A Database for Galaxy Evolution Modeling

Leitherer, Claus; Alloin, D.; FritzVonAlvensleben, U; Gallagher, J. S.; Huchra, J.; Matteuccí, F.; O'Connell, R. W.; Beckman, J.; Bertelli, G.; Bica, E.; Boisson, C.; Bonatto, Charles Jose; Bothun, G.; Bressan, A.; Brodie, J.; Bruzual, G.; Burstein, David; Buser, R.; Caldwell, Nelson; Casuso, E.; Cerviño, M.; Charlot, S.; Chávez, M.; Chiosi, C.; Christian, C. A.; Cuisinier, F.; Dallier, R.; deKoter, A; Delisle, Sonya; Diaz, A. I.; Dopita, Michael A.; Dorman, Ben; Fagotto, F.; Fanelli, M.; Fioc, Michel; GarciaVargas, ML; Girardi, L.; Goldader, JD; Hardy, Eduardo; Heckman, TM; Iglesias, Josefa Montalban; Jablonka, P.; Joly, M.; Jones, Lewis A.; Kurth, Oliver; Lançon, A.; Lejeune, T.; Loxen, J.; Maeder, A.; Malagnini, ML; Marigo, Paola; Mas-Hesse, J. M.; Meynet, Georges; Moller, CS; Mollá, M.; Morossi, C.; Nasi, E.; Nichols, J.; Odegaard, Kjr; Parker, J. W.; Pastoriza, M. G.; Peletier, Reynier F.; Robert, Carmelle; Rocca‐Volmerange, B.; Schaerer, D.; Schmidt, Ann; Schmitt, H.; Schommer, RA; Schmutz, W.; Silva, L; Stasińska, G.; Sutherland, Ralph S.; Tantalo, R.; Traat, P.; Vallenari, A.; Vazdekis, Alexandre; Walborn, N.R.; Worthey, Guy

doi:10.1086/133825

Cited by 166 publications

(108 citation statements)

References 64 publications

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“…We must use either synthetic spectra or spectra taken through other spectroscopic configurations and transform these to our system. We use templates from two sources: the Coudé Feed Spectral Library at KPNO (Leitherer et al 1996), and the stellar templates observed by Kobulnicky & Gebhardt (2000). The KPNO library consists of 684 stars having a broad range of spectral types, with 1.8 Å FWHM resolution.…”

Section: Kinematic Propertiesmentioning

confidence: 99%

The DEEP Groth Strip Survey. IX. Evolution of the Fundamental Plane of Field Galaxies

Gebhardt

Faber

Koo

et al. 2003

ApJ

113

165

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Fundamental plane studies provide an excellent means of understanding the evolutionary history of earlytype galaxies. Using the Low Resolution Imaging Spectrograph on the Keck Telescope, we obtained internal stellar kinematic information for 36 field galaxies in the Groth Strip, 21 early-type and 15 disk galaxies. Their redshifts range from 0.3 to 1.0, with a median redshift of 0.8. The slope of the relation shows no difference compared with the local slope. However, there is significant evolution in the zero-point offset; an offset due to evolution in magnitude requires a 2.4 mag luminosity brightening at z ¼ 1. We see little differences of the offset with bulge fraction, which is a good surrogate for galaxy type. Correcting for the luminosity evolution reduces the orthogonal scatter in the fundamental plane to 8%, consistent with the local scatter. This scatter is measured for our sample and does not include results from other studies, which may have different selection effects. The difference in the degree of evolution between our field sample and published cluster galaxies suggests a more recent formation epoch, around z ¼ 1:5 for field galaxies compared to z > 2:0 for cluster galaxies. The magnitude difference implies that the field early-type galaxies are about 2 Gyr younger than the cluster ellipticals using standard single-burst models. However, the same models imply a significant change in the rest-frame UÀB color from then to the present, which is not seen in our sample. Continuous low-level star formation, however, would serve to explain the constant colors over this large magnitude change. A consistent model has 7% of the stellar mass created after the initial burst, using an exponentially decaying star formation rate with an e-folding time of 5 Gyr.

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Section: Kinematic Propertiesmentioning

confidence: 99%

The DEEP Groth Strip Survey. IX. Evolution of the Fundamental Plane of Field Galaxies

Gebhardt

Faber

Koo

et al. 2003

ApJ

113

165

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“…In our study we adopt the isochrones by Tantalo (1998) (anticipated in the data base for galaxy evolution models by Leitherer et al 1996). The underlying stellar models are those of the Padova Library.…”

Section: Libraries Of Stellar Models and Stellar Spectramentioning

confidence: 99%

Shells of dust around AGB stars: Effects on the integrated spectrum of Single Stellar Populations

