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12 results on '"Zanmar Sánchez, R."'

1. The ASTRI Mini-Array of Cherenkov telescopes at the Observatorio del Teide

Author

Scuderi, S., Giuliani, A., Pareschi, G., Tosti, G., Catalano, O., Amato, E., Antonelli, L.A., Becerra Gonzàles, J., Bellassai, G., Bigongiari, C., Biondo, B., Böttcher, M., Bonanno, G., Bonnoli, G., Bruno, P., Bulgarelli, A., Canestrari, R., Capalbi, M., Caraveo, P., Cardillo, M., Conforti, V., Contino, G., Corpora, M., Costa, A., Cusumano, G., D'Aì, A., de Gouveia Dal Pino, E., Della Ceca, R., Escribano Rodriguez, E., Falceta-Gonçalves, D., Fermino, C., Fiori, M., Fioretti, V., Fiorini, M., Gallozzi, S., Gargano, C., Garozzo, S., Germani, S., Ghedina, A., Gianotti, F., Giarrusso, S., Gimenes, R., Giordano, V., Grillo, A., Grivel Gelly, C., Impiombato, D., Incardona, F., Incorvaia, S., Iovenitti, S., La Barbera, A., La Palombara, N., La Parola, V., Lamastra, A., Lessio, L., Leto, G., Lo Gerfo, F., Lodi, M., Lombardi, S., Longo, F., Lucarelli, F., Maccarone, M.C., Marano, D., Martinetti, E., Mereghetti, S., Micciché, A., Millul, R., Mineo, T., Mollica, D., Morlino, G., Morselli, A., Naletto, G., Nicotra, G., Pagliaro, A., Parmiggiani, N., Piano, G., Pintore, F., Poretti, E., Olmi, B., Rodeghiero, G., Rodriguez Fernandez, G., Romano, P., Romeo, G., Russo, F., Sangiorgi, P., Saturni, F.G., Schwarz, J.H., Sciacca, E., Sironi, G., Sottile, G., Stamerra, A., Tagliaferri, G., Testa, V., Umana, G., Uslenghi, M., Vercellone, S., Zampieri, L., and Zanmar Sanchez, R.

Published
2022
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2. HADES RV Programme with HARPS-N at TNG

Author

Pinamonti, M., primary, Sozzetti, A., additional, Maldonado, J., additional, Affer, L., additional, Micela, G., additional, Bonomo, A. S., additional, Lanza, A. F., additional, Perger, M., additional, Ribas, I., additional, González Hernández, J. I., additional, Bignamini, A., additional, Claudi, R., additional, Covino, E., additional, Damasso, M., additional, Desidera, S., additional, Giacobbe, P., additional, González-Álvarez, E., additional, Herrero, E., additional, Leto, G., additional, Maggio, A., additional, Molinari, E., additional, Morales, J. C., additional, Pagano, I., additional, Petralia, A., additional, Piotto, G., additional, Poretti, E., additional, Rebolo, R., additional, Scandariato, G., additional, Suárez Mascareño, A., additional, Toledo-Padrón, B., additional, and Zanmar Sánchez, R., additional

Published
2022
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3. Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations

