Optically selected QSO candidates in the field 0112 – 35

Savage, A.; Trew, Arthur; Chen, Jiansheng; Weston, Tony

doi:10.1093/mnras/207.3.393

Cited by 18 publications

(5 citation statements)

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“…Q 0101-337 was classified as a radio quiet quasar discovered by a visual search for emission lines and UV continuum objects on UKST objective prism plates (Savage et al 1984). The source is not detected in the 2MASS (Barkhouse & Hall 2001) but it appears in the NRAO VLA Sky Survey at a flux level of 27.1 mJy at 1.4 GHz.…”

Section: Results For Individual Objectsmentioning

confidence: 99%

VLT adaptive optics imaging of QSO host galaxies and their close environment at z $\mathsf{\sim}$ 2.5: Results from a pilot program

Falomo

Kotilainen

Scarpa

et al. 2005

A&A

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Abstract. We report on ESO-VLT near-IR adaptive optics imaging of one radio-loud (PKS 0113-283) and two radio quiet (Q 0045-3337 and Q 0101-337) quasars at z > 2. In the first case we are able to resolve the QSO and find that it is hosted by an elliptical of absolute magnitude M K = −27.6. For the other two objects no extended emission has been unambiguously detected. This result, although restricted to a single object, extends up to z = 2.5 the finding that cosmic evolution of radio-loud quasar hosts follows the trend expected for luminous and massive spheroids undergoing passive evolution. For Q 0045-3337 our high resolution images show that it is located 1.2 arcsec from a K = 17.5 foreground disc galaxy, which may act as a gravitational lens, since the QSO most probably lies within the galaxy Einstein radius.

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Section: Results For Individual Objectsmentioning

confidence: 99%

VLT adaptive optics imaging of QSO host galaxies and their close environment at z $\mathsf{\sim}$ 2.5: Results from a pilot program

Falomo

Kotilainen

Scarpa

et al. 2005

A&A

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“…All the other sources have been flagged as having secure redshift estimates. For this paper, we used only sources with redshifts marked as "secure" in Véron-Cetty & Véron (2010) and in other papers on their redshift estimates, for example Savage et al (1984) and Abazajian et al (2003), except for a single source that is marked as insecure in Véron-Cetty & Véron (2010), but not on the original reference (Savage et al 1984). We include under the generic AGN denomination all objects classified in the VCV catalogue as either AGN or QSO.…”

Section: Parent Surveysmentioning

confidence: 99%

Relativistic reflection in the average X-ray spectrum of active galactic nuclei in the Véron-Cetty and Véron catalogue

Falocco

Carrera

Barcons

et al. 2014

A&A

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Context. The X-ray spectra of active galactic nuclei (AGN) unveil properties of matter around the super-massive black hole (SMBH). Aims. We investigate the X-ray spectra of AGN focusing on Compton reflection and fluorescence. These are two of the most important processes of interaction between primary radiation and circumnuclear material that is located far away from the SMBH, as indicated by the unresolved spectral emission lines (most notably the Fe line) in the X-ray spectra of AGN. Contributions from the inner accretion disk, affected by relativistic effects as expected, have also been detected in several cases. Methods. We studied the average X-ray spectrum of a sample of 263 X-ray unabsorbed AGN that yield 419 023 counts in the 2−12 keV rest-frame band distributed among 388 XMM-Newton spectra. Results. We fitted the average spectrum using a (basically) unabsorbed power law (representing the primary radiation). From a second model that represents the interaction (through Compton reflection and fluorescence) of this primary radiation with matter located far away from the central engine (e.g. the putative torus), we found that it was very significantly detected. Finally, we added a contribution from interaction with neutral material in the accretion disk close to the central SMBH, which is therefore smeared by relativistic effects, which improved the fit at a 6 sigma. The reflection factors are 0.65 for the accretion disk and 0.25 for the torus. Replacing the neutral disk-reflection with low-ionisation disk reflection, also relativistically smeared, fits the data equally well, suggesting that we do not find evidence for significant ionisation of the accretion disk. Conclusions. We detect distant neutral reflection associated with a narrow Fe line in the average spectrum of unabsorbed AGN with z = 0.8. Adding the disk-reflection component associated with a relativistic Fe line improves the data description at a 6 sigma confidence level, suggesting that both reflection components are present. The disk-reflection component accounts for about 70% of the total reflected flux.

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“…The catalogue by Veron-Cetty & Veron (2006) reports tentative redshifts for quasars 0119-370 (z = 1.32, Savage et al 1984) and 0152-4055 (z = 1.65, Drinkwater 1987)…”

Section: Appendix A: Notes On Individual Targetsmentioning

confidence: 99%

The quasar relation through cosmic time - I. Data set and black hole masses

Decarli

Falomo

Treves

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We study the M BH -M host relation as a function of cosmic time in a sample of 96 quasars from z = 3 to the present epoch. In this paper, we describe the sample, the data sources and the new spectroscopic observations. We then illustrate how we derive M BH from single-epoch spectra, pointing out the uncertainties in the procedure. In a companion paper, we address the dependence of the ratio between the black hole mass and the host-galaxy luminosity and mass on cosmic time.

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Optically selected QSO candidates in the field 0112 – 35

Cited by 18 publications

References 0 publications

VLT adaptive optics imaging of QSO host galaxies and their close environment at z $\mathsf{\sim}$ 2.5: Results from a pilot program

VLT adaptive optics imaging of QSO host galaxies and their close environment at z $\mathsf{\sim}$ 2.5: Results from a pilot program

Relativistic reflection in the average X-ray spectrum of active galactic nuclei in the Véron-Cetty and Véron catalogue

The quasar relation through cosmic time - I. Data set and black hole masses

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