Reiners, Ansgar

[["dc.bibliographiccitation.firstpage","A22"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","645"],["dc.contributor.author","Yan, F."],["dc.contributor.author","Wyttenbach, A."],["dc.contributor.author","Casasayas-Barris, N."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Pallé, E."],["dc.contributor.author","Henning, Th."],["dc.contributor.author","Mollière, P."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Nortmann, L."],["dc.contributor.author","Molaverdikhani, K."],["dc.contributor.author","Chen, G."],["dc.contributor.author","Snellen, I. A. G."],["dc.contributor.author","Zechmeister, M."],["dc.contributor.author","Huang, C."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Cont, D."],["dc.contributor.author","Khalafinejad, S."],["dc.contributor.author","Khaimova, J."],["dc.contributor.author","López-Puertas, M."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Oshagh, M."],["dc.contributor.author","Pedraz, S."],["dc.contributor.author","Stangret, M."],["dc.date.accessioned","2021-04-14T08:30:14Z"],["dc.date.available","2021-04-14T08:30:14Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/202039302"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/83161"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","Detection of the hydrogen Balmer lines in the ultra-hot Jupiter WASP-33b"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A50"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","640"],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Zechmeister, M."],["dc.contributor.author","Kaminski, A."],["dc.contributor.author","Rodríguez López, C."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Azzaro, M."],["dc.contributor.author","Stahl, O."],["dc.contributor.author","Kossakowski, D."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Becerril Jarque, S."],["dc.contributor.author","Rodríguez, E."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Seifert, W."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Schäfer, S."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Béjar, V. J. S."],["dc.contributor.author","Cortés-Contreras, M."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Hatzes, A."],["dc.contributor.author","Henning, T."],["dc.contributor.author","Jeffers, S. V."],["dc.contributor.author","Kürster, M."],["dc.contributor.author","Lafarga, M."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Morales, J. C."],["dc.contributor.author","Schmitt, J. H. M. M."],["dc.contributor.author","Schweitzer, A."],["dc.contributor.author","Solano, E."],["dc.date.accessioned","2021-04-14T08:24:23Z"],["dc.date.available","2021-04-14T08:24:23Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/202038031"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/81267"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","The CARMENES search for exoplanets around M dwarfs"],["dc.title.alternative","Measuring precise radial velocities in the near infrared: The example of the super-Earth CD Cet b"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A116"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","652"],["dc.contributor.author","Perdelwitz, V."],["dc.contributor.author","Mittag, M."],["dc.contributor.author","Tal-Or, L."],["dc.contributor.author","Schmitt, J. H. M. M."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Jeffers, S. V."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Schweitzer, A."],["dc.contributor.author","Trifonov, T."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Skrzypinski, S. L."],["dc.date.accessioned","2021-09-01T06:42:18Z"],["dc.date.available","2021-09-01T06:42:18Z"],["dc.date.issued","2021"],["dc.description.abstract","Context. Radial-velocity (RV) jitter caused by stellar magnetic activity is an important factor in state-of-the-art exoplanet discovery surveys such as CARMENES. Stellar rotation, along with heterogeneities in the photosphere and chromosphere caused by activity, can result in false-positive planet detections. Hence, it is necessary to determine the stellar rotation period and compare it to any putative planetary RV signature. Long-term measurements of activity indicators such as the chromospheric emission in the Ca  II H&K lines ( R HK ′ ) enable the identification of magnetic activity cycles. Aims. In order to determine stellar rotation periods and study the long-term behavior of magnetic activity of the CARMENES guaranteed time observations (GTO) sample, it is advantageous to extract R HK ′ time series from archival data, since the CARMENES spectrograph does not cover the blue range of the stellar spectrum containing the Ca  II H&K lines. Methods. We have assembled a catalog of 11 634 archival spectra of 186 M dwarfs acquired by seven different instruments covering the