Titlebook: ;

INERT

Mechanisms of Disease Resistance,The hot phase of the ISM in nearby elliptical galaxies is observed to have temperatures in the range of 10 Mio degrees. While stellar wind and mass–loss by planetary nebulae are widely seen as the sources for the interstellar gas, there is no generally established model to explain the heating of the ISM (supernovae, AGN heating and collisions).

不法行为

Mireille Cormont,Vincent KaddaiHard X–ray surveys efficiently sample the obscured AGN population and in particular those with redder colors which would not be selected by UVX surveys. The discovery that a sizable fraction (~20%) of hard X–ray sources are also associated to extremely red objects (EROs) with optical to near–infrared colour R-K>5 is even more intriguing [1,2,1].

Mumble

Evolution of the ISM in Elliptical Galaxiesand Black Hole Growth,The hot phase of the ISM in nearby elliptical galaxies is observed to have temperatures in the range of 10 Mio degrees. While stellar wind and mass–loss by planetary nebulae are widely seen as the sources for the interstellar gas, there is no generally established model to explain the heating of the ISM (supernovae, AGN heating and collisions).

飞镖

Transfusion

严重伤害

VLT Adaptive Optics Imaging of QSO at z ~ 2.5,the QSO and find that it is hosted by an elliptical of M. = –27.6. This result, though restricted to a single object, extends up to z=2.5 the finding that cosmic evolution of radio-loud hosts follows the trend expected for luminous and massive spheroids undergoing passive evolution.

Lime石灰

https://doi.org/10.1007/978-1-4684-4574-9redicted to be heavily skewed towards fast-rotating Kerr holes, already in place at early epochs, and not to change significantly below redshift 5. Decaying MBH binaries may shape the innermost central regions of galaxies and should be detected in significant numbers by ..

弄污

商谈

圆锥

Black Hole Accretion and Starbursts Triggered by Interactions in Hierarchical Galaxy Formation,t distribution of galaxies in K-band at . < 2 are all in good agreement with the existing observations concerning the bright galaxy population. As for the AGNs, our results closely fit the observed luminosity functions of QSOs, their density from .≈ 5 to .≈ 0, and the local .–. relation.