Fritze-von Alvensleben, Uta

[["dc.bibliographiccitation.firstpage","1"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","11"],["dc.bibliographiccitation.volume","392"],["dc.contributor.author","Schulz, J."],["dc.contributor.author","Fritze-von Alvensleben, Uta"],["dc.contributor.author","Moller, C. S."],["dc.contributor.author","Fricke, K. J."],["dc.date.accessioned","2018-11-07T10:03:52Z"],["dc.date.available","2018-11-07T10:03:52Z"],["dc.date.issued","2002"],["dc.description.abstract","A new set of evolutionary synthesis spectra are presented for Simple Stellar Populations (SSPs) covering ranges in metallicity from 0.02 less than or equal to Z/Z(.) less than or equal to 2.5 and ages from 4 x 10(6) yr less than or equal to t less than or equal to 16 Gyr. They are based on the most recent isochrones from the Padova group that extend earlier models by the inclusion of the thermal pulsing AGB phase for stars in the mass range 2 M-. less than or equal to m less than or equal to 7 M-. in accordance with the fuel consumption theorem. We show that with respect to earlier models, inclusion of the TP-AGB phase leads to significant changes in the (V-I) and(V-K) colors of SSPs in the age range from 10(8) to greater than or similar to 10(9) yr. Using model atmosphere spectra from Lejeune et al. (1997, 1998), we calculate the spectral evolution of single burst populations of various metallicities covering the wavelength range from 90 Angstrom through 160 mum. Isochrone spectra are convolved with filter response functions to describe the time evolution of luminosities and colors in Johnson, Thuan & Gunn, Koo, HST, Washington and Stromgren filters. The models and their results are not only intended for use in the interpretation of star clusters but also for combination with any kind of dynamical galaxy formation and/or evolution model that contains a star formation criterion. Moreover, the evolution of these single burst single metallicity stellar populations is readily folded with any kind of star formation - and eventually chemical enrichment - history to describe the evolutionary spectral synthesis of composite stellar populations like galaxies of any type with continuous or discontinuous star formation. For these latter purposes we also present the time evolution of ejection rates for gas and metals for two different Initial Mass Functions (IMFs) as well as cosmological and evolutionary corrections for all the filters as a function of redshift for 0 less than or equal to z less than or equal to 5 and two different cosmologies. Extensive data files are provided in the electronic version, at CDS, and at our above www-address."],["dc.identifier.doi","10.1051/0004-6361:20020657"],["dc.identifier.isi","000177868700006"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9730"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/38572"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Spectral and photometric evolution of simple stellar populations at various metallicities"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","37"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","48"],["dc.bibliographiccitation.volume","413"],["dc.contributor.author","Bicker, J."],["dc.contributor.author","Fritze-von Alvensleben, Uta"],["dc.contributor.author","Moller, C. S."],["dc.contributor.author","Fricke, K. J."],["dc.date.accessioned","2018-11-07T10:52:04Z"],["dc.date.available","2018-11-07T10:52:04Z"],["dc.date.issued","2004"],["dc.description.abstract","The composite stellar populations of galaxies comprise stars of a wide range of metallicities. Subsolar metallicities become increasingly important, both in the local universe when going from early towards later galaxy types as well as for dwarf galaxies and for all types of galaxies towards higher redshifts. We present a new generation of chemically consistent evolutionary synthesis models for galaxies of various spectral types from E through Sd. The models follow the chemical enrichment of the ISM and take into account the increasing initial metallicity of successive stellar generations using recently published metallicity dependent stellar evolutionary isochrones, spectra and yields. Our first set of closed-box 1-zone models does not include any spatial resolution or dynamics. For a Salpeter initial mass function ( IMF) the star formation rate (SFR) and its time evolution are shown to successfully parameterise spectral galaxy types E,..., Sd. We show how the stellar metallicity distribution in various galaxy types build up with time to yield after similar to12 Gyr agreement with stellar metallicity distributions observed in our and other local galaxies. The models give integrated galaxy spectra over a wide wavelength range (90.9 Angstrom-160 mum), which for ages of similar to12 Gyr are in good agreement not only with observed broad band colours but also with template spectra for the respective galaxy types. Using filter functions for Johnson-Cousins U, B, V, R-C, I-C, as well as for HST broad band filters in the optical and Bessel & Brett's NIR J, H, K filter system, we calculate the luminosity and colour evolution of model galaxies over