Day 754

Tuesday.

1409.7693
Clustering properties of moderate luminosity X-ray selected Type 1 and Type 2 AGN at z~3
Allevato et al

Type 1 and 2 COSMOS AGN at z=3 inhabit DM haloes with typical mass of log Mh=12.84 pm 0.1 and 11.73 pm 0.4, respectively.  This result requires a drop in the halo masses of Type 1 and 2 COSMOS AGN at z~3 compared to z<2 XMM COSMOS AGN with similar luminosities.  Additionally, we infer that unobscured COSMOS AGN at z~3 reside in 10x more massive haloes compared to obscured COSMOS AGN (2.6 sigma).  The result extend to z~3 that found in COSMOS at z<1, and rules out the picture in which obscuration is purely an orientation effect.   A model which assumes that the AGN activity is triggered by major mergers is quite successful in predicting both the low halo mass of COSMOS AGN and the typical mass of luminous SDSS quasars at z~3, which the latter inhabiting more massive haloes respect to moderate luminosity AGN.  Alternatively, can argue at least for Type 1 COSMOS AGN, that they are possibly representative of an early phase of fast (Eddington limited) BH growth induced by cosmic cold flows or disk instabilities.  Given the moderate luminosity, these new fast growing BHs have masses of e7-8 Msun at z~3 which might evolve into e8.5-9 Msun mass BHs at z=0.  Following the clustering measurements, argue that this fast BH growth at z~3 in AGN with moderate luminosity occurs in DMHs with typical mass of 6e12 Msun/h.
1409.7701
The Norma Arm region Chandra survey: X-ray populations in the spiral arms
Fornasini et al

1415 X-ray sources in Norma arm, 1130 are point-like sources.  Since most sources have too few counts to permit individual classification, they are divided into five spectral groups defined by their quantile properties.  Analyze stacked spectra of X-ray sources within each group, in conjunction with their fluxes, variability ,and IR counterparts, to ID the dominant population in the survey.  Find that ~50% of sources are FG sources located within 1-2 kpc, which is consistent with expectations from previous surveys.  ~20% of sources are likely located in the proximity of the Scutum-Crux and near Norma arm, while 30% are more distant, in the proximity of the far Norma arm or beyond.  Argue that a mixture of B and non-B CVs dominates the Scutum-Crux and near Norma arms, while intermediate polars and high-mass stars (isolated or in binaries) dominate the far Norma arm.  Population of very hard sources in the vicinity of the far Norma arm and AGN dominate the hard X-ray emission, but the distribution curve flattens at fainter fluxes.  Find good agreement between the observed distribution and predictions based on other surveys.

1409.7718
Comparing Planck and WMAP: maps, spectra, and parameters
Larson, Weiland, Hinshaw, Bennett

Examine the consistency of WMAP9 and Planck data.  Compare sky maps, PS, and inferred LCDM cosmo parameters.  Residual dipoles are seen in the WMAP and Planck sky map differences, but are consistent within the uncertainties and are not large enough to explain the widely-noted differences in angular PS at higher ell.  After removing residual dipoles and galactic FG, the residual difference maps exhibit a quadrupole and other large-scale systematic structure.  Identify this structure as possibly originating from Planck's beam side lobe pick-up, but note that it appears to have insignificant cosmological impact.  Develop an extension of the internal linear combination technique and find features that plausibly originate in the Planck data. Examine LCDM model fits to the angular PS and conclude that at the ~2.5% difference in the spectra at multipoles greater than ell~100 are significant at the 3-5 sigma level.  Revisit the analysis of WMAP's beam data and conclude that previously derived uncertainties are robust and cannot explain the PS differences.  Finally, examine the consistency of the LCDM parameters inferred from each data set taking into account the fact that both experiments observe the same sky, but cover different multipole ranges, apply different sky masks, and have different noise.  While individual parameter values agree within the uncertainties, the 6 parameters taken together are discrepant at the ~6 sigma level, with chi2=56 for 6 dof (PTE=3e-10).  Of the 6 parameters, chi2 is best improved by marginalizing over Omega_c h^2, given chi2=5.2 for 5 degrees of freedom.  Find that perturbing the WMAP window function by its dominant beam error profile has little effect on Omega_c h^2, while perturbing the Planck window function by its corresponding error profile has a much greater effect on Omega_c h^2.

1409.8246
Strong chromatic microlensing in HE0047-1756 and SDSS1155+6346
Rojas, et al

Use spectra of double lensed quasars to study their unresolved structure through microlensing.  No strong evidence of ML except in Lya line in SDSS 1155, which show strong differences in the shapes for A and B images.  (But the continuum of B image spectrum is strongly contaminated by the lens galaxy.)  Using the flux ratios of the emission lines, detected strong chromatic ML in the continuum in both lens systems.  Contrary to other lens systems, the chromaticity detected is large enough to fulfill the thin disk prediction.  The inferred sizes, however, are very large compared to the predictions of this model.