KOKORI, A., A. TSIARAS, B. EDWARDS, A. JONES, G. PANTELIDOU, G. TINETTI, L. BEWERSDORFF, A. ILIADOU, Y. JONGEN, G. LEKKAS, A. NASTASI, E. POULTOURTZIDIS, C. SIDIROPOULOS, F. WALTER, A. WUENSCHE, R. ABRAHAM, V. K. AGNIHOTRI, R. ALBANESI, E. ARCE-MANSEGO, D. ARNOT, M. AUDEJEAN, C. AUMASSON, M. BACHSCHMIDT, G. BAJ, P. R. BARROY, A. A. BELINSKI, D. BENNETT, P. BENNI, K. BERNACKI, L. BETTI, A. BIAGINI, P. BOSCH, P. BRANDEBOURG, L. BRAT, M. BRETTON, S M BRINCAT, S. BROUILLARD, A. BRUZAS, A. BRUZZONE, R. A. BUCKLAND, M. CALO, F. CAMPOS, A. CARRENO, J. A. CARRION RODRIGO, R. CASALI, G. CASALNUOVO, M. CATANEO, C. -M. CHANG, L. CHANGEAT, V. CHOWDHURY, R. CIANTINI, M. CILLUFFO, J. -F. COLIAC, G. CONZO, M. CORREA, G. COULON, N. CROUZET, M. V. CROW, I. A. CURTIS, D. DANIEL, B. DAUCHET, S. DAWES, M. DELDEM, D. DELIGEORGOPOULOS, G. DRANSFIELD, R. DYMOCK, T. EENMAEE, N. ESSEIVA, P. EVANS, C. FALCO, R. G. FARFAN, E. FERNANDEZ-LAJUS, S. FERRATFIAT, S. L. FERREIRA, A. FERRETTI, J. FIOLKA, M. FOWLER, S. R. FUTCHER, D. GABELLINI, T. GAINEY, J. GAITAN, P. GAJDOS, A. GARCIA-SANCHEZ, J. GARLITZ, C. GILLIER, C. GISON, J. GONZALES, D. GORSHANOV, F. GRAU HORTA, G. GRIVAS, P. GUERRA, T. GUILLOT, C. A. HASWELL, T. HAYMES, V. -P. HENTUNEN, K. HILLS, K. HOSE, T. HUMBERT, F. HURTER, T. HYNEK, M. IRZYK, J. JACOBSEN, A. L. JANNETTA, K. JOHNSON, P. JOZWIK-WABIK, A. E. KAEOUACH, W. KANG, H. KIISKINEN, T. KIM, Ue. KIVILA, B. KOCH, U. KOLB, Hana KUČÁKOVÁ, S. -P. LAI, D. LALOUM, S. LASOTA, L. A. LEWIS, G. -I. LIAKOS, F. LIBOTTE, F. LOMOZ, C. LOPRESTI, R. MAJEWSKI, A. MALCHER, M. MALLONN, M. MANNUCCI, A. MARCHINI, J. -M. MARI, A. MARINO, G. MARINO, J. -C. MARIO, J. -B. MARQUETTE, F. A. MARTINEZ-BRAVO, M. MASEK, P. MATASSA, P. MICHEL, J. MICHELET, M. MILLER, E. MINY, D. MOLINA, T. MOLLIER, B. MONTELEONE, N. MONTIGIANI, M. MORALES-AIMAR, F. MORTARI, M. MORVAN, L. V. MUGNAI, G. MURAWSKI, L. NAPONIELLO, J. -L. NAUDIN, R. NAVES, D. NEEL, R. NEITO, S. NEVEU, A. NOSCHESE, Y. OEGMEN, O. OHSHIMA, Z. ORBANIC, E. P. PACE, C. PANTACCHINI, N. I. PASCHALIS, C. PEREIRA, I. PERETTO, V. PERROUD, M. PHILLIPS, P. PINTR, J. -B. PIOPPA, J. PLAZAS, A. J. POELARENDS, A. POPOWICZ, J. PURCELL, N. QUINN, M. RAETZ, D. REES, F. REGEMBAL, M. ROCCHETTO, P. -F. ROCCI, M. ROCKENBAUER, R. ROTH, L. ROUSSELOT, X. RUBIA, N. RUOCCO, E. RUSSO, M. SALISBURY, F. SALVAGGIO, A. SANTOS, J. SAVAGE, F. SCAGGIANTE, D. SEDITA, S. SHADICK, A. F. SILVA, N. SIOULAS, V. SKOLNIK, M. SMITH, M. SMOLKA, A. SOLMAZ, N. STANBURY, D. STOURAITIS, T. -G. TAN, M. THEUSNER, G. THURSTON, F. P. TIFNER, A. TOMACELLI, A. TOMATIS, J. TRNKA, M. TYLSAR, P. VALEAU, J. -P. VIGNES, A. VILLA, A. Vives SUREDA, K. VORA, M. VRASTAK, D. WALLIANG, B. WENZEL, D. E. WRIGHT, R. ZAMBELLI, M. ZHANG and M. ZIBAR. ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations. Astrophysical Journal Supplement Series. GB - Spojené království Velké Británie a, 2023, vol. 265, No 1, p. "4-1"-"4-20", 20 pp. ISSN 0067-0049. Available from: https://dx.doi.org/10.3847/1538-4365/ac9da4.
