18 results on '"Cirasuolo, Michele"'
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2. MOONS – multi object spectroscopy for the VLT: integration and tests of the field corrector and the rotating front end
3. Status of the ESO's ELT construction
4. The ESO's ELT construction progress
5. TIPTOP: a new tool to efficiently predict your favorite AO PSF
6. Instrumentation for ESO's Extremely Large Telescope
7. Rising MOONS: an update on the VLT’s next multi-object spectrograph as it begins to grow
8. Progress along the E-ELT instrumentation roadmap
9. Implementation and performance of the metrology system for the multi-object optical and near-infrared spectrograph MOONS
10. The E-ELT program status
11. MOONS – multi object spectroscopy for the VLT: overview and instrument integration update
12. The metrology system for the multi-object optical and near-infrared spectrograph MOONS
13. Performance of the K-band multi-object spectrograph (KMOS) on the ESO VLT
14. DISCOVERY OF A GIANT Ly? EMITTER NEAR THE REIONIZATION EPOCH
15. Optical-Radio Mapping: the Kinetic Efficiency of Radio-Loud AGNs
- Abstract
We constrain the mean kinetic efficiency of radio-loud active galactic nuclei by using an optically selected sample for which both the optical and the radio luminosity functions (LFs) have been determined; the former traces the bolometric luminosity L, while the latter traces the kinetic power Lk, empirically correlated to the radio emission. Thus in terms of the ratio
!["g_{k}=L_{k}/L"/]("eq-00001.gif")
gk = Lk/L, we can convert the optical LF of the sample into a radio one. This computed LF is shown to match the directly observed LF for the same sample if !["g_{k}=0.10^{+0.05}_{-0.01}"/]("eq-00002.gif")
gk = 0.10[?]0.01+0.05 holds, with a scatter !["\sigma]("eq-00003.gif")
s = 0.38[?]0.09+0.04 dex; with these values we also match a number of independent correlations between !["L_{k},L"/]("eq-00004.gif")
Lk,L and radio emission, that we derive through Monte Carlo simulations. We proceed to translate the value of !["g_{k}"/]("eq-00005.gif")
gk into a constraint on the kinetic efficiency for the production of radio jets or winds, namely, \epsilon _{k}=L_{k}/\dot{M}_{a}c^{2}\sim 0.01 $εk = Lk/˙{M}ac2 ∼ 0.01$ in terms of the rate \dot{M}_{a}$˙{M}a$ of mass accretion onto the central black hole. Then, on assuming that on average the radio sources share the same kinetic efficiency, we compute a solid lower limit of about 25% on the contribution of radio sources to the local black hole mass density.
16. Dynamical and Photometric Imprints of Feedback Processes on the Formation and Evolution of E/S0 Galaxies
17. The ESO Extremely Large Telescope instrumentation programme
18. The ESO's ELT construction status
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