McCully, C., Arcavi, I., Valenti, S., Hiramatsu, D., Burke, J., Rest, A., Garnavich, P., Tucker, B. E., Narayan, G., Shaya, E., Margheim, S., Zenteno, A., Villar, A., Dimitriadis, G., Foley, R. J., Pan, Y.-C., Coulter, D. A., Fox, O. D., Jha, S. W., Jones, D. O., Kasen, D. N., Kilpatrick, C. D., Piro, A. L., Riess, A. G., Rojas-Bravo, C., Shappee, B. J., Holoien, T. W.-S., Stanek, K. Z., Drout, M. R., Auchettl, K., Kochanek, C. S., Brown, J. S., Bose, S., Bersier, D., Brimacombe, J., Chen, P., Dong, S., Holmbo, S., Muñoz, J. A., Mutel, R. L., Post, R. S., Prieto, J. L., Shields, J., Tallon, D., Thompson, T. A., Vallely, P. J., Villanueva, S., Jr., Smartt, S. J., Smith, K. W., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Sárneczky, K., Pál, A., Wheeler, J. C., Bódi, A., Bognár, Zs., Csák, B., Cseh, B., Csörnyei, G., Hanyecz, O., Ignácz, B., Kalup, Cs., Könyves-Tóth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sódor, A., Szabó, R., Szakáts, R., Zsidi, G., Milne, P., Andrews, J. E., Smith, N., Bilinski, C., Brown, P. J., Nordin, J., Williams, S. C., Galbany, L., Palmerio, J., Hook, I. M., Inserra, C., Maguire, K., Cartier, Régis, Razza, A., Gutiérrez, C. P., Hermes, J. J., Reding, J. S., Kaiser, B. C., Tonry, J. L., Heinze, A. N., Denneau, L., Weiland, H., Stalder, B., Barentsen, G., Dotson, J., Barclay, T., Gully-Santiago, M., Hedges, C., Cody, A. M., Howell, S., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinícius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., Elsaesser, B., Li, W., Wang, X., Vinkó, J., Mo, J., Hosseinzadeh, G., Sand, D. J., Zhang, J., Lin, H., Zhang, T., Wang, L., Chen, Z., Xiang, D., Rui, L., Huang, F., Li, X., Zhang, X., Li, L., Baron, E., Derkacy, J. M., Zhao, X., Sai, H., Zhang, K., Howell, D. A., McCully, C., Arcavi, I., Valenti, S., Hiramatsu, D., Burke, J., Rest, A., Garnavich, P., Tucker, B. E., Narayan, G., Shaya, E., Margheim, S., Zenteno, A., Villar, A., Dimitriadis, G., Foley, R. J., Pan, Y.-C., Coulter, D. A., Fox, O. D., Jha, S. W., Jones, D. O., Kasen, D. N., Kilpatrick, C. D., Piro, A. L., Riess, A. G., Rojas-Bravo, C., Shappee, B. J., Holoien, T. W.-S., Stanek, K. Z., Drout, M. R., Auchettl, K., Kochanek, C. S., Brown, J. S., Bose, S., Bersier, D., Brimacombe, J., Chen, P., Dong, S., Holmbo, S., Muñoz, J. A., Mutel, R. L., Post, R. S., Prieto, J. L., Shields, J., Tallon, D., Thompson, T. A., Vallely, P. J., Villanueva, S., Jr., Smartt, S. J., Smith, K. W., Chambers, K. C., Flewelling, H. A., Huber, M. E., Magnier, E. A., Waters, C. Z., Schultz, A. S. B., Bulger, J., Lowe, T. B., Willman, M., Sárneczky, K., Pál, A., Wheeler, J. C., Bódi, A., Bognár, Zs., Csák, B., Cseh, B., Csörnyei, G., Hanyecz, O., Ignácz, B., Kalup, Cs., Könyves-Tóth, R., Kriskovics, L., Ordasi, A., Rajmon, I., Sódor, A., Szabó, R., Szakáts, R., Zsidi, G., Milne, P., Andrews, J. E., Smith, N., Bilinski, C., Brown, P. J., Nordin, J., Williams, S. C., Galbany, L., Palmerio, J., Hook, I. M., Inserra, C., Maguire, K., Cartier, Régis, Razza, A., Gutiérrez, C. P., Hermes, J. J., Reding, J. S., Kaiser, B. C., Tonry, J. L., Heinze, A. N., Denneau, L., Weiland, H., Stalder, B., Barentsen, G., Dotson, J., Barclay, T., Gully-Santiago, M., Hedges, C., Cody, A. M., Howell, S., Coughlin, J., Van Cleve, J. E., Cardoso, J. Vinícius de Miranda, Larson, K. A., McCalmont-Everton, K. M., Peterson, C. A., Ross, S. E., Reedy, L. H., Osborne, D., McGinn, C., Kohnert, L., Migliorini, L., Wheaton, A., Spencer, B., Labonde, C., Castillo, G., Beerman, G., Steward, K., Hanley, M., Larsen, R., Gangopadhyay, R., Kloetzel, R., Weschler, T., Nystrom, V., Moffatt, J., Redick, M., Griest, K., Packard, M., Muszynski, M., Kampmeier, J., Bjella, R., Flynn, S., and Elsaesser, B.

