activity
19942026
most citedCosmological Evolution of the Hard X-ray AGN Luminosity Function and the Origin of the Hard X-ray Background

1.1k citations · 11.2k across the 115 of their papers we have counts for

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Showing 2017Show all

5 papers · 1 filter

astro-ph.GA2017

North Ecliptic Pole multi-wavelength survey : new optical data with Hyper Suprime-Cam and near-future prospects with eROSITA

Nagisa Oi, Hideo Matsuhara, Tomotsugu Goto +19

The AKARI North Ecliptic Pole (NEP) survey consists of two survey projects: NEP-Deep (0.5 sq.deg) and NEP-Wide (5.4 sq.deg), providing with tens of thousands of galaxies. A continu…

astro-ph.GA2017★ 37 cited

Spatial clustering and halo occupation distribution modeling of local AGN via cross-correlation measurements with 2MASS galaxies

Mirko Krumpe, Takamitsu Miyaji, Alison L. Coil +1

We present the clustering properties and halo occupation distribution (HOD) modelling of very low redshift, hard X-ray-detected active galactic nuclei (AGN) using cross-correlation…

astro-ph.GA2017

Overview of North Ecliptic Pole Deep multi-wavelength Survey (NEP-Deep)

H. Matsuhara, T. Wada, N. Oi +22

The recent updates of the North Ecliptic Pole deep (0.5~deg, NEP-Deep) multi-wavelength survey covering from X-ray to radio-wave is presented. The NEP-Deep provides us with sev…

astro-ph.GA2017★ 6 cited

An Optically Faint Quasar Survey at z~5 in the CFHTLS Wide Field: Estimates of the Black Hole Masses and Eddington Ratios

H. Ikeda, T. Nagao, K. Matsuoka +5

We present the result of our spectroscopic follow-up observation for faint quasar candidates at z~5 in a part of the Canada-France-Hawaii Telescope Legacy Survey wide field. We sel…

astro-ph.GA2017★ 8 cited

High Excitation Emission Line Nebula associated with an Ultra Luminous X-ray Source at 0.027 in the \textit{AKARI} North Ecliptic Pole Deep Field

J. Díaz Tello, T. Miyaji, T. Ishigaki +6

Aims. We report our finding of a high excitation emission line nebula associated with an Ultra Luminous X-ray source (ULX) at 0.027, which we found in our Chandra observation…