Fritze-von Alvensleben, Uta

[["dc.bibliographiccitation.issue","204"],["dc.bibliographiccitation.seriesnr","204"],["dc.contributor.author","Moller, C. S."],["dc.contributor.author","Fritze-Von Alvensleben, U."],["dc.contributor.author","Calzetti, D."],["dc.contributor.author","Fricke, K. J."],["dc.date.accessioned","2018-11-07T09:32:17Z"],["dc.date.available","2018-11-07T09:32:17Z"],["dc.date.issued","2001"],["dc.identifier.isi","000175997600051"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/31720"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Astronomical Soc Pacific"],["dc.publisher.place","San Francisco"],["dc.relation.conference","24th General Assembly of the International-Astronomical-Union"],["dc.relation.crisseries","Proceedings of the ... Symposium of the International Astronomical Union"],["dc.relation.eventend","2000-08-18"],["dc.relation.eventlocation","Manchester, United Kingdom"],["dc.relation.eventstart","2000-08-15"],["dc.relation.isbn","1-58381-062-5"],["dc.relation.ispartof","The extragalactic infrared background and its cosmological implications"],["dc.relation.ispartofseries","Symposium International Astronomical Union; 204"],["dc.title","Metallicities and dust in high-z galaxies"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["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","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","819"],["dc.bibliographiccitation.issue","3"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.lastpage","834"],["dc.bibliographiccitation.volume","358"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Duc, P. A."],["dc.contributor.author","von Alvensleben, U. F."],["dc.contributor.author","Martin, P."],["dc.contributor.author","Fricke, K. J."],["dc.date.accessioned","2018-11-07T10:45:53Z"],["dc.date.available","2018-11-07T10:45:53Z"],["dc.date.issued","2000"],["dc.description.abstract","We present deep optical B,V,R images of a sample of 10 interacting systems which were selected for their resemblance to disturbed galaxies at high redshift. Photometry is performed on knots in the tidal features of the galaxies. We calculate a grid of evolutionary synthesis models with two metallicities and various burst strengths for systems consisting of some fraction of the stellar population of a progenitor spiral plus starburst. By comparison with two-color diagrams we interpret the photometric data, select from a total of about 100 condensations 36 star-forming objects that ale located in the tidal features and predict their further evolution. Being more luminous by 4 mag than normal HII regions we argue that these objects could be tidal dw,uf galaxies or their progenitors, although they differ in number and mean luminosity from the already known tidal dwarf galaxies typically located at the end of tidal tails in nearby giant interacting systems. From comparison with our models we note that all objects show young burst ages. The young stellar component formed in these tidal dwarf candidates contributes up to 18% to the total stellar mass at the end of the starburst and dominates the optical luminosity. This may result in fading by up to 2.5 mag in B during the next 200 Myrs after the burst."],["dc.identifier.isi","000088424200011"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/47610"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation.issn","0004-6361"],["dc.title","Tidal dwarf candidates in a sample of interacting galaxies"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["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.artnumber","L79"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal Letters"],["dc.bibliographiccitation.volume","579"],["dc.contributor.author","Weilbacher, Peter M."],["dc.contributor.author","Fritze-von Alvensleben, Uta"],["dc.contributor.author","Duc, P. A."],["dc.contributor.author","Fricke, K. J."],["dc.date.accessioned","2018-11-07T09:49:22Z"],["dc.date.available","2018-11-07T09:49:22Z"],["dc.date.issued","2002"],["dc.description.abstract","We present Very Large Telescope observations of the interacting system AM 1353-272. Using the FORS2 instrument, we studied the kinematics of the ionized gas along its prominent tidal tails and discovered strikingly large velocity gradients associated with seven luminous tidal knots. These kinematical structures cannot be caused by streaming motion and most likely do not result from projection effects. More probably, instabilities in the tidal tails have led to the formation of kinematically decoupled objects that could be the progenitors of self-gravitating tidal dwarf galaxies."],["dc.identifier.doi","10.1086/345318"],["dc.identifier.isi","000179063400007"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/35496"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.relation.issn","0004-637X"],["dc.title","Large velocity gradients in the tidal tails of the interacting galaxy AM 1353-272 (\"The Dentist's Chair\")"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","147"],["dc.bibliographiccitation.journal","Proceedings of the International Astronomical Union"],["dc.bibliographiccitation.lastpage","151"],["dc.bibliographiccitation.volume","187"],["dc.contributor.author","Fritze, Uta"],["dc.contributor.author","Alvensleben, V."],["dc.contributor.author","Lindner, U."],["dc.contributor.author","Fricke, K. J."],["dc.contributor.editor","Nomoto, Ken'ichi"],["dc.contributor.editor","Truran, James W."],["dc.date.accessioned","2018-11-07T10:32:56Z"],["dc.date.available","2018-11-07T10:32:56Z"],["dc.date.issued","2002"],["dc.identifier.isi","000176502200018"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/44476"],["dc.language.iso","en"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Springer"],["dc.publisher.place","Dordrecht"],["dc.relation.conference","IAU Symposium 187 on \"Cosmic Chemical Evolution\""],["dc.relation.eventend","1997-08-30"],["dc.relation.eventlocation","Kyoto"],["dc.relation.eventstart","1997-08-26"],["dc.relation.isbn","1-4020-0449-4"],["dc.relation.isbn","1-4020-0448-6"],["dc.relation.issn","0074-1809"],["dc.title","Chemical evolution of spiral galaxies from redshift 4 to the present"],["dc.type","conference_paper"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dspace.entity.type","Publication"]]