Volume-limited dependent Galactic model parameters

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dc.contributor.authorKaraali, S.
dc.contributor.authorBilir, S.
dc.contributor.authorYaz, E.
dc.contributor.authorHamzaoglu, E.
dc.contributor.authorBuser, R.
dc.date.accessioned2024-03-13T10:35:19Z
dc.date.available2024-03-13T10:35:19Z
dc.date.issued2007
dc.departmentİstanbul Beykent Üniversitesien_US
dc.description.abstractWe estimate 34 sets of Galactic model parameters for three intermediate-latitude fields with Galactic longitudes l = 60 degrees, l = 90 degrees, and l= 180 degrees, and we discussed their dependence on the volume. Also, we confirm the variation of these parameters with absolute magnitude and Galactic longitude. The star samples in two fields are restricted with bright and unit absolute-magnitude intervals, 4 < M-g <= 5, and 5 < M-g <= 6, whereas for the third field (l= 60 degrees) a larger absolute-magnitude interval is adopted, 4 < M-g <= 10. The limiting apparent magnitudes of the star samples are g(0) = 15 and g(0) = 22.5 mag, which provide space densities within distances in the line of sight of similar to 0.9 and 25 kpc. The Galactic model parameters for the thin disc are not volume dependent. However, the ones for the thick disc and halo do show spectacular trends in their variation with volume, except for the scalelength of the thick disc. The local space density of the thick disc increases, whereas the scaleheight of the same Galactic component decreases monotonically. However, both model parameters approach asymptotic values at large distances. The relative local space density of the halo estimated by fitting the density laws to the space densities evaluated for all volumes is constant, except for the small ones. However it is absolute-magnitude and Galactic-longitude dependent. The axial ratio of the halo increases abruptly for the volumes where a thick disc is dominant, whereas it approaches an asymptotic value gradually for larger volumes, indicating a continuous transition from a disc-like structure to a spherical one at the outermost region of the Galaxy. The variation of the Galactic model parameters with absolute magnitude can be explained by their dependence on the stellar luminosity, whereas the variation with volume and Galactic longitude at short distances is a bias in analysis.en_US
dc.identifier.doi10.1071/AS07006
dc.identifier.endpage219en_US
dc.identifier.issn1323-3580
dc.identifier.issue4en_US
dc.identifier.scopus2-s2.0-36849049221en_US
dc.identifier.scopusqualityQ1en_US
dc.identifier.startpage208en_US
dc.identifier.urihttps://doi.org/10.1071/AS07006
dc.identifier.urihttps://hdl.handle.net/20.500.12662/4358
dc.identifier.volume24en_US
dc.identifier.wosWOS:000251428000004en_US
dc.identifier.wosqualityQ3en_US
dc.indekslendigikaynakWeb of Scienceen_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.publisherCsiro Publishingen_US
dc.relation.ispartofPublications Of The Astronomical Society Of Australiaen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.subjectGalaxy : structureen_US
dc.subjectGalaxy : fundamental parametersen_US
dc.subjectGalaxy : solar neighborhooden_US
dc.titleVolume-limited dependent Galactic model parametersen_US
dc.typeArticleen_US

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