Reinsch, Klaus

[["dc.bibliographiccitation.firstpage","671"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","681"],["dc.bibliographiccitation.volume","451"],["dc.contributor.author","Euchner, F."],["dc.contributor.author","Jordan, S."],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Gansicke, B. T."],["dc.date.accessioned","2018-11-07T09:50:53Z"],["dc.date.available","2018-11-07T09:50:53Z"],["dc.date.issued","2006"],["dc.description.abstract","Aims. We analyse the magnetic field geometry of the magnetic DA white dwarf PG1015+014 with our Zeeman tomography method. Methods. This study is based on rotation-phase resolved optical flux and circular polarization spectra of PG1015+014 obtained with FORS1 at the ESO VLT. Our tomographic code makes use of an extensive database of pre-computed Zeeman spectra. The general approach has been described in Papers I and II of this series. Results. The surface field strength distributions for all rotational phases of PG1015+014 are characterised by a strong peak at 70 MG. A separate peak at 80MG is seen for about one third of the rotation cycle. Significant contributions to the Zeeman features arise from regions with field strengths between 50 and 90 MG. We obtain equally good simultaneous fits to the observations, collected in five phase bins, for two different field parametrizations: (i) a superposition of individually tilted and off-centred zonal multipole components; and (ii) a truncated multipole expansion up to degree l = 4 including all zonal and tesseral components. The magnetic fields generated by both parametrizations exhibit a similar global structure of the absolute surface field values, but differ considerably in the topology of the field lines. An effective photospheric temperature of T-eff = 10 000 +/- 1000 K was found. Conclusions. Remaining discrepancies between the observations and our best-fit models suggest that additional small-scale structure of the magnetic field exists which our field models are unable to cover due to the restricted number of free parameters."],["dc.identifier.doi","10.1051/0004-6361:20064840"],["dc.identifier.fs","45028"],["dc.identifier.isi","237272100027"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9385"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/35801"],["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","Zeeman tomography of magnetic white dwarfs - III. The 70-80 Megagauss magnetic field of PG1015+014"],["dc.title.original","9385"],["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","771"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","776"],["dc.bibliographiccitation.volume","481"],["dc.contributor.author","Beuermann, K."],["dc.contributor.author","El Kholy, E."],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2019-07-09T11:55:00Z"],["dc.date.available","2019-07-09T11:55:00Z"],["dc.date.issued","2008-04-03"],["dc.description.abstract","Context. Polars (AM Herculis binaries) are a prominent class of bright soft X-ray sources, many of which were discovered with ROSAT. Aims. We present a homogenous analysis of all the pointed ROSAT PSPC observations of polars subdivided into two papers that discuss the prototype polar AM Her in detail and summarize the class properties of all other polars. Methods. We derive the high-state soft X-ray flux and short-term spectral variability of AM Her using a new detector response matrix and a confirmed flux calibration of the ROSAT PSPC below 0.28 keV. Results. The best-fit mean single-blackbody temperature and integrated bright-phase energy flux of AM Her in its April 1991 high state are 7.2\\pm1.0$ eV and \\times 10^{-9}$ erg cm-2 s-1, respectively. The total blackbody flux of a multi-temperature model that fits both the soft X-ray and the fluctuating far-ultraviolet components is \\mathrm{bb}=(4.5\\pm1.5)\\times 10^{-9}$ erg cm-2 s-1. The total accretion luminosity at a distance of 80 pc, \\mathrm{bb}=(2.1\\pm0.7)\\times 10^{33}$ erg s-1, implies an accretion rate of $\\dot M=(2.4\\pm0.8)\\times 10^{-10}$ \\odot\\,\\mathrm{yr}^{-1}$ for an 0.78 \\odot$ white dwarf. The soft X-ray flux displays significant variability on time scales down to 200 ms. Correlated spectral and count-rate variations are seen in flares on time scales down to 1 s, demonstrating the heating and cooling associated with individual accretion events. Conclusions. Our spectral and temporal analysis provides direct evidence for the blobby accretion model and suggests a connection between the soft X-ray and the fluctuating far-ultraviolet components."],["dc.identifier.doi","10.1051/0004-6361:20079335"],["dc.identifier.fs","513461"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9948"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60777"],["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","Soft X-ray spectral variability of AM Herculis"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","651"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","660"],["dc.bibliographiccitation.volume","442"],["dc.contributor.author","Euchner, F."],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Jordan, S."],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Gansicke, B. T."],["dc.date.accessioned","2018-11-07T10:54:29Z"],["dc.date.available","2018-11-07T10:54:29Z"],["dc.date.issued","2005"],["dc.description.abstract","We report time-resolved