[PDF] Top 20 Faint optically selected AGN at z=3
Has 10000 "Faint optically selected AGN at z=3" found on our website. Below are the top 20 most common "Faint optically selected AGN at z=3".
Faint optically selected AGN at z=3
... the AGN selection function and a derivation of the UV luminosity function of faint AGN are deferred to Chapter 3, here we make some approximate statements on the completeness of our ... See full document
100
The nature of luminous Lyman alpha emitters at z~2 3:maximal dust poor starbursts and highly ionising AGN
... at z ∼ 2 − 3 which does not apply to ...the AGN activity can lead to even larger observed UV and Lyα lumi- ...dust) selected sources (Sobral et al. 2016) show an increase of the AGN ... See full document
26
Enhancement of AGN in a protocluster at z=1 6
... be selected as protocluster galaxies (Hatch et ...protocluster AGN are redder than field AGN, with 100 per cent of protocluster AGN being red (z − J > ...red AGN host galaxies ... See full document
9
On the nature of the red, 2MASS-selected AGN in the local Universe I: an optical spectroscopic study
... Low-resolution optical spectroscopic observations of the sam- ple were taken with the ISIS dual-arm spectrograph on the 4.2 m William Herschel Telescope (WHT) on La Palma in three runs: the 2006 July 28, 2007 February 8 ... See full document
27
Measurements of X ray selected AGN and novel superconducting X ray detectors
... We have imaged the SEXSI fields using the Palomar 60-inch (P60) and 200-inch (P200) telescopes, the MDM 2.4-meter (MDM-2.4) and 1.3-meter (MDM-1.3) telescopes, and the Keck I telescope. Much of the early optical imaging ... See full document
309
The faint end of the 250μm luminosity function at z< 0 5
... to z = ...we selected galaxies (located in the three Galaxy And Mass Assembly (GAMA) equatorial fields with Herschel coverage) with photoErrorClass equal to 1, −1, 2, and 3, which have an average RMS ... See full document
6
The GLARE Survey II Faint z 6 Ly line emitters in the HUDF
... JWST becomes available, requires unreasonable exposure times to obtain a high signal-to-noise ratio (S/N) spectrum for the contin- uum. However, line emission (e.g. Lyα) may be within reach of ultradeep ... See full document
13
Faint Galaxies in the Megaparsec-Scale Environments of Hyperluminous QSOs at Redshifts 2 < z < 3
... targeting optically-bright HLQSOs, an exciting possibility exists in the detection of Lyα emission around obscured QSOs at high ...of AGN suggests that obscuration is primarily a function of QSO ... See full document
118
Cosmic dance at z ~ 3:Detecting the host galaxies of the dual AGN system LBQS 0302–0019 and Jil with HAWK I+GRAAL
... Observations were taken in nod-to-sky mode with an ABAABAAB pattern, where A and B represent the two nod po- sitions. Given the proximity of Jil to LBQS 0302−0019, we were unable to place IFUs on the two targets ... See full document
5
The Lyman alpha luminosity function at z=5 7 6 6 and the steep drop of the faint end:implications for reionization
... UV selected galaxies with strong Lyα, or the evolution of the number density of Lyα emitters) as consequences of reionization, one needs to accurately understand the contribution from poten- tially varying ... See full document
16
Discovery of a single faint AGN in a large sample of z > 5 Lyman break galaxies
... at z ∼ 3 Steidel et al. (2003) found a AGN fraction of 3 per cent in their compara- ble LBG ...same z ∼ 3 sample (Laird et al. 2006). From the one AGN detected in this ... See full document
7
Active Galactic Nucleus and Starburst Classification from Spitzer Mid‐Infrared Spectra for High‐Redshift SWIRE Sources
... scured AGN, based primarily on X-ray detections of optically faint sources, and sources with indicators of a star- burst, based on optical and near-infrared spectral energy distributions (SEDs), ... See full document
12
Multi Wavelength Properties of Submillimeter Selected Galaxies
... separate z > 1 . 5 SMGs from lower- z SMGs, even if a source contains an X-ray detected AGN, as well as indicate mid-IR counterparts to submm ...have z > 1 ...with z > 1 . 5, ... See full document
241
Galaxy and Mass Assembly (GAMA): active galactic nuclei in pairs of galaxies
... line AGN di ff er and this consequently questions the validity of the AGN unification ...line AGN within GAMA, we use a double- Gaussian emission line fitting method to model the more complex line ... See full document
16
High Redshift LAEs and their Cosmic Evolution: Morphologies, SFR and AGN Activity from z~2 to 6
... nosity at redshift z. These values were then used to isolate which galaxies in our data set would later evolve into dwarf- like, Milky Way-like and cluster-like galaxies. No dwarf-like, a small number of Milky ... See full document
20
The Interstellar Medium in [O III] selected Star forming Galaxies at z similar to 3 2
... We note that locally calibrated relations between line ratios and gas metallicity might not be applicable to star-forming galaxies at high redshifts because their typ- ical ISM conditions seem to change from z = 0 ... See full document
20
Fuel and Power in Ireland: Part 2 Electricity and Turf
... PAGE Quarterly and Annual Variations in Consumption of Electricity; Selected Years Table z Monthly Consumption of Electricity; 1962 and 1963 Table 3 Loads at Selected Hours on Representa[r] ... See full document
58
Herschel ATLAS/GAMA: how does the far IR luminosity function depend on galaxy group properties?
... Observations at far-IR wavelengths are an essential complement to the traditional UV and optical tracers of star formation. We have combined far-IR data from the H-ATLAS survey with the galaxy group catalogue from the ... See full document
18
(Z) 3 Ferrocenyl 2 phenylacrylonitrile
... The chemistry of ferrocene has received much attention because of its applications in many fields, such as in catalysis, organic or organometallic synthesis and materials (Togni, et al. (1995)). The use of ferrocene and ... See full document
8
Circosta, Chiara (2019): A multi-wavelength study of the interstellar medium in active galactic nuclei at cosmic noon. Dissertation, LMU München: Fakultät für Physik
... of AGN feedback. The presence of outflows in AGN host galaxies is now quite well established: they have been detected at different physical scales ...of AGN outflows on the gas and star formation in ... See full document
170
Related subjects