Ca  II H&K regime: ESPaDOnS, FEROS, HARPS, HIRES, NARVAL, TIGRE, and UVES. The relative chromospheric flux in these lines, R HK ′ , was directly extracted from the spectra by rectification with PHOENIX synthetic spectra via narrow passbands around the Ca  II H&K line cores. Results. The combination of archival spectra from various instruments results in time series for 186 stars from the CARMENES GTO sample. As an example of the use of the catalog, we report the tentative discovery of three previously unknown activity cycles of M dwarfs. Conclusions. We conclude that the method of extracting $ R_{\\mathrm{HK}}^\\prime $ with the use of model spectra yields consistent results for different instruments and that the compilation of this catalog will enable the analysis of long-term activity time series for a large number of M dwarfs."],["dc.description.abstract","Context. Radial-velocity (RV) jitter caused by stellar magnetic activity is an important factor in state-of-the-art exoplanet discovery surveys such as CARMENES. Stellar rotation, along with heterogeneities in the photosphere and chromosphere caused by activity, can result in false-positive planet detections. Hence, it is necessary to determine the stellar rotation period and compare it to any putative planetary RV signature. Long-term measurements of activity indicators such as the chromospheric emission in the Ca  II H&K lines ( R HK ′ ) enable the identification of magnetic activity cycles. Aims. In order to determine stellar rotation periods and study the long-term behavior of magnetic activity of the CARMENES guaranteed time observations (GTO) sample, it is advantageous to extract R HK ′ time series from archival data, since the CARMENES spectrograph does not cover the blue range of the stellar spectrum containing the Ca  II H&K lines. Methods. We have assembled a catalog of 11 634 archival spectra of 186 M dwarfs acquired by seven different instruments covering the Ca  II H&K regime: ESPaDOnS, FEROS, HARPS, HIRES, NARVAL, TIGRE, and UVES. The relative chromospheric flux in these lines, R HK ′ , was directly extracted from the spectra by rectification with PHOENIX synthetic spectra via narrow passbands around the Ca  II H&K line cores. Results. The combination of archival spectra from various instruments results in time series for 186 stars from the CARMENES GTO sample. As an example of the use of the catalog, we report the tentative discovery of three previously unknown activity cycles of M dwarfs. Conclusions. We conclude that the method of extracting $ R_{\\mathrm{HK}}^\\prime $ with the use of model spectra yields consistent results for different instruments and that the compilation of this catalog will enable the analysis of long-term activity time series for a large number of M dwarfs."],["dc.identifier.doi","10.1051/0004-6361/202140889"],["dc.identifier.pii","aa40889-21"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/89027"],["dc.notes.intern","DOI-Import GROB-455"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","CARMENES input catalog of M dwarfs"],["dc.title.alternative","VI. A time-resolved Ca II H&K catalog from archival data"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A129"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","647"],["dc.contributor.author","Lampón, M."],["dc.contributor.author","López-Puertas, M."],["dc.contributor.author","Sanz-Forcada, J."],["dc.contributor.author","Sánchez-López, A."],["dc.contributor.author","Molaverdikhani, K."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Pallé, E."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Henning, T."],["dc.contributor.author","Salz, M."],["dc.contributor.author","Nortmann, L."],["dc.contributor.author","Aceituno, J."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Ribas, I."],["dc.date.accessioned","2021-04-14T08:28:33Z"],["dc.date.available","2021-04-14T08:28:33Z"],["dc.date.issued","2021"],["dc.identifier.doi","10.1051/0004-6361/202039417"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/82641"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","Modelling the He I triplet absorption at 10 830 Å in the atmospheres of HD 189733 b and GJ 3470 b"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A24"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","632"],["dc.contributor.author","Fuhrmeister, B."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Hildebrandt, L."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Schmitt, J. H. M. M."],["dc.contributor.author","Hintz, D."],["dc.contributor.author","Johnson, E. N."],["dc.contributor.author","Sanz-Forcada, J."],["dc.contributor.author","Schöfer, P."],["dc.contributor.author","Jeffers, S. V."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Zechmeister, M."