Kamann, Sebastian

[["dc.bibliographiccitation.firstpage","85"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","919"],["dc.contributor.affiliation","Braga, V. F.;"],["dc.contributor.affiliation","Crestani, J.;"],["dc.contributor.affiliation","Fabrizio, M.;"],["dc.contributor.affiliation","Bono, G.;"],["dc.contributor.affiliation","Sneden, C.;"],["dc.contributor.affiliation","Preston, G. W.;"],["dc.contributor.affiliation","Storm, J.;"],["dc.contributor.affiliation","Kamann, S.;"],["dc.contributor.affiliation","Latour, M.;"],["dc.contributor.affiliation","Lala, H.;"],["dc.contributor.affiliation","Lemasle, B.;"],["dc.contributor.affiliation","Prudil, Z.;"],["dc.contributor.affiliation","Altavilla, G.;"],["dc.contributor.affiliation","Chaboyer, B.;"],["dc.contributor.affiliation","Dall’Ora, M.;"],["dc.contributor.affiliation","Ferraro, I.;"],["dc.contributor.affiliation","Gilligan, C. K.;"],["dc.contributor.affiliation","Fiorentino, G.;"],["dc.contributor.affiliation","Iannicola, G.;"],["dc.contributor.affiliation","Inno, L.;"],["dc.contributor.affiliation","Kwak, S.;"],["dc.contributor.affiliation","Marengo, M.;"],["dc.contributor.affiliation","Marinoni, S.;"],["dc.contributor.affiliation","Marrese, P. M.;"],["dc.contributor.affiliation","Martínez-Vázquez, C. E.;"],["dc.contributor.affiliation","Monelli, M.;"],["dc.contributor.affiliation","Mullen, J. P.;"],["dc.contributor.affiliation","Matsunaga, N.;"],["dc.contributor.affiliation","Neeley, J.;"],["dc.contributor.affiliation","Stetson, P. B.;"],["dc.contributor.affiliation","Valenti, E.;"],["dc.contributor.affiliation","Zoccali, M.;"],["dc.contributor.author","Braga, V. F."],["dc.contributor.author","Crestani, J."],["dc.contributor.author","Fabrizio, M."],["dc.contributor.author","Bono, G."],["dc.contributor.author","Sneden, C."],["dc.contributor.author","Preston, G. W."],["dc.contributor.author","Storm, J."],["dc.contributor.author","Kamann, S."],["dc.contributor.author","Latour, M."],["dc.contributor.author","Lala, H."],["dc.contributor.author","Zoccali, M."],["dc.date.accessioned","2021-12-01T09:24:07Z"],["dc.date.available","2021-12-01T09:24:07Z"],["dc.date.issued","2021"],["dc.date.updated","2022-02-09T13:18:19Z"],["dc.description.abstract","AbstractWe collected the largest spectroscopic catalog of RR Lyrae (RRLs) including ≈20,000 high-, medium-, and low-resolution spectra for ≈10,000 RRLs. We provide the analytical forms of radial velocity curve (RVC) templates. These were built using 36 RRLs (31 fundamental—split into three period bins—and five first-overtone pulsators) with well-sampled RVCs based on three groups of metallic lines (Fe, Mg, Na) and four Balmer lines (H α , H β , H γ , H δ ). We tackled the long-standing problem of the reference epoch to anchor light-curve and RVC templates. For the V-band, we found that the residuals of the templates anchored to the phase of the mean magnitude along the rising branch are ∼35% to ∼45% smaller than those anchored to the phase of maximum light. For the RVC, we used two independent reference epochs for metallic and Balmer lines and we verified that the residuals of the RVC templates anchored to the phase of mean RV are from 30% (metallic lines) up to 45% (Balmer lines) smaller than those anchored to the phase of minimum RV. We validated our RVC templates by using both the single-point and the three phase point approaches. We found that barycentric velocities based on our RVC templates are two to three times more accurate than those available in the literature. We applied the current RVC templates to Balmer lines RVs of RRLs in the globular NGC 3201 collected with MUSE at VLT. We found the cluster barycentric RV of V γ = 496.89 ± 8.37(error) ± 3.43 (standard deviation) km s−1, which agrees well with literature estimates."],["dc.description.sponsorship","INAF SSDC"],["dc.identifier.doi","10.3847/1538-4357/ac1074"],["dc.identifier.eissn","1538-4357"],["dc.identifier.issn","0004-637X"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/94854"],["dc.language.iso","en"],["dc.notes.intern","DOI-Import GROB-478"],["dc.publisher","The American Astronomical Society"],["dc.relation.eissn","1538-4357"],["dc.relation.issn","0004-637X"],["dc.rights.uri","http://creativecommons.org/licenses/by/4.0/"],["dc.title","On the Use of Field RR Lyrae as Galactic Probes. V. Optical and Radial Velocity Curve Templates"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A149"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","588"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Husser, T.