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• W2016709072 abstract "We present a detailed study of the stellar populations (SPs) and kinematics of the bulge and inner disc regions of eight nearby spiral galaxies (Sa–Sd) based on deep Gemini/GMOS data. The long-slit spectra extend to 1–2 disc scalelengths with S/N/Å≥ 50. Several different model fitting techniques involving absorption-line indices and full spectrum fitting are explored, and found to weigh age, metallicity and abundance ratios differently. We find that the SPs of spiral galaxies are not well matched by single episodes of star formation; more representative SPs must involve average SP values integrated over the star formation history (SFH) of the galaxy. Our ‘full population synthesis’ method is an optimized linear combination of model templates to the full spectrum with masking of regions poorly represented by the models. Realistic determinations of the SP parameters and kinematics (rotation and velocity dispersion) also rely on careful attention to data/model matching (resolution and flux calibration). The population fits reveal a wide range of age and metallicity gradients (from negative to positive) in the bulge, allowing for diverse formation mechanisms. The observed positive age gradients within the effective radius of some late-type bulges helps reconcile the long-standing conundrum of the coexistence of secular-like kinematics, light profile shape and stellar bar with the ‘classical’-like old and α-enhanced SPs in the Milky Way bulge. The discs, on the other hand, almost always show mildly decreasing to flat profiles in both age and metallicity, consistent with inside-out formation. Our spiral bulges follow the same correlations of increasing light-weighted age and metallicity with central velocity dispersion as those of elliptical galaxies and early-type bulges found in other studies, but when SFHs more complex and realistic than a single burst are invoked, the trend with age is shallower and the scatter much reduced. In a mass-weighted context, however, all bulges are predominantly composed of old and metal-rich SPs. While secular contributions to the evolution of many of our bulges are clearly evident, with young (0.001–1 Gyr) SPs contributing as much as 90 per cent of the optical (V-band) light, the bulge mass fraction from young stars is small (≲25 per cent). The implies a bulge formation dominated by early processes that are common to all spheroids, whether they currently reside in discs or not. While monolithic collapse cannot be ruled out in some cases, merging must be invoked to explain the SP gradients in most bulges. Further bulge growth via secular processes or ‘rejuvenated’ star formation generally contributes minimally to the stellar mass budget, with the relative secular weight increasing with decreasing central velocity dispersion." @default.
• W2016709072 created "2016-06-24" @default.
• W2016709072 creator A5014952030 @default.
• W2016709072 creator A5044884072 @default.
• W2016709072 creator A5079210253 @default.
• W2016709072 date "2009-05-01" @default.
• W2016709072 modified "2023-10-03" @default.
• W2016709072 title "Stellar population and kinematic profiles in spiral bulges and discs: population synthesis of integrated spectra" @default.
• W2016709072 cites W1773558392 @default.
• W2016709072 cites W1968595293 @default.
• W2016709072 cites W1968596800 @default.
• W2016709072 cites W1969141849 @default.
• W2016709072 cites W1969195053 @default.
• W2016709072 cites W1970333333 @default.
• W2016709072 cites W1971191206 @default.
• W2016709072 cites W1974866549 @default.
• W2016709072 cites W1978642495 @default.
• W2016709072 cites W1978850795 @default.
• W2016709072 cites W1982684089 @default.
• W2016709072 cites W1985370957 @default.
• W2016709072 cites W1985501348 @default.
• W2016709072 cites W1986010423 @default.
• W2016709072 cites W1994671833 @default.
• W2016709072 cites W1997384998 @default.
• W2016709072 cites W1999105363 @default.
• W2016709072 cites W1999367759 @default.
• W2016709072 cites W2000359198 @default.
• W2016709072 cites W2000784645 @default.
• W2016709072 cites W2009994796 @default.
• W2016709072 cites W2010581546 @default.
• W2016709072 cites W2014706761 @default.
• W2016709072 cites W2017524870 @default.
• W2016709072 cites W2027686843 @default.
• W2016709072 cites W2028515412 @default.
• W2016709072 cites W2045895958 @default.
• W2016709072 cites W2051879158 @default.
• W2016709072 cites W2063232778 @default.
• W2016709072 cites W2065392390 @default.
• W2016709072 cites W2070304421 @default.
• W2016709072 cites W2073956619 @default.
• W2016709072 cites W2078590695 @default.
• W2016709072 cites W2082735313 @default.
• W2016709072 cites W2089017458 @default.
• W2016709072 cites W2090325809 @default.
• W2016709072 cites W2091591632 @default.
• W2016709072 cites W2091739399 @default.
• W2016709072 cites W2098830799 @default.
• W2016709072 cites W2099955627 @default.
• W2016709072 cites W2108191436 @default.
• W2016709072 cites W2111817932 @default.
• W2016709072 cites W2112633621 @default.
• W2016709072 cites W2116319113 @default.
• W2016709072 cites W2116958776 @default.
• W2016709072 cites W2129276959 @default.
• W2016709072 cites W2140751452 @default.
• W2016709072 cites W2145321334 @default.
• W2016709072 cites W2146942797 @default.
• W2016709072 cites W2155211801 @default.
• W2016709072 cites W2163447141 @default.
• W2016709072 cites W2164159860 @default.
• W2016709072 cites W2166408168 @default.
• W2016709072 cites W2169037488 @default.
• W2016709072 cites W2719761689 @default.
• W2016709072 cites W3099847878 @default.
• W2016709072 cites W3100024326 @default.
• W2016709072 cites W3100334026 @default.
• W2016709072 cites W3100386365 @default.
• W2016709072 cites W3100436717 @default.
• W2016709072 cites W3101314049 @default.
• W2016709072 cites W3102203343 @default.
• W2016709072 cites W3102453218 @default.
• W2016709072 cites W3103438512 @default.
• W2016709072 cites W3104052881 @default.
• W2016709072 cites W3104109985 @default.
• W2016709072 cites W3104225838 @default.
• W2016709072 cites W3104395689 @default.
• W2016709072 cites W3104900477 @default.
• W2016709072 cites W3106037901 @default.
• W2016709072 cites W3106275045 @default.
• W2016709072 cites W3106487884 @default.
• W2016709072 cites W3121651637 @default.
• W2016709072 cites W3166554277 @default.
• W2016709072 cites W4211245634 @default.
• W2016709072 cites W4244818491 @default.
• W2016709072 cites W4255974936 @default.
• W2016709072 cites W4289253265 @default.
• W2016709072 cites W4297889203 @default.
• W2016709072 cites W4302043173 @default.
• W2016709072 doi "https://doi.org/10.1111/j.1365-2966.2009.14519.x" @default.
• W2016709072 hasPublicationYear "2009" @default.
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