optical flux and circular polarization spectroscopy of the magnetic DA white dwarf HE 1045- 0908 obtained with FORS1 at the ESO VLT. Considering published results, we estimate a likely rotational period of P-rot similar or equal to 2.7 h, but cannot exclude values as high as about 9 h. Our detailed Zeeman tomographic analysis reveals a field structure which is dominated by a quadrupole and contains additional dipole and octupole contributions, and which does not depend strongly on the assumed value of the period. A good fit to the Zeeman flux and polarization spectra is obtained if all field components are centred and inclinations of their magnetic axes with respect to each other are allowed for. The fit can be slightly improved if an offset from the centre of the star is included. The prevailing surface field strength is 16 MG, but values between 10 and similar to 75 MG do occur. We derive an effective photospheric temperature of HE 1045- 0908 of T-eff = 10 000 +/- 1000 K. The tomographic code makes use of an extensive database of pre-computed Zeeman spectra ( Paper I)."],["dc.identifier.doi","10.1051/0004-6361:20053038"],["dc.identifier.isi","232404400032"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9389"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/49572"],["dc.notes.intern","In goescholar not merged with http://resolver.sub.uni-goettingen.de/purl?gs-1/9853 but duplicate"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.rights","Goescholar"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","Zeeman tomography of magnetic white dwarfs - II. The quadrupole-dominated magnetic field of HE 1045-0908"],["dc.title.original","9389"],["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","199"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","212"],["dc.bibliographiccitation.volume","480"],["dc.contributor.author","Beuermann, K."],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2019-07-09T11:54:35Z"],["dc.date.available","2019-07-09T11:54:35Z"],["dc.date.issued","2008"],["dc.description.abstract","Context. EXHya is one of the few double-lined eclipsing cataclysmic variables that allow an accurate measurement of the binary masses. Aims. We analyze orbital phase-resolved UVES/VLT high resolution (λ/Δλ 27 000) spectroscopic observations of EXHya with the aims of deriving the binary masses and obtaining a tomographic image of the illuminated secondary star. Methods. We present a novel method for determining the binary parameters by directly fitting an emission model of the illuminated secondary star to the phase-resolved line profiles of NaIλ8183/8195 in absorption and emission and CaIIλ8498 in emission. Results. The fit to the NaI and CaII line profiles, combined with the published K1, yields a white-dwarf mass M1 = 0.790 ± 0.026 M , a secondary mass M2 = 0.108 ± 0.008 M , and a velocity amplitude of the secondary star K2 = 432.4 ± 4.8 kms−1. The secondary is of spectral type dM5.5 ± 0.5 and has an absolute K-band magnitude of MK = 8.8. Its Roche radius places it on or very close to the main sequence of low-mass stars. It differs from a main sequence star by its illuminated hemisphere that faces the white dwarf. The secondary star contributes only 5% to the observed spin-phase averaged flux at 7500 Å, 7.5% at 8200 Å, and 37% in the K-band. We present images of the secondary star in the light of the NaI doublet and the CaII emission line derived with a simplified version of Roche tomography. Line emission is restricted to the illuminated part of the star, but its distribution differs from that of the incident energy flux. Conclusions. We have discovered narrow spectral lines from the secondary star in EXHya that delineate its orbital motion and allow us to derive accurate masses of both components. The primary mass significantly exceeds recently published values. The secondary is a low-mass main sequence star that displays a rich emission line spectrum on its illuminated side, but lacks chromospheric emission on its dark side."],["dc.identifier.doi","10.1051/0004-6361:20079010"],["dc.identifier.fs","513376"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9386"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60685"],["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","High-resolution spectroscopy of the intermediate polar EX Hydrae"],["dc.title.alternative","I. Kinematic study and Roche tomography"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1043"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","1046"],["dc.bibliographiccitation.volume","457"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Kim, Y."],["dc.contributor.author","Beuermann, K."],["dc.date.accessioned","2019-07-09T11:54:56Z"],["dc.date.available","2019-07-09T11:54:56Z"],["dc.date.issued","2006-10-03"],["dc.description.abstract","Context. The first phase-resolved JHK light curves of the eclipsing polar (AM Herculis binary) V1309Ori are presented and interpreted. Aims. We separate the contributions from the secondary star and from other sources with the aim of determining a photometric distance. Methods. Simple model calculations show that the accretion stream and the cyclotron source on the accreting white dwarf are minor contributors to the infrared light, allowing an accurate determination of spectral type and absolute flux of the secondary star. Results. The