Seemann, Ulf

[["dc.bibliographiccitation.firstpage","A50"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","613"],["dc.contributor.author","Carleo, I."],["dc.contributor.author","Benatti, S."],["dc.contributor.author","Lanza, A. F."],["dc.contributor.author","Gratton, R."],["dc.contributor.author","Claudi, R."],["dc.contributor.author","Desidera, S."],["dc.contributor.author","Mace, G. N."],["dc.contributor.author","Messina, S."],["dc.contributor.author","Sanna, N."],["dc.contributor.author","Sissa, E."],["dc.contributor.author","Ghedina, A."],["dc.contributor.author","Ghinassi, F."],["dc.contributor.author","Guerra, J."],["dc.contributor.author","Harutyunyan, A."],["dc.contributor.author","Micela, G."],["dc.contributor.author","Molinari, E."],["dc.contributor.author","Oliva, E."],["dc.contributor.author","Tozzi, A."],["dc.contributor.author","Baffa, C."],["dc.contributor.author","Baruffolo, A."],["dc.contributor.author","Bignamini, A."],["dc.contributor.author","Buchschacher, N."],["dc.contributor.author","Cecconi, M."],["dc.contributor.author","Cosentino, R."],["dc.contributor.author","Endl, M."],["dc.contributor.author","Falcini, G."],["dc.contributor.author","Fantinel, D."],["dc.contributor.author","Fini, L."],["dc.contributor.author","Fugazza, D."],["dc.contributor.author","Galli, A."],["dc.contributor.author","Giani, E."],["dc.contributor.author","González, C."],["dc.contributor.author","González-Álvarez, E."],["dc.contributor.author","González, M."],["dc.contributor.author","Hernandez, N."],["dc.contributor.author","Hernandez Diaz, M."],["dc.contributor.author","Iuzzolino, M."],["dc.contributor.author","Kaplan, K. F."],["dc.contributor.author","Kidder, B. T."],["dc.contributor.author","Lodi, M."],["dc.contributor.author","Malavolta, L."],["dc.contributor.author","Maldonado, J."],["dc.contributor.author","Origlia, L."],["dc.contributor.author","Perez Ventura, H."],["dc.contributor.author","Puglisi, A."],["dc.contributor.author","Rainer, M."],["dc.contributor.author","Riverol, L."],["dc.contributor.author","Riverol, C."],["dc.contributor.author","San Juan, J."],["dc.contributor.author","Scuderi, S."],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Sokal, K. R."],["dc.contributor.author","Sozzetti, A."],["dc.contributor.author","Sozzi, M."],["dc.date.accessioned","2020-12-10T18:11:38Z"],["dc.date.available","2020-12-10T18:11:38Z"],["dc.date.issued","2018"],["dc.identifier.doi","10.1051/0004-6361/201732350"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74091"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Multi-band high resolution spectroscopy rules out the hot Jupiter BD+20 1790b"],["dc.title.alternative","First data from the GIARPS Commissioning"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A109"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","539"],["dc.contributor.author","Lebzelter, T."],["dc.contributor.author","Seifahrt, Andreas"],["dc.contributor.author","Uttenthaler, S."],["dc.contributor.author","Ramsay, S."],["dc.contributor.author","Hartman, Henrik"],["dc.contributor.author","Nieva, M.-F."],["dc.contributor.author","Przybilla, Norbert"],["dc.contributor.author","Smette, A."],["dc.contributor.author","Wahlgren, G. M."],["dc.contributor.author","Wolff, B."],["dc.contributor.author","Hussain, G. A. J."],["dc.contributor.author","Kaeufl, H. U."],["dc.contributor.author","Seemann, U."],["dc.date.accessioned","2018-11-07T09:12:29Z"],["dc.date.available","2018-11-07T09:12:29Z"],["dc.date.issued","2012"],["dc.description.abstract","Context. New instrumental capabilities and the wealth of astrophysical information extractable from the near-infrared wavelength region have led to a growing interest in the field of high resolution spectroscopy at 1-5 mu m. Aims. We aim to provide a library of observed high-resolution and high signal-to-noise-ratio near-infrared spectra of stars of various types throughout the Hertzsprung-Russell diagram. This is needed for the exploration of spectral features in this wavelength range and for comparison of reference targets with observations and models. Methods. High quality spectra were obtained using the CRIRES near-infrared spectrograph at ESO's VLT covering the range from 0.97 mu m to 5.3 mu m at high spectral resolution. Accurate wavelength calibration and correction for telluric lines were performed by fitting synthetic transmission spectra for the Earth's atmosphere to each spectrum individually. Results. We describe the observational strategy and the current status and content of the library which