Author

Física aplicada I, Fisika aplikatua I, Marques Oliveira, Joana, Sicardy, Bruno, Gómes Junior, A.R., Ortiz, J.L., Strobel, D.F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos Sanz, Pablo, Morales, N., Duffard, Rene, Fernández Valenzuela, Estela, Castro Tirado, A.J., Braga Ribas, Felipe, Morgado, Bruno, Assafin, Marcelo, Bueno de Camargo, Julio Ignacio, Vieira Martins, Roberto, Benedetti Rossi, Gustavo, Santos Filho, S., Banda Huarca, M.V., Quispe Huaynasi, F., Pereira, Chrystian Luciano, Rommel, Flavia Luane, Margoti, Giuliano, Dias Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, Ricardo, Pérez Hoyos, Santiago, Sánchez Lavega, Agustín María, Rojas Palenzuela, José Félix, Beisker, W., Kretlow, Mike, Herald, D., Gault, D., Bath, K.-L., Bode, H.-J., Bredner, E., Guhl, K., Haymes, T.V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, Chrysa, Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A.A., Xilouris, Emmanuel, Alikakos, I., Gourzelas, A., Liakos, Alexios, Charmandaris, Vassilis, Jelínek, Martin, Štrobl, Jan, Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, Dirk, Brandis, L., Pütz, I., Perdelwitz, Volker, Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J.-M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, Giuseppe, Zanmar Sánchez, R., Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, Cesare, Lo Savio, R., Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., G. Gallego, Sofía, Tortorelli, Luca, Sposetti, S., Sussenbach, J., Van Den Abbeel, F., André, P., Llibre, M., Pailler, Frédéric, Ardissone, J., Boutet, Michel, Sánchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J.L., Dechambre, O., Delay, P., Delcroix, Marc, Rousselot, Lionel, Ferreira, João, Machado, Pedro, Tanga, P., Rivet, J.-P., Frappa, Eric, Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A.N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, Jean-François, Metz, F., Erpelding, D., Nougayrede, Jean-Philippe, Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Baba Aissa, D., Grigahcene, Z., Briggs, D., Broadbent, Stephen, Denyer, P., Haigh, Nicholas, Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., talbot, J., Alonso Burgos, Sergio, Román Reche, A., Casanova, V., Briggs, E., Iglesias Marzoa, Ramón, Abril Ibáñez, J., Díaz Martín, M.C., González, H., Maestre García, J.L., Marchant, Jonathan, Ordoñez Etxeberria, Iñaki, Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perelló Pérez, Carlos, Cabedo, V., Gonçalves, Rui M. D., Ferreira, M., Marques Dias, Filipe, Daassou, A., Barkaoui, Khalid, Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., El Moutamid, Maryame, Lamarche, C., Pollock, J.T., caton, D.B., Kouprianov, Vladimir, Timerson, B.W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J.-P., Françoise, J., Mondon, Bernard, Payet, Thierry, Boissel, C., Castets, M., Hubbard, William, Hill, R., Reitsema, H. J., Mousis, Olivier, Ball, L., Neilsen, G., Hutcheon, S., lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., Downs, B., Física aplicada I, Fisika aplikatua I, Marques Oliveira, Joana, Sicardy, Bruno, Gómes Junior, A.R., Ortiz, J.L., Strobel, D.F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos Sanz, Pablo, Morales, N., Duffard, Rene, Fernández Valenzuela, Estela, Castro Tirado, A.J., Braga Ribas, Felipe, Morgado, Bruno, Assafin, Marcelo, Bueno de Camargo, Julio Ignacio, Vieira Martins, Roberto, Benedetti Rossi, Gustavo, Santos Filho, S., Banda Huarca, M.V., Quispe Huaynasi, F., Pereira, Chrystian Luciano, Rommel, Flavia Luane, Margoti, Giuliano, Dias Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, Ricardo, Pérez Hoyos, Santiago, Sánchez Lavega, Agustín María, Rojas Palenzuela, José Félix, Beisker, W., Kretlow, Mike, Herald, D., Gault, D., Bath, K.-L., Bode, H.-J., Bredner, E., Guhl, K., Haymes, T.V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, Chrysa, Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A.A., Xilouris, Emmanuel, Alikakos, I., Gourzelas, A., Liakos, Alexios, Charmandaris, Vassilis, Jelínek, Martin, Štrobl, Jan, Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, Dirk, Brandis, L., Pütz, I., Perdelwitz, Volker, Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J.-M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, Giuseppe, Zanmar Sánchez, R., Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, Cesare, Lo Savio, R., Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., G. Gallego, Sofía, Tortorelli, Luca, Sposetti, S., Sussenbach, J., Van Den Abbeel, F., André, P., Llibre, M., Pailler, Frédéric, Ardissone, J., Boutet, Michel, Sánchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J.L., Dechambre, O., Delay, P., Delcroix, Marc, Rousselot, Lionel, Ferreira, João, Machado, Pedro, Tanga, P., Rivet, J.-P., Frappa, Eric, Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A.N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, Jean-François, Metz, F., Erpelding, D., Nougayrede, Jean-Philippe, Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Baba Aissa, D., Grigahcene, Z., Briggs, D., Broadbent, Stephen, Denyer, P., Haigh, Nicholas, Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., talbot, J., Alonso Burgos, Sergio, Román Reche, A., Casanova, V., Briggs, E., Iglesias Marzoa, Ramón, Abril Ibáñez, J., Díaz Martín, M.C., González, H., Maestre García, J.L., Marchant, Jonathan, Ordoñez Etxeberria, Iñaki, Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perelló Pérez, Carlos, Cabedo, V., Gonçalves, Rui M. D., Ferreira, M., Marques Dias, Filipe, Daassou, A., Barkaoui, Khalid, Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., El Moutamid, Maryame, Lamarche, C., Pollock, J.T., caton, D.B., Kouprianov, Vladimir, Timerson, B.W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J.-P., Françoise, J., Mondon, Bernard, Payet, Thierry, Boissel, C., Castets, M., Hubbard, William, Hill, R., Reitsema, H. J., Mousis, Olivier, Ball, L., Neilsen, G., Hutcheon, S., lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., and Downs, B.

