Friday. I think Nina is mad at me. I'm trying my best not to get depressed, but maybe I'm doing too good of a job. Saturday. Went IKEA shopping with Zahra and Jef (Zahra has a nice apartment). Sunday. Went back to IKEA to purchase the closet with the correct height. Rented a manual van from IKEA, and panicked the whole way through. Helped Jef move his stuff to his new apartment, then he helped me move my wrong-sized closet back to IKEA. Also, I realized that I should grow up a bit more. Wished I were in Siegburg instead of panicking. Monday. No internet until the 20th, will read astro-ph from work till then?
Astro Colloquium, Bonn (9 Dec 2011, 11:00, 0.02)
Non-equilibrium chemistry in the shocked inner winds of AGB stars: a close look at the carbon star IRC+10216
Isabelle Cherchneff
Winds of AGN develops in the dust formation zone ("the inner wind"). The narrow region above the stellar photosphere is crossed by periodic shocks induced by the pulsation of the star. The postshock gas is characterized by an active chemistry which destroys and produces molecules, in particular chemical species that are not present in the photosphere. Present new results for the carbon star IRC+10216 based on the modeling of the inner wind: includes formation of water, hydrocarbons, aromatics, hydrides, halogens and phosphorous-bearing molecules. Compare results to latest data from Herschel. Prescription for dust formation in carbon stars discussed from synthesis of dust molecular precursors in these shocked gas layers.
Lunch Colloquium, bonn (7 Dec 2011, 12:45, 0.02)
A giant polar structure of streams, globular clusters and satellite galaxies around the MW
Marcel Pawlowski
Satellite galaxies of the MW show a significant amount of phase-space correlation: they are distributed in a highly inclined Disc of Satellites (DoS). Suggested explanations: infall of groups of dwarf galaxies, accretion along filaments, tidal origin. Extend previous studies on DoS by including orientations of streams of gas and stars, and the distributions of globular clusters within the halo of the MW. SHown: spatial distribution of MW globular clusters classified as young halo clusters is similar to the DoS and half of the analyzed streams align well with the DoS. The existence of a disc-line distribution of sybsystems, spreading from 10 kpc out to 250 kpc, becomes established beyond resonable doubt. potential consequences of this realizaton: if all satellite galaxies and young halo globular clusters are of tidal origin, then the MW does not have any luminous DM substructures and the missing satellites problem becomes a catastrophic failure. [failure of the problem?]
1112.0312
The Arizon CDFS environment survey (ACES): A Magellan/IMACS Spectroscopic survey of the Chandra deep field south
Cooper, Yan, Dickinson, Juneau, Lotz, Newman, Papovich, Salim, Walth, Weiner, Willmer
Spectra for 7277 unique sources in the CDFS field, down to R=24.1. 5080 secure redshifts across the 30'x30' extended CDFS region [no overlap with SDSS]. Enables local galaxy density (or environment) on relatively small scales (~1Mpc) to be measured at z<1 at a well-observed region of the sky. Describe motivation, design, and implementation of the survey; present a preliminary redshift and environment catalog. In addition, utilize the ACES catalog to assess the quality of photoz from both COMBO-17 and MUSYC imaging surveys of the CDFS.
1112.0313
A large population of massive compact post-starburst galaxies at z>1: implications for the size evolution and quenching mechanism of quiescent galaxies
Whitaker, Kriek, van Dokkum, Bezanson, Brammer, Frax, Labbe
Study the growth of the red sequence through the number density and structural evolution of a sample of young and old quiescent galaxies at 0<z<2 from COSMOS. Find large population of massive young recently quenched ("post-starburst") galaxies at z>1 that are almost non-existent at z<1; their number density is 5e-5 Mpc^-3 at z=2, and a factor of 10 less at z=0.5. Population consistent with a simple model in which all old quiescent galaxies were once identified as post-starburst galaxies. Overall population of quiescent galaxies have smaller sizes and slightly more elongated shapes at higher redshift. The most recently quenched galaxies at 1<z<2 are possibly smaller than older galaxies at that z; inconsistent with the idea that the evolution of the average size of quiescent galaxies is largely driven by continuous transformations of larger, star-forming galaxies (in which case the youngest quiescent galaxies would also be the largest). Instead, mergers or other mechanisms appear to be required to explain the size growth of quiescent galaxies from z=2 to the present.
1112.0317
Identification of a fundamental transition in a turbulently supported interstellar medium
Scannapieco, Gray, Pan
Sustaining turbulent support (which is as important as thermal pressure) requires continuous radiative cooling, such that the average cooling rate matches the decay rate of turbulent energy into the medium. Simulations show fundamental transition for 1d turbulent velocity of ~35 km/s. At turbulent velocities below ~35 km/s, correponding to temperatures below 3e5K, the medium is stable (time for gas to cool is roughly constant as a function of temperature); above the critical value, the gas is shocked into an unstable regime in which the cooling time increases strongly with temperature--substantial fraction of the ISM is unable to cool on a turbulent dissipation timescale. This leads to runaway heating and ejection of gas from any stratified medium with 1d turbulent velocity above ~35 km/s.
1112.0319
The DM density profile of the Fornax dwarf
Jardel, Gebhardt
Mass profile of Fornax modeled from axisymmetric Schwarzchild ([metric?]). Test a variety of parameterizations of DM density profiles; find cored models with uniform density rho_c = 1.6e-2 Msun/pc^3 fit better than the cuspy halos predicted by CDM. Intermediate-mass BH unable to detect; upper limit of M_BH < 3.2e4 Msun.
1112.0321
The LABOCA survey of the extended CDFS: clustering of submillimeter galaxies
Hickox, .. Smail, ... Gawiser, Lutz, et al
Clustering of SMGs at z=1-3. Clustering of SMGs at z~2 is consistent with measurements for optically selected qso's, supporting evolutionary scenarios linking starbursts and qsos. SMG's reside in haloes of characteristic mass ~6e12 Msun/h; demonstrate the z distribution of SMGs can be described remarkably well by combination of : cosmological growth of structure and the evolution of the molecular gas fraction in galaxies. Conclude that the powerful starbursts in SMGs likely represent a short-lived by universal phase in massive galaxy evolution, associated with the transition between cold gas-rich, star-forming galaxies and passively evolving systems.
1112.0495
Tomography and WL statistics
Munshi, Coles, Kilbinger
Derive generic predictions for lower order cumulants and their correlators for individual tomographic bins. Derive one- and two-point joint probability distribution function for the tomographic convergence maps from different bins as a function of angular smoothing scale. Modeling of WL statistics is obtained by adopting a detailed prescription for the underlying density contrast. Concentrate on the convergence field kappa and use top-hat filter. ...I have no idea what's going on with this paper.
1112.0503
Anisotropy in the matter distribution beyond the BAO scale
Faltenbacher, Li, Wang
Correlation of peaks (halos) and the overall matter distribution around it show more correlation for matter distributed along the direction of peak separation, and less for matter perpendicular to it. This happens at ~150 Mpc/h, larger than BAO scale of ~100 Mpc/h. Clustering is anisotropic!
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