includes 13 objects. The first examples of finally reduced spectra are presented. This publication will serve as a reference paper to introduce the library to the community and explore the extensive amount of material."],["dc.identifier.doi","10.1051/0004-6361/201117728"],["dc.identifier.fs","596772"],["dc.identifier.isi","000303262000116"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9591"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/26955"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","CRIRES-POP A library of high resolution spectra in the near-infrared"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","124501"],["dc.bibliographiccitation.issue","1018"],["dc.bibliographiccitation.journal","Publications of the Astronomical Society of the Pacific"],["dc.bibliographiccitation.volume","132"],["dc.contributor.author","Rodeghiero, Gabriele"],["dc.contributor.author","Häberle, Maximilian"],["dc.contributor.author","Sauter, Jonas"],["dc.contributor.author","Sawczuck, Miriam"],["dc.contributor.author","Pott, Jörg-Uwe"],["dc.contributor.author","Münch, Norbert"],["dc.contributor.author","Ramos, José Ricardo"],["dc.contributor.author","Naranjo, Vianak"],["dc.contributor.author","Kausch, Wolfgang"],["dc.contributor.author","Sabha, Nadeen B."],["dc.contributor.author","Biancalani, Enrico"],["dc.contributor.author","Barboza, Santiago"],["dc.contributor.author","Bizenberger, Peter"],["dc.contributor.author","Rohloff, Ralf-Rainer"],["dc.contributor.author","Müller, Friedrich"],["dc.contributor.author","Hofferbert, Ralph"],["dc.contributor.author","Mohr, Lars"],["dc.contributor.author","Neumann, Udo"],["dc.contributor.author","Seemann, Ulf"],["dc.contributor.author","Schäfer, Sebastian"],["dc.contributor.author","Leschinski, Kieran"],["dc.contributor.author","Czoske, Oliver"],["dc.contributor.author","Laun, Werner"],["dc.date.accessioned","2021-04-14T08:25:10Z"],["dc.date.available","2021-04-14T08:25:10Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1088/1538-3873/abbff3"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/81542"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1538-3873"],["dc.title","Development of the MICADO Flat-field and Wavelength Calibration Unit: From Design to Prototyping"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A118"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","618"],["dc.contributor.author","Sarmiento, L. F."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Huke, P."],["dc.contributor.author","Bauer, F. F."],["dc.contributor.author","Guenter, E. W."],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Wolter, U."],["dc.date.accessioned","2020-12-10T18:11:40Z"],["dc.date.available","2020-12-10T18:11:40Z"],["dc.date.issued","2018"],["dc.identifier.doi","10.1051/0004-6361/201832871"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74099"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Comparing the emission spectra of U and Th hollow cathode lamps and a new U line list"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A40"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","563"],["dc.contributor.author","Chen, G."],["dc.contributor.author","van Boekel, R."],["dc.contributor.author","Wang, H."],["dc.contributor.author","Nikolov, N."],["dc.contributor.author","Fortney, J. J."],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Wang, W."],["dc.contributor.author","Mancini, L."],["dc.contributor.author","Henning, Th."],["dc.date.accessioned","2019-07-09T11:40:19Z"],["dc.date.available","2019-07-09T11:40:19Z"],["dc.date.issued","2014"],["dc.description.abstract","Aims. WASP-43b is the closest-orbiting hot Jupiter, and it has high bulk density. It causes deep eclipse depths in the system’s light curve in both transit and occultation that is attributed to the cool temperature and small radius of its host star. We aim to secure a broad-band transmission spectrum and to detect its near-infrared thermal emission in order to characterize its atmosphere. Methods. We observed one transit and one occultation event simultaneously in the g′, r′, i′, z′, J, H, K bands using the GROND instrument on the MPG/ESO 2.2-m telescope, where the telescope was heavily defocused in staring mode. After modeling the light curves, we derived wavelength-dependent transit depths and flux ratios and compared them to atmospheric models. Results. From the transit event, we have independently derived WASP-43’s system parameters with high precision and improved the period to be 0.81347437(13) days based on all the available timings. No