Day 426

Friday.

1305.0268
SINFONI/VLT 3D spectroscopy of massive galaxies: strong rotational support at z~1.4
Buitrago et al

Look for dynamical evidence of more disk-like galaxies (not just morphological) at higher z.  Use NIR integrated field spectra in the H-band for 10 massive galaxies (M* > 1e11 h_70^-2 Msun) at z~1.4.  Sample selected for ability to measure kinematics (EW[OII]>15AA), but not on morphology.  About 50% of galaxies compatible with being rotationally supported disks, in agreement with morphological expectations.  Majority of the sample of massive galaxies show clear and fairly large rotational velocity maps, implying that massive galaxies acquire rapidly rotational support, and hence gravitational equilibrium.  Also show evidence for ongoing interactions and mergers.  Massive galaxies at the epoch are not a homogeneous sample, but show significant diversity and must have continued evolution beyond the fading of stellar populations, to becomes the massive galaxies found today.



1305.0286
Cosmological growth and feedback from supermassive black holes
Mocz, Blundell, Fabian

Develop scenario for growth of SMBHs, assuming growth due to accretion only, to learn about the evolution of the BH mass function from z=3 to 0, and from it calculate the energy budgets of different modes of feedback.  Tune the parameters of the model by matching the derived X-ray LF with the observed XLF of AGN.  Calculate the amount of comoving kinetic and bolometric feedback as a function of z, derive a kinetic luminosity function and estimate the amount of kinetic feedback and PdV work done by classical Fanaroff-Riley II (FR II) radio sources.  Also derive the radio luminosity function for FR IIs from synthesized population and set constraints on jet duty cycles.Around 1/6 of the jet power from FR II sources goes into PdV work done in the expanding lobes during the time the jet is on.  Anti hierarchical growth of BHs is seen in the model due to addition of an amount of mass being accreted onto all BHs independent of the BH mass.  The contribution to the total kinetic feedback by AG in low accretion, kinetically efficient mode is found to be the most significant at z<1.5.  FR II feedback is found to be a significant mode of feedback above redshifts z~1.5, which has not been highlighted by previous studies.

1305.0350
Detection of galaxy assembly bias
Wang, Weinmann, De Lucia, Yang

Assembly bias: describes the finding that clustering of DM haloes depends on halo formation time at fixed halo mass.  In this paper, analyse the influence of assembly bias on galaxy clustering using both SAMs and observational data.  At fixed stellar mass, SAMs predict that the clustering of central galaxies depends on the sSFR, with more passive galaxies having a higher clustering amplitude [that doesn't seem like the correct interpretation.  SAMs presumably populate passive galaxies at the center of massive haloes, which are more clustered to begin with].  Find similar trends using SDSS group catalogues, and verify that these are not affected by possible biases due to the group finding algorithm.  Low mass central galaxies reside in narrow bins of halo mass, so the observed trends of higher clustering amplitude for galaxies with lower sSFR is not driven by variations of the parent halo mass.  Argue that the clustering dependence on sSFR represent a direct detection of assembly bias.  In addition, contrary to what is expected based on clustering of DM haloes, find that low-mass central galaxies in SAMs with larger host halo mass have a lower clustering amplitude than their counter-parts residing in lower mass haloes.  This results from the fact that, at fixed stellar mass, assembly bias has a stronger influence on clustering than the dependence on the parent halo mass.

1305.0364
Structural parameters for globular clusters in M31
Wang, Ma

Surface brightness profiles for 79 globular clusters in M31 from HST images.  11 clusters best fitted by Sersic with n>2; most fit well with King model (seems like exponential in the kinetic energy).  There is a bimodality in the size distribution of M31 clusters at large radii, which is different from their Galactic counterparts.  In general, the properties of clusters in M31 and the MW fall in the same regions of parameter spaces.  The tight correlations of cluster properties indicate a "fundamental plane" for clusters, which reflects some universal physical conditions and processes operating at the epoch of cluster formation.

1305.0476
Mirror actively deformed and regulated for applications in space: design and performance
Laslandes et al

AO for space-based telescopes.  24-actuator, 90mm-diameter active mirror; designed for expected wavefront errors from 3-m class lightweight primary mirrors, while also taking into account constraints for space use.  Correction better than 10 nm RMS.  Composed of telescope simulator, active correction loop, a PSF imager, and Fizeau interferometer.  Maturity to TRL4 [?].

1305.0498
Can dark energy be gravitational waves?
Biermann, Harms

This may explain DE's strength and its time-evolution.  DE is the ensemble of coherent bursts of GWs originally produced when the first generation of SMBHs formed.  These solitons get their initial energy as well as keep up their energy density throughout the evolution of the universe by stimulating emission from a BG, a process which we model by working out this energy transfer in a Boltzmann equation approach.  New Planck data suggest that DE has increased in strength over cosmic time, supporting the concept here.  The transit of these gravitational wave solitons may be detectable.  Key tests include pulsar timing, clock jitter and the radio background.