Abstract

Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range similar to 8 km to similar to 190 km, corresponding to pressure levels from 9 mu bar down to a few nanobars. Results. (i) A pressure of 1.18 +/- 0.03 mu bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 mu bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude.

Published
2022

4. A super-Earth on a close-in orbit around the M1V star GJ 740 A HADES and CARMENES collaboration

Author

Toledo Padrón, B., Suárez Mascareño, A., González Hernández, J. I., Rebolo, R., Pinamonti, M., Perger, M., Scandariato, G., Damasso, M., Sozzetti, A., Moldonado, J., Desidera, S., Ribas, I., Micela, G., Affer, L., González Álvarez, E., Leto, G., Pagano, I., Zanmar Sánchez, R., Giacobbe, P., Herrero, E., Morales, J. C., Amado, P. J., Caballero, J. A., Quirrenbach, A., Reiners, A., Zechmeister, M., Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), and Generalitat de Catalunya

Subjects
individual: GJ 740 [Stars], detection [Planets and satellites], radial velocities [Techniques], photometric [Techniques], spectrographs [Instrumentation], activity [Stars]
Abstract

RV data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/648/A20 Based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the INAF - Fundación Galileo Galilei at the Roche de Los Muchachos Observatory of the Instituto de Astrofísica de Canarias (IAC); and the CARMENES instrument installed at the 3.5m telescope of the Calar Alto Observatory, Spain. Context. M-dwarfs have proven to be ideal targets for planetary radial velocity (RV) searches due to their higher planet-star mass contrast, which favors the detection of low-mass planets. The abundance of super-Earth and Earth-like planets detected around this type of star motivates further such research on hosts without reported planetary companions. Aims. The HADES and CARMENES programs are aimed at carrying out extensive searches of exoplanetary systems around M-type stars in the northern hemisphere, allowing us to address, in a statistical sense, the properties of the planets orbiting these objects. In this work, we perform a spectroscopic and photometric study of one of the program stars (GJ 740), which exhibits a short-period RV signal that is compatible with a planetary companion. Methods. We carried out a spectroscopic analysis based on 129 HARPS-N spectra taken over a time span of 6 yr combined with 57 HARPS spectra taken over 4 yr, as well as 32 CARMENES spectra taken during more than 1 yr, resulting in a dataset with a time coverage of 10 yr. We also relied on 459 measurements from the public ASAS survey with a time-coverage of 8 yr, along with 5 yr of photometric magnitudes from the EXORAP project taken in the V, B, R, and I filters to carry out a photometric study. Both analyses were made using Markov chain Monte Carlo simulations and Gaussian process regression to model the activity of the star. Results. We present the discovery of a short-period super-Earth with an orbital period of 2.37756−0.00011+0.00013 d and a minimum mass of 2.96−0.48+0.50 M⊕. We offer an update to the previously reported characterization of the magnetic cycle and rotation period of the star, obtaining values of Prot = 35.563 ± 0.071 d and Pcycle = 2800 ± 150 d. Furthermore, the RV time series exhibits a possibly periodic long-term signal, which might be related to a Saturn-mass planet of ~100 M⊕. B.T.P. acknowledges Fundación La Caixa for the financial support received in the form of a Ph.D. contract. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the 2019 Juan de la Cierva Programme. J.I.G.H. acknowledges financial support from Spanish MICINN under the 2013 Ramón y Cajal program RYC-2013-14875. B.T.P., A.S.M., J.I.G.H. and R.R. acknowledge financial support from the Spanish MICINN AYA2017-86389-P. I.R. and M.Pe. acknowledge support from the Spanish MICINN and the Fondo Europeo de Desarrollo Regional (FEDER) through grant PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya/CERCA program. G.A.P.S. acknowledges support from INAF through the Progetti Premiali funding scheme of the Italian Ministry of Education, University, and Research. G.A.P.S. acknowledges financial support from Progetto Premiale 2015 FRONTIERA (OB.FU. 1.05.06.11) funding scheme of the Italian Ministry of Education, University, and Research. G.S. acknowledges the funding support from Italian Space Agency (ASI) regulated by “Accordo ASI-INAF n. 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015”. This research has received financial support from the agreement ASI-INAF n.2018-16-HH.0. The results of this paper were based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the INAF-Fundación Galileo Galilei at the Roque de Los Muchachos Observatory of the Instituto de Astrofísica de Canarias (IAC); observations made with the HARPS instrument on the ESO 3.6-m telescope at La Silla Observatory (Chile); and observations made with the CARMENES instrument. CARMENES is an instrument for the Centro Astronómico Hispano-Alemán de Calar Alto (CAHA, Almería, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Científicas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Andalucía, Landessternwarte Königstuhl, Institut de Ciències de l’Espai, Insitut für Astrophysik Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg, Instituto de Astrofísica de Canarias, Hamburger Sternwarte, Centro de Astrobiología and Centro Astronómico Hispano-Alemán), with additional contributions by the Spanish MICINN through projects RYC2013-14875, AYA2015-69350-C3-2-P, AYA2016-79425-C3-1/2/3-P, ESP2016-80435-C2-1-R, ESP2017-87143-R, ESP2017-87676-C05-1/2/5-R, and AYA2017-86389-P, the German Science Foundation through the Major Research Instrumentation Program and DFG Research Unit FOR2544 “Blue Planets around Red Stars”, the Klaus Tschira Stiftung, the states of Baden-Württemberg and Niedersachsen, and by the Junta de Andalucía. This paper made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/), partly financed by the MICINN with FEDER funds, code IACA13-3E-2493. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper makes use of data from the first public release of the WASP data (Butters et al. 2010)as provided by the WASP consortium and services at the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has made 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, https://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. Peerreview

