Kamann, Sebastian

[["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","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","2"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","18"],["dc.bibliographiccitation.volume","452"],["dc.contributor.author","Krajnovic, Davor"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Urrutia, Tanya"],["dc.contributor.author","Emsellem, Eric"],["dc.contributor.author","Carollo, C. Marcella"],["dc.contributor.author","Shirazi, Maryam"],["dc.contributor.author","Bacon, Roland"],["dc.contributor.author","Contini, Thierry"],["dc.contributor.author","Epinat, Benoit"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Martinsson, Thomas"],["dc.contributor.author","Steinmetz, Matthias"],["dc.date.accessioned","2018-11-07T09:52:33Z"],["dc.date.available","2018-11-07T09:52:33Z"],["dc.date.issued","2015"],["dc.description.abstract","Multi-Unit Spectroscopic Explorer (MUSE) observations of NGC 5813 reveal a complex structure in the velocity dispersion map, previously hinted at by SAURON observations. The structure is reminiscent of velocity dispersion maps of galaxies comprising two counter-rotating discs, and might explain the existence of the kinematically distinct core (KDC). Further evidence for two counter-rotating components comes from the analysis of the higher moments of the stellar line-of-sight velocity distributions and fitting MUSE spectra with two separate Gaussian line-of-sight velocity distributions. The emission-line kinematics show evidence of being linked to the present cooling flows and the buoyant cavities seen in X-rays. We detect ionized gas in a nuclear disc-like structure, oriented like the KDC, which is, however, not directly related to the KDC. We build an axisymmetric Schwarzschild dynamical model, which shows that the MUSE kinematics can be reproduced well with two counter-rotating orbit families, characterized by relatively low angular momentum components, but clearly separated in integral phase space and with radially varying contributions. The model indicates that the counter-rotating components in NGC 5813 are not thin discs, but dynamically hot structures. Our findings give further evidence that KDCs in massive galaxies should not necessarily be considered as structurally or dynamically decoupled regions, but as the outcomes of the mixing of different orbital families, where the balance in the distribution of mass of the orbital families is crucial. We discuss the formation of the KDC in NGC 5813 within the framework of gas accretion, binary mergers and formation of turbulent thick discs from cold streams at high redshift."],["dc.identifier.doi","10.1093/mnras/stv958"],["dc.identifier.isi","000360851100001"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/36151"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Oxford Univ Press"],["dc.relation.issn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","Unveiling the counter-rotating nature of the kinematically distinct core in NGC 5813 with MUSE"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A118"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","631"],["dc.contributor.author","Göttgens, Fabian"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Kollatschny, Wolfram"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Roth, Martin M."],["dc.contributor.author","Wendt, Martin"],["dc.date.accessioned","2020-12-10T18:11:53Z"],["dc.date.available","2020-12-10T18:11:53Z"],["dc.date.issued","2019"],["dc.identifier.doi","10.1051/0004-6361/201936485"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74170"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","A stellar census in globular clusters with MUSE: A spectral catalogue of emission-line sources"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","L3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","576"],["dc.contributor.author","Monreal-Ibero, Ana"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Wendt, M."],["dc.contributor.author","Selman, Fernando"],["dc.contributor.author","Lallement, R."],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Sandin, Christer"],["dc.date.accessioned","2018-11-07T09:58:46Z"],["dc.date.available","2018-11-07T09:58:46Z"],["dc.date.issued","2015"],["dc.description.abstract","Context. Diffuse interstellar bands (DIBs) are non-stellar weak absorption features of unknown origin found in the spectra of stars viewed through one or several clouds of the interstellar medium (ISM). Research of DIBs outside the Milky Way is currently very limited. In particular, spatially resolved investigations of DIBs outside of the Local Group are, to our knowledge, inexistent. Aims. In this contribution, we explore the capability of the high-sensitivity integral field spectrograph, MUSE, as a tool for mapping diffuse interstellar bands at distances larger than 100 Mpc. Methods. We used MUSE commissioning data for AM1353-272 B, the member with the highest extinction of the Dentist's Chair, an interacting system of two spiral galaxies. High signal-to-noise spectra were created by co-adding the signal of many spatial elements distributed in a geometry of concentric elliptical half-rings. Results. We derived decreasing radial profiles for the equivalent width of the lambda 5780.5 DIB both in the receding and approaching side of the companion galaxy up to distances of similar to 4.6 kpc from the centre of the galaxy. The interstellar extinction as derived from the Ha/H beta line ratio displays a similar trend, with decreasing values towards the external parts. This translates into an intrinsic correlation between the strength of the DIB and the extinction within AM1353-272 B, consistent with the currently existing global trend between these quantities when using measurements for Galactic and extragalactic sightlines. Conclusions. It seems feasible to map the DIB strength in the Local Universe, which has up to now only been performed for the Milky Way. This offers a new approach to studying the relationship between DIBs and other characteristics and species of the ISM in addition to using galaxies in the Local Group or sightlines towards very bright targets outside the Local Group."],["dc.identifier.doi","10.1051/0004-6361/201525854"],["dc.identifier.isi","000357274600074"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/12399"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/37437"],["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.