Giesers, Benjamin

[["dc.bibliographiccitation.firstpage","996"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","1007"],["dc.bibliographiccitation.volume","467"],["dc.contributor.author","Coleman, Gavin A. L."],["dc.contributor.author","Nelson, R. P."],["dc.contributor.author","Paardekooper, Sijme-Jan"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Anglada-Escude, Guillem"],["dc.date.accessioned","2018-11-07T10:24:46Z"],["dc.date.available","2018-11-07T10:24:46Z"],["dc.date.issued","2017"],["dc.description.abstract","We present a study of four different formation scenarios that may be able to explain the origin of the recently announced planet ('Proxima b') orbiting Proxima Centauri. The aim is to examine how the formation scenarios differ in their predictions for the multiplicity of the Proxima system, the water/volatile content of Proxima b and its orbital eccentricity, so that these can be tested by future observations. A scenario of in situ formation via giant impacts from a locally enhanced disc of planetary embryos/planetesimals predicts that Proxima b will be in a multiplanet system with a measurably finite eccentricity. Assuming that the local solid enhancement needed to form a Proxima b analogue arises because of the inwards drift of solids in the form of small planetesimals/boulders, this scenario also results in Proxima b analogues being only moderately endowed with water/volatiles. A scenario in which multiple embryos form, migrate and mutually collide within a gas disc results in Proxima b being a member of a multiple system, possibly displaying mean-motion resonances, but where the constituent members are Ocean planets due to accretion occurring mainly outside of the snowline. A scenario in which a single accreting embryo forms outside the snowline, and migrates inwards while accreting planetesimals/pebbles results in Proxima b being an isolated Ocean planet on a circular orbit. A scenario in which Proxima b formed via pebble accretion interior to the snowline produces a dry planet on a circular orbit. Future observations that characterize the physical and orbital properties of Proxima b, and any additional planets in the system, will provide valuable insights into the formation history of this neighbouring planetary system."],["dc.description.sponsorship","QMULResearch-IT; EPSRC grant [EP/K000128/1]"],["dc.identifier.doi","10.1093/mnras/stx169"],["dc.identifier.isi","000398418900070"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/42719"],["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","Exploring plausible formation scenarios for the planet candidate orbiting Proxima Centauri"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["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","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"]]

[["dc.bibliographiccitation.firstpage","4472"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","4480"],["dc.bibliographiccitation.volume","498"],["dc.contributor.author","Saracino, S"],["dc.contributor.author","Kamann, S"],["dc.contributor.author","Usher, C"],["dc.contributor.author","Bastian, N"],["dc.contributor.author","Martocchia, S"],["dc.contributor.author","Lardo, C"],["dc.contributor.author","Latour, M"],["dc.contributor.author","Cabrera-Ziri, I"],["dc.contributor.author","Dreizler, S"],["dc.contributor.author","Giesers, B"],["dc.contributor.author","Husser, T-O"],["dc.contributor.author","Kacharov, N"],["dc.contributor.author","Salaris, M"],["dc.date.accessioned","2021-04-14T08:31:37Z"],["dc.date.available","2021-04-14T08:31:37Z"],["dc.date.issued","2020"],["dc.identifier.doi","10.1093/mnras/staa2748"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/83657"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-399"],["dc.relation.eissn","1365-2966"],["dc.relation.issn","0035-8711"],["dc.title","Leveraging HST with MUSE – I. Sodium abundance variations within the 2-Gyr-old cluster NGC 1978"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","L15"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Monthly notices of the Royal Astronomical Society. Letters"],["dc.bibliographiccitation.lastpage","L19"],["dc.bibliographiccitation.volume","475"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Husser, Tim-Oliver"],["dc.contributor.author","Kamann, Sebastian"],["dc.contributor.author","Anglada Escudé, Guillem"],["dc.contributor.author","Brinchmann, Jarle"],["dc.contributor.author","Carollo, C Marcella"],["dc.contributor.author","Roth, Martin M"],["dc.contributor.author","Weilbacher, Peter M"],["dc.contributor.author","Wisotzki, Lutz"],["dc.date.accessioned","2020-12-10T18:19:23Z"],["dc.date.available","2020-12-10T18:19:23Z"],["dc.date.issued","2018"],["dc.identifier.doi","10.1093/mnrasl/slx203"],["dc.identifier.eissn","1745-3933"],["dc.identifier.issn","1745-3925"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/75230"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","A