Published
2021

5. HADES RV programme with HARPS-N at TNG

Author

Maldonado, J., primary, Petralia, A., additional, Damasso, M., additional, Pinamonti, M., additional, Scandariato, G., additional, González-Álvarez, E., additional, Affer, L., additional, Micela, G., additional, Lanza, A. F., additional, Leto, G., additional, Poretti, E., additional, Sozzetti, A., additional, Perger, M., additional, Giacobbe, P., additional, Zanmar Sánchez, R., additional, Maggio, A., additional, González Hernández, J. I., additional, Rebolo, R., additional, Ribas, I., additional, Suárez-Mascareño, A., additional, Toledo-Padrón, B., additional, Bignamini, A., additional, Molinari, E., additional, Covino, E., additional, Claudi, R., additional, Desidera, S., additional, Herrero, E., additional, Morales, J. C., additional, Pagano, I., additional, and Piotto, G., additional

Published
2021
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6. A super-Earth on a close-in orbit around the M1V star GJ 740: A HADES and CARMENES collaboration

Author

Ministerio de Ciencia e Innovación (España), European Commission, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), German Research Foundation, Ministero dell'Istruzione, dell'Università e della Ricerca, Toledo-Padrón, B., Suárez Mascareño, A., González Hernández, Jonay I., Rebolo López, Rafael, Pinamonti, M., Perger, M., Scandariato, G., Damasso, M., Sozzetti, Alessandro, Maldonado, J., Desidera, S., Ribas, Ignasi, Micela, Giusi, Affer, L., González-Álvarez, E., Leto, G., Pagano, Isabella, Zanmar Sánchez, R., Giacobbe, P., Herrero, E., Morales, Juan Carlos, Amado, Pedro J., Caballero, J. A., Quirrenbach, Andreas, Reiners, Ansgar, Zechmeister, Mathias, Ministerio de Ciencia e Innovación (España), European Commission, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), German Research Foundation, Ministero dell'Istruzione, dell'Università e della Ricerca, Toledo-Padrón, B., Suárez Mascareño, A., González Hernández, Jonay I., Rebolo López, Rafael, Pinamonti, M., Perger, M., Scandariato, G., Damasso, M., Sozzetti, Alessandro, Maldonado, J., Desidera, S., Ribas, Ignasi, Micela, Giusi, Affer, L., González-Álvarez, E., Leto, G., Pagano, Isabella, Zanmar Sánchez, R., Giacobbe, P., Herrero, E., Morales, Juan Carlos, Amado, Pedro J., Caballero, J. A., Quirrenbach, Andreas, Reiners, Ansgar, and Zechmeister, Mathias