significant variation in transit depths is detected, with the largest deviations coming from the i′-, H-, and K-bands. Given the observational uncertainties, the broad-band transmission spectrum can be explained by either (i) a flat featureless straight line that indicates thick clouds; (ii) synthetic spectra with absorption signatures of atomic Na/K, or molecular TiO/VO that in turn indicate cloud-free atmosphere; or (iii) a Rayleigh scattering profile that indicates high-altitude hazes. From the occultation event, we detected planetary dayside thermal emission in the K-band with a flux ratio of 0.197 ± 0.042%, which confirms previous detections obtained in the 2.09 μm narrow band and KS-band. The K-band brightness temperature 1878+108-116 K favors an atmosphere with poor day- to nightside heat redistribution. We also have a marginal detection in the i′-band (0.037+0.023-0.021%), corresponding to TB = 2225+139-225 K, which is either a false positive, a signature of non-blackbody radiation at this wavelength, or an indication of reflective hazes at high altitude."],["dc.format.extent","14"],["dc.identifier.doi","10.1051/0004-6361/201322740"],["dc.identifier.fs","609741"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10911"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/58144"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.rights","Goescholar"],["dc.rights.access","openAccess"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","Broad-band transmission spectrum and K-band thermal emission of WASP-43b as observed from the ground"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A79"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","598"],["dc.contributor.author","Nicholls, C. P."],["dc.contributor.author","Lebzelter, T."],["dc.contributor.author","Smette, A."],["dc.contributor.author","Wolff, B."],["dc.contributor.author","Hartman, Henrik"],["dc.contributor.author","Kaeufl, H. U."],["dc.contributor.author","Przybilla, Norbert"],["dc.contributor.author","Ramsay, S."],["dc.contributor.author","Uttenthaler, S."],["dc.contributor.author","Wahlgren, G. M."],["dc.contributor.author","Bagnulo, S."],["dc.contributor.author","Hussain, G. A. J."],["dc.contributor.author","Nieva, M.-F."],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Seifahrt, Andreas"],["dc.date.accessioned","2018-11-07T10:27:40Z"],["dc.date.available","2018-11-07T10:27:40Z"],["dc.date.issued","2017"],["dc.description.abstract","Context. High resolution stellar spectral atlases are valuable resources to astronomy. They are rare in the 1-5 mu m region for historical reasons, but once available, high resolution atlases in this part of the spectrum will aid the study of a wide range of astrophysical phenomena. Aims. The aim of the CRIRES-POP project is to produce a high resolution near-infrared spectral library of stars across the H-R diagram. The aim of this paper is to present the fully reduced spectrum of the K giant 10 Leo that will form the basis of the first atlas within the CRIRES-POP library, to provide a full description of the data reduction processes involved, and to provide an update on the CRIRES-POP project. Methods. All CRIRES-POP targets were observed with almost 200 different observational settings of CRIRES on the ESO Very Large Telescope, resulting in a basically complete coverage of its spectral range as accessible from the ground. We reduced the spectra of 10 Leo with the CRIRES pipeline, corrected the wavelength solution and removed telluric absorption with Molecfit, then resampled the spectra to a common wavelength scale, shifted them to rest wavelengths, flux normalised, and median combined them into one final data product. Results. We present the fully reduced, high resolution, near-infrared spectrum of 10 Leo. This is also the first complete spectrum from the CRIRES instrument. The spectrum is available online. Conclusions. The first CRIRES-POP spectrum has exceeded our quality expectations and will form the centre of a state-of-the-art stellar atlas. This first CRIRES-POP atlas will soon be available, and further atlases will follow. All CRIRES-POP data products will be freely and publicly available online."],["dc.identifier.doi","10.1051/0004-6361/201629244"],["dc.identifier.isi","000394465000078"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/14264"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43277"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","PUB_WoS_Import"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","CRIRES-POP: a library of high