[PDF] Top 20 X-ray and optical studies of active galactic nuclei

... the X-ray d ata for a sample of QSO’s than the flux at ...at optical wavelengths and discussed by Shields (1978) for the quasar ...the optical excess as therm al radiation from an accretion ... See full document

... The resultant total (DR+RR) rate coefficients are then an order of magnitude larger than those cur- rently in use by photoionized plasma modeling codes such as cloudy, ion and xstar. These rate coefficients, together ... See full document

... of active galactic nuclei (AGN) invokes an anisotropic ob- scuring structure, usually referred to as a torus, to explain the diverse phenomenol- ogy of AGN as an angle-dependent ...of ... See full document

... the optical region) due to the low tem pera­ ...that optical spectroscopy cannot re­ solve the difference between pressure effects caused by increased helium abundance in the atmosphere and those from an ... See full document

... Soft X-rays (^ O .lk e V ) might also be expected if a fraction of the hard X-rays are absorbed by the white dwarf and re-em itted as optically thick blackbody radi­ ation (T 10 ® K), as is often seen in ... See full document

... AGN X-ray luminosity functions ( XLFs ) , which are well constrained ( except in the very local universe ) only below 10 keV, together with models for the broadband (∼ 1 – 1000 keV ) AGN spectra and ... See full document

... e X -ray sp ectra of radio quiet AGN, which are in general softer th an those from radio loud objects (Lawson et a i ...the X -rays are reflected from m aterial near th e black hole; in MCG 6-30-15, ... See full document

... of X-rays from outside the solar system (Giacconi et ...of X-ray ...the X-ray emission mechanisms in individual objects however, since none of the missions after HEAO-1 performed an ... See full document

... of X-ray ...keV) X-ray luminosities, Saikia et ...the optical FP relations for supermassive black holes is due to environmental ... See full document

... Statistical studies are reported in this article for an active galactic nuclei sample of different type of active galaxies Seyferts 1, Seyferts 2, and ...bright X-ray ... See full document

... for X-ray and optical AGN; these were found to have a higher velocity dispersion in comparison to the general clus- ter population and avoid the phase space with low relative velocities and ... See full document

... We do not find significant evidence of absorption intrinsic to the source in the XMM-Newton or archival d ata studied here. This is in agreement with the findings of previous observations (Hall et al. 1981; Petre et al. ... See full document

... In der Gesamtstichprobe wurden ungef¨ahr 1000 kompakte R¨ontgenquellen detektiert, von denen ∼ 300 aktive Galaxienkerne (engl.: active galactic nuclei; AGN) im Hintergrund sein d¨ urften. Bei der ... See full document

... Thus, if we only consider the galaxies classified in groups 1, 2 and 3, we find that 62 per cent of the PRGs at z < 0.2 show signs of interactions. However, it is worth considering the percentage of dis- turbance ... See full document

... of Galactic X-ray sources with Be stars was first suggested by Maraschi, Treves and van den Heuvel (1976) when they identified 4 such ...hard X-ray sources (>3 keV), and half of them ... See full document

... faint X–ray transients found towards the Galactic Centre might be dwarf Novae in ...I X–ray bursts) a good way to distinguish between a nova or a low–mass X–ray binary ... See full document

... Apart from single element nanostructures, group IV and III-V nanostructured compounds have also attracted extensive interest due to their structural similarity to silicon and carbon. Although Si is not light-emitting, ... See full document

... the optical/infrared (OIR) data using an extinction estimate of mag (6, ...and x-ray bands exhibit quasi-independent ...the optical lightcurves, including slow modulations of a few minutes ... See full document

... We also suggest a test for the proposed nature of the Galactic population, i.e., that these are intrinsicly faint cataclysmic variables. Regardless of whether these are non-magnetic CVs or magnetic ones (e.g., ... See full document

... powder X-ray diffraction beamline (09A) at TPS is desirable for the study of the static and dynamic structures of hard condensed matter with hard-X-ray ...the X-ray source with ... See full document