Abstract

Context. M-dwarfs have proven to be ideal targets for planetary radial velocity (RV) searches due to their higher planet-star mass contrast, which favors the detection of low-mass planets. The abundance of super-Earth and Earth-like planets detected around this type of star motivates further such research on hosts without reported planetary companions. Aims. The HADES and CARMENES programs are aimed at carrying out extensive searches of exoplanetary systems around M-type stars in the northern hemisphere, allowing us to address, in a statistical sense, the properties of the planets orbiting these objects. In this work, we perform a spectroscopic and photometric study of one of the program stars (GJ 740), which exhibits a short-period RV signal that is compatible with a planetary companion. Methods. We carried out a spectroscopic analysis based on 129 HARPS-N spectra taken over a time span of 6 yr combined with 57 HARPS spectra taken over 4 yr, as well as 32 CARMENES spectra taken during more than 1 yr, resulting in a dataset with a time coverage of 10 yr. We also relied on 459 measurements from the public ASAS survey with a time-coverage of 8 yr, along with 5 yr of photometric magnitudes from the EXORAP project taken in the V, B, R, and I filters to carry out a photometric study. Both analyses were made using Markov chain Monte Carlo simulations and Gaussian process regression to model the activity of the star. Results. We present the discovery of a short-period super-Earth with an orbital period of 2.37756-0.00011+0.00013 d and a minimum mass of 2.96-0.48+0.50 M . We offer an update to the previously reported characterization of the magnetic cycle and rotation period of the star, obtaining values of Prot = 35.563 ± 0.071 d and Pcycle = 2800 ± 150 d. Furthermore, the RV time series exhibits a possibly periodic long-term signal, which might be related to a Saturn-mass planet of ~100 M . © ESO 2021.

Published
2021

7. HADES RV Programme with HARPS-N at TNG

Author

González-Álvarez, E., primary, Petralia, A., additional, Micela, G., additional, Maldonado, J., additional, Affer, L., additional, Maggio, A., additional, Covino, E., additional, Damasso, M., additional, Lanza, A. F., additional, Perger, M., additional, Pinamonti, M., additional, Poretti, E., additional, Scandariato, G., additional, Sozzetti, A., additional, Bignamini, A., additional, Giacobbe, P., additional, Leto, G., additional, Pagano, I., additional, Zanmar Sánchez, R., additional, González Hernández, J. I., additional, Rebolo, R., additional, Ribas, I., additional, Suárez Mascareño, A., additional, and Toledo-Padrón, B., additional

Published
2021
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8. A super-Earth on a close-in orbit around the M1V star GJ 740

Author

Toledo-Padrón, B., primary, Suárez Mascareño, A., additional, González Hernández, J. I., additional, Rebolo, R., additional, Pinamonti, M., additional, Perger, M., additional, Scandariato, G., additional, Damasso, M., additional, Sozzetti, A., additional, Maldonado, J., additional, Desidera, S., additional, Ribas, I., additional, Micela, G., additional, Affer, L., additional, González-Alvarez, E., additional, Leto, G., additional, Pagano, I., additional, Zanmar Sánchez, R., additional, Giacobbe, P., additional, Herrero, E., additional, Morales, J. C., additional, Amado, P. J., additional, Caballero, J. A., additional, Quirrenbach, A., additional, Reiners, A., additional, and Zechmeister, M., additional

Published
2021
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9. Gliese 49: activity evolution and detection of a super-Earth

Author

Perger, M., primary, Scandariato, G., additional, Ribas, I., additional, Morales, J. C., additional, Affer, L., additional, Azzaro, M., additional, Amado, P. J., additional, Anglada-Escudé, G., additional, Baroch, D., additional, Barrado, D., additional, Bauer, F. F., additional, Béjar, V. J. S., additional, Caballero, J. A., additional, Cortés-Contreras, M., additional, Damasso, M., additional, Dreizler, S., additional, González-Cuesta, L., additional, González Hernández, J. I., additional, Guenther, E. W., additional, Henning, T., additional, Herrero, E., additional, Jeffers, S. V., additional, Kaminski, A., additional, Kürster, M., additional, Lafarga, M., additional, Leto, G., additional, López-González, M. J., additional, Maldonado, J., additional, Micela, G., additional, Montes, D., additional, Pinamonti, M., additional, Quirrenbach, A., additional, Rebolo, R., additional, Reiners, A., additional, Rodríguez, E., additional, Rodríguez-López, C., additional, Schmitt, J. H. M. M., additional, Sozzetti, A., additional, Suárez Mascareño, A., additional, Toledo-Padrón, B., additional, Zanmar Sánchez, R., additional, Zapatero Osorio, M. R., additional, and Zechmeister, M., additional

Published
2019
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10. Gliese 49: Activity evolution and detection of a super-Earth: A HADES and CARMENES collaboration

