1202.4275
The effect of feedback on the emission properties of the WHIM
Roncarelli, Cappelluti, Borgani, Branchini, Moscardini
Half of all the unresolved X-ray BG in the 1-2 keV band must be emission from faint groups and WHIM. (Presently, 30-40% of baryons in the local universe still undetected; must be in the form of WHIM in LSS filaments at temperatures of 1e5-1e7 K.) Characterize the properties of X-ray emission of WHIM from (1) Galactic winds, (2) BH feedback and (3) star formation. Use simulation to calculate x-ray emission in the 0.3-10 keV range. O VII and O VIII lines increase by a factor of 3 due to GWs. GWs increase x-ray by factor of 2 in both clusters and WHIM.
1202.4277
A density independent formation of SPH
Saitoh, Makino
SPH assumes local density distribution differentiable; problems occur when there is contact discontinuity--unphysical repulsive force appears, resulting in the effective surface tension, suppressing KH and RT instabilities. Present new formulation of SPH that does not require differentiability of density. Seems to do well in instability tests.
1202.4321
A study of optical observing techniques for extra-galactic SNe remnants: Case of NGC 300
Millar, White, Filipovic
Using [S II]/Halpha > 0.4 in optical SNR surveys ad identifying feature of extra-galactic SNRs is a questionable technique, and very high-resolution images may be needed to confirm a valid identification of some egSNRs.
1202.4328
Ultra deep sub-kpc view of nearby massive compact galaxies
Trujillo, Carrasco, Ferre-Mateu
Study 4 nearby ultra-compact galaxies (M~1e11 Msun, R<1.5 kpc, z~0.15). These galaxies are typically found at high-z; they also share similar characteristics in size, mass, velocity dispersion, but also the shape profiles and age of stellar populations.
1202.4433 (1112.5045)
An anomaly in the angular distribution of quasar magnitudes: evidence for a bubble universe with a mass 1e21 Msun
Longo
Quasar magnitude anisotropy toward (alpha, delta)~(195 deg, 0 deg) for all wavelengths, can be explained by a massive bubble lens with 1e21 Msun with lens radius ~350 Mpc, with the lens subtending an angle 15 deg on the sky. Anomaly in the distribution of LRG, CMB and bulk flow all appear roughly in the same direction.
1202.4450
The XMM Cluster survey: the stellar mass assembly of fossil galaxies
Harrison, ... Liddle, et al
Fossile (cluster/group) systems formed early and in the highest density regions of the universe; fossil galaxies represent the end products of galaxy mergers in groups and clusters. Gap between BCG and 4th brightest cluster is positively correlated to: total luminosity / fraction luminosity of the brightest galaxy. The fossil galaxies (BCG in fossil systems) have stellar pops and SFH similar to normal brightest cluster galaxies; but the stellar masses of fossil galaxies are larger compared to normal BCG. Fossil systems have most (as high as 85%) of their optical luminosity within 1/2 r200, where for other systems it could be a low as 10%.
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