resolution spectra in the near-infrared II. Data reduction and the spectrum of the K giant 10 Leonis"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","556"],["dc.contributor.author","Mueller, A."],["dc.contributor.author","Roccatagliata, V."],["dc.contributor.author","Henning, Th."],["dc.contributor.author","Fedele, D."],["dc.contributor.author","Pasquali, A."],["dc.contributor.author","Caffau, E."],["dc.contributor.author","Rodriguez-Ledesma, M. V."],["dc.contributor.author","Mohler-Fischer, M."],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Klement, R. J."],["dc.date.accessioned","2018-11-07T09:21:42Z"],["dc.date.available","2018-11-07T09:21:42Z"],["dc.date.issued","2013"],["dc.description.abstract","Aims. We reanalyze FEROS observations of the star HIP 11952 to reassess the existence of the proposed planetary system. Methods. The radial velocity of the spectra were measured by cross-correlating the observed spectrum with a synthetic template. We also analyzed a large dataset of FEROS and HARPS archival data of the calibrator HD 10700 spanning over more than five years. We compared the barycentric velocities computed by the FEROS and HARPS pipelines. Results. The barycentric correction of the FEROS-DRS pipeline was found to be inaccurate and to introduce an artificial one-year period with a semi-amplitude of 62 m s(-1). Thus the reanalysis of the FEROS data does not support the existence of planets around HIP 11952."],["dc.description.sponsorship","DLR [50 OR 1109]; Bayerischen Gleichstellungsforderung (BGF)"],["dc.identifier.doi","10.1051/0004-6361/201321497"],["dc.identifier.isi","000323893500003"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10864"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/29170"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Reanalysis of the FEROS observations of HIP 11952 (Research Note)"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A35"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","563"],["dc.contributor.author","Shulyak, D."],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Kochukhov, Oleg"],["dc.contributor.author","Piskunov, Nikolai E."],["dc.date.accessioned","2018-11-07T09:43:00Z"],["dc.date.available","2018-11-07T09:43:00Z"],["dc.date.issued","2014"],["dc.description.abstract","Context. Magnetic fields play a pivotal role in the formation and evolution of low-mass stars, but the dynamo mechanisms generating these fields are poorly understood. Measuring cool star magnetism is a complicated task because of the complexity of cool star spectra and the subtle signatures of magnetic fields. Aims. Based on detailed spectral synthesis, we carry out quantitative measurements of the strength and complexity of surface magnetic fields in the four well-known M dwarfs GJ 388, GJ 729, GJ 285, and GJ 406 that populate the mass regime around the boundary between partially and fully convective stars. Very high-resolution (R = 100 000), high signal-to-noise (up to 400), near-infrared Stokes I spectra were obtained with CRIRES at ESO's Very Large Telescope covering regions of the FeH Wing-Ford transitions at 1 mu m and Na I lines at 2.2 mu m. Methods. A modified version of the Molecular Zeeman Library (MZL) was used to compute Lande g-factors for FeH lines. We determined the distribution of magnetic fields by magnetic spectral synthesis performed with the SYNMAST code. We tested two different magnetic geometries to probe the influence of field orientation effects. Results. Our analysis confirms that FeH lines are excellent indicators of surface magnetic fields in low-mass stars of type M, particularly in comparison to profiles of Na I lines that are heavily affected by water lines and that suffer problems with continuum normalization. The field distributions in all four stars are characterized by three distinct groups of field components, and the data are consistent neither with a smooth distribution of different field strengths nor with one average field strength covering the full star. We find evidence of a subtle difference in the field distribution of GJ 285 compared to the other three targets. GJ 285 also has the highest average field of 3.5 kG and the strongest maximum field component of 7-7.5 kG. The maximum local field strengths in our sample seem to be correlated with rotation rate. While the average field strength is saturated, the maximum local field strengths in our sample show no evidence of saturation. Conclusions. We find no difference between the field distributions of partially and fully convective