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    188宝金博页面版: stellar population properties in the nuclei and bulges of the nearby lenticular galaxies

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    内容提示： arXiv:astro-ph/0404357v1 19 Apr 2004The Interplay among Black Holes, Stars and ISMin Galactic NucleiProceedings IAU Symposium No. 222, 2004Th. Storchi Bergmann, L.C. Ho & H.R. Schmitt, eds.c ? 2004 International Astronomical UnionDOI: 00.0000/X000000000000000XStellar population properties in the nucleiand bulges of nearby lenticular galaxiesOlga K. Sil’chenko11Sternberg Astronomical Institute, Moscow State University, University av. 13, Moscow119992, Russia, email: olga@sai.msu.suAbstract. The properties...

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    arXiv:astro-ph/0404357v1 19 Apr 2004The Interplay among Black Holes, Stars and ISMin Galactic NucleiProceedings IAU Symposium No. 222, 2004Th. Storchi Bergmann, L.C. Ho & H.R. Schmitt, eds.c ? 2004 International Astronomical UnionDOI: 00.0000/X000000000000000XStellar population properties in the nucleiand bulges of nearby lenticular galaxiesOlga K. Sil’chenko11Sternberg Astronomical Institute, Moscow State University, University av. 13, Moscow119992, Russia, email: olga@sai.msu.suAbstract. The properties of stellar populations in the centers of nearby lenticular galaxies areinvestigated by means of 2D spectroscopy. All the galaxies are divided into 4 groups dependingon the environment type; every subsample contains more than 10 galaxies. Clear distinctionsbetween the mean stellar ages and abundance ratios both for the nuclei and for the bulges ofthe S0s in the different environments are found.During 1996–2003 we have obtained 2D spectroscopic data in the spectral rangeof 4600–5400? A for 54 nearby lenticular galaxies over various types of environments,namely, for the field galaxies, for the brightest group galaxies (‘group centers’) and sec-ondary group members, and for the cluster lenticular galaxies. The observations havebeen made with the Multi-Pupil Spectrograph of the 6m telescope (MPFS). Here wecompare the stellar population properties in the nuclei and in the ‘bulges’ of thesegalaxies, the term ‘bulges’ being ascribed to the rings between R = 3′′and R =7′′. The stellar population abundances and ages are determined by comparing mea-sured Lick indices Mgb, Fe5270, Fe5335, and Hβ to the evolutionary synthesis modelsof Thomas, Maraston, & Bender (2003). As we have reported earlier (Sil’chenko 1993,Sil’chenko 2002), a significant part of nearby lenticular galaxies possess young stellarnuclei; according to the present estimates, among field S0s and group second- or third-ranked members 50% galaxies and among group centers and cluster members 25% galax-ies reveal mean age of the nuclear stellar population of less than 5 Gyr. A bulge is almostalways older than the nucleus. An effect of environments is seen both for the nuclei andfor the bulges: if we consider the clusters (Virgo and Ursa Major) and group centers asdense environments and the field and group periphery as sparse environments, then inthe dense environments the stellar populations of S0s are in average older by 4–5 Gyrthan in the sparse ones.We have analysed carefully the index-index diagrams, ?Fe? ≡(Fe5270+Fe5335)/2 vsMgb and Hβ vs [MgFe]≡?Mgb?Fe?, for all four types of environments; the stellarabsorption-line index Hβ has been corrected for the emission contamination mostly byusing the Hα emission estimates from Ho et al. (1997). We have come to the followingparticular conclusions:(a) In the dense environments, [Mg/Fe]nucvaries from +0.2 to +0.4 under [m/H] ≈const ≈ +0.3. This result implies very brief and very effective last star formation epochsin the nuclei of the lenticulars in the dense environments.(b) In the sparse environments, [Mg/Fe]nuc ≈ const ≈ +0.1 − +0.2, while [m/H]varies from −0.3 to +0.3. The metallicity variations seem to reflect a well-known mass-metallicity relation for early-type galaxies.(c) The bulges within each type of environments represent a metallicity sequence under1

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