Evolutionary synthesis models for the formation of S0 galaxies   in
 clusters

Bicker, Jens; Alvensleben, U. Fritze–v.; Fricke, K. J.

doi:10.1051/0004-6361:20020410

Cited by 21 publications

(25 citation statements)

References 38 publications

(43 reference statements)

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“…Cluster S0 galaxies are found to be most plausibly transformed into what they are from the spiral-rich field galaxy population falling into the cluster potential. Spectroscopic analyses by Jones et al (2000), our own comparison of their photometric properties with evolutionary synthesis models including SF truncation with or without prior starbursts (Bicker et al 2002) and dynamical modelling (Moore et al 1998;Quilis et al 2000) together draft a scenario where rapid interactions with the cluster potential and environment largely destroy the stellar disks of infalling spirals and the dense and hot intracluster medium sweeps away their HI supply, ultimately leaving remnants with S0 morphologies and SF completely truncated. This, however, is not the subject of the present paper where we want to explore the effects of bulge versus disk SF along the Hubble sequence.…”

Section: Bulge and Disk Formation Scenariosmentioning

confidence: 96%

Wavelength and redshift dependence of bulge/total light ratios in galaxies

Schulz¹,

Alvensleben²,

Fricke³

2003

A&A

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Abstract. HST has opened the possibility to decompose the surface brightness profiles of galaxies up to significant redshifts and look-back times into r 1/4 −bulge and exponential disk components. This should allow to study the redshift evolution of bulge and disk luminosity contributions and discriminate between the different formation scenarios for these galaxy components currently discussed, i.e. decide if star formation in bulges and disks started at the same time or was delayed in either of the two components. An indispensable prerequisite for the comparison of bulge-to-disk ratios of galaxies at different redshifts is to properly account for cosmological band shift and evolutionary effects. We present evolutionary synthesis models for both components and add their spectra in various proportions to obtain the full range of local galaxies' B-band bulge-to-total light ratios. Bulge star formation is assumed to occur on a short timescale of 10 9 yr, disk star formation proceeds at a constant rate. We study the evolution of the relative light contributions of both components backward in time and, for a given cosmological model, as a function of redshift. This allows us to see how far back into the past the locally well-established correlation between galaxy morphologies and spectral properties can hold. To cope with the present uncertainty about the formation epochs of bulge and disk components we present models for three scenarios: bulges and disks of equal age, old bulges and delayed disk star formation, and old disks with subsequent bulge star formation. We quantitatively show the wavelength dependence of bulge-to-total (=B/T ) light ratios for local galaxies. The different star formation timescales for bulge and disk components lead to B/T ratios that significantly increase from U through I-bands (by factors 4-6 for weak bulge systems ∼Sc) with the rate of increase slightly depending on the relative ages of the two components. The redshift evolution of B/T -ratios in various bands U, B, V, I, H is calculated accounting both for cosmological and evolutionary corrections assuming a standard cosmology (H 0 = 65, Ω 0 = 0.1, Λ 0 = 0). In particular, for the two scenarios with old bulges and old or younger disks, the redshift evolution of B/T -ratios is dramatic in every band and both for galaxies ending up at z ∼ 0 with low and high B-band B/T light ratios. Our results clearly show that it does not make any sense to compare B/T ratios measured in one and the same band for galaxies at different redshifts without fully accounting for evolutionary and cosmological effects. These, unfortunately, significantly depend on the relative ages of the two components and, hence, on the galaxy formation scenario adopted. We also show that simultaneous decomposition of galaxy profiles in several bands can give direct information about these relative ages and constrain formation scenarios for the different galaxy components. Of the wavelength bands we explore (U, B, V, I, H), the I-and H-bands show the smoothest redshift evolut...

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Section: Bulge and Disk Formation Scenariosmentioning

confidence: 96%

Wavelength and redshift dependence of bulge/total light ratios in galaxies

Schulz¹,

Alvensleben²,

Fricke³

2003

A&A

Self Cite

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“…The derived quantities are age, mass and metallicity of the star cluster as well as the extinction in front of the star cluster (see e.g., among many others, Bicker et al 2002;Kassin et al 2003;Anders et al 2004b;de Grijs et al 2004;Kundu et al 2005;Smith et al 2007). …”

