References

F., Steinmetz M., Eke V. R., 2003a, ApJ, 591, 499 Benson A. J., Frenk C. S., Lacey C. G., Baugh C. M., Cole S., 2002, MNRAS, 333, 177 Brinchmann J. et al. 2004, MNRAS, 351, 1151 Giovanelli, R. et al. 1997, AJ, 113, 53 Governato F., Mayer L., Wadsley J., Gardner J. P., Willman B., Hayashi E., Quinn T., Stadel J., Lake G., 2004, ApJ, 607 Governato F., Stinson G., Wadsley J. & Quinn, T. 2005 (astro-ph 0509263) Gurovich, S., McGaugh, S. S., Freeman, K. C., Jerjen, H.,...

Measuring Structural Properties Of Galaxies In The Local Universe

Driver1, Jochen Liske2 and Alister W. Graham1 1 Australian National University, Mount Stromlo Observatory, Australia. 2European Southern Observatory, Germany. * paul mso.anu.edu.au Abstract The Millennium Galaxy Catalogue provides a representative and complete sample of nearby galaxies for structural analysis. GIM2D is used to model the light profiles for over 10000 resolved galaxies, using three different schemes R1 4+Exponential, R1 n+Exponential, and R1 n. The...

Assessment and Calibration of Star Formation Tracers

Since the days of IRAS the far-infrared luminosities of galaxies have been applied as quantitative measures of the SFR (see Kennicutt 1998a and references therein). This diagnostic is especially useful in extreme starburst galaxies, where the dust re-emits virtually all of the luminosity of the galaxy and young stars dominate the dust heating thus making the infrared luminosity essentially a bolometric measure of the SFR. However in normal galaxies all of these conditions are broken dust only...

Specific Star Formation Rates

Redshift and SFR distributions for both samples can be found in Figure 1 of Bauer et al. (2005). The majority of galaxies in the full samples (52 for MUNICS and 80 for FDF) have detectable SF, via the OII A3727 emission feature, and the closely matching redshift distributions indicating little redshift bias in sample selection. The maximum SFR increases with redshift, and is consistent between the two samples. Figure 1 shows the SSFR versus galaxy stellar mass as a function of redshift, to z...

Color Magnitude Diagram

The color-magnitude diagram (Figure 1) shows two main cluster populations a red one around F435W-F555W 0.7 (likely globular clusters) and another, broader distribution around F435W-F555W 0, which are likely young cluster candidates. Figure 1. NGC 45 color magnitude diagram. Here we plot objects with UBVI photometry. Approximately 3400 stars are shown (black dots) and 52 star cluster candidates. Filled squares correspond to a 1-10 Myr cluster population, filled triangles to cluster age 10-100...

Azimuthal Velocities from PV Diagram Modeling

The envelope tracing method is sensitive to the changing signal-to-noise ratio of the data with z. To account for this effect and the radial gas distribution, we have generated galaxy models. The Ha image presented in Fig. 1 was used to obtain estimates of the radial density profile at each of the heights considered in the model. Because the distribution of the DIG is not axisymmetric, the profiles were modified by hand to better match the shape of the data PV diagrams. The amplitude of the...

Dark Halo Evolution

Figure 2 shows the relationship between Vmax and rmax for all of our surviving satellites before accretion (open circles) and at z 0 (solid circles). The line running through the open points reflects the mean relationship expected Figure 2. Open circles show the radius of the maximum rotation velocity, rmax versus the maximum rotation velocity Vmax for our ensemble of (field) dwarf galaxies before they were accreted onto the host halo. These points include only those systems that survive until...

Summary and Outlook

In conclusion, it is certainly encouraging to reflect on the advances made over the last few years in charting the high redshift universe and in determining some important physical characteristics of the galaxies which inhabit it. Galaxies which are sufficiently bright to be detected in deep imaging surveys exhibit high star formation rates, of the order of tens of solar masses per year rapid timescales of chemical enrichment and stellar mass assembly, of the order of a few hundred Myr and the...

