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.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.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.artnumber","A148"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","588"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Wendt, Martin"],["dc.contributor.author","Wulff, Nina"],["dc.contributor.author","Bacon, Roland"],["dc.contributor.author","Wisotzki, Lutz"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Roth, Martin M."],["dc.contributor.author","Monreal-Ibero, Ana"],["dc.date.accessioned","2018-11-07T10:16:10Z"],["dc.date.available","2018-11-07T10:16:10Z"],["dc.date.issued","2016"],["dc.description.abstract","Aims. We demonstrate the high multiplex advantage of crowded field 3D spectroscopy with the new integral field spectrograph MUSE by means of a spectroscopic analysis of more than 12 000 individual stars in the globular cluster NGC 6397. Methods. The stars are deblended with a point spread function fitting technique, using a photometric reference catalogue from HST as prior, including relative positions and brightnesses. This catalogue is also used for a first analysis of the extracted spectra, followed by an automatic in-depth analysis via a full-spectrum fitting method based on a large grid of PHOENIX spectra. Results. We analysed the largest sample so far available for a single globular cluster of 18 932 spectra from 12 307 stars in NGC 6397. We derived a mean radial velocity of v(rad) = 17.84 +/- 0.07 km s(-1) and a mean metallicity of [Fe/H] = -2.120 +/- 0.002, with the latter seemingly varying with temperature for stars on the red giant branch (RGB). We determine Teff and [Fe/H] from the spectra, and log g from HST photometry. This is the first very comprehensive Hertzsprung-Russell diagram (HRD) for a globular cluster based on the analysis of several thousands of stellar spectra, ranging from the main sequence to the tip of the RGB. Furthermore, two interesting objects were identified; one is a post-AGB star and the other is a possible millisecond-pulsar companion."],["dc.description.sponsorship","BMBF Verbundforschung (project MUSE-AO) [05A14BAC, 05A14MGA]"],["dc.identifier.doi","10.1051/0004-6361/201526949"],["dc.identifier.isi","000373207800160"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/13436"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/40983"],["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 I. The first comprehensive HRD of a globular cluster"],["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","A98"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","587"],["dc.contributor.author","Wisotzki, Lutz"],["dc.contributor.author","Bacon, Roland"],["dc.contributor.author","Blaizot, J."],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Herenz, E. C."],["dc.contributor.author","Schaye, J."],["dc.contributor.author","Bouche, N."],["dc.contributor.author","Cantalupo, S."],["dc.contributor.author","Contini, Thierry"],["dc.contributor.author","Carollo, C. Marcella"],["dc.contributor.author","Caruana, Joseph"],["dc.contributor.author","Courbot, J.-B."],["dc.contributor.author","Emsellem, Eric"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Kerutt, J."],["dc.contributor.author","Leclercq, F."],["dc.contributor.author","Lilly, S. J."],["dc.contributor.author","Patricio, V."],["dc.contributor.author","Sandin, Christer"],["dc.contributor.author","Steinmetz, M."],["dc.contributor.author","Straka, L. A."],["dc.contributor.author","Urrutia, Tanya"],["dc.contributor.author","Verhamme, A."],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Wendt, M."],["dc.date.accessioned","2018-11-07T10:17:12Z"],["dc.date.available","2018-11-07T10:17:12Z"],["dc.date.issued","2016"],["dc.description.abstract","We report the detection of extended Ly alpha emission around individual star-forming galaxies at redshifts z = 3-6 in an ultradeep exposure of the Hubble Deep Field South obtained with MUSE on the ESO-VLT. The data reach a limiting surface brightness (1 sigma) of similar to 1 x 10(-19) erg s(-1) cm(-2) arcsec(-2) in azimuthally averaged radial profiles, an order of magnitude improvement over previous narrowband imaging. Our sample consists of 26 spectroscopically confirmed Ly alpha-emitting, but mostly continuum-faint (m(AB) greater than or similar to 27) galaxies. In most objects the Ly alpha emission is considerably more extended than the UV continuum light. While five of the faintest galaxies in the sample show no significantly detected Ly alpha haloes, the derived upper limits suggest that this is due to insufficient S/N. Ly alpha haloes therefore appear to be ubiquitous even for low-mass (similar to 10(8)-10(9) M-circle dot) star-forming galaxies at z > 3. We decompose the Ly alpha emission of each object into a compact component tracing the UV continuum and an extended halo component, and infer sizes and luminosities of the haloes. The extended Ly alpha emission approximately follows an exponential surface brightness distribution with a scale length of a few kpc. While these haloes are thus quite modest in terms of their absolute sizes, they are larger by a factor of 5-15 than the corresponding rest-frame UV continuum sources as seen by HST. They are also much more extended, by a factor similar to 5, than Ly alpha haloes around low-redshift star-forming galaxies. Between similar to 40% and greater than or similar to 90% of the observed Ly alpha flux comes from the extended halo component, with no obvious correlation of this fraction with either the absolute or the relative size of the Ly alpha halo. Our observations provide direct insights into the spatial distribution of at least partly neutral gas residing in the circumgalactic medium of low to intermediate mass galaxies at z > 3."],["dc.identifier.doi","10.1051/0004-6361/201527384"],["dc.identifier.isi","000371589800109"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/13433"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/41185"],["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/FP7/278594/EU//GASAROUNDGALAXIES"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/336736/EU//CALENDS"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Extended Lyman alpha haloes around individual high-redshift galaxies revealed by MUSE"],["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"]]