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Basic information
Original name ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations
Authors KOKORI, A., A. TSIARAS, B. EDWARDS, A. JONES, G. PANTELIDOU, G. TINETTI, L. BEWERSDORFF, A. ILIADOU, Y. JONGEN, G. LEKKAS, A. NASTASI, E. POULTOURTZIDIS, C. SIDIROPOULOS, F. WALTER, A. WUENSCHE, R. ABRAHAM, V. K. AGNIHOTRI, R. ALBANESI, E. ARCE-MANSEGO, D. ARNOT, M. AUDEJEAN, C. AUMASSON, M. BACHSCHMIDT, G. BAJ, P. R. BARROY, A. A. BELINSKI, D. BENNETT, P. BENNI, K. BERNACKI, L. BETTI, A. BIAGINI, P. BOSCH, P. BRANDEBOURG, L. BRAT, M. BRETTON, S M BRINCAT, S. BROUILLARD, A. BRUZAS, A. BRUZZONE, R. A. BUCKLAND, M. CALO, F. CAMPOS, A. CARRENO, J. A. CARRION RODRIGO, R. CASALI, G. CASALNUOVO, M. CATANEO, C. -M. CHANG, L. CHANGEAT, V. CHOWDHURY, R. CIANTINI, M. CILLUFFO, J. -F. COLIAC, G. CONZO, M. CORREA, G. COULON, N. CROUZET, M. V. CROW, I. A. CURTIS, D. DANIEL, B. DAUCHET, S. DAWES, M. DELDEM, D. DELIGEORGOPOULOS, G. DRANSFIELD, R. DYMOCK, T. EENMAEE, N. ESSEIVA, P. EVANS, C. FALCO, R. G. FARFAN, E. FERNANDEZ-LAJUS, S. FERRATFIAT, S. L. FERREIRA, A. FERRETTI, J. FIOLKA, M. FOWLER, S. R. FUTCHER, D. GABELLINI, T. GAINEY, J. GAITAN, P. GAJDOS, A. GARCIA-SANCHEZ, J. GARLITZ, C. GILLIER, C. GISON, J. GONZALES, D. GORSHANOV, F. GRAU HORTA, G. GRIVAS, P. GUERRA, T. GUILLOT, C. A. HASWELL, T. HAYMES, V. -P. HENTUNEN, K. HILLS, K. HOSE, T. HUMBERT, F. HURTER, T. HYNEK, M. IRZYK, J. JACOBSEN, A. L. JANNETTA, K. JOHNSON, P. JOZWIK-WABIK, A. E. KAEOUACH, W. KANG, H. KIISKINEN, T. KIM, Ue. KIVILA, B. KOCH, U. KOLB, Hana KUČÁKOVÁ (203 Czech Republic, belonging to the institution), S. -P. LAI, D. LALOUM, S. LASOTA, L. A. LEWIS, G. -I. LIAKOS, F. LIBOTTE, F. LOMOZ, C. LOPRESTI, R. MAJEWSKI, A. MALCHER, M. MALLONN, M. MANNUCCI, A. MARCHINI, J. -M. MARI, A. MARINO, G. MARINO, J. -C. MARIO, J. -B. MARQUETTE, F. A. MARTINEZ-BRAVO, M. MASEK, P. MATASSA, P. MICHEL, J. MICHELET, M. MILLER, E. MINY, D. MOLINA, T. MOLLIER, B. MONTELEONE, N. MONTIGIANI, M. MORALES-AIMAR, F. MORTARI, M. MORVAN, L. V. MUGNAI, G. MURAWSKI, L. NAPONIELLO, J. -L. NAUDIN, R. NAVES, D. NEEL, R. NEITO, S. NEVEU, A. NOSCHESE, Y. OEGMEN, O. OHSHIMA, Z. ORBANIC, E. P. PACE, C. PANTACCHINI, N. I. PASCHALIS, C. PEREIRA, I. PERETTO, V. PERROUD, M. PHILLIPS, P. PINTR, J. -B. PIOPPA, J. PLAZAS, A. J. POELARENDS, A. POPOWICZ, J. PURCELL, N. QUINN, M. RAETZ, D. REES, F. REGEMBAL, M. ROCCHETTO, P. -F. ROCCI, M. ROCKENBAUER, R. ROTH, L. ROUSSELOT, X. RUBIA, N. RUOCCO, E. RUSSO, M. SALISBURY, F. SALVAGGIO, A. SANTOS, J. SAVAGE, F. SCAGGIANTE, D. SEDITA, S. SHADICK, A. F. SILVA, N. SIOULAS, V. SKOLNIK, M. SMITH, M. SMOLKA, A. SOLMAZ, N. STANBURY, D. STOURAITIS, T. -G. TAN, M. THEUSNER, G. THURSTON, F. P. TIFNER, A. TOMACELLI, A. TOMATIS, J. TRNKA, M. TYLSAR, P. VALEAU, J. -P. VIGNES, A. VILLA, A. Vives SUREDA, K. VORA, M. VRASTAK, D. WALLIANG, B. WENZEL, D. E. WRIGHT, R. ZAMBELLI, M. ZHANG and M. ZIBAR.
