Italian Art Song Masterclass with Carlo Bergonzi, November 16, 1988

This is the concert program of the Italian Art Song Masterclass with Carlo Bergonzi performance on Wednesday, November 16, 1988 at 10:00 a.m., at the Boston University Concert Hall, 855 Commonwealth Avenue, Boston, Massachusetts. Works performed were Se tu m'ami by Giovanni Battista Pergolesi, Cangiò d'aspetto, from Admeto by George Frederic Handel, Lascia ch'io pianga, from Rinaldo by George Frederic Handel, Piangerò la sorte mia, from Giulio Cesare by George Frederic Handel, L'alba Separa dalla luca l'omba by Paolo Tosti, Sole e Amore by Giacomo Puccini, and I pastori by Ildebrando Pizzetti. Digitization for Boston University Concert Programs was supported by the Boston University Humanities Library Endowed Fund

Piano Recital, May 4, 1995

This is the concert program of the Piano Recital performance on Thursday, May 4, 1995 at 6:00 p.m., at the Marshall Room, 855 Commonwealth Avenue, Boston, Massachusetts. Works performed were from Pictures at an Exhibition: Promenade, Gnomus by Modest Mussorgsky, Sonata Op. 26, No. 3, Movement 1 by Muzio Clementi, Valse brilliante Op. 34 No. 2 by Frederic Chopin, Sonata Quasi una Fantasia Op. 27 No. 2, Movement 1 by Ludwig van Beethoven, Sonata K545 in C major, movement 1 by Wolfgang Amadeus Mozart, Two Valses: Op. 64 No. 3 and Op. 70 No. 1 by Frederic Chopin, From the French Clavier Suite in c minor, Courante by Johann Sebastian Bach, Two Preludes: Op. 32 No. 5 in G major, Op. 3 No. 2 in c sharp minor by Sergei Rachmaninov, Traumerei by Robert Schumann, and Nocturne Op. 48 No. 1 in c minor by Frederic Chopin. Digitization for Boston University Concert Programs was supported by the Boston University Humanities Library Endowed Fund

Henry IV, Part I (1982)

Playwright: William Shakespeare Director: Hal J. Todd Set Design: Frederic Youens Costumes: Eliza Chugg Academic Year: 1981-1982https://scholarworks.sjsu.edu/productions_1980s/1047/thumbnail.jp

Faculty recital by Alfred Kanwischer, piano, March 30, 1965

This is the concert program of the Faculty Recital by Alfred Kanwischer, piano on Tuesday, March 30, 1965 at 8:30 p.m., at the Concert Hall, 855 Commonwealth Avenue. Works performed were Choral Prelude "Wachet auf, ruft uns die Stimme" by Johann Sebastian Bach (Busoni), Organ Prelude and Fugue (St. Anne's Fugue) in E Flat major by J. S. Bach (Busoni), Three Improvisations by Alfred Kanwischer, Nocturne in C minor, Op. 48, No. 1 by Frederic Chopin, Ballade in A flat major, Op. 47 by Frederic Chopin, Sonata in D major, Op. 10, No. 3 by Ludwig van Beethoven, Sonata in F minor, Op. 57 by L. v. Beethoven. Digitization for Boston University Concert Programs was supported by the Boston University Humanities Library Endowed Fund

Jingchao Zhou, piano

Frederic ChopinJohannes Brahm

Galaxy groups in the 2dF redshift survey: The catalogue

We construct a galaxy groups catalogue from the public 100K data release of the 2dF galaxy redshift survey. The group identification is carried out using a slightly modified version of the group finding algorithm developed by Huchra & Geller. Several tests using mock catalogues allow us to find the optimal conditions to increase the reliability of the final group sample. A minimum number of 4 members, an outer number density enhancement of 80 and a linking radial cutoff of $200 km sec^{-1}$, are the best obtained values from the analysis. Using these parameters, approximately 90% of groups identified in real space have a redshift space counterpart. On the other hand the level of contamination in redshift space reaches to 30 % including a $\sim 6$ of artificial groups and $\sim 24$ of groups associated with binaries or triplets in real space. The final sample comprise 2209 galaxy groups covering the sky region described by Colless et al. spanning over the redshift range of $0.003 \leq z \leq 0.25$ with a mean redshift of 0.1.Comment: Accepted for publication in the MNRAS. 8 figures 8 page

