We explore the connection between different classes of active galactic nuclei (AGNs) and the evolution of their host galaxies, by deriving host galaxy properties, clustering, and Eddington ratios of AGNs selected in the radio, X-ray, and infrared (IR) wavebands. We study a sample of 585 AGNs at 0.25 < z < 0.8 using redshifts from the AGN and Galaxy Evolution Survey (AGES). We select AGNs with observations in the radio at 1.4 GHz from the Westerbork Synthesis Radio Telescope, X-rays from the Chandra XBoötes Survey, and mid-IR from the Spitzer IRAC Shallow Survey. The radio, X-ray, and IR AGN samples show modest overlap, indicating that to the flux limits of the survey, they represent largely distinct classes of AGNs. We derive host galaxy colors and luminosities, as well as Eddington ratios, for obscured or optically faint AGNs. We also measure the two-point cross-correlation between AGNs and galaxies on scales of 0.3-10 h −1 Mpc, and derive typical dark matter halo masses. We find that: (1) radio AGNs are mainly found in luminous red sequence galaxies, are strongly clustered (with M halo ∼ 3 × 10 13 h −1 M ⊙ ), and have very low Eddington ratios (λ 10 −3 ); (2) X-rayselected AGNs are preferentially found in galaxies that lie in the "green valley" of color-magnitude space and are clustered similar to typical AGES galaxies (M halo ∼ 10 13 h −1 M ⊙ ), with 10 −3 λ 1; (3) IR AGNs reside in slightly bluer, slightly less luminous galaxies than X-ray AGNs, are weakly clustered (M halo 10 12 h −1 M ⊙ ), and have λ > 10 −2 . We interpret these results in terms of a simple model of AGN and galaxy evolution, whereby a "quasar" phase and the growth of the stellar bulge occurs when a galaxy's dark matter halo reaches a critical mass between ∼10 12 and 10 13 M ⊙ . After this event, star formation ceases and AGN accretion shifts from radiatively efficient (optical-and IR-bright) to radiatively inefficient (optically faint, radio-bright) modes.

Objective This study evaluates the long-term outcomes, biliary complication rates, and risk factors for biliary complications after liver transplantation from donation after cardiac death (DCD) donors. Summary Background Data Recent enthusiasm toward increased use of DCD donor livers is mitigated by high biliary complication rates. Predictive risk factors for the development of biliary complications after DCD liver transplantation remain incompletely defined. Methods We performed a retrospective review of 1157 donation after brain death (DBD) and 87 DCD liver transplants performed between January 1, 1993 and December 31, 2008. Patient and graft survivals, and complication rates within the first year of transplantation were compared between DBD and DCD groups. Cox proportional hazards models were used to assess the influence of potential risk factors. Results Patient survival was significantly lower in the DCD group compared to the DBD group at 1, 5, 10 and 15 years (DCD: 84%, 68%, 54%, 54% vs. DBD: 91%, 81%, 67%, 58%, p<0.01). Graft survival was also significantly lower in the DCD group compared to the DBD group at 1, 5, 10 and 15 years (DCD: 69%, 56%, 43%, 43% vs. DBD: 86%, 76%, 60%, 51%, p<0.001). Rates of overall biliary complications (OBC) (DCD: 47% vs. DBD: 26%, p<0.01) and ischemic cholangiopathy (IC) (DCD: 34% vs. DBD: 1%, p<0.01) were significantly higher in the DCD group. Donor age (HR: 1.04, p<0.01) and donor age >40 years (HR: 3.13, p < 0.01) were significant risk factors for the development of OBC. Multivariate analysis revealed cold ischemic time (CIT) >8 hours (HR: 2.46, p=0.05), donor age >40 (HR: 2.90, p< 0.01) significantly increased the risk of IC. Conclusions Long-term patient and graft survival after DCD liver transplantation remain significantly lower but acceptable when compared to DBD liver transplants. Donor age and CIT >8 hours are the strongest predictors for the development of ischemic cholangiopathy. Careful selection of younger DCD donors and minimizing CIT may limit the incidence of severe biliary complications and improve the successful utilization of DCD donor livers.

Galaxies are missing most of their baryons, and many models predict these baryons lie in a hot halo around galaxies. We establish observationally motivated constraints on the mass and radii of these haloes using a variety of independent arguments. First, the observed dispersion measure of pulsars in the Large Magellanic Cloud allows us to constrain the hot halo around the Milky Way: if it obeys the standard NFW profile, it must contain less than 4-5% of the missing baryons from the Galaxy. This is similar to other upper limits on the Galactic hot halo, such as the soft X-ray background and the pressure around high velocity clouds. Second, we note that the X-ray surface brightness of hot haloes with NFW profiles around large isolated galaxies is high enough that such emission should be observed, unless their haloes contain less than 10-25% of their missing baryons. Third, we place constraints on the column density of hot haloes using nondetections of OVII absorption along AGN sightlines: in general they must contain less than 70% of the missing baryons or extend to no more than 40 kpc. Flattening the density profile of galactic hot haloes weakens the surface brightness constraint so that a typical L * galaxy may hold half its missing baryons in its halo, but the OVII constraint remains unchanged, and around the Milky Way a flattened profile may only hold 6 − 13% of the missing baryons from the Galaxy (2 − 4 × 10 10 M ⊙ ). We also show that AGN and supernovae at low to moderate redshift -the theoretical sources of winds responsible for driving out the missing baryons -do not produce the expected correlations with the baryonic Tully-Fisher relationship and so are insufficient to explain the missing baryons from galaxies. We conclude that most of missing baryons from galaxies do not lie in hot haloes around the galaxies, and that the missing baryons never fell into the potential wells of protogalaxies in the first place. They may have been expelled from the galaxies as part of the process of galaxy formation.

(2015) 'Unifying X-ray scaling relations from galaxies to clusters.', Monthly notices of the Royal Astronomical Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details.