Two Custombuilt Integral Field Units

As mentioned above, measuring az requires spectroscopy at moderately high spectral resolution of diffuse low surface brightness light. To achieve this, we have built two special-purpose wide-field IFUs consisting of large aperture fibers which carry light from a focal plane to the pseudo-slit of a pre-existing spectrograph. The diameter of the fibers is maximized while providing a spectral resolution of no less than R 8000. The maximum number of fibers is then determined by the length of the...

Radiative Transfer Equation in Spherical Symmetry

In addition to eq. (1) - (4) we solve non-relativistic, time-independent equation for radiation transport in spherical geometry i * j (r) - Kv (r) Iv , (10) where Iv Iv (r, ) is the intensity of radiation of frequency v, at radius r and in the direction cos d, where d is the angle between the outward normal and photon direction. kv (r) is the emissivity and jv (r) opacity at radius r. Our scheme of solving this equation is similar to method from Mihalas & Mihalas (1984) and York (1980)....

Rotation Curve Fits

We fit the combined rotation curves with pseudo-isothermal and NFW ree halos for the minimum disk case. We also fit an NFW constrained halo which was required to match the velocities at the outer radii of each galaxy, in effect, constraining the concentrations to agree with cosmology. We highlight the Figure 1. Top left coverage of the DensePak data for UGC 5750, overlaid on a Ha image. Top right observed velocity field of UGC 5750 derived from the DensePak data. Bottom left comparison of the...

Frictional Torque

In a classic paper, Tremaine & Weinberg (1984) laid out the mathematical apparatus for friction in a spherical system. Following the precepts of Lynden-Bell & Kalnajs (1972), they derived a formula for the torque experienced by a rotating perturbation potential, . They work in action-angle variables (see Binney & Tremaine 1987, 3.5). In a spherical potential, there are two nonzero actions the total angular momentum per unit mass L J and the radial action Jr, each associated with two...

Introduction

The morphology-density relationship (Oemler 1974 Melnick & Sargent 1977 Treu et al. 2003) is one of the clearest examples of the effect that clusters have on their member galaxies. There are several cluster processes that may contribute to this observed effect (Treu et al. 2003). ISM-ICM stripping (which includes both ram-pressure stripping and turbulent viscous stripping) may be among the most important processes in the transformation of late-type cluster spirals into Sa's and S0's. This...

Discussion

Combining the new data with the old, we argue (a) If attributed to gravitation, changes in velocity of galactic size over galactic scales, as seen here, require masses of galactic proportions. On dimensional grounds the velocity wrench AV ( 200 kms-1) seen at VIRGOHI 21 over a conservative length-scale Ax ( 14 kpc 5 x 1022 cm 3 arc minutes at the Virgo Cluster distance of 16 Mpc Minchin et al. 2005) implies a mass M > Figure 2. As Fig. 1, but expanded and superimposed on a negative of our...

Reprocessing of IRAS Data

We obtained the IRAS fluxes at 12, 25, 60 and 100 m using the utility ADDSCAN SCANPI at IPAC. We followed the recommendation for the calculation of the total fluxes and visually inspected all spectra in order to check for (i) the presence of cirrus emission, (ii) confusing with neighboring galaxies and (iii) the significance of the detection (e.g. confusing with noise spikes). A more detailed description of the data processing will be presented in Lisenfeld et al. (in prep.). This reprocessing...

Damped Lyman alpha Systems Early Stages in the Formation of Spiral Galaxies

While an evolutionary link between star-forming galaxies at z 2 3 and the spheroidal component of the local galaxy population is strongly suggested by the available evidence, an analogous connection for DLAs is still a matter for debate. The working hypothesis that in DLAs we see the progenitors of today's disk galaxies like the Milky Way (Wolfe et al. 1986), while consistent with the kinematics of the associated metal absorption lines (Wolfe et al. 2005), runs into some difficulties when...