Day 35

Friday!  Going to Myongdong for seafood later today, with Sasaki-san and others from KIAS (visiting from Kyoto).


1107.0963
The effect of the environment on the gas kinematics and the structure of distant galaxies
Jaffe, ..., Zaritsky et al


* EDisCS: ESO Distant Clusters Survey (MPA).  EDisCS aims at studying the evolution of cluster populations over more than 50% of cosmic time by comparing the photometric and spectroscopic properties of galaxies in rich clusters at z~0.5 and z>0.8 with those of galaxies in well studied nearby clusters.  Samples consist of the most luminous objects in eaach redshift band in the Las Campanas Cluster Survey, the largest area optical survey for distant clusters so far completed.  It runs in 3 stages: I. Cluster confirmation (get approximate z with 2-band photometry), II. Deep photometry (BVI photometry for 10 at z~0.5 and 10 at z>0.8; near-IR photometry at K' for near clusters, and J K' for distant clusters), III. Spectroscopy (spectra for possible cluster members; obtain both stellar population and kinematic information).
* Tully-Fisher: empirical relationship between luminosity and rotation velocity in spiral galaxies.
* Faber-Jackson: empirical power-law relation between luminosity and stellar velocity dispersion of elliptical galaxies.
* Fundamental plane: relationship between the effective radius, surface brightness and central velocity dispersion of normal elliptical galaxies.


From spectra, study the effects of cluster environments to kinematic disturbance of the galaxy, up to z~1, for 422 emission line galaxies in EDisCS.  Fraction of kinematically disturbed galaxies increases in clusters (wrt field); increases with cluster velocity dispersion; decreases with distance from the cluster center; remains constant with projected galaxy density.  Also study morphological disturbances in stellar light from HST/F814W images; disturbance fraction similar in all environments. Also study the dependence of Tully-Fisher, SF, and extent of the emission on environment: conclude that gas disks in cluster galaxies have been truncated, so SF more concentrated than in low-density environments.  If spirals turn into S0s, then mechanism efficiently disturbs SF gas and reduces their SFR---removed more efficiently from the outskirts of galaxies or driven towards the center (or both), helping to build the S0 bulges.  Physical processes involved in "disturbances" must be related to the intracluster medium, with galaxy-galaxy interactions playing only a limited role in clusters.


* galaxies may not appear morphologically disturbed, but the emission line can show disturbance.  The closer they are to the cluster core, the more disturbed (emission line wise) they are.  The disturbance are mostly from ICM, not from gg interactions.
* Nice paper/abstract.


1107.1049
GOODS-HERSCHEL: evidence for a UV extinction bump in galaxies at z>1
Buat et al.


* what's a UV extinction bump?


(I have a truncated abstract.)  Dust attenuation curves are useful to study galaxy dust properties as well as to interpret their intrinsic SED.  


1107.0972
Redshift evolution of the galaxy velocity dispersion function
Bezanson, van Dokkum, ... et al