a Hubble time. Including a standard cosmological model (H-0 = 65, Omega 0 = 0.1) and the attenuation by intergalactic hydrogen we present evolutionary and cosmological corrections as well as apparent luminosities in various filters over the redshift range from z similar to 5 to the present for our galaxy types and compare to earlier models using single (= solar) metallicity input physics only. We also resent a first comparison of our cc models to HDF data. A more detailed comparison with Hubble Deep Field ( HDF) and other deep field data and an analysis and interpretation of high redshift galaxies in terms of ages, metallicities, star formation histories and, galaxy types will be the subject of a forthcoming paper."],["dc.identifier.doi","10.1051/0004-6361:20031483"],["dc.identifier.fs","21413"],["dc.identifier.isi","000187356300005"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9821"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/49035"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Chemically consistent evolution of galaxies - II. Spectrophotometric evolution from zero to high redshift"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","L9"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","L12"],["dc.bibliographiccitation.volume","373"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Fritze-von Alvensleben, Uta"],["dc.date.accessioned","2018-11-07T08:53:43Z"],["dc.date.available","2018-11-07T08:53:43Z"],["dc.date.issued","2001"],["dc.description.abstract","We present evolutionary synthesis models of starbursts on top of old stellar populations to investigate in detailed time evolution the relation between H-alpha luminosity and star formation rate (SFR). The models show that several effects have an impact on the ratio between L(H-alpha) and SFR. Metallicity different from solar abundance, a time delay between star formation and maximum H-alpha-luminosity, and a varying stellar initial mass function give rise to strong variations in the ratio of H-alpha luminosity to SFR and can cause large errors in the determination of the SFR when employing well-known calibrations. When studying star-bursting dwarf galaxies, and sub-galactic fragments at high redshift, which show SFR fluctuating on short timescales, these effects can add up to errors of two orders of magnitude compared with the calibrations. To accurately determine the true current SFR additional data in combination with models for the spectral energy distribution are needed."],["dc.identifier.doi","10.1051/0004-6361:20010704"],["dc.identifier.isi","000169967200003"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9708"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/22488"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","On star formation rates in dwarf galaxies"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","67"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","76"],["dc.bibliographiccitation.volume","454"],["dc.contributor.author","Fritze-von Alvensleben, Uta"],["dc.contributor.author","Bicker, J."],["dc.date.accessioned","2018-11-07T09:33:39Z"],["dc.date.available","2018-11-07T09:33:39Z"],["dc.date.issued","2006"],["dc.description.abstract","We present evolutionary synthesis models for galaxies of spectral types Sa through Sd with starbursts of various strengths triggered at various redshifts and study their photometric evolution before, during, and after their bursts in a cosmological context. We find that bursts at high redshift, even very strong ones, only cause a small blueing of their intrinsically blue young parent galaxies. At lower redshift, in contrast, even small bursts cause a significant blueing of their intrinsically redder galaxies. While the burst phase is generally short, typically a few hundred Myr in normal-mass galaxies, the postburst stage with its red colors and, in particular the very red ones for early bursts at high redshift, lasts much longer, on the order of several Gyr. We find that, even without any dust, which in the postburst stage is not expected to play an important role anyway, models easily reach the colors of EROs in the redshift range z similar to 2 through z similar to 0.5 after starbursts at redshifts between 2 and 4. We therefore propose a third alternative for the ERO galaxies beyond the two established ones of passive galaxies vs. dusty starbursts: the dust-free post-(strong-) starbursts. A very first comparison of our models to HDF data with photometric redshifts shows that almost all of the outliers that could not be described with our chemically consistent models for undisturbed normal galaxy types E through Sd can now be explained very well. Galaxies in the redshift range from z similar to 2.5 to z similar to 0.5 that are redder, and in some cases much redder, than our reddest undisturbed model for a high-metallicity classical elliptical are well described by post-starburst models after starbursts at redshifts between 2 and 4. Galaxies bluer than our bluest low metallicity Sd model, most of which have redshifts lower than 1, are well explained by ongoing starbursts."],["dc.identifier.doi","10.1051/0004-6361:20053387"],["dc.identifier.fs","45029"],["dc.identifier.isi","000238726300010"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9883"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/32013"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","89"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","100"],["dc.bibliographiccitation.volume","398"],["dc.contributor.author","Schulz, J."],["dc.contributor.author","Fritze von Alvensleben, U."],["dc.contributor.author","Fricke, K. J."],["dc.date.accessioned","2018-11-07T10:42:00Z"],["dc.date.available","2018-11-07T10:42:00Z"],["dc.date.issued","2003"],["dc.description.