Author

Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Junta de Andalucía, German Research Foundation, Generalitat de Catalunya, Ministerio de Ciencia e Innovación (España), Ministerio de Economía, Industria y Competitividad (España), Perger, M., Scandariato, G., Ribas, Ignasi, Morales, Juan Carlos, Affer, L., Azzaro, M., Amado, Pedro J., Anglada-Escudé, Guillem, Baroch, David, Barrado y Navascués, David, Bauer, FF, Béjar, Victor J. S., Caballero, J. A., Cortés-Contreras, M., Damasso, M., Dreizler, S., González-Cuesta, L., González Hernández, Jonay I., Guenther, E. W., Henning, Thomas, Herrero, E., Jeffers, Sandra V., Kaminski, Adrian, Kürster, M., Lafarga, M., Leto, G., López González, Maria J., Maldonado, J., Micela, Giusi, Montes, D., Pinamonti, M., Quirrenbach, Andreas, Rebolo López, Rafael, Reiners, Ansgar, Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Schmitt, Jürgen H. M. M., Sozzetti, Alessandro, Suárez Mascareño, A., Toledo-Padrón, B., Zanmar Sánchez, R., Zapatero Osorio, María Rosa, Zechmeister, Mathias, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Junta de Andalucía, German Research Foundation, Generalitat de Catalunya, Ministerio de Ciencia e Innovación (España), Ministerio de Economía, Industria y Competitividad (España), Perger, M., Scandariato, G., Ribas, Ignasi, Morales, Juan Carlos, Affer, L., Azzaro, M., Amado, Pedro J., Anglada-Escudé, Guillem, Baroch, David, Barrado y Navascués, David, Bauer, FF, Béjar, Victor J. S., Caballero, J. A., Cortés-Contreras, M., Damasso, M., Dreizler, S., González-Cuesta, L., González Hernández, Jonay I., Guenther, E. W., Henning, Thomas, Herrero, E., Jeffers, Sandra V., Kaminski, Adrian, Kürster, M., Lafarga, M., Leto, G., López González, Maria J., Maldonado, J., Micela, Giusi, Montes, D., Pinamonti, M., Quirrenbach, Andreas, Rebolo López, Rafael, Reiners, Ansgar, Rodríguez Martínez, Eloy, Rodríguez-López, Cristina, Schmitt, Jürgen H. M. M., Sozzetti, Alessandro, Suárez Mascareño, A., Toledo-Padrón, B., Zanmar Sánchez, R., Zapatero Osorio, María Rosa, and Zechmeister, Mathias

Abstract

Context. Small planets around low-mass stars often show orbital periods in a range that corresponds to the temperate zones of their host stars which are therefore of prime interest for planet searches. Surface phenomena such as spots and faculae create periodic signals in radial velocities and in observational activity tracers in the same range, so they can mimic or hide true planetary signals. Aims. We aim to detect Doppler signals corresponding to planetary companions, determine their most probable orbital configurations, and understand the stellar activity and its impact on different datasets. Methods. We analyzed 22 yr of data of the M1.5 V-type star Gl 49 (BD+61 195) including HARPS-N and CARMENES spectrographs, complemented by APT2 and SNO photometry. Activity indices are calculated from the observed spectra, and all datasets are analyzed with periodograms and noise models. We investigated how the variation of stellar activity imprints on our datasets. We further tested the origin of the signals and investigate phase shifts between the different sets. To search for the best-fit model we maximize the likelihood function in a Markov chain Monte Carlo approach. Results. As a result of this study, we are able to detect the super-Earth Gl 49b with a minimum mass of 5.6 M. It orbits its host star with a period of 13.85 d at a semi-major axis of 0.090 au and we calculate an equilibrium temperature of 350 K and a transit probability of 2.0%. The contribution from the spot-dominated host star to the different datasets is complex, and includes signals from the stellar rotation at 18.86 d, evolutionary timescales of activity phenomena at 40-80 d, and a long-term variation of at least four years.© 2019 ESO.