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Béjar, V. J. S."],["dc.contributor.author","Cortés-Contreras, M."],["dc.contributor.author","Díez-Alonso, E."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Galadí-Enríquez, D."],["dc.contributor.author","Günther, E. W."],["dc.contributor.author","Kaminski, A."],["dc.contributor.author","Kürster, M."],["dc.contributor.author","Lafarga, M."],["dc.contributor.author","Montes, D."],["dc.date.accessioned","2020-04-06T07:56:28Z"],["dc.date.available","2020-04-06T07:56:28Z"],["dc.date.issued","2019-11-01"],["dc.description.abstract","The He I infrared (IR) triplet at 10830 AA is an important activity indicator for the Sun and in solar-type stars, however, it has rarely been studied in relation to M dwarfs to date. In this study, we use the time-averaged spectra of 319 single stars with spectral types ranging from M0.0 V to M9.0 V obtained with the CARMENES high resolution optical and near-infrared spectrograph at Calar Alto to study the properties of the He I IR triplet lines. In quiescence, we find the triplet in absorption with a decrease of the measured pseudo equivalent width (pEW) towards later sub-types. For stars later than M5.0 V, the He I triplet becomes undetectable in our study. This dependence on effective temperature may be related to a change in chromospheric conditions along the M dwarf sequence. When an emission in the triplet is observed, we attribute it to flaring. The absence of emission during quiescence is consistent with line formation by photo-ionisation and recombination, while flare emission may be caused by collisions within dense material. The He I triplet tends to increase in depth according to increasing activity levels, ultimately becoming filled in; however, we do not find a correlation between the pEW(He IR) and X-ray properties. This behaviour may be attributed to the absence of very inactive stars ($L_{\\rm X}/L_{\\rm bol}$ < -5.5) in our sample or to the complex behaviour with regard to increasing depth and filling in."],["dc.identifier.arxiv","1911.00246v1"],["dc.identifier.doi","10.1051/0004-6361/201936193"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/63790"],["dc.relation.issn","0004-6361"],["dc.relation.issn","1432-0746"],["dc.title","The CARMENES search for exoplanets around M dwarfs"],["dc.title.subtitle","The He I triplet at 10830 Å across the M dwarf sequence"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A69"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","641"],["dc.contributor.author","Baroch, D."],["dc.contributor.author","Morales, J. C."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Herrero, E."],["dc.contributor.author","Rosich, A."],["dc.contributor.author","Perger, M."],["dc.contributor.author","Anglada-Escudé, G."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Jeffers, S. V."],["dc.contributor.author","Cifuentes, C."],["dc.contributor.author","Passegger, V. M."],["dc.contributor.author","Schweitzer, A."],["dc.contributor.author","Lafarga, M."],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Béjar, V. J. S."],["dc.contributor.author","Colomé, J."],["dc.contributor.author","Cortés-Contreras, M."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Galadí-Enríquez, D."],["dc.contributor.author","Hatzes, A. P."],["dc.contributor.author","Henning, Th."],["dc.contributor.author","Kaminski, A."],["dc.contributor.author","Kürster, M."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Rodríguez-López, C."],["dc.contributor.author","Zechmeister, M."],["dc.date.accessioned","2021-04-14T08:23:09Z"],["dc.date.available","2021-04-14T08:23:09Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/202038213"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/80811"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","The CARMENES search for exoplanets around M dwarfs"],["dc.title.alternative","Convective shift and starspot constraints from chromatic radial velocities"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A69"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","632"],["dc.contributor.author","Yan, F."],["dc.contributor.author","Casasayas-Barris, N."],["dc.contributor.author","Molaverdikhani, K."],["dc.contributor.author","Alonso-Floriano, F. J."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Palle, E."],["dc.contributor.author","Henning, Th."],["dc.contributor.author","Mollière, P."],["dc.contributor.author","Chen, G."],["dc.contributor.author","Nortmann, L."],["dc.contributor.author","Snellen, I. A. G."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Azzaro, M."],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Cortés Contreras, M."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Khalafinejad, S."],["dc.contributor.author","Lara, L. M."],["dc.contributor.author","López-Puertas, M."