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Towards DIB mapping in galaxies beyond 100 Mpc A radial profile of the lambda 5780.5 diffuse interstellar band in AM1353-272 B"],["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","A114"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","635"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Latour, Marilyn"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Göttgens, Fabian"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Roth, Martin M."],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Wendt, Martin"],["dc.date.accessioned","2020-12-10T18:11:53Z"],["dc.date.available","2020-12-10T18:11:53Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1051/0004-6361/201936508"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74171"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","A stellar census in globular clusters with MUSE"],["dc.title.alternative","Extending the CaT-metallicity relation below the horizontal branch and applying it to multiple populations"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","A3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","632"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Askar, Abbas"],["dc.contributor.author","Göttgens, Fabian"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Latour, Marilyn"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Wendt, Martin"],["dc.contributor.author","Roth, Martin M."],["dc.date.accessioned","2020-04-06T07:44:40Z"],["dc.date.available","2020-04-06T07:44:40Z"],["dc.date.issued","2019-09-09"],["dc.description.abstract","We utilize multi-epoch MUSE spectroscopy to study binaries in the core of NGC 3201. Our sample consists of 3553 stars with 54883 spectra in total comprising 3200 main-sequence stars up to 4 magnitudes below the turn-off. Each star in our sample has between 3 and 63 (with a median of 14) reliable radial velocity (RV) measurements within five years of observations. We introduce a statistical method to determine the probability of a star showing RV variations based on the whole inhomogeneous RV sample. Using HST photometry and an advanced dynamical MOCCA simulation of this specific GC we overcome observational biases that previous spectroscopic studies had to deal with. This allows us to infer a binary frequency in the MUSE FoV and enables us to deduce the underlying true binary frequency of (6.75+-0.72) % in NGC 3201. The comparison of the MUSE observations with the MOCCA simulation suggests a significant fraction of primordial binaries. We can also confirm a radial increase of the binary fraction towards the GC centre due to mass segregation. We discovered that in our sample at least (57.5+-7.9) % of blue straggler stars (BSS) are in a binary system. For the first time in a study of GCs, we were able to fit Keplerian orbits to a significant sample of 95 binaries. We present the binary system properties of eleven BSS and show evidence that two BSS formation scenarios, the mass transfer in binary (or triple) star systems and the coalescence due to binary-binary interactions, are present in our data. We also describe the binary and spectroscopic properties of four sub-subgiant (or red straggler) stars. Furthermore, we discovered two new black hole (BH) candidates with minimum masses (Msini) of (7.68+-0.50) M_sun, (4.4+-2.8) M_sun, and refine the minimum mass estimate on the already published BH to (4.53+-0.21) M_sun. These BHs are consistent with an extensive BH subsystem hosted by NGC 3201."],["dc.identifier.arxiv","1909.04050v1"],["dc.identifier.doi","10.1051/0004-6361/201936203"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/63782"],["dc.relation.issn","0004-6361"],["dc.relation.issn","1432-0746"],["dc.title","A stellar census in globular clusters with MUSE: Binaries in NGC 3201"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A114"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","582"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Monreal-Ibero, Ana"],["dc.contributor.author","Kollatschny, Wolfram"],["dc.contributor.author","Ginsburg, Adam"],["dc.contributor.author","McLeod, Anna F."],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Sandin, Christer"],["dc.contributor.author","Palsa, Ralf"],["dc.contributor.author","Wisotzki, Lutz"],["dc.contributor.author","Bacon, Roland"],["dc.contributor.author","Selman, Fernando"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Caruana, Joseph"],["dc.contributor.author","Kelz, Andreas"],["dc.contributor.author","Martinsson, Thomas"],["dc.contributor.author","Pecontal-Rousset, Arlette"],["dc.contributor.author","Richard, Johan"],["dc.contributor.author","Wendt, Martin"],["dc.date.accessioned","2018-11-07T09:50:33Z"],["dc.date.available","2018-11-07T09:50:33Z"],["dc.date.issued","2015"],["dc.description.abstract","We present a new integral field spectroscopic dataset of the central part of the Orion Nebula (M 42), observed with the MUSE instrument at the ESO VLT. We reduced the data with the public MUSE pipeline. The output products are two FITS cubes with a spatial size of similar to 5'9 x 4'9 (corresponding to similar to 0.76 x 0.63 pc(2)) and a contiguous wavelength coverage of 4595 ... 9366 angstrom, spatially sampled at 0 '.2. We provide two versions with a sampling of 1.25 angstrom and 0.85 angstrom in dispersion direction. Together with variance cubes these files have a size of 75 and 110 GiB on disk. They are the largest integral field mosaics to date in terms of information content. We make them available for use in the community. To validate this dataset, we compare world coordinates, reconstructed magnitudes, velocities, and absolute and relative emission line fluxes to the literature values and find excellent agreement. We derive a 2D map of extinction and present de-reddened flux maps of several individual emission lines and of diagnostic line ratios. We estimate physical properties of the Orion Nebula, using the emission line ratios [N II] and [S III] (for the electron temperature T-e) and [S II] and [Cl III] (for the electron density N-e), and show 2D images of the velocity measured from several bright emission lines."],["dc.identifier.doi","10.1051/0004-6361/201526529"],["dc.identifier.isi","000363538500114"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/12401"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/35728"],["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.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","A MUSE map of the central Orion Nebula (M 42)"],["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","A69"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","626"],["dc.contributor.author","Göttgens, Fabian"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Roth, Martin M."],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Kollatschny, Wolfram"],["dc.contributor.author","Monreal-Ibero, Ana"],["dc.contributor.author","Schmidt, Kasper B."],["dc.contributor.author","Wendt, Martin"],["dc.contributor.author","Wisotzki, Lutz"],["dc.contributor.author","Bacon, Roland"],["dc.date.accessioned","2020-12-10T18:11:48Z"],["dc.date.available","2020-12-10T18:11:48Z"],["dc.date.issued","2019"],["dc.identifier.doi","10.1051/0004-6361/201935221"],["dc.identifier.eissn","1432-0746"],["dc.identifier.issn","0004-6361"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/74144"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","Discovery of an old nova remnant in the Galactic globular cluster M 22"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]