stars. The one star with evidence of field distribution different from the other three is the most active star (i.e. with X-ray luminosity and mean surface magnetic field) rotating relatively fast. A possible explanation is that rotation determines the distribution of surface magnetic fields, and that local field strengths grow with rotation even in stars in which the average field is already saturated."],["dc.identifier.doi","10.1051/0004-6361/201322136"],["dc.identifier.fs","609676"],["dc.identifier.isi","000333798000035"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10910"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/34081"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Exploring the magnetic field complexity in M dwarfs at the boundary to full convection"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A141"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","540"],["dc.contributor.author","Setiawan, J."],["dc.contributor.author","Roccatagliata, V."],["dc.contributor.author","Fedele, D."],["dc.contributor.author","Henning, T. H."],["dc.contributor.author","Pasquali, A."],["dc.contributor.author","Rodriguez-Ledesma, M. V."],["dc.contributor.author","Caffau, E."],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Klement, R. J."],["dc.date.accessioned","2018-11-07T09:11:28Z"],["dc.date.available","2018-11-07T09:11:28Z"],["dc.date.issued","2012"],["dc.description.abstract","Aims. We carried out a radial-velocity survey to search for planets around metal-poor stars. In this paper we report the discovery of two planets around HIP 11952, a metal-poor star with [Fe/H] = -1.9 that belongs to our target sample. Methods. Radial velocity variations of HIP 11952 were monitored systematically with FEROS at the 2.2 m telescope located at the ESO La Silla observatory from August 2009 until January 2011. We used a cross-correlation technique to measure the stellar radial velocities (RV). Results. We detected a long-period RV variation of 290 d and a short-period one of 6.95 d. The spectroscopic analysis of the stellar activity reveals a stellar rotation period of 4.8 d. The HIPPARCOS photometry data shows intra-day variabilities, which give evidence for stellar pulsations. Based on our analysis, the observed RV variations are most likely caused by the presence of unseen planetary companions. Assuming a primary mass of 0.83 M-circle dot, we computed minimum planetary masses of 0.78 M-Jup for the inner and 2.93 M-Jup for the outer planet. The semi-major axes are a(1) = 0.07 AU and a(2) = 0.81 AU, respectively. Conclusions. HIP 11952 is one of very few stars with [Fe/H] < -1.0 which have planetary companions. This discovery is important to understand planet formation around metal-poor stars."],["dc.identifier.doi","10.1051/0004-6361/201117826"],["dc.identifier.fs","596752"],["dc.identifier.isi","000303315400155"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9601"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/26728"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Planetary companions around the metal-poor star HIP 11952"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A150"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","646"],["dc.contributor.author","Otten, G. P. P. L."],["dc.contributor.author","Vigan, A."],["dc.contributor.author","Muslimov, E."],["dc.contributor.author","N’Diaye, M."],["dc.contributor.author","Choquet, E."],["dc.contributor.author","Seemann, U."],["dc.contributor.author","Dohlen, K."],["dc.contributor.author","Houllé, M."],["dc.contributor.author","Cristofari, P."],["dc.contributor.author","Phillips, M. W."],["dc.contributor.author","Charles, Y."],["dc.contributor.author","Baraffe, I."],["dc.contributor.author","Beuzit, J.-L."],["dc.contributor.author","Costille, A."],["dc.contributor.author","Dorn, R."],["dc.contributor.author","El Morsy, M."],["dc.contributor.author","Kasper, M."],["dc.contributor.author","Lopez, M."],["dc.contributor.author","Mordasini, C."],["dc.contributor.author","Pourcelot, R."],["dc.contributor.author","Reiners, A."],["dc.contributor.author","Sauvage, J.-F."],["dc.date.accessioned","2021-04-14T08:28:33Z"],["dc.date.available","2021-04-14T08:28:33Z"],["dc.date.issued","2021"],["dc.identifier.doi","10.1051/0004-6361/202038517"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/82643"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","Direct characterization of young giant exoplanets at high spectral resolution by coupling SPHERE and CRIRES+"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]