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Oshagh, M."],["dc.contributor.author","Sánchez-López, A."],["dc.contributor.author","Stangret, M."],["dc.contributor.author","Zechmeister, M."],["dc.date.accessioned","2020-04-06T07:20:35Z"],["dc.date.available","2020-04-06T07:20:35Z"],["dc.date.issued","2019-11-01"],["dc.description.abstract","Ultra-hot Jupiters are emerging as a new class of exoplanets. Studying their chemical compositions and temperature structures will improve the understanding of their mass loss rate as well as their formation and evolution. We present the detection of ionized calcium in the two hottest giant exoplanets - KELT-9b and WASP-33b. By utilizing transit datasets from CARMENES and HARPS-N observations, we achieved high confidence level detections of Ca II using the cross-correlation method. We further obtain the transmission spectra around the individual lines of the Ca II H&K doublet and the near-infrared triplet, and measure their line profiles. The Ca II H&K lines have an average line depth of 2.02 $\\pm$ 0.17 % (effective radius of 1.56 Rp) for WASP-33b and an average line depth of 0.78 $\\pm$ 0.04 % (effective radius of 1.47 Rp) for KELT-9b, which indicates that the absorptions are from very high upper atmosphere layers close to the planetary Roche lobes. The observed Ca II lines are significantly deeper than the predicted values from the hydrostatic models. Such a discrepancy is probably a result of hydrodynamic outflow that transports a significant amount of Ca II into the upper atmosphere. The prominent Ca II detection with the lack of significant Ca I detection implies that calcium is mostly ionized in the upper atmospheres of the two planets."],["dc.identifier.arxiv","1911.00380v1"],["dc.identifier.doi","10.1051/0004-6361/201936396"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/63758"],["dc.relation.issn","0004-6361"],["dc.relation.issn","1432-0746"],["dc.title","Ionized calcium in the atmospheres of two ultra-hot exoplanets WASP-33b and KELT-9b"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A49"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","612"],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Zechmeister, M."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Morales, J. C."],["dc.contributor.author","Jeffers, Sandra V."],["dc.contributor.author","Schöfer, P."],["dc.contributor.author","Tal-Or, L."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Kaminski, A."],["dc.contributor.author","Maroto Fernández, D."],["dc.contributor.author","Martín, E. L."],["dc.contributor.author","Martín-Ruiz, S."],["dc.contributor.author","Marvin, Christopher J."],["dc.contributor.author","Mathar, R. J."],["dc.contributor.author","Mirabet, E."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Moreno-Raya, M. E."],["dc.contributor.author","Moya, A."],["dc.contributor.author","Mundt, R."],["dc.contributor.author","Seifert, W."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Naranjo, V."],["dc.contributor.author","Nortmann, Lisa"],["dc.contributor.author","Nowak, G."],["dc.contributor.author","Ofir, A."],["dc.contributor.author","Oreiro, R."],["dc.contributor.author","Pallé, E."],["dc.contributor.author","Panduro, J."],["dc.contributor.author","Pascual, J."],["dc.contributor.author","Passegger, Vera Maria"],["dc.contributor.author","Abril, M."],["dc.contributor.author","Pavlov, A."],["dc.contributor.author","Pedraz, S."],["dc.contributor.author","Pérez-Calpena, A."],["dc.contributor.author","Medialdea, D. Pérez"],["dc.contributor.author","Perger, M."],["dc.contributor.author","Perryman, M. A. C."],["dc.contributor.author","Pluto, M."],["dc.contributor.author","Rabaza, O."],["dc.contributor.author","Ramón, A."],["dc.contributor.author","Rebolo, R."],["dc.contributor.author","Aceituno, J."],["dc.contributor.author","Redondo, P."],["dc.contributor.author","Reffert, S."],["dc.contributor.author","Reinhart, S."],["dc.contributor.author","Rhode, P."],["dc.contributor.author","Rix, H.-W."],["dc.contributor.author","Rodler, F."],["dc.contributor.author","Rodríguez, E."],["dc.contributor.author","Rodríguez-López, C."],["dc.contributor.author","Rodríguez Trinidad, A."],["dc.contributor.author","Rohloff, R.