detached stellar-mass black hole candidate in the globular cluster NGC 3201"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","437"],["dc.bibliographiccitation.issue","7617"],["dc.bibliographiccitation.journal","Nature"],["dc.bibliographiccitation.lastpage","+"],["dc.bibliographiccitation.volume","536"],["dc.contributor.author","Anglada-Escude, Guillem"],["dc.contributor.author","Amado, Pedro J."],["dc.contributor.author","Barnes, John"],["dc.contributor.author","Berdinas, Zaira M."],["dc.contributor.author","Butler, R. Paul"],["dc.contributor.author","Coleman, Gavin A. L."],["dc.contributor.author","de la Cueva, Ignacio"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Endl, Michael"],["dc.contributor.author","Giesers, Benjamin"],["dc.contributor.author","Jeffers, Sandra V."],["dc.contributor.author","Jenkins, James S."],["dc.contributor.author","Jones, Hugh R. A."],["dc.contributor.author","Kiraga, Marcin"],["dc.contributor.author","Kuerster, Martin"],["dc.contributor.author","Lopez-Gonzalez, Maria J."],["dc.contributor.author","Marvin, Christopher J."],["dc.contributor.author","Morales, Nicolas"],["dc.contributor.author","Morin, Julien"],["dc.contributor.author","Nelson, Richard P."],["dc.contributor.author","Ortiz, Jose L."],["dc.contributor.author","Ofir, Aviv"],["dc.contributor.author","Paardekooper, Sijme-Jan"],["dc.contributor.author","Reiners, Ansgar"],["dc.contributor.author","Rodriguez, Eloy"],["dc.contributor.author","Rodriguez-Lopez, Cristina"],["dc.contributor.author","Sarmiento, Luis F."],["dc.contributor.author","Strachan, John P."],["dc.contributor.author","Tsapras, Yiannis"],["dc.contributor.author","Tuomi, Mikko"],["dc.contributor.author","Zechmeister, Mathias"],["dc.date.accessioned","2018-11-07T10:10:03Z"],["dc.date.available","2018-11-07T10:10:03Z"],["dc.date.issued","2016"],["dc.description.abstract","At a distance of 1.295 parsecs(1), the red dwarf Proxima Centauri (a Centauri C, GL 551, HIP 70890 or simply Proxima) is the Sun's closest stellar neighbour and one of the best-studied low-mass stars. It has an effective temperature of only around 3,050 kelvin, a luminosity of 0.15 per cent of that of the Sun, a measured radius of 14 per cent of the radius of the Sun2 and a mass of about 12 per cent of the mass of the Sun. Although Proxima is considered a moderately active star, its rotation period is about 83 days (ref. 3) and its quiescent activity levels and X-ray luminosity(4) are comparable to those of the Sun. Here we report observations that reveal the presence of a small planet with a minimum mass of about 1.3 Earth masses orbiting Proxima with a period of approximately 11.2 days at a semi-major-axis distance of around 0.05 astronomical units. Its equilibrium temperature is within the range where water could be liquid on its surface(5)."],["dc.identifier.doi","10.1038/nature19106"],["dc.identifier.isi","000382646600037"],["dc.identifier.pmid","27558064"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/39781"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Nature Publishing Group"],["dc.relation.issn","1476-4687"],["dc.relation.issn","0028-0836"],["dc.title","A terrestrial planet candidate in a temperate orbit around Proxima Centauri"],["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.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.firstpage","2177"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Monthly Notices of the Royal Astronomical Society"],["dc.bibliographiccitation.lastpage","2192"],["dc.bibliographiccitation.volume","492"],["dc.contributor.author","Kamann, S."],["dc.contributor.author","Bastian, N."],["dc.contributor.author","Gossage, S."],["dc.contributor.author","Baade, D."],["dc.contributor.author","Cabrera-Ziri, I."],["dc.contributor.author","Da Costa, G."],["dc.contributor.author","de Mink, S. E."],["dc.contributor.author","Georgy, C."],["dc.contributor.author","Giesers, B."],["dc.contributor.author","Göttgens, F."],["dc.contributor.author","Hilker, M."],["dc.contributor.author","Husser, T.-O."],["dc.contributor.author","Lardo, C."],["dc.contributor.author","Larsen, S. S."],["dc.contributor.author","Mackey, D."],["dc.contributor.author","Martocchia, S."],["dc.contributor.author","Mucciarelli, A."],["dc.contributor.author","Platais, I."],["dc.contributor.author","Roth, M. M."],["dc.contributor.author","Salaris, M."],["dc.contributor.author","Usher, C."],["dc.contributor.author","Yong, D."],["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/stz3583"],["dc.identifier.eissn","1365-2966"],["dc.identifier.issn","0035-8711"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/75285"],["dc.language.iso","en"],["dc.notes.intern","DOI Import GROB-354"],["dc.title","How stellar rotation shapes the colour−magnitude diagram of the massive intermediate-age star cluster NGC 1846"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dspace.entity.type","Publication"]]