Abstract

Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically-confirmed type Ia supernova (SN Ia) observed in the $Kepler$ field. The $Kepler$ data revealed an excess emission in its early light curve, allowing to place interesting constraints on its progenitor system (Dimitriadis et al. 2018, Shappee et al. 2018b). Here, we present extensive optical, ultraviolet, and near-infrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3$\pm$0.3 days and $\Delta$m$_{15}(B)=0.96\pm$0.03 mag, but it seems to have bluer $B - V$ colors. We construct the "uvoir" bolometric light curve having peak luminosity as 1.49$\times$10$^{43}$erg s$^{-1}$, from which we derive a nickel mass as 0.55$\pm$0.04M$_{\odot}$ by fitting radiation diffusion models powered by centrally located $^{56}$Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of $^{56}$Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a non-degenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia, but is characterized by prominent and persistent carbon absorption features. The C II features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in a SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers.

Published
2019

210. Rotation and pulsation in Ap stars: First light results from TESS sectors 1 and 2

Author

Danish National Research Foundation, Science and Technology Facilities Council (UK), European Space Agency, Universidad Nacional Autónoma de México, European Research Council, National Science Centre (Poland), Ministerio de Ciencia e Innovación (España), National Research, Development and Innovation Office (Hungary), Hungarian Academy of Sciences, Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), European Commission, Fundação para a Ciência e a Tecnologia (Portugal), National Aeronautics and Space Administration (US), Cunha, M.S., Antoci, V., Holdsworth, D.L., Kurtz, D.W., Balona, L.A., Bognár, Z., Bowman, D.M., Guo, Z., Kolaczek-Szymanski, P.A., Lares Martiz, M., Paunzen, E., Skarka, M., Smalley, B., Sódor, Kochukhov, O., Pepper, J., Richey-Yowell, T., Ricker, G.R., Seager, S., Buzasi, D.L., Fox-Machado, L., Hasanzadeh, A., Niemczura, E., Quitral-Manosalva, P., Monteiro, M.J.P.F.G., Stateva, I., De Cat, P., García Hernández, A., Ghasemi, H., Handler, G., Hey, D., Matthews, J.M., Nemec, J.M., Pascual Granado, J., Safari, H., Suárez Yanes, Juan Carlos, Szabó, R., Tkachenko, A., Weiss, W.W., Danish National Research Foundation, Science and Technology Facilities Council (UK), European Space Agency, Universidad Nacional Autónoma de México, European Research Council, National Science Centre (Poland), Ministerio de Ciencia e Innovación (España), National Research, Development and Innovation Office (Hungary), Hungarian Academy of Sciences, Ministerio de Ciencia, Innovación y Universidades (España), National Science Foundation (US), European Commission, Fundação para a Ciência e a Tecnologia (Portugal), National Aeronautics and Space Administration (US), Cunha, M.S., Antoci, V., Holdsworth, D.L., Kurtz, D.W., Balona, L.A., Bognár, Z., Bowman, D.M., Guo, Z., Kolaczek-Szymanski, P.A., Lares Martiz, M., Paunzen, E., Skarka, M., Smalley, B., Sódor, Kochukhov, O., Pepper, J., Richey-Yowell, T., Ricker, G.R., Seager, S., Buzasi, D.L., Fox-Machado, L., Hasanzadeh, A., Niemczura, E., Quitral-Manosalva, P., Monteiro, M.J.P.F.G., Stateva, I., De Cat, P., García Hernández, A., Ghasemi, H., Handler, G., Hey, D., Matthews, J.M., Nemec, J.M., Pascual Granado, J., Safari, H., Suárez Yanes, Juan Carlos, Szabó, R., Tkachenko, A., and Weiss, W.W.