-O."],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Emsellem, Eric"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Wisotzki, Lutz"],["dc.contributor.author","Wendt, M."],["dc.contributor.author","Krajnovic, Davor"],["dc.contributor.author","Roth, M. M."],["dc.contributor.author","Bacon, Roland"],["dc.contributor.author","Dreizler, Stefan"],["dc.date.accessioned","2018-11-07T10:16:10Z"],["dc.date.available","2018-11-07T10:16:10Z"],["dc.date.issued","2016"],["dc.description.abstract","We present a detailed analysis of the kinematics of the Galactic globular cluster NGC 6397 based on more than similar to 18 000 spectra obtained with the novel integral field spectrograph MUSE. While NGC 6397 is often considered a core collapse cluster, our analysis suggests a flattening of the surface brightness profile at the smallest radii. Although it is among the nearest globular clusters, the low velocity dispersion of NGC 6397 of < 5 km s(-1) imposes heavy demands on the quality of the kinematical data. We show that despite its limited spectral resolution, MUSE reaches an accuracy of 1 km s(-1) in the analysis of stellar spectra. We find slight evidence for a rotational component in the cluster and the velocity dispersion profile that we obtain shows a mild central cusp. To investigate the nature of this feature, we calculate spherical Jeans models and compare these models to our kinematical data. This comparison shows that if a constant mass-to-light ratio is assumed, the addition of an intermediate-mass black hole with a mass of 600 M-circle dot brings the model predictions into agreement with our data, and therefore could be at the origin of the velocity dispersion profile. We further investigate cases with varying mass-to-light ratios and find that a compact dark stellar component can also explain our observations. However, such a component would closely resemble the black hole from the constant mass-to-light ratio models as this component must be confined to the central similar to 5 '' of the cluster and must have a similar mass. Independent constraints on the distribution of stellar remnants in the cluster or kinematic measurements at the highest possible spatial resolution should be able to distinguish the two alternatives."],["dc.identifier.doi","10.1051/0004-6361/201527065"],["dc.identifier.isi","000373207800161"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/13437"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/40984"],["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","MUSE crowded field 3D spectroscopy of over 12 000 stars in the globular cluster NGC 6397"],["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","A133"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","607"],["dc.contributor.author","Wendt, Martin"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Monreal-Ibero, Ana"],["dc.contributor.author","Richter, Philipp"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Wisotzki, Lutz"],["dc.date.accessioned","2020-12-10T18:11:34Z"],["dc.date.available","2020-12-10T18:11:34Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.1051/0004-6361/201629816"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74062"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Mapping diffuse interstellar bands in the local ISM on small scales via MUSE 3D spectroscopy"],["dc.title.alternative","A pilot study based on globular cluster NGC 6397"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","3090"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","3100"],["dc.bibliographiccitation.volume","464"],["dc.contributor.author","Askar, Abbas"],["dc.contributor.author","Bianchini, Paolo"],["dc.contributor.author","de Vita, Ruggero"],["dc.contributor.author","Giersz, Mirek"],["dc.contributor.author","Hypki, Arkadiusz"],["dc.contributor.author","Kamann, Sebastian"],["dc.date.accessioned","2018-11-07T10:29:09Z"],["dc.date.available","2018-11-07T10:29:09Z"],["dc.date.issued","2017"],["dc.description.abstract","We describe the dynamical evolution of a unique type of dark star cluster model in which the majority of the cluster mass at Hubble time is dominated by an intermediate-mass black hole (IMBH). We analysed results from about 2000 star cluster models (Survey Database I) simulated using the Monte Carlo code MOnte Carlo Cluster simulAtor and identified these dark star cluster models. Taking one of these models, we apply the method of simulating realistic ` mock observations' by utilizing the Cluster simulatiOn Comparison with ObservAtions (COCOA) and Simulating Stellar Cluster Observation (SISCO) codes to obtain the photometric and kinematic observational properties of the dark star cluster model at 12 Gyr. We find that the perplexing Galactic globular cluster NGC6535 closely matches the observational photometric and kinematic properties of the dark star cluster model presented in this paper. Based on our analysis and currently observed properties of NGC6535, we suggest that this globular cluster could potentially harbour an IMBH. If it exists, the presence of this IMBH can be detected robustly with proposed kinematic observations of NGC6535."],["dc.identifier.doi","10.1093/mnras/stw2573"],["dc.identifier.isi","000393647600046"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43583"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","PUB_WoS_Import"],["dc.publisher","Oxford Univ Press"],["dc.relation.issn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","MOCCA-SURVEY Database I: Is NGC 6535 a dark star cluster harbouring an IMBH?"