Piovan¹,

Tantalo²,

Chiosi³

2003

A&A

172

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Abstract. In this paper we present models for Single Stellar Populations (SSPs) of intermediate and old ages where dust enshrouded Asymptotic Giant Branch (AGB) stars are introduced. As long known AGB stars are surrounded by dust-rich shells of matter caused by their own stellar wind, which absorb the radiation coming from the central object and re-emit it in the far infrared (IR). To this aim, particular care is devoted to follow the evolution of the AGB stars throughout the quiet and thermally pulsing regimes, to evaluate the effect of self contamination in the outermost layers by the third dredge-up mechanism, to follow the transition from oxygen-rich to carbon-rich objects (as appropriate to their initial mass and chemical composition), and finally to estimate the efficiency of mass-loss by stellar winds, all aspects that concur to the formation and properties of the dusty shells around. In addition to this, accurate physical models of the dusty shells are presented in which the re-processing of radiation from the central stars is calculated by solving the radiative transfer equations in presence of dust particles of different chemical composition. The resulting spectral energy distribution (SED) is examined to show how important features, like the 10 µm Si−O stretching mode feature and the 11 µm SiC feature, evolve with time. The SEDs are then convolved with the IRAS filters to obtain the flux in various pass-bands, i.e. 12, 25 and 60 µm, for individual AGB stars of different mass, chemical composition, and age. The comparison is made by means of SSPs along which AGB stars of the same age but different initial masses are located. This allows us to explore the whole range of masses and ages spanned by AGB stars. The theoretical results are compared to the observational data for selected groups of stars. The same is made for the J, H, K, L pass-bands of the Johnson system. Finally, from the integrated SEDs of the SSPs, we derive the integrated Johnson J, H, K, L magnitudes and colors to be compared to infrared data for star clusters of the Magellanic Clouds. In general good agreement with the data is possible if the effects of the circumstellar shells of dust are taken into account.

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“…The templates also extend further to the UV and near-IR domains, which can be used as additional constraints in the analysis. A detailed description of these templates is given by Bica and collaborators in°4.1 of Leitherer et al (1996). To represent a 3 Myr stellar population, we adopt the integrated spectrum of 30 Doradus (BAS94, Bica & Alloin 1986 In the old stellar population template, typical of elliptical galaxies or of the bulge of spirals, the main absorption features are the Ca II K (j3933) and H (j3970) lines and a blend of absorptions caused by CN, Mg I, Si I, and Fe I.…”

Section: Near-ultraviolet Features and Adopted Templatesmentioning

confidence: 99%

The Frequency of Nuclear Star Formation in Seyfert 2 Galaxies

Storchi‐Bergmann

Raimann

Bica

et al. 2000

ApJ

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We investigate the detectability of starburst signatures in the nuclear spectrum of Seyfert 2 galaxies by constructing spectral models in the wavelength range jj3500È4100, combining the spectrum of a bulge population (of age B10 Gyr) with that of younger stellar populations, spanning ages from B3 Myr to 1 Gyr. The major constraints in the analysis are (1) the continuum ratio jj3660/4020, which efficiently discriminates between models combining a bulge spectrum with a stellar population younger than B50 Myr and those with older stellar populations ; (2) the presence of the Balmer lines H8, H9, and H10 in absorption, which are unambiguous signatures of stellar populations with ages in the range 10 MyrÈ1 Gyr for the relevant metallicities. Their detectability depends both on the age of the young component and on its contribution to the total Ñux relative to that of the bulge. We also construct models combining the bulge template with a power-law (PL) continuum, which is observed in some Seyfert 2 galaxies in polarized light, contributing with typically 10%È40% of the Ñux at 4020We conclude that such con-A . tinuum cannot be distinguished from that of a very young stellar population (age ¹ 10 Myr), contributing with less than B0.02% of the mass of the bulge. The models are compared with nuclear spectraÈcorresponding to a radius of 200È300 pc at the galaxyÈof 20 Seyfert 2 galaxies, in which we speciÐcally look for the signatures above of young-to intermediate-aged stellar populations. We Ðnd them in 10 galaxies, thus 50% of the sample. But only in six cases (30% of the sample) can they be attributed to young stars (age \ 500 Myr) : Mrk 1210, ESO 362-G8, NGC 5135, NGC 5643, NGC 7130, and NGC 7582. In the remaining four cases, the signatures are caused by intermediate-aged stars (B1 Gyr). We Ðnd a tendency for the young stars to be found more frequently among the late-type Seyfert galaxies, a well-known e †ect in the nuclei of normal galaxies. This tendency is supported by a comparison between the equivalent widths (W ) of absorption lines of the nuclear spectra of the Seyfert 2 galaxies with those of normal galaxies of the same Hubble type. For the late-type galaxies, the W values of the Seyfert galaxies are within the observed range of the normal galaxies, suggesting a similar stellar population. On the other hand, the W values are lower than those of the normal galaxies for seven out of the 11 Seyferts in early-type galaxies.

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A Database for Galaxy Evolution Modeling

Cited by 166 publications

References 64 publications

The DEEP Groth Strip Survey. IX. Evolution of the Fundamental Plane of Field Galaxies

The DEEP Groth Strip Survey. IX. Evolution of the Fundamental Plane of Field Galaxies

Shells of dust around AGB stars: Effects on the integrated spectrum of Single Stellar Populations

The Frequency of Nuclear Star Formation in Seyfert 2 Galaxies

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