Abstract

We present the first results from the Transiting Exoplanet Survey Satellite (TESS) on the rotational and pulsational variability of magnetic chemically peculiar A-type stars. We analyse TESS 2-min cadence data from sectors 1 and 2 on a sample of 83 stars. Five new rapidly oscillating Ap (roAp) stars are announced. One of these pulsates with periods around 4.7 min, making it the shortest period roAp star known to date. Four out of the five new roAp stars are multiperiodic. Three of these and the singly periodic one show the presence of rotational mode splitting. Individual frequencies are provided in all cases. In addition, seven previously known roAp stars are analysed. Additional modes of oscillation are found in some stars, while in others we are able to distinguish the true pulsations from possible aliases present in the ground-based data. We find that the pulsation amplitude in the TESS filter is typically a factor of 6 smaller than that in the B filter, which is usually used for ground-based observations. For four roAp stars we set constraints on the inclination angle and magnetic obliquity, through the application of the oblique pulsator model. We also confirm the absence of roAp-type pulsations down to amplitude limits of 6 and 13 \mumag, respectively, in two of the best characterized non-oscillating Ap (noAp) stars. We announce 27 new rotational variables along with their rotation periods, and provide different rotation periods for seven other stars. Finally, we discuss how these results challenge state-of-the-art pulsation models for roAp stars.© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.

Published
2019

215. The first view of δ Scuti and γ Doradus stars with the TESS mission

Author

Antoci, V, primary, Cunha, M S, additional, Bowman, D M, additional, Murphy, S J, additional, Kurtz, D W, additional, Bedding, T R, additional, Borre, C C, additional, Christophe, S, additional, Daszyńska-Daszkiewicz, J, additional, Fox-Machado, L, additional, García Hernández, A, additional, Ghasemi, H, additional, Handberg, R, additional, Hansen, H, additional, Hasanzadeh, A, additional, Houdek, G, additional, Johnston, C, additional, Justesen, A B, additional, Kahraman Alicavus, F, additional, Kotysz, K, additional, Latham, D, additional, Matthews, J M, additional, Mønster, J, additional, Niemczura, E, additional, Paunzen, E, additional, Sánchez Arias, J P, additional, Pigulski, A, additional, Pepper, J, additional, Richey-Yowell, T, additional, Safari, H, additional, Seager, S, additional, Smalley, B, additional, Shutt, T, additional, Sódor, A, additional, Suárez, J-C, additional, Tkachenko, A, additional, Wu, T, additional, Zwintz, K, additional, Barceló Forteza, S, additional, Brunsden, E, additional, Bognár, Z, additional, Buzasi, D L, additional, Chowdhury, S, additional, De Cat, P, additional, Evans, J A, additional, Guo, Z, additional, Guzik, J A, additional, Jevtic, N, additional, Lampens, P, additional, Lares Martiz, M, additional, Lovekin, C, additional, Li, G, additional, Mirouh, G M, additional, Mkrtichian, D, additional, Monteiro, M J P F G, additional, Nemec, J M, additional, Ouazzani, R-M, additional, Pascual-Granado, J, additional, Reese, D R, additional, Rieutord, M, additional, Rodon, J R, additional, Skarka, M, additional, Sowicka, P, additional, Stateva, I, additional, Szabó, R, additional, and Weiss, W W, additional