Edition Astrophysical Journal Supplement Series, GB - Spojené království Velké Británie a, 2023, 0067-0049.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United Kingdom of Great Britain and Northern Ireland
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19630/23:A0000326
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.3847/1538-4365/ac9da4
UT WoS 000981818400001
Keywords in English transiting hot Jupiter;optical-transmission spectrum; high-precision phometry; Saturn-mass planet;light-curve project;low-density planet;refined physical-properties;spin-orbit alignment; short-period planet; earth-sized planet
Tags RIV24, UF
Tags International impact, Reviewed
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 23/2/2024 10:50.
Abstract
The ExoClock project has been created to increase the efficiency of the Ariel mission. It will achieve this by continuously monitoring and updating the ephemerides of Ariel candidates, in order to produce a consistent catalog of reliable and precise ephemerides. This work presents a homogenous catalog of updated ephemerides for 450 planets, generated by the integration of similar to 18,000 data points from multiple sources. These sources include observations from ground-based telescopes (the ExoClock network and the Exoplanet Transit Database), midtime values from the literature, and light curves from space telescopes (Kepler, K2, and TESS). With all the above, we manage to collect observations for half of the postdiscovery years (median), with data that have a median uncertainty less than 1 minute. In comparison with the literature, the ephemerides generated by the project are more precise and less biased. More than 40% of the initial literature ephemerides had to be updated to reach the goals of the project, as they were either of low precision or drifting. Moreover, the integrated approach of the project enables both the monitoring of the majority of the Ariel candidates (95%), and also the identification of missing data. These results highlight the need for continuous monitoring to increase the observing coverage of the candidate planets. Finally, the extended observing coverage of planets allows us to detect trends (transit-timing variations) for a sample of 19 planets. All the products, data, and codes used in this work are open and accessible to the wider scientific community.
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