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","618"],["dc.contributor.author","Roth, Martin M."],["dc.contributor.author","Sandin, Christer"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Monreal-Ibero, Ana"],["dc.contributor.author","Bacon, Roland"],["dc.contributor.author","den Brok, Mark"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Kelz, Andreas"],["dc.contributor.author","Marino, Raffaella Anna"],["dc.contributor.author","Steinmetz, Matthias"],["dc.date.accessioned","2020-12-10T18:11:40Z"],["dc.date.available","2020-12-10T18:11:40Z"],["dc.date.issued","2018"],["dc.identifier.doi","10.1051/0004-6361/201833007"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74101"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","MUSE crowded field 3D spectroscopy in NGC 300"],["dc.title.alternative","I. First results from central fields"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1689"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","1695"],["dc.bibliographiccitation.volume","480"],["dc.contributor.author","Kamann, S"],["dc.contributor.author","Bastian, N"],["dc.contributor.author","Husser, T-O"],["dc.contributor.author","Martocchia, S"],["dc.contributor.author","Usher, C"],["dc.contributor.author","den Brok, M"],["dc.contributor.author","Dreizler, S"],["dc.contributor.author","Kelz, A"],["dc.contributor.author","Krajnović, D"],["dc.contributor.author","Richard, J"],["dc.contributor.author","Steinmetz, M"],["dc.contributor.author","Weilbacher, P M"],["dc.date.accessioned","2020-12-10T18:19:29Z"],["dc.date.available","2020-12-10T18:19:29Z"],["dc.date.issued","2018"],["dc.identifier.doi","10.1093/mnras/sty1958"],["dc.identifier.eissn","1365-2966"],["dc.identifier.issn","0035-8711"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/75266"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Cluster kinematics and stellar rotation in NGC 419 with MUSE and adaptive optics"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","4788"],["dc.bibliographiccitation.issue","4"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","4803"],["dc.bibliographiccitation.volume","507"],["dc.contributor.author","Göttgens, Fabian"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Baumgardt, Holger"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","den Brok, Mark"],["dc.contributor.author","Fétick, Romain"],["dc.contributor.author","Krajnovic, Davor"],["dc.contributor.author","Weilbacher, Peter M"],["dc.date.accessioned","2021-12-01T09:23:51Z"],["dc.date.available","2021-12-01T09:23:51Z"],["dc.date.issued","2021"],["dc.description.abstract","ABSTRACT We use spectra observed with the integral-field spectrograph Multi Unit Spectroscopic Explorer (MUSE) to reveal the central kinematics of the Galactic globular cluster Messier 80 (M80, NGC 6093). Using observations obtained with the recently commissioned narrow-field mode of MUSE, we are able to analyse 932 stars in the central 7.5 arcsec by 7.5 arcsec of the cluster for which no useful spectra previously existed. Mean radial velocities of individual stars derived from the spectra are compared to predictions from axisymmetric Jeans models, resulting in radial profiles of the velocity dispersion, the rotation amplitude, and the mass-to-light ratio. The new data allow us to search for an intermediate-mass black hole (IMBH) in the centre of the cluster. Our Jeans model finds two similarly probable solutions around different dynamical cluster centres. The first solution has a centre close to the photometric estimates available in the literature and does not need an IMBH to fit the observed kinematics. The second solution contains a location of the cluster centre that is offset by about 2.4 arcsec from the first one and it needs an IMBH mass of 600^{+1700}_{-1400}~\\text{M}_\\odot {}$. N-body models support the existence of an IMBH in this cluster with a mass of up to 6000 M⊙ in this cluster, although models without an IMBH provide a better fit to the observed surface brightness profile. They further indicate that the cluster has lost nearly all stellar-mass black holes. We further discuss the detection of two potential high-velocity stars with radial velocities of 80–90 $\\text{km}\\, \\text{s}^{-1}$ relative to the cluster mean."],["dc.description.abstract","ABSTRACT We use spectra observed with the integral-field spectrograph Multi Unit Spectroscopic Explorer (MUSE) to reveal the central kinematics of the Galactic globular cluster Messier 80 (M80, NGC 6093). Using observations obtained with the recently commissioned narrow-field mode of MUSE, we are able to analyse 932 stars in the central 7.5 arcsec by 7.5 