Day 25

Friday (already).  Photoz paper almost ready to put out into the World.


LBL INPA
GRB talk, re-read abstract
Antonio Cucchiara


GRB science: its own physics, factory of high energy gamma rays, SF tracers, diagnostics for the chemical evolution of interstellar and intergalactic medium.


* how do they trace SF?  GRB thought to be collapsing SNe (or NS binary merger) seen along spinning axis.  Can we see spectra of GRB?


LBL RPM
Testing strong-field CED and QED with intense field lasers, reread abstract
Antonino Di Piazza (MPI-Heidelberg)


Want to see back-reaction of a charged particle (i.e., e-) after emitting a photon in a strong field.  If the field is strong enough, one should be able to measure this back-reaction.  Also, look at the difference between classical and quantum equation of back-reaction.  Some not-understandable quotes about photon-only interference pattern.


1106.4308
The relative abundance of compact and normal massive early-type galaxies and its evolution from redshift z~2 to the present
Cassata, ...Grogin... et al.


* compact (vs normal) massive early types.  its abundance and evolution.  from z~2 to now.


563 early types (sSFR<1e-2 /Gyr), massive (M>1e10 Msun), morphologically spheroidal galaxies.    Significant evolution of the mass-size relation of early type galaxies---fractional increment almost independent on the stellar mass.  Early types formed at z>1 are preferentially small; evolution of mass-size relation at z<1 driven by both the continuous size growth of compact gals and appearance of new early types with large sizes.  Number density of early types increases rapidly (x5) from z~2 to 1, and more mildly from z~1 to 0 (x1.5).  Bulk of early types formed at z=1.


* what is the mass-size relation doing?  How does it evolve?  description not given in abstract.


1106.4007
Galaxy formation with self-consistently modeled stars and massive black holes. I: Feedback-regulated star formation and BH growth.
Kim, Wise, Alvarez, Abel


* another galaxy formation modeling code?


BH and galaxy co-evolution in a hierarchical structure formation paradigm.  AMR code Enzo modified to model the formation and feedback of molecular clouds at their characteristic scale of 15.2 pc and the accretion of gas onto a massive BH.  AGN radiative (X-ray) and mechanical (jets) feedback employed.  1e12 M_sun galo and 1e5 Msun BH at z=3 in LCDM sim: BH ionizes and heats surroundings (1e6K), suppresses SF & changes stellar distribution at core, locally dominant.  BH self-regulates by keeping ISM hot.


* what is the "feedback of molecular clouds" with it's scale 15.2 pc?


1106.4008
Constraining Type Ia supernovae progenitors from 3 years of SNLS data
Bianco, ...Perlmutter...  et al.


* Federica!  I didn't know she was on SNLS.


SNIa: thought to be Carbon-Oxygen WD accreting mass in a binary system---but details of genesis, nature of companion still uncertain.  Non-degenerate companion observable: flux excess in the early rise portion of the lightcurve, as ejecta impacts with companion.  Has a favorable viewing angle; intensity depends on the nature of the companion.  Search for such signature in SNLS by generating synthetic lightcurves (effects of shock included).   Shocking effect more prominent in rest-frame B than V band.  Rule out contribution from WL-RG binary systems to Type Ia SN > 10% at 2 sigma, or >20% at 3 sigma.


* wait, so was it or was it not detected?  Sounds like it wasn't detected?


1106.4284
GOODS-Hershel: the far-IR view of star formation in AGN host galaxies since z~3
Mullaney et al.


* AGN and star formation?  They supposedly go hand-in-hand.


GOODS-H: IR properties of X-ray AGN.  100um and 160um fluxes dominated by the host galaxies in most cases; hence a good SF signal.  No correlation between AGN levels and global SF activity.  SFR increase strongly with redshift, by x43(+30-20) from z<0.1 to z2-3 for AGN hosts of L_X 1e42-44 ergs/s. Consistent with sSFR increase by x25-50 of normal, SF (main-sequence) galaxies.  80+/-10 percent of moderate luminosity AGNs are hosted by main-sequence galaxies.  15+/-7 in quiescent galaxies, and <10 percent in strongly starbursting galaxies.  Derive fractions of all main sequence galaxies at z...(garbled text?)  Majority of moderate nuclear activity fueled by internal mechanisms rather than violent mergers--high redshift disk instabilities could be an important AGN feeding mechanism.  Stellar mass is the best indicator whether a galaxy hosts a moderate luminosity AGN.


* AGN occurrence mostly in "main sequence" galaxies--it's not fueled by mergers.
* main sequence galaxy:  This seems to be something that "disproves current theory of hierarchical galaxy formation".  Something analogous to the MS (HR diagram) of stars.


0610031
A primer on hierarchical galaxy formation: the semi-analytical approach (68 pages)
Baugh


Physics of galaxy formation.  Hierarchical paradigm.  SAM vs numerical simulations.  


0811.1554
Galaxies appear simpler than expected
Disney, Romano, Garcia-Appadoo, West, Dalcanton, Cortese


Galaxies: dynamics, star formation, chemical enrichment, SN & BH feedback.  Hierarchical theory--galaxies are assembled from smaller pieces.  Six parameters: mass, angular-momentum, baryon-fraction, age, size, merger history.  Galaxies detected through their HI radio frequency emission (no optical selection effects), show five independent correlations among six independent observables.  Single parameter undecernable.