The Local Group as a test of cosmological models

The dynamics of the Local Group and its environment provide a unique challenge to cosmological models. The velocity field within 5h-1 Mpc of the Local Group (LG) is extremely ``cold''. The deviation from a pure Hubble flow, characterized by the observed radial peculiar velocity dispersion, is measured to be about 60km/s. We compare the local velocity field with similarly defined regions extracted from N-body simulations of Universes dominated by cold dark matter (CDM). This test is able to strongly discriminate between models that have different mean mass densities. We find that neither the Omega=1 (SCDM) nor Omega=0.3 (OCDM) cold dark matter models can produce a single candidate Local Group that is embedded in a region with such small peculiar velocities. For these models, we measure velocity dispersions between 500-700km/s and 150-300km/s respectively, more than twice the observed value. Although both CDM models fail to produce environments similar to those of our Local Group on a scale of a few Mpc, they can give rise to many binary systems that have similar orbital properties as the Milky Way--Andromeda system. The local, gravitationally induced bias of halos in the CDM ``Local Group'' environment, if defined within a sphere of 10 Mpc around each Local Group is about 1.5, independent of Omega. No biasing scheme could reconcile the measured velocity dispersions around Local Groups with the observed one. Identification of binary systems using a halo finder (named Skid (http://www-hpcc.astro.washington.edu/tools/DENMAX for a public version)) based on local density maxima instead of a simple linking algorithm, gives a much more complete sample. We show that a standard ``friend of friends'' algorithm would miss 40% of the LG candidates present in the simulations.Comment: Latex file (19 pages) + 13 figures. Submitted to New Astronomy. Two MPEG movies were not included. Also available (this time with the movies) at http://www-hpcc.astro.washington.edu/faculty/fabio/index.htm

The Build-up of the Colour-Magnitude Relation as a Function of Environment

We discuss the environmental dependence of galaxy evolution based on deep panoramic imaging of two distant clusters taken with Suprime-Cam as part of the PISCES project. By combining with the SDSS data as a local counterpart for comparison, we construct a large sample of galaxies that spans wide ranges in environment, time, and stellar mass (or luminosity). We find that colours of galaxies, especially those of faint galaxies ($M_V>M_V^*+1$), change from blue to red at a break density as we go to denser regions. Based on local and global densities of galaxies, we classify three environments: field, groups, and clusters. We show that the cluster colour-magnitude relation is already built at $z=0.83$. In contrast to this, the bright-end of the field colour-magnitude relation has been vigorously built all the way down to the present-day and the build-up at the faint-end has not started yet. A possible interpretation of these results is that galaxies evolve in the 'down-sizing' fashion. That is, massive galaxies complete their star formation first and the truncation of star formation is propagated to smaller objects as time progresses. This trend is likely to depend on environment since the build-up of the colour-magnitude relation is delayed in lower-density environments. Therefore, we may suggest that the evolution of galaxies took place earliest in massive galaxies and in high density regions, and it is delayed in less massive galaxies and in lower density regions.Comment: 23pages, 19 figures, accepted for publication in MNRA

The Relation Between Halo Shape, Velocity Dispersion and Formation Time

We use dark matter haloes identified in the MareNostrum Universe and galaxy groups identified in the Sloan Data Release 7 galaxy catalogue, to study the relation between halo shape and halo dynamics, parametrizing out the mass of the systems. A strong shape-dynamics, independent of mass, correlation is present in the simulation data, which we find it to be due to different halo formation times. Early formation time haloes are, at the present epoch, more spherical and have higher velocity dispersions than late forming-time haloes. The halo shape-dynamics correlation, albeit weaker, survives the projection in 2D (ie., among projected shape and 1-D velocity dispersion). A similar shape-dynamics correlation, independent of mass, is also found in the SDSS DR7 groups of galaxies and in order to investigate its cause we have tested and used, as a proxy of the group formation time, a concentration parameter. We have found, as in the case of the simulated haloes, that less concentrated groups, corresponding to late formation times, have lower velocity dispersions and higher elongations than groups with higher values of concentration, corresponding to early formation times.Comment: MNRAS in press (10 pages, 10 figures