Published
2019

11. XV. Planetary occurrence rates around early-M dwarfs

Author

Pinamonti, M., Sozzetti, A., Maldonado, Jesús, Affer, L., Micela, G., Bonomo, A. S., Lanza, A. F., Perger, M., Ribas, Ignasi, González Hernández, J. I., Bignamini, A., Claudi, Riccardo, Covino, Elvira, Damasso, M., Desidera, S., Giacobbe, P., González-Álvarez, E., Herrero, E., Leto, G., Maggio, Antonio, Molinari, Emilio, Morales, J.C., Pagano, I., Petralia, Antonino, Piotto, Giampaolo, Poretti, Ennio, Rebolo López, Rafael, Scandariato, G., Suárez Mascareño, A., Toledo-Padrón, B., Zanmar Sánchez, R., Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Gobierno de Canarias, and Fundación 'la Caixa'

Subjects
Methods:statistical, Stars:activity, Planets and satellites: detection, Techniques:radialvelocities, Stars:low-mass
Abstract

[Aims] We present the complete Bayesian statistical analysis of the HArps-n red Dwarf Exoplanet Survey (HADES), which monitored the radial velocities of a large sample of M dwarfs with HARPS-N at TNG over the last 6 yr., [Methods] The targets were selected in a narrow range of spectral types from M0 to M3, 0.3 M⊙ < M★ < 0.71 M⊙, in order to study the planetary population around a well-defined class of host stars. We take advantage of Bayesian statistics to derive an accurate estimate of the detectability function of the survey. Our analysis also includes the application of a Gaussian Process approach to take into account stellar-activity-induced radial velocity variations and improve the detection limits around the most-observed and most-active targets. The Markov chain Monte Carlo and Gaussian process technique we apply in this analysis has proven very effective in the study of M-dwarf planetary systems, helping the detection of most of the HADES planets., [Results] From the detectability function we can calculate the occurrence rate of small-mass planets around early-M dwarfs, either taking into account only the 11 already published HADES planets or adding the five new planetary candidates discovered in this analysis, and compare them with the previous estimates of planet occurrence around M-dwarf or solar-type stars: considering only the confirmed planets, we find the highest frequency for low-mass planets (1 M⊕ < mp sin i < 10 M⊕) with periods 10 d < P < 100 d, , while for short-period planets (1 d < P < 10 d) we find a frequency of , significantly lower than for later-M dwarfs; if instead we also take into account the new candidates, we observe the same general behaviours, but with consistently higher frequencies of low-mass planets. We also present new estimates of the occurrence rates of long-period giant planets and temperate planets inside the habitable zone of early-M dwarfs: in particular we find that the frequency of habitable planets could be as low as η⊕ < 0.23. These results, and their comparison with other surveys focused on different stellar types, confirm the central role that stellar mass plays in the formation and evolution of planetary systems., M.Pi., A.P., A.M., and A.S. acknowledge partial contribution from the agreement ASI-INAF n.2018-16-HH.0. M.Pi. acknowledges partial contribution from OB.FU. 1.05.02.85.13 “Planetary Systems At Early Ages (PLATEA)”. J.M., and G.M. acknowledge support from the accordo attuativo ASI-INAF n.2021-5-HH.0 “Partecipazione italiana alla fase B2/C della missione Ariel”. E.G.A. acknowledge support from the Spanish Ministery for Science, Innovation, and Universities through projects AYA-2016-79425-C31/2/3-P, AYA2015-69350-C3-2-P, ESP2017-87676-C5-2-R, ESP2017-87143-R. The Centro de Astrobiología (CAB, CSIC-INTA) is a Center of Excellence “Maria de Maeztu”. M.D. acknowledges financial support from the FP7-SPACE Project ETAEARTH (GA no. 313014). P.G. gratefully acknowledges support from the Italian Space Agency (ASI) under contract 2018-24-HH.0. M.Pe. and I.R. acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018098153-B- C33, as well as the support of the Generalitat de Catalunya/CERCA programme. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramón y Cajal program RYC2013- 14875. B.T.P. acknowledges Fundación La Caixa for the financial support received in the form of a Ph.D. contract. A.S.M. acknowledges financial support from the Spanish MICINN under the 2019 Juan de la Cierva Programme. B.T.P., A.S.M., J.I.G.H. and R.R. acknowledge financial support from the Spanish MICINN project PID2020-117493GB-I00, and from the Government of the Canary Islands project ProID2020010129. The HARPS-N Project is a collaboration between the Astronomical Observatory of the Geneva University (lead), the CfA in Cambridge, the Universities of St. Andrews and Edinburgh, the Queen’ss University of Belfast, and the TNG-INAF Observatory.