Published
2019
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216. Rotation and pulsation in Ap stars: first light results from TESS sectors 1 and 2

Author

Cunha, M S, primary, Antoci, V, additional, Holdsworth, D L, additional, Kurtz, D W, additional, Balona, L A, additional, Bognár, Zs, additional, Bowman, D M, additional, Guo, Z, additional, Kołaczek-Szymański, P A, additional, Lares-Martiz, M, additional, Paunzen, E, additional, Skarka, M, additional, Smalley, B, additional, Sódor, Á, additional, Kochukhov, O, additional, Pepper, J, additional, Richey-Yowell, T, additional, Ricker, G R, additional, Seager, S, additional, Buzasi, D L, additional, Fox-Machado, L, additional, Hasanzadeh, A, additional, Niemczura, E, additional, Quitral-Manosalva, P, additional, Monteiro, M J P F G, additional, Stateva, I, additional, De Cat, P, additional, García Hernández, A, additional, Ghasemi, H, additional, Handler, G, additional, Hey, D, additional, Matthews, J M, additional, Nemec, J M, additional, Pascual-Granado, J, additional, Safari, H, additional, Suárez, J C, additional, Szabó, R, additional, Tkachenko, A, additional, and Weiss, W W, additional

Published
2019
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219. Spectroscopic confirmation of the binary nature of the hybrid pulsator KIC 5709664 found with the frequency modulation method

Author

Derekas, A, primary, Murphy, S J, additional, Dálya, G, additional, Szabó, R, additional, Borkovits, T, additional, Bókon, A, additional, Lehmann, H, additional, Kinemuchi, K, additional, Southworth, J, additional, Bloemen, S, additional, Csák, B, additional, Isaacson, H, additional, Kovács, J, additional, Shporer, A, additional, Szabó, Gy M, additional, Thygesen, A O, additional, and Mészáros, Sz, additional

Published
2019
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225. Main-belt Asteroids in the K 2 Uranus Field

Author

Molnár, L., primary, Pál, A., additional, Sárneczky, K., additional, Szabó, R., additional, Vinkó, J., additional, Szabó, Gy. M., additional, Kiss, Cs., additional, Hanyecz, O., additional, Marton, G., additional, and Kiss, L. L., additional

Published
2018
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228. The PLATO 2.0 mission