unilluminated backside of the secondary star as seen in eclipse has spectral type dM0 to dM0+. Its dereddened magnitude is K = 13.58 at orbital phase φ = 0 (eclipse). Using the calibrated surface brightness of M-stars and the published mass of the secondary, M2 = 0.46 M , we obtain a distance d = 600 ± 25 pc which scales as M1/2 2 . The radius of the Roche-lobe filling secondary exceeds the main-sequence radius of an M0 star by 21+11 −6 %. Conclusions. The debated origin of the infrared light of V1309 Ori has been settled in favor of the secondary star as the main contributor and an accurate distance has been derived that will place estimates of the luminosity and synchronization time scale on a more secure basis."],["dc.identifier.doi","10.1051/0004-6361:20065655"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9879"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60760"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","The secondary star and distance of the polar V1309 Orionis"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A41"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","543"],["dc.contributor.author","Beuermann, K."],["dc.contributor.author","Burwitz, V."],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2019-07-09T11:54:43Z"],["dc.date.available","2019-07-09T11:54:43Z"],["dc.date.issued","2012-06-25"],["dc.description.abstract","We present a simple heuristic model for the time-averaged soft X-ray temperature distribution in the accretion spot on the white dwarf in polars. The model is based on the analysis of the Chandra LETG spectrum of the prototype polar AM Her and involves an exponential distribution of the emitting area vs. blackbody temperature a(T) = a0 exp(−T/T0). With one free parameter besides the normalization, it is mathematically as simple as the single blackbody, but is physically more plausible and fits the soft X-ray and far-ultraviolet spectral fluxes much better. The model yields more reliable values of the wavelength-integrated flux of the soft X-ray component and the implied accretion rate than reported previously."],["dc.format.extent","5"],["dc.identifier.doi","10.1051/0004-6361/201219217"],["dc.identifier.fs","596640"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9606"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60712"],["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","A new soft X-ray spectral model for polars with an application to AM Herculis"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","487"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","490"],["dc.bibliographiccitation.volume","381"],["dc.contributor.author","Beuermann, Klaus"],["dc.contributor.author","Reinsch, K."],["dc.date.accessioned","2018-11-07T10:32:46Z"],["dc.date.available","2018-11-07T10:32:46Z"],["dc.date.issued","2002"],["dc.description.abstract","We have investigated the nature of the magnetic white dwarf LP 790-29 = LHS 2293 by polarimetric monitoring, searching for short-term variability. No periodicity was found and we can exclude rotation periods between 4 s and 1.5 hour with a high confidence. Maximum amplitudes of sinusoidal variations are DeltaR < 0.009 mag and Delta V-R < 0.7% for a mean value of the R-band circular polarization of V-R = -9.1 +/- 0.3%. Combined with earlier results by other authors, our observation suggests that LP 790-29 is, in fact, an extremely slowly rotating single white dwarf and not an unrecognized fast rotator and/or disguised cataclysmic variable."],["dc.identifier.doi","10.1051/0004-6361:20011478"],["dc.identifier.fs","19137"],["dc.identifier.isi","000173343100014"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9720"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44434"],["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","The high-field magnetic white dwarf LP790-29: Not a fast rotator"],["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","A42"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","562"],["dc.contributor.author","Traulsen, Imke"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Schwope, Axel D."],["dc.contributor.author","Schwarz, R."],["dc.contributor.author","Walter, F. M."],["dc.contributor.author","Burwitz, Vadim"],["dc.date.accessioned","2018-11-07T09:44:00Z"],["dc.date.available","2018-11-07T09:44:00Z"],["dc.date.issued","2014"],["dc.description.abstract","Context. RS Cae is the third target in our series of XMM-Newton observations of soft X-ray-dominated polars. Aims. Our observational campaign aims to better understand and describe the multiwavelength data, the physical properties of the system components, and the short-and long-term behavior of the component fluxes in RS Cae. Methods. We employ stellar atmosphere, stratified accretion-column, and widely used X-ray spectral models. We fit the XMM-Newton spectra, model the multiband light curves, and opt for a mostly consistent description of the spectral energy distribution. Results. Our XMM-Newton data of RS Cae are clearly dominated by soft X-ray emission. The X-ray light curves are shaped by emission from the main accretion region, which is visible over the whole orbital cycle, interrupted only by a stream eclipse. The optical light curves are formed by cyclotron and stream emission. The XMM-Newton X-ray spectra comprise a black-body-like and a plasma component at