Section: Impact On Age Determinationmentioning

confidence: 99%

The photometric evolution of dissolving star clusters

Anders¹,

Lamers²,

Baumgardt

2009

A&A

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Context. Evolutionary synthesis models are the primary means of constructing spectrophotometric models of stellar populations, and deriving physical parameters from observations compared with these models. One of the basic assumptions of evolutionary synthesis models has been the time-independence of the stellar mass function, apart from the successive removal of high-mass stars by stellar evolution. However, dynamical simulations of star clusters in tidal fields have demonstrated that the mass function can be changed by the preferential removal of low-mass stars from clusters. Aims. We combine the results of dynamical simulations of star clusters in tidal fields with our evolutionary synthesis code GALEV. We extend the models to consider the total cluster disruption time as additional parameter. Methods. Following up on our earlier work, which was based on simplifying assumptions, we reanalyse the mass-function evolution found in N-body simulations of star clusters in tidal fields, parametrise it as a function of age and total disruption time of the cluster, and use this parametrisation to compute GALEV models as a function of age, metallicity, and total cluster disruption time. Results. We study the impact of cluster dissolution on colours (which generally become redder) and magnitudes (which become fainter) of star clusters, their mass-to-light ratios (which can deviate by a factor of ∼2-4 from predictions of standard models without cluster dissolution), and quantify the effect of the altered integrated photometry on cluster age determination. In most cases, clusters appear to be older than they are, where the age difference can range from 20% to 200%. By comparing our model results with observed M/L ratios for old compact objects in the mass range 10 4.5 -10 8 M , we find a strong discrepancy for objects more massive than 10 7 M , such that observed M/L ratios are higher than predicted by our models. This could be caused either by differences in the underlying stellar mass function or be an indication of the presence of dark matter in these objects. Less massive objects are well described by the models.

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“…Together with my age distribution map, I am able to tell the story of this galaxy more clearly. For its outer disk regions, the molecular component of the interstellar medium (ISM) was quickly depleted for three reasons (and thus star formation activities in these regions were slowed; Young et al 1983): (1) a global wide starburst consumed much of the molecular gas (Bicker et al 2002); (2) dynamical instabilities, such as strong density waves and spiral patterns, caused by the interaction channel the ISM from the outer disk down to the inner region of the galaxy very efficiently (Zhang et al 1993(Zhang et al , 1994Reuter et al 1996); and (3) NGC 3627 may have lost part of its H i gas during the encounter with NGC 3628 ( Zhang et al1993). In the inner disk, however, star formation is still going on ( Dahlem et al 1996).…”

Section: Star Formation In the Leo Tripletmentioning

confidence: 99%

Multicolor Photometry and Stellar Population Synthesis Study of the Interacting Galaxies of the Leo Triplet

Duan¹

2006

Astron J

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This paper studies the nearby interacting group the Leo Triplet using multicolor photometry data obtained with the National Astronomical Observatories of China 60 cm/90 cm Schmidt telescope. The observation covers the entire area of the three galaxies ( NGC 3623, NGC 3627, and NGC 3628), and spectral energy distributions (SEDs) of each galaxy are obtained. By comparing the observed SEDs of each part of the galaxies with the theoretical ones generated by instantaneous burst evolutionary synthesis models with different metallicities (Z ¼ 0:0001, 0.008, 0.02, and 0.05), two-dimensional relative age distribution maps of the three galaxies were obtained. NGC 3623 exhibits a very weak age gradient from the bulge to the disk. This gradient is absent in NGC 3627. The ages of the dominant stellar populations of NGC 3627 and NGC 3628 are consistent, and this consistency is model independent (0.5-0.6 Gyr, Z ¼ 0:02), but the ages of NGC 3623 are systematically older (0.7-0.9 Gyr, Z ¼ 0:02). The results indicate that NGC 3627 and NGC 3628 have undergone synchronous evolution and that the interaction has likely triggered starbursts in both galaxies. For NGC 3623, however, the weak age gradient may indicate recent star formation in its bulge, which has caused its color to turn blue. Evidence is found for a potential bar existing in the bulge of NGC 3623, and my results support the view that NGC 3623 does interact with NGC 3627 and NGC 3628.

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Evolutionary synthesis models for the formation of S0 galaxies in clusters

Cited by 21 publications

References 38 publications

Wavelength and redshift dependence of bulge/total light ratios in galaxies

Wavelength and redshift dependence of bulge/total light ratios in galaxies

The photometric evolution of dissolving star clusters

Multicolor Photometry and Stellar Population Synthesis Study of the Interacting Galaxies of the Leo Triplet

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