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 BIT ratios that significantly increase from U through I-bands (by factors 4-6 for weak bulge systems similar toSc) 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, 1, H is calculated accounting both for cosmological and evolutionary corrections assuming a standard cosmology (H-0 = 65, Omega(0) = 0.1, Lambda(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 similar to 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 evolution and, hence, are best suited for a first order comparison of galaxies over the redshift range from z = 0 to z greater than or similar to 1. Our robust result that - irrespective of the respective ages of the bulge and disk stellar components - I-band B/T-ratios apparently increase with increasing redshift for all galaxy types with present B/T > 0.1 implies that the scarcity of bulge-strong systems at z greater than or equal to 0.8 reported by Marleau & Simard (1998) and Aguerri & Trujillo (2002) for HDF and Hawaiian Deep Field galaxies is further enhanced."],["dc.identifier.doi","10.1051/0004-6361:20021631"],["dc.identifier.isi","000180395700011"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9789"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/46681"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Wavelength and redshift dependence of bulge/total light ratios in galaxies"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","412"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","421"],["dc.bibliographiccitation.volume","387"],["dc.contributor.author","Bicker, J."],["dc.contributor.author","Alvensleben, U. F."],["dc.contributor.author","Fricke, K. J."],["dc.date.accessioned","2018-11-07T10:30:03Z"],["dc.date.available","2018-11-07T10:30:03Z"],["dc.date.issued","2002"],["dc.description.abstract","Rich galaxy clusters in the local Universe show a large population of S0 galaxies (similar to40% of all luminous galaxies). With increasing redshift the fraction of this S0 galaxy population is observed to strongly decrease (e.g. by a factor similar to2-3 to z=0.5) in favor of the spiral galaxy fraction while the number of bright ellipticals does not seem to change. The infalling field galaxy population that successively builds up the cluster also is spiral rich and S0 poor. It has hence been suspected that galaxy transformation processes, either due to galaxy-galaxy or to galaxy-ICM interactions, are responsible for this change. Complementing dynamical and morphological studies, we use evolutionary synthesis models describing various possible effects of those interactions on the star formation rates of the infalling spirals. We study the effects of starbursts of various strengths as well as of the truncation of star formation on the color and luminosity evolution of model galaxies of various spectral types. Comparison with observed properties of the local S0 galaxy population is used to constrain possible S0 formation mechanisms. We find that star formation truncation in spiral galaxies earlier than Sd-type, if occurring not too long ago, as well as starbursts more than 3 Gyr ago and followed by complete star formation extinction in spirals-again earlier than Sd-may well account for the observed average S0 luminosities and colors. Late-type galaxies (Sd), even after a strong burst, remain either too blue or too faint. Our results are in agreement with studies of spectral features of cluster S0s but allow for stronger constraints."],["dc.identifier.doi","10.1051/0004-6361:20020410"],["dc.identifier.isi","000175858200009"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9728"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43772"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Evolutionary synthesis models for the formation of S0 galaxies in clusters"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","545"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","555"],["dc.bibliographiccitation.volume","397"],["dc.contributor.author","Weilbacher, P. A."],["dc.contributor.author","Duc, P. A."],["dc.contributor.author","Fritz-von Alvensleben, U."],["dc.date.accessioned","2018-11-07T10:42:01Z"],["dc.date.available","2018-11-07T10:42:01Z"],["dc.date.issued","2003"],["dc.description.abstract","We present low-resolution spectroscopy of the ionized gas in a sample of optical knots located along the tidal features of 14 interacting galaxies previously selected as candidate Tidal Dwarf Galaxies (TDGs). From redshift measurements, we are able to confirm their physical