Published
2018

12. HADES RV programme with HARPS-N at TNG: XIV. A candidate super-Earth orbiting the M-dwarf GJ 9689 with a period close to half the stellar rotation period

Author

J. Maldonado, A. Petralia, M. Damasso, M. Pinamonti, G. Scandariato, E. González-Álvarez, L. Affer, G. Micela, A. F. Lanza, G. Leto, E. Poretti, A. Sozzetti, M. Perger, P. Giacobbe, R. Zanmar Sánchez, A. Maggio, J. I. González Hernández, R. Rebolo, I. Ribas, A. Suárez-Mascareño, B. Toledo-Padrón, A. Bignamini, E. Molinari, E. Covino, R. Claudi, S. Desidera, E. Herrero, J. C. Morales, I. Pagano, G. Piotto, La Caixa, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Ministerio de Ciencia e Innovación (España), European Commission, Maldonado, J. [0000-0002-2218-5689], Petralia, A. [0000-0002-9882-1020], Damasso, M. [0000-0001-9984-4278], Pinamonti, M. [0000-0002-4445-1845], Affer, L. [0000-0001-5600-3778], Lanza, A. F. [0000-0001-5928-7251], Leto, G. [0000-0002-0040-5011], Poretti, E. [0000-0003-1200-0473], Sozzetti, A. [0000-0002-7504-365X], Perger, M. [0000-0001-7098-0372], Zanmar Sánchez, R. [0000-0002-6997-0887], Maggio, A. [0000-0001-5154-6108], González Hernández, J. I. [0000-0002-0264-7356], Ribas, I. [0000-0002-6689-0312], Toledo Padrón, B. [0000-0002-8194-215X], Bignamini, A. [0000-0002-5606-6354], Molinari, E. [0000-0002-1742-7735], Covino, E. [0000-0002-7579-2298], Claudi, R. [0000-0001-7707-5105], Desidera, S. [0000-0001-8613-2589], and Agencia Estatal de Investigación (AEI)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), GJ 9689, radial velocities [Techniques], 010308 nuclear & particles physics, Stars: individual, FOS: Physical sciences, Techniques: spectroscopic, Astronomy and Astrophysics, individual: GJ 9689 [Stars], Stars: late-type, 01 natural sciences, spectroscopic [Techniques], late type [Stars], Planetary systems, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [Stars], individual [Stars], Techniques: radial velocities, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

[Context] It is now well-established that small, rocky planets are common around low-mass stars. However, the detection of such planets is challenged by the short-term activity of host stars. [Aims] The HARPS-N red Dwarf Exoplanet Survey programme is a long-term project at the Telescopio Nazionale Galileo aimed at monitoring nearby, early-type, M dwarfs, using the HARPS-N spectrograph to search for small, rocky planets. [Methods] A total of 174 HARPS-N spectroscopic observations of the M0.5V-type star GJ 9689 taken over the past seven years have been analysed. We combined these data with photometric measurements to disentangle signals related to the stellar activity of the star from possible Keplerian signals in the radial velocity data. We ran an MCMC analysis, applying Gaussian process regression techniques to model the signals present in the data. [Results] We identify two periodic signals in the radial velocity time series, with periods of 18.27 and 39.31 d. The analysis of the activity indexes, photometric data, and wavelength dependency of the signals reveals that the 39.31 d signal corresponds to the stellar rotation period. On the other hand, the 18.27 d signal shows no relation to any activity proxy or the first harmonic of the rotation period. We, therefore, identify it as a genuine Keplerian signal. The best-fit model describing the newly found planet, GJ 9689 b, corresponds to an orbital period of Pb = 18.27 ± 0.01 d and a minimum mass of MP sini = 9.65 ± 1.41 M⊕., J.M. and G.M. acknowledge support from the accordo attua-tivo ASI-INAF n.2021-5-HH.0 “Partecipazione italiana alla fase B2/C della mis-sione Ariel”. A.P., A.M., M.P., and A.S. acknowledge partial contribution from the agreement ASI-INAF n.2018-16-HH.0. E.G.A. acknowledges support from the Spanish Ministery for Science, Innovation, and Universities through projects AYA-2016-79425-C3-1/2/3-P, AYA2015-69350-C3-2-P, ESP2017-87676-C5-2-R, ESP2017-87143-R. The Centro de Astrobiología (CAB, CSIC-INTA) is a Center of Excellence “Maria de Maeztu”. M.P and I.R acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-BC33, as well as the support of the Generalitat de Catalunya/CERCA programme. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramón y Cajal program RYC-2013-14875. B.T.P. acknowledges Fundación La Caixa for the financial support received in the form of a Ph.D. contract. A.S.M. acknowledges financial support from the Spanish MICINN under the 2019 Juan de la Cierva Programme. B.T.P., A.S.M., J.I.G.H., R.R. acknowledge financial support from the Spanish MICINN AYA2017-86389-P. This work has made 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, https://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.

Published
2021

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