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Valencia, Diana, Rauer, H., Catala, C., Aerts, C., Appourchaux, T., Benz, W., Brandeker, A., Christensen-Dalsgaard, J., Deleuil, M., Gizon, L., Goupil, M.-J., Güdel, M., Janot-Pacheco, E., Mas-Hesse, M., Pagano, I., Piotto, G., Pollacco, D., Santos, Ċ., Smith, A., Suárez, J.-C., Szabó, R., Udry, S., Adibekyan, V., Alibert, Y., Almenara, J.-M., Amaro-Seoane, P., Eiff, M. A, Asplund, M., Antonello, E., Barnes, S., Baudin, F., Belkacem, K., Bergemann, M., Bihain, G., Birch, A. C, Bonfils, X., Boisse, I., Bonomo, A. S, Borsa, F., Brandão, I. M, Brocato, E., Brun, S., Burleigh, M., Burston, R., Cabrera, J., Cassisi, S., Chaplin, W., Charpinet, S., Chiappini, C., Church, R. P, Csizmadia, Sz., Cunha, M., Damasso, M., Davies, M. B, Deeg, H. J, Díaz, R. F, Dreizler, S., Dreyer, C., Eggenberger, P., Ehrenreich, D., Eigmüller, P., Erikson, A., Farmer, R., Feltzing, S., Oliveira Fialho, F. d, Figueira, P., Forveille, T., Fridlund, M., García, R. A, Giommi, P., Giuffrida, G., Godolt, M., da Silva, J. G, Granzer, T., Grenfell, J. L, Grotsch-Noels, A., Günther, E., Haswell, C. A, Hatzes, A. P, Hébrard, G., Hekker, S., Helled, R., Heng, K., Jenkins, J. M, Johansen, A., Khodachenko, M. L, Kislyakova, K. G, Kley, W., Kolb, U., Krivova, N., Kupka, F., Lammer, H., Lanza, A. F, Lebreton, Y., Magrin, D., Marcos-Arenal, P., Marrese, P. M, Marques, J. P, Martins, J., Mathis, S., Mathur, S., Messina, S., Miglio, A., Montalban, J., Montalto, M., P. F. G. Monteiro, M. J, Moradi, H., Moravveji, E., Mordasini, C., Morel, T., Mortier, A., Nascimbeni, V., Nelson, R. P, Nielsen, M. B, Noack, L., Norton, A. J, Ofir, A., Oshagh, M., Ouazzani, R.-M., Pápics, P., Parro, V. C, Petit, P., Plez, B., Poretti, E., Quirrenbach, A., Ragazzoni, R., Raimondo, G., Rainer, M., Reese, D. R, Redmer, R., Reffert, S., Rojas-Ayala, B., Roxburgh, I. W, Salmon, S., Santerne, A., Schneider, J., Schou, J., Schuh, S., Schunker, H., Silva-Valio, A., Silvotti, R., Skillen, I., Snellen, I., Sohl, F., Sousa, S. G, Sozzetti, A., Stello, D., Strassmeier, K. G, Švanda, M., Szabó, Gy. M, Tkachenko, A., Van Grootel, V., Vauclair, S. D, Ventura, P., Wagner, F. W, Walton, N. A, Weingrill, J., Werner, S. C, Wheatley, P. J, Zwintz, K., Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Valencia, Diana, Rauer, H., Catala, C., Aerts, C., Appourchaux, T., Benz, W., Brandeker, A., Christensen-Dalsgaard, J., Deleuil, M., Gizon, L., Goupil, M.-J., Güdel, M., Janot-Pacheco, E., Mas-Hesse, M., Pagano, I., Piotto, G., Pollacco, D., Santos, Ċ., Smith, A., Suárez, J.-C., Szabó, R., Udry, S., Adibekyan, V., Alibert, Y., Almenara, J.-M., Amaro-Seoane, P., Eiff, M. A, Asplund, M., Antonello, E., Barnes, S., Baudin, F., Belkacem, K., Bergemann, M., Bihain, G., Birch, A. C, Bonfils, X., Boisse, I., Bonomo, A. S, Borsa, F., Brandão, I. M, Brocato, E., Brun, S., Burleigh, M., Burston, R., Cabrera, J., Cassisi, S., Chaplin, W., Charpinet, S., Chiappini, C., Church, R. P, Csizmadia, Sz., Cunha, M., Damasso, M., Davies, M. B, Deeg, H. J, Díaz, R. F, Dreizler, S., Dreyer, C., Eggenberger, P., Ehrenreich, D., Eigmüller, P., Erikson, A., Farmer, R., Feltzing, S., Oliveira Fialho, F. d, Figueira, P., Forveille, T., Fridlund, M., García, R. A, Giommi, P., Giuffrida, G., Godolt, M., da Silva, J. G, Granzer, T., Grenfell, J. L, Grotsch-Noels, A., Günther, E., Haswell, C. A, Hatzes, A. P, Hébrard, G., Hekker, S., Helled, R., Heng, K., Jenkins, J. M, Johansen, A., Khodachenko, M. L, Kislyakova, K. G, Kley, W., Kolb, U., Krivova, N., Kupka, F., Lammer, H., Lanza, A. F, Lebreton, Y., Magrin, D., Marcos-Arenal, P., Marrese, P. M, Marques, J. P, Martins, J., Mathis, S., Mathur, S., Messina, S., Miglio, A., Montalban, J., Montalto, M., P. F. G. Monteiro, M. J, Moradi, H., Moravveji, E., Mordasini, C., Morel, T., Mortier, A., Nascimbeni, V., Nelson, R. P, Nielsen, M. B, Noack, L., Norton, A. J, Ofir, A., Oshagh, M., Ouazzani, R.-M., Pápics, P., Parro, V. C, Petit, P., Plez, B., Poretti, E., Quirrenbach, A., Ragazzoni, R., Raimondo, G., Rainer, M., Reese, D. R, Redmer, R., Reffert, S., Rojas-Ayala, B., Roxburgh, I. W, Salmon, S., Santerne, A., Schneider, J., Schou, J., Schuh, S., Schunker, H., Silva-Valio, A., Silvotti, R., Skillen, I., Snellen, I., Sohl, F., Sousa, S. G, Sozzetti, A., Stello, D., Strassmeier, K. G, Švanda, M., Szabó, Gy. M, Tkachenko, A., Van Grootel, V., Vauclair, S. D, Ventura, P., Wagner, F. W, Walton, N. A, Weingrill, J., Werner, S. C, Wheatley, P. J, and Zwintz, K.