association with the interacting system in almost all cases. For most knots, the oxygen abundance does not depend on the blue luminosity. The average, 12 + log(O/H) = 8.34 +/- 0.20, is typical of TDGs and is comparable to that measured in the outer stellar disk of spirals from which they were formed. A few knots showing low metallicities are probably pre-existing low-mass companions. The estimated Ha luminosity of the TDG candidates is higher than that of typical individual H II regions in spiral disks and is comparable to the global Ha luminosity of dwarf galaxies. We find several instances of velocity gradients with amplitudes apparently larger than 100 km s(-1) in the ionized gas in the tidal knots and discuss various possible origins for the large velocity amplitudes. While we can exclude tidal streaming motions and outflows, we cannot rule out projection effects with the current resolution. The velocity gradients could be indicative of the internal kinematic characteristic of self-gravitating objects. Higher resolution spectra are required to confirm whether the tidal knots in our sample have already acquired their dynamical independence and are therefore genuine Tidal Dwarf Galaxies."],["dc.identifier.doi","10.1051/0004-6361:20021522"],["dc.identifier.isi","000179896800016"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9806"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/46683"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","E D P Sciences"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Tidal dwarf candidates in a sample of interacting galaxies - II. Properties and kinematics of the ionized gas"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","515"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","530"],["dc.bibliographiccitation.volume","414"],["dc.contributor.author","Fritze-von Alvensleben, Uta"],["dc.date.accessioned","2018-11-07T10:51:16Z"],["dc.date.available","2018-11-07T10:51:16Z"],["dc.date.issued","2004"],["dc.description.abstract","This study is motivated by two facts: 1. The formation of populous star cluster systems is widely observed to accompany violent star formation episodes in gas-rich galaxies as e. g. those triggered by strong interactions or merging. 2. The Globular Cluster (GC) systems of most but not all early-type galaxies show bimodal optical color distributions with fairly universal blue peaks and somewhat variable red peak colors, yet their Luminosity Functions (LFs) look like simple Gaussians with apparently universal turn-over magnitudes that are used for distance measurements and the determination of Ho. Based on a new set of evolutionary synthesis models for Simple (= single burst) Stellar Populations (SSPs) of various metallicities using the latest Padova isochrones I study the color and luminosity evolution of GC populations over the wavelength range from U through K, providing an extensive grid of models for comparison with observations. I assume the intrinsic widths of the color distributions and LFs to be constant in time at the values observed today for the Milky Way orM31 halo GC populations. Taking the color distributions and LFs of the Milky Way or M31 halo GC population as a reference for old metal-poor GC populations in general, I study for which combinations of age and metallicity a secondary GC population formed in some violent star formation event in the history of its parent galaxy may or may not be detected in the observed GC color distributions. I also investigate the effect of these secondary GCs on the LFs of the total GC system. Significant differences are found among the diagnostic efficiencies in various wavelength regions. In particular, we predict the NIR to be able to reveal the presence of GC subpopulations with different age - metallicity combinations that may perfectly hide within one inconspicuous optical color peak. If the entire manifold of possible age - metallicity combinations is admitted for a secondary GC population, we find several cases where the resulting LF of the whole GC system is significantly affected and its turn-over could not serve as a reliable distance indicator. If, on the other hand, we assume some age - metallicity relation for GC populations, the second peak of the LFs vanishes and models indicate single-peak GC LFs even in GC systems with bimodal color distributions. A broad but sufficient age - metallicity relation is, for example, obtained if the secondary GC populations form in mergers of various spiral galaxy types from the ISM pre-enriched over the redshift range from z greater than or similar to 4.4 to z greater than or similar to 0. As a first illustrative example we apply our models to V- and I-band data presented by Larsen et al. ( 2001) for blue and red peak GCs in three early-type galaxies. We point out the importance of having multi-band information to independently constrain ages and metallicities of different GC subpopulations and again stress the diagnostic potential of K-band data in addition to optical observations. The models presented here will be used for the interpretation of multi-wavelength data on GC systems in galaxies of various