arcsec of the cluster for which no useful spectra previously existed. Mean radial velocities of individual stars derived from the spectra are compared to predictions from axisymmetric Jeans models, resulting in radial profiles of the velocity dispersion, the rotation amplitude, and the mass-to-light ratio. The new data allow us to search for an intermediate-mass black hole (IMBH) in the centre of the cluster. Our Jeans model finds two similarly probable solutions around different dynamical cluster centres. The first solution has a centre close to the photometric estimates available in the literature and does not need an IMBH to fit the observed kinematics. The second solution contains a location of the cluster centre that is offset by about 2.4 arcsec from the first one and it needs an IMBH mass of 600^{+1700}_{-1400}~\\text{M}_\\odot {}$. N-body models support the existence of an IMBH in this cluster with a mass of up to 6000 M⊙ in this cluster, although models without an IMBH provide a better fit to the observed surface brightness profile. They further indicate that the cluster has lost nearly all stellar-mass black holes. We further discuss the detection of two potential high-velocity stars with radial velocities of 80–90 $\\text{km}\\, \\text{s}^{-1}$ relative to the cluster mean."],["dc.identifier.doi","10.1093/mnras/stab2449"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/94772"],["dc.language.iso","en"],["dc.notes.intern","DOI-Import GROB-478"],["dc.relation.eissn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.rights.uri","https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model"],["dc.title","Central kinematics of the Galactic globular cluster M80"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A117"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","658"],["dc.contributor.author","González-Torà, G."],["dc.contributor.author","Urbaneja, M. A."],["dc.contributor.author","Przybilla, N."],["dc.contributor.author","Dreizler, S."],["dc.contributor.author","Roth, M. M."],["dc.contributor.author","Kamann, S."],["dc.contributor.author","Castro, N."],["dc.date.accessioned","2022-04-01T10:02:43Z"],["dc.date.available","2022-04-01T10:02:43Z"],["dc.date.issued","2022"],["dc.description.abstract","Aims. A quantitative spectral analysis of BA-type supergiants and bright giants in an inner spiral arm region of the nearby spiral galaxy NGC 300 is presented, based on observations with the Multi Unit Spectroscopic Explorer (MUSE) on the European Southern Obsevatory, Very Large Telescope. The flux-weighted gravity–luminosity relationship (FGLR), a stellar spectroscopic distance determination method for galaxies, is extended towards stars at lower luminosities. Methods. Point spread function fitting 3D spectroscopy was performed with PampelMUSE on the datacube. The 16 stars with the highest signal-to-noise ratios are classified with regard to their spectral type and luminosity class using Galactic templates. They were analysed using hybrid non-local thermodynamic equilibrium model spectra to fit the strongest observed hydrogen, helium, and metal lines in the intermediate-resolution spectra. Supplemented by photometric data, this facilitates fundamental stellar parameters and interstellar reddening which have yet to be determined. Results. Effective temperatures, surface gravities, reddening E ( B − V ), bolometric magnitudes and luminosities, as well as radii and masses are presented for the sample stars. The majority of the objects follow the FGLR as established from more luminous BA-type supergiants in NGC 300. An increase in the scatter in the flux-weighted gravity–luminosity plane is observed at these lower luminosities, which is in line with predictions from population synthesis models."],["dc.identifier.doi","10.1051/0004-6361/202142372"],["dc.identifier.pii","aa42372-21"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/105989"],["dc.notes.intern","DOI-Import GROB-530"],["dc.relation.eissn","1432-0746"],["dc.relation.issn","0004-6361"],["dc.title","MUSE crowded field 3D spectroscopy in NGC 300"],["dc.title.alternative","II. Quantitative spectroscopy of BA-type supergiants"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A75"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","575"],["dc.contributor.author","Bacon, Roland"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Richard, Johan"],["dc.contributor.author","Contini, Thierry"],["dc.contributor.author","Drake, A."],["dc.contributor.author","Franx, M."],["dc.contributor.author","Tacchella, S."],["dc.contributor.author","Vernet, J."],["dc.contributor.author","Wisotzki, Lutz"],["dc.contributor.author","Blaizot, J."],["dc.contributor.author","Bouche, N."],["dc.contributor.author","Bouwens, R."],["dc.contributor.author","Cantalupo, S."],["dc.contributor.author","Carollo, C. Marcella"],["dc.contributor.author","Carton, D."],["dc.contributor.author","Caruana, Joseph"],["dc.contributor.author","Clement, B."