Abstract

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

Published
2017

229. Pulsational and evolutionary analysis of the double-mode RR Lyrae star BS Com

Author

Dékány, I., Kovács, G., Jurcsik, J., Szabó, R., Váradi, M., Sódor, Á., Posztobányi, K., Hurta, Zs, Vida, K., Vityi, N., Szing, A., Dékány, I., Kovács, G., Jurcsik, J., Szabó, R., Váradi, M., Sódor, Á., Posztobányi, K., Hurta, Zs, Vida, K., Vityi, N., and Szing, A.

Abstract

We derive the basic physical parameters of the field double-mode RR Lyrae star BS Com from its observed periods and the requirement of consistency between the pulsational and evolutionary constraints. By using the current solar-scaled horizontal branch evolutionary models of Pietrinferni et al. and our linear non-adiabatic purely radiative pulsational models, we get M/M⊙= 0.698 ± 0.004, log(L/L⊙) = 1.712 ± 0.005, Teff= 6840 ± 14 K, [Fe/H]=−1.67 ± 0.01, where the errors are standard deviations assuming uniform age distribution along the full range of uncertainty in age. The last two parameters are in a good agreement with the ones derived from the observed BVIC colours and the updated atlas9 stellar atmosphere models. We get Teff= 6842 ± 10 K, [Fe/H]=−1.58 ± 0.11, where the errors are purely statistical ones. It is remarkable that the derived parameters are nearly independent of stellar age at early evolutionary stages. Later stages, corresponding to the evolution towards the asymptotic giant branch, are most probably excluded because the required high temperatures are less likely to satisfy the constraints posed by the colours. We also show that our conclusions are only weakly sensitive to non-linear period shifts predicted by current hydrodynamical models

Published
2017

237. V473 Lyr, a modulated, period-doubled Cepheid, and U TrA, a double-mode Cepheid observed by MOST

Author

Molnár, L., primary, Derekas, A., additional, Szabó, R., additional, Matthews, J. M., additional, Cameron, C., additional, Moffat, A. F. J., additional, Richardson, N. D., additional, Csák, B., additional, Dózsa, Á., additional, Reed, P., additional, Szabados, L., additional, Heathcote, B., additional, Bohlsen, T., additional, Cacella, P., additional, Luckas, P., additional, Sódor, Á., additional, Skarka, M., additional, Szabó, Gy. M., additional, Plachy, E., additional, Kovács, J., additional, Evans, N. R., additional, Kolenberg, K., additional, Collins, K. A., additional, Pepper, J., additional, Stassun, K. G., additional, Rodriguez, J. E., additional, Siverd, R. J., additional, Henden, A., additional, Mankiewicz, L., additional, .Zarnecki, A. F., additional, Cwiek, A., additional, Sokolowski, M., additional, Pál, A., additional, Guenther, D. B., additional, Kuschnig, R., additional, Rowe, J., additional, Rucinski, S. M., additional, Sasselov, D., additional, and Weiss, W. W., additional

Published
2016
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240. SZÍNÉSZEK A VÁSZON SZÍNPADÁN.