mean temperatures of 36 eV and 7 keV. The spectral fits give evidence of a partially absorbing and a reflection component. Multitemperature models, covering a broader temperature range in the X-ray emitting accretion regions, reproduce the spectra appropriately well. Including archival data, we describe the spectral energy distribution with a combination of models based on a consistent set of parameters and derive a lower limit estimate of the distance d greater than or similar to 750 pc. Conclusions. The high bolometric soft-to-hard flux ratios and short-term variability of the (X-ray) light curves are characteristic of inhomogeneous accretion. RS Cae clearly belongs in the group of polars that show a very strong soft X-ray flux compared to their hard X-ray flux. The different black-body fluxes and similar hard X-ray and optical fluxes during the XMM-Newton and ROSAT observations show that soft and hard X-ray emission are not directly correlated."],["dc.identifier.doi","10.1051/0004-6361/201321383"],["dc.identifier.isi","000332161800016"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/10906"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/34299"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.rights","Goescholar"],["dc.rights.uri","https://goedoc.uni-goettingen.de/licenses"],["dc.title","Phase-resolved X-ray spectroscopy and spectral energy distribution of the X-ray soft polar RS Caeli"],["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","A116"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","529"],["dc.contributor.author","Traulsen, Imke"],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Schwope, Axel D."],["dc.contributor.author","Burwitz, Vadim"],["dc.contributor.author","Dreizler, Stefan"],["dc.contributor.author","Schwarz, R."],["dc.contributor.author","Walter, F. M."],["dc.date.accessioned","2018-11-07T08:56:44Z"],["dc.date.available","2018-11-07T08:56:44Z"],["dc.date.issued","2011"],["dc.description.abstract","Context. On the basis of XMM-Newton observations, we investigate the energy balance of selected magnetic cataclysmic variables, which have shown an extreme soft-to-hard X-ray flux ratio in the ROSAT All-Sky Survey. Aims. We intend to establish the X-ray properties of the system components, their flux contributions, and the accretion geometry of the X-ray soft polar QS Tel. In the context of high-resolution X-ray analyses of magnetic cataclysmic variables, this study will contribute to better understanding the accretion processes on magnetic white dwarfs. Methods. During an intermediate high state of accretion of QS Tel, we have obtained 20 ks of XMM-Newton data, corresponding to more than two orbital periods, accompanied by simultaneous optical photometry and phase-resolved spectroscopy. We analyze the multi-wavelength spectra and light curves and compare them to former high-and low-state observations. Results. Soft emission at energies below 2 keV dominates the X-ray light curves. The complex double-peaked maxima are disrupted by a sharp dip in the very soft energy range (0.1-0.5 keV), where the count rate abruptly drops to zero. The EPIC spectra are described by a minimally absorbed black body at 20 eV and two partially absorbed MEKAL plasma models with temperatures around 0.2 and 3 keV. The black-body-like component arises from one mainly active, soft X-ray bright accretion region nearly facing the mass donor. Parts of the plasma emission might be attributed to the second, virtually inactive pole. High soft-to-hard X-ray flux ratios and hardness ratios demonstrate that the high-energy emission of QS Tel is substantially dominated by its X-ray soft component."],["dc.description.sponsorship","ESA; NASA; DLR [50 OR0501, 50OR0807]"],["dc.identifier.doi","10.1051/0004-6361/201016352"],["dc.identifier.isi","289557200124"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9232"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/23218"],["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","XMM-Newton observations of the X-ray soft polar QS Telescopii"],["dc.title.original","9232"],["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","341"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics Supplement Series"],["dc.bibliographiccitation.lastpage","359"],["dc.bibliographiccitation.volume","132"],["dc.contributor.author","Motch, C."],["dc.contributor.author","Guillout, P."],["dc.contributor.author","Haberl, F."],["dc.contributor.author","Krautter, J."],["dc.contributor.author","Pakull, M. W."],["dc.contributor.author","Pietsch, W."],["dc.contributor.author","Reinsch, K."],["dc.contributor.author","Voges, W."],["dc.contributor.author","Zickgraf, F.-J."],["dc.date.accessioned","2019-07-09T11:54:51Z"],["dc.date.available","2019-07-09T11:54:51Z"],["dc.date.issued","1998"],["dc.description.abstract","We report on optical searches in the error circles of 93 ROSAT survey sources located at low galactic latitudes ("],["dc.identifier.doi","10.1051/aas:1998299"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9760"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/60746"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.relation.issn","1286-4846"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Identification of selected sources from the ROSAT Galactic PlaneSurvey. I."],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]