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Epinat, Benoit"],["dc.contributor.author","Guiderdoni, B."],["dc.contributor.author","Herenz, E. C."],["dc.contributor.author","Husser, T.-O."],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Kerutt, J."],["dc.contributor.author","Kollatschny, Wolfram"],["dc.contributor.author","Krajnovic, Davor"],["dc.contributor.author","Lilly, S."],["dc.contributor.author","Martinsson, Thomas"],["dc.contributor.author","Michel-Dansac, L."],["dc.contributor.author","Patricio, V."],["dc.contributor.author","Schaye, J."],["dc.contributor.author","Shirazi, Maryam"],["dc.contributor.author","Soto, K."],["dc.contributor.author","Soucail, G."],["dc.contributor.author","Steinmetz, M."],["dc.contributor.author","Urrutia, Tanya"],["dc.contributor.author","Weilbacher, P."],["dc.contributor.author","de Zeeuw, T."],["dc.date.accessioned","2018-11-07T10:00:22Z"],["dc.date.available","2018-11-07T10:00:22Z"],["dc.date.issued","2015"],["dc.description.abstract","We observed Hubble Deep Field South with the new panoramic integral-field spectrograph MUSE that we built and have just commissioned at the VLT. The data cube resulting from 27 h of integration covers one arcmin(2) field of view at an unprecedented depth with a 1 sigma emission-line surface brightness limit of 1 x 10(-19) erg s(-1) cm(-2) arcsec(-2), and contains similar to 90 000 spectra. We present the combined and calibrated data cube, and we performed a first-pass analysis of the sources detected in the Hubble Deep Field South imaging. We measured the redshifts of 189 sources up to a magnitude I-814 = 29.5, increasing the number of known spectroscopic redshifts in this field by more than an order of magnitude. We also discovered 26 Ly alpha emitting galaxies that are not detected in the HST WFPC2 deep broad-band images. The intermediate spectral resolution of 2.3 angstrom allows us to separate resolved asymmetric Ly alpha emitters, [O II] 3727 emitters, and C III] 1908 emitters, and the broad instantaneous wavelength range of 4500 angstrom helps to identify single emission lines, such as [O III] 5007, H beta, and H alpha, over a very wide redshift range. We also show how the three-dimensional information of MUSE helps to resolve sources that are confused at ground-based image quality. Overall, secure identifications are provided for 83% of the 227 emission line sources detected in the MUSE data cube and for 32% of the 586 sources identified in the HST catalogue. The overall redshift distribution is fairly flat to z = 6.3, with a reduction between z = 1.5 to 2.9, in the well-known redshift desert. The field of view of MUSE also allowed us to detect 17 groups within the field. We checked that the number counts of [O II] 3727 and Ly alpha emitters are roughly consistent with predictions from the literature. Using two examples, we demonstrate that MUSE is able to provide exquisite spatially resolved spectroscopic information on the intermediate-redshift galaxies present in the field. This unique data set can be used for a wide range of follow-up studies. We release the data cube, the associated products, and the source catalogue with redshifts, spectra, and emission-line fluxes."],["dc.identifier.doi","10.1051/0004-6361/201425419"],["dc.identifier.isi","000350249100075"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/12400"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/37789"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/339659/EU//MUSICOS"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/336736/EU//CALENDS"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","The MUSE 3D view of the Hubble Deep Field South"],["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.firstpage","966"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","977"],["dc.bibliographiccitation.volume","492"],["dc.contributor.author","Kamann, S"],["dc.contributor.author","Dalessandro, E"],["dc.contributor.author","Bastian, N"],["dc.contributor.author","Brinchmann, J"],["dc.contributor.author","den Brok, M"],["dc.contributor.author","Dreizler, S"],["dc.contributor.author","Giesers, B"],["dc.contributor.author","Göttgens, F"],["dc.contributor.author","Husser, T-O"],["dc.contributor.author","Krajnović, D"],["dc.contributor.author","van de Ven, G"],["dc.contributor.author","Watkins, L L"],["dc.contributor.author","Wisotzki, L"],["dc.date.accessioned","2020-12-10T18:19:32Z"],["dc.date.available","2020-12-10T18:19:32Z"],["dc.date.issued","2019"],["dc.identifier.doi","10.1093/mnras/stz3506"],["dc.identifier.eissn","1365-2966"],["dc.identifier.issn","0035-8711"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/75284"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","The peculiar kinematics of the multiple populations in the globular cluster Messier 80 (NGC 6093)"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]