Author

ÁDÁM, SZABÓ R.

Abstract

The article is about the various interpretations of theatre and stage actors on the silver screen. It shows the tendencies of Hollywood in this regard through examining three films, the Oscar-winning, but somehow still ignored Birdman (The Unexpected Virtue of Ignorance) (2015), the awarded and celebrated, but nowadays totally forgotten Shakespeare in Love (1998) and through the main-actorless, low budget, spoof horror cult movie Rubber (2010). Hollywood can sometimes display a surprising amount of maturity in dealing with life behind the scenes in the theatre, other times it can show no real empathy and knowing respect to a great classic author, while the American filmmakers of off-Hollywood can be just as meta and philosophical as European art films, while also deep cuttingly, ironically funny about the subject. [ABSTRACT FROM AUTHOR]

Published
2019

246. Lamost observations in the kepler field. I. Database of low-resolution spectra*

Author

Cat, P. De, Fu, J. N., Ren, A. B., Yang, X. H., Shi, J. R., Luo, A. L., Yang, M., Wang, J. L., Zhang, H. T., Shi, H. M., Zhang, W., Dong, Subo, Catanzaro, G., Corbally, C. J., Frasca, A., Gray, R. O., Żakowicz, J. Molenda, Uytterhoeven, K., Briquet, M., Bruntt, H., Frandsen, S., Kiss, L., Kurtz, Donald Wayne, Marconi, M., Niemczura, E., Østensen, R. H., Ripepi, V., Smalley, B., Southworth, J., Szabó, R., Telting, J. H., Karoff, C., Aguirre, V. Silva, Wu, Y., Hou, Y. H., Jin, G., Zhou, X. L., Cat, P. De, Fu, J. N., Ren, A. B., Yang, X. H., Shi, J. R., Luo, A. L., Yang, M., Wang, J. L., Zhang, H. T., Shi, H. M., Zhang, W., Dong, Subo, Catanzaro, G., Corbally, C. J., Frasca, A., Gray, R. O., Żakowicz, J. Molenda, Uytterhoeven, K., Briquet, M., Bruntt, H., Frandsen, S., Kiss, L., Kurtz, Donald Wayne, Marconi, M., Niemczura, E., Østensen, R. H., Ripepi, V., Smalley, B., Southworth, J., Szabó, R., Telting, J. H., Karoff, C., Aguirre, V. Silva, Wu, Y., Hou, Y. H., Jin, G., and Zhou, X. L.

Abstract

The nearly continuous light curves with micromagnitude precision provided by the space mission Kepler are revolutionizing our view of pulsating stars. They have revealed a vast sea of low-amplitude pulsation modes that were undetectable from Earth. The long time base of Kepler light curves allows for the accurate determination of the frequencies and amplitudes of pulsation modes needed for in-depth asteroseismic modeling. However, for an asteroseismic study to be successful, the first estimates of stellar parameters need to be known and they cannot be derived from the Kepler photometry itself. The Kepler Input Catalog provides values for the effective temperature, surface gravity, and metallicity, but not always with sufficient accuracy. Moreover, information on the chemical composition and rotation rate is lacking. We are collecting low-resolution spectra for objects in the Kepler field of view with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, Xinglong observatory, China). All of the requested fields have now been observed at least once. In this paper, we describe those observations and provide a useful database for the whole astronomical community

Published
2015

247. 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

248. Pushing the limits, episode 2: K2 observations of extragalactic RR Lyrae stars in the dwarf galaxy Leo IV

Author

Molnár, L., Pál, A., Plachy, E., Ripepi, V., Moretti, M. I., Szabó, R., Kiss, L. L., Molnár, L., Pál, A., Plachy, E., Ripepi, V., Moretti, M. I., Szabó, R., and Kiss, L. L.