-R."],["dc.contributor.author","Alonso-Floriano, F. J."],["dc.contributor.author","Rosich, A."],["dc.contributor.author","Sadegi, S."],["dc.contributor.author","Sánchez-Blanco, E."],["dc.contributor.author","Sánchez Carrasco, M. A."],["dc.contributor.author","Sánchez-López, A."],["dc.contributor.author","Sanz-Forcada, J."],["dc.contributor.author","Sarkis, P."],["dc.contributor.author","Sarmiento, L. F."],["dc.contributor.author","Schäfer, Sascha"],["dc.contributor.author","Schmitt, J. H. M. M."],["dc.contributor.author","Ammler-von Eiff, M."],["dc.contributor.author","Schiller, J."],["dc.contributor.author","Schweitzer, A."],["dc.contributor.author","Solano, E."],["dc.contributor.author","Stahl, O."],["dc.contributor.author","Strachan, J. B. P."],["dc.contributor.author","Stürmer, J."],["dc.contributor.author","Suárez, J. C."],["dc.contributor.author","Tabernero, H. M."],["dc.contributor.author","Tala, M."],["dc.contributor.author","Trifonov, T."],["dc.contributor.author","Antona, R."],["dc.contributor.author","Tulloch, S. M."],["dc.contributor.author","Ulbrich, R. G."],["dc.contributor.author","Veredas, G."],["dc.contributor.author","Vico Linares, J. I."],["dc.contributor.author","Vilardell, F."],["dc.contributor.author","Wagner, K."],["dc.contributor.author","Winkler, J."],["dc.contributor.author","Wolthoff, V."],["dc.contributor.author","Xu, W."],["dc.contributor.author","Yan, F."],["dc.contributor.author","Anglada-Escudé, G."],["dc.contributor.author","Zapatero Osorio, M. R."],["dc.contributor.author","Anwand-Heerwart, H."],["dc.contributor.author","Arroyo-Torres, B."],["dc.contributor.author","Azzaro, M."],["dc.contributor.author","Baroch, D."],["dc.contributor.author","Barrado, D."],["dc.contributor.author","Bauer, Florian F."],["dc.contributor.author","Becerril, S."],["dc.contributor.author","Béjar, V. J. S."],["dc.contributor.author","Benítez, D."],["dc.contributor.author","Berdinas̃, Z. M."],["dc.contributor.author","Bergond, G."],["dc.contributor.author","Blümcke, M."],["dc.contributor.author","Brinkmöller, M."],["dc.contributor.author","del Burgo, C."],["dc.contributor.author","Cano, J."],["dc.contributor.author","Cárdenas Vázquez, M. C."],["dc.contributor.author","Casal, E."],["dc.contributor.author","Cifuentes, C."],["dc.contributor.author","Claret, A."],["dc.contributor.author","Colomé, J."],["dc.contributor.author","Cortés-Contreras, M."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Díez-Alonso, E."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Feiz, C."],["dc.contributor.author","Fernández, M."],["dc.contributor.author","Ferro, I. M."],["dc.contributor.author","Fuhrmeister, B."],["dc.contributor.author","Galadí-Enríquez, D."],["dc.contributor.author","Garcia-Piquer, A."],["dc.contributor.author","García Vargas, M. L."],["dc.contributor.author","Gesa, L."],["dc.contributor.author","Galera, V. Gómez"],["dc.contributor.author","González Hernández, J. I."],["dc.contributor.author","González-Peinado, R."],["dc.contributor.author","Grözinger, U."],["dc.contributor.author","Grohnert, S."],["dc.contributor.author","Guàrdia, J."],["dc.contributor.author","Guenther, E. W."],["dc.contributor.author","Guijarro, A."],["dc.contributor.author","Guindos, E. de"],["dc.contributor.author","Gutiérrez-Soto, J."],["dc.contributor.author","Hagen, H.-J."],["dc.contributor.author","Hatzes, A. P."],["dc.contributor.author","Hauschildt, P. H."],["dc.contributor.author","Hedrosa, R. P."],["dc.contributor.author","Helmling, J."],["dc.contributor.author","Henning, Th."],["dc.contributor.author","Hermelo, I."],["dc.contributor.author","Hernández Arabí, R."],["dc.contributor.author","Hernández Castaño, L."],["dc.contributor.author","Hernández Hernando, F."],["dc.contributor.author","Herrero, E."],["dc.contributor.author","Huber, A."],["dc.contributor.author","Huke, Philipp"],["dc.contributor.author","Johnson, E. N."],["dc.contributor.author","Juan, E. de"],["dc.contributor.author","Kim, M."],["dc.contributor.author","Klein, R."],["dc.contributor.author","Klüter, J."],["dc.contributor.author","Klutsch, A."],["dc.contributor.author","Kürster, M."],["dc.contributor.author","Lafarga, M."],["dc.contributor.author","Lamert, A."],["dc.contributor.author","Lampón, M."],["dc.contributor.author","Lara, L. M."],["dc.contributor.author","Laun, W."],["dc.contributor.author","Lemke, U."],["dc.contributor.author","Lenzen, R."],["dc.contributor.author","Launhardt, R."],["dc.contributor.author","López del Fresno, M."],["dc.contributor.author","López-González, J."],["dc.contributor.author","López-Puertas, M."],["dc.contributor.author","López Salas, J. F."],["dc.contributor.author","López-Santiago, J."],["dc.contributor.author","Luque, R."],["dc.contributor.author","Magán Madinabeitia, H."],["dc.contributor.author","Mall, U."],["dc.contributor.author","Mancini, L."],["dc.contributor.author","Mandel, H."],["dc.contributor.author","Marfil, E."],["dc.contributor.author","Marín Molina, J. A."],["dc.date.accessioned","2021-11-22T14:31:40Z"],["dc.date.available","2021-11-22T14:31:40Z"],["dc.date.issued","2018"],["dc.identifier.doi","10.1051/0004-6361/201732054"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/15628"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/93396"],["dc.notes.intern","Migrated from goescholar"],["dc.relation.issn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","The CARMENES search for exoplanets around M dwarfs"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A118"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","654"],["dc.contributor.author","Shan, Y."],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Fabbian, D."],["dc.contributor.author","Marfil, E."