types, luminosities and environments as well as on young star cluster systems in interacting galaxies and mergers. By independently constraining ages and metallicities of individual clusters we expect to shed light on both cluster and galaxy formation scenarios."],["dc.identifier.doi","10.1051/0004-6361:20031639"],["dc.identifier.fs","21431"],["dc.identifier.isi","000188249200016"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9815"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/48852"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Secondary globular cluster populations"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1063"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","1070"],["dc.bibliographiccitation.volume","401"],["dc.contributor.author","Anders, Peter"],["dc.contributor.author","von Alvensleben, U. F."],["dc.date.accessioned","2018-11-07T10:39:37Z"],["dc.date.available","2018-11-07T10:39:37Z"],["dc.date.issued","2003"],["dc.description.abstract","We include gaseous continuum and line emission into our g a l e v models for the spectral and photometric evolution of Simple Stellar Populations (SSPs) for various metallicities in the range 0.02 less than or equal to Z/Z. less than or equal to 2.5. This allows to extend them to significantly younger ages than before. They now cover the age range from 4 Myr all through 14 Gyr. We point out the very important contributions of gaseous emission to broad band fluxes and their strong metallicity dependence during very early evolutionary stages of star clusters, galaxies or subgalactic fragments with vigorous ongoing star formation. Emission-line contributions are commonly seen in these actively star-forming regions. Models without gaseous emission cannot explain their observed colors at all, or lead to wrong age estimates. We use up-to-date Lyman continuum (=Lyc) emission rates and decided to use recent empirical determinations of emission line ratios relative to H(beta) for subsolar metallicities. We justify this approach for all situations where no or not enough spectral information is available to determine all the parameters required by photoionization models. The effects of gaseous line and continuum emission on broad band fluxes are shown for different metallicities and as a function of age. In addition to the many filter systems already included in our earlier models, we here also include the HST NICMOS and Advanced Camera for Surveys (=ACS) filter systems."],["dc.identifier.doi","10.1051/0004-6361:20030151"],["dc.identifier.isi","000181929900025"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9804"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/46093"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Spectral and photometric evolution of young stellar populations: The impact of gaseous emission at various metallicities"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","843"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","861"],["dc.bibliographiccitation.volume","447"],["dc.contributor.author","Temporin, S."],["dc.contributor.author","von Alvensleben, U. F."],["dc.date.accessioned","2018-11-07T10:09:46Z"],["dc.date.available","2018-11-07T10:09:46Z"],["dc.date.issued","2006"],["dc.description.abstract","This paper is part of a series devoted to a detailed analysis of the properties of the compact group CG J1720- 67.8 and its member galaxies with the aim of shedding light on its evolutionary history. Here we interpret our previously published observational results through comparison with chemically consistent spectrophotometric evolutionary synthesis models to gain further clues to the evolution of the galaxies in this group. In order to reduce the number of free parameters, we considered the simplest case of a single burst of star-formation turned on after 11-12 Gyr of undisturbed galaxy evolution. However, we also briefly explored the effect of multiple, interaction-induced bursts of star-formation. We found that the two spiral galaxies are consistent with interaction-induced strong starbursts switched on similar to 40 to 180 Myr ago and still active. For the early-type galaxy, a less than or similar to 0.9- 1.3 Gyr old star-formation event ( depending on the considered model) appears consistent with the observed properties. The comparison with models cannot rule out the possibility that this galaxy is already the result of a merger. Alternatively, a star-formation episode in this galaxy might have been triggered by gas inflow as a consequence of the interaction with the companion galaxies. Estimates of galaxy masses were derived from the comparison with the models. Finally our results are discussed in comparison with other well-studied, poor galaxy systems."],["dc.identifier.doi","10.1051/0004-6361:20053576"],["dc.identifier.fs","45040"],["dc.identifier.isi","000235777500005"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/9884"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/39714"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Interpreting the galaxy group CG J1720-67.8 through evolutionary synthesis models"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]