Abstract

We present the first observations of extragalactic pulsating stars in the K2 ecliptic survey of the Kepler space telescope. Variability of all three RR Lyrae stars in the dwarf spheroidal galaxy Leo IV were successfully detected, at a brightness of Kp~21.5 mag, from data collected during Campaign 1. We identified one modulated star and another likely Blazhko candidate with periods of 29.8+-0.9 d and more than 80 d, respectively. EPIC 210282473 represents the first star beyond the Magellanic Clouds for which the Blazhko period and cycle-to-cycle variations in the modulation were unambiguously measured.The photometric [Fe/H] indices of the stars agree with earlier results that Leo IV is a very metal-poor galaxy. Two out of three stars blend with brighter background galaxies in the K2 frames. We demonstrate that image subtraction can be reliably used to extract photometry from faint confused sources that will be crucial not only for the K2 mission but for future space photometric missions as well., Comment: 8 pages, 6 figures, accepted for publication in the Astrophysical Journal. Light curves can be downloaded from http://konkoly.hu/KIK/data.html

Published
2015
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249. The Blazhko effect and additional excited modes in RR Lyrae stars

Author

Benkő, J. M., Szabó, R., Benkő, J. M., and Szabó, R.

Abstract

Recent photometric space missions, such as CoRoT and Kepler revealed that many RR Lyrae stars pulsate -- beyond their main radial pulsation mode -- in low amplitude modes. Space data seem to indicate a clear trend, namely overtone (RRc) stars and modulated fundamental (RRab) RR Lyrae stars ubiquitously show additional modes, while non-Blazhko RRab stars never do. Two Kepler stars (V350 Lyr and KIC 7021124), however, apparently seemed to break this rule: they were classified as non-Blazhko RRab stars showing additional modes. We processed Kepler pixel photometric data of these stars. We detected small amplitude, but significant Blazhko effect for both stars by using the resulted light curves and O$-$C diagrams. This finding strengthens the apparent connection between the Blazhko effect and the excitation of additional modes. In addition, it yields a potential tool for detecting Blazhko stars through the additional frequency patterns even if we have only short but accurate time series observations. V350 Lyr shows the smallest amplitude multiperiodic Blazhko effect ever detected., Comment: 6 pages, 4 figures and 2 tables. Accepted for publication in ApJ Letters

Published
2015
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250. An RR Lyrae family portrait: 33 stars observed in Pisces with K2-E2

Author

Molnár, L., Szabó, R., Moskalik, P. A., Nemec, J. M., Guggenberger, E., Smolec, R., Poleski, R., Plachy, E., Kolenberg, K., Kolláth, Z., Molnár, L., Szabó, R., Moskalik, P. A., Nemec, J. M., Guggenberger, E., Smolec, R., Poleski, R., Plachy, E., Kolenberg, K., and Kolláth, Z.

Abstract

A detailed analysis is presented of 33 RR Lyrae stars in Pisces observed with the Kepler space telescope over the 8.9-day long K2 Two-Wheel Concept Engineering Test. The sample includes not only fundamental-mode and first overtone (RRab and RRc) stars but the first two double-mode (RRd) stars that Kepler detected and the only modulated first-overtone star ever observed from space so far. The precision of the extracted K2 light curves made it possible to detect low-amplitude additional modes in all subtypes. All RRd and non-modulated RRc stars show the additional mode at P_X/P_1~0.61 that was detected in previous space-based photometric measurements. A periodicity longer than the fundamental mode was tentatively identified in one RRab star that might belong to a gravity mode. We determined the photometric [Fe/H] values for all fundamental-mode stars and provide the preliminary results of our efforts to fit the double-mode stars with non-linear hydrodynamic pulsation models. The results from this short test run indicate that the K2 mission will be, and has started to be, an ideal tool to expand our knowledge about RR Lyrae stars. As a by-product of the target search and analysis, we identified 165 bona-fide double-mode RR Lyrae stars from the Catalina Sky Survey observations throughout the sky, 130 of which are new discoveries., Comment: 15 pages, 14 figures, accepted for publication in MNRAS. Data files can be accessed at http://konkoly.hu/KIK/data.html

Published
2015
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