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Tabernero, H. M."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Zechmeister, M."],["dc.date.accessioned","2021-12-01T09:20:58Z"],["dc.date.available","2021-12-01T09:20:58Z"],["dc.date.issued","2021"],["dc.description.abstract","Context. M-dwarf spectra are complex and notoriously difficult to model, posing challenges to understanding their photospheric properties and compositions in depth. Vanadium (V) is an iron-group element whose abundance supposedly closely tracks that of iron, but has origins that are not completely understood. Aims. Our aim is to characterize a series of neutral vanadium atomic absorption lines in the 800–910 nm wavelength region of high signal-to-noise, high-resolution, telluric-corrected M-dwarf spectra from the CARMENES survey. Many of these lines are prominent and exhibit a distinctive broad and flat-bottom shape, which is a result of hyperfine structure (HFS). We investigate the potential and implications of these HFS split lines for abundance analysis of cool stars. Methods. With standard spectral synthesis routines, as provided by the spectroscopy software iSpec and the latest atomic data (including HFS) available from the VALD3 database, we modeled these striking line profiles. We used them to measure V abundances of cool dwarfs. Results. We determined V abundances for 135 early M dwarfs (M0.0 V to M3.5 V) in the CARMENES guaranteed time observations sample. They exhibit a [V/Fe]–[Fe/H] trend consistent with that derived from nearby FG dwarfs. The tight (±0.1 dex) correlation between [V/H] and [Fe/H] suggests the potential application of V as an alternative metallicity indicator in M dwarfs. We also show hints that neglecting to model HFS could partially explain the temperature correlation in V abundance measurements observed in previous studies of samples involving dwarf stars with T eff ≲ 5300 K. Conclusions. Our work suggests that HFS can impact certain absorption lines in cool photospheres more severely than in Sun-like ones. Therefore, we advocate that HFS should be carefully treated in abundance studies in stars cooler than ~5000 K. On the other hand, strong HFS split lines in high-resolution spectra present an opportunity for precision chemical analyses of large samples of cool stars. The V-to-Fe trends exhibited by the local M dwarfs continue to challenge theoretical models of V production in the Galaxy."],["dc.identifier.doi","10.1051/0004-6361/202141530"],["dc.identifier.pii","aa41530-21"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/94313"],["dc.notes.intern","DOI-Import GROB-478"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.rights.uri","https://www.edpsciences.org/en/authors/copyright-and-licensing"],["dc.title","The CARMENES search for exoplanets around M dwarfs"],["dc.title.alternative","Not-so-fine hyperfine-split vanadium lines in cool star spectra"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A24"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","643"],["dc.contributor.author","Sánchez-López, A."],["dc.contributor.author","López-Puertas, M."],["dc.contributor.author","Snellen, I. A. G."],["dc.contributor.author","Nagel, E."],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Pallé, E."],["dc.contributor.author","Tal-Or, L."],["dc.contributor.author","Amado, P. J."],["dc.contributor.author","Caballero, J. A."],["dc.contributor.author","Czesla, S."],["dc.contributor.author","Nortmann, L."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Ribas, I."],["dc.contributor.author","Quirrenbach, A."],["dc.contributor.author","Aceituno, J."],["dc.contributor.author","Béjar, V. J. S."],["dc.contributor.author","Casasayas-Barris, N."],["dc.contributor.author","Henning, Th."],["dc.contributor.author","Molaverdikhani, K."],["dc.contributor.author","Montes, D."],["dc.contributor.author","Stangret, M."],["dc.contributor.author","Zapatero Osorio, M. R."],["dc.contributor.author","Zechmeister, M."],["dc.date.accessioned","2021-04-14T08:31:44Z"],["dc.date.available","2021-04-14T08:31:44Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/202038629"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/83698"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","Discriminating between hazy and clear hot-Jupiter atmospheres with CARMENES"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]