Chandra survey in the AKARI North Ecliptic Pole Deep Field - I. X-ray data, point-like source catalogue, sensitivity maps, and number counts

摘要: Mon. Not. R. Astron. Soc. 000, 1–?? (2015) Printed 25 March 2015 (MN LaTEX style file v2.2) arXiv:1409.7697v2 [astro-ph.HE] 24 Mar Chandra survey in the AKARI North Ecliptic Pole Deep Field. I. X-ray data, point-like source catalog, sensitivity maps, and number counts M. Krumpe, 1,3⋆ T. Miyaji, 2,3 H. Brunner, 4 Hanami, 5 Ishigaki, Takagi, 6 A. G. Markowitz, 3,7 Goto, 8 Malkan, 9 Matsuhara, 6,10 C. Pearson, 11,12,13 Y. Ueda, 14 Wada 1 European Southern Observatory, ESO Headquarters, Karl-Schwarzschild-Strase 2, 85748 Garching bei M¨ unchen, Germany de Astronom´ia, Universidad Nacional Aut´ onoma M´ exico, Carret. Tijuana-Ensenada, Ensenada 22860, BC, Mexico (mailing addr. P.O. Box 439027, San Diego, CA, 92143, USA) 3 University of California, Center for Astrophysics Space Sciences, 9500 Gilman Dr., La Jolla, 92093-0424, USA Max-Planck-Institut f¨ ur extraterrestrische Physik, Giesenbachstrase, Iwate University, 3-18-8 Morioka, Iwate, 020-8550, Japan Institute Astronautical Science, Aerospace Exploration Agency, Sagamihara, 229-8510, Kanagawa, 7 Karl Remeis Observatory Erlangen Centre Astroparticle Physics, Sternwartstrase 7, 96049 Bamberg, Germany; Alexander von Humboldt Fellow Astronomy, Hawaii 2680 Woodlawn Drive, Honolulu, HI, 96822, Los Angeles, Division Astronomy & Astrophysics, 430 Portola Plaza, 90095-1547, 10 Department The Graduate Advanced Studies, Shonan Village, Hayama, 240-0193, 11 RAL Space, STFC Rutherford Appleton Laboratory, Didcot, Oxon, OX11 0QX, UK 12 Open Milton Keynes, MK7 6AA, 13 Oxford, Keble Rd, OX1 3RH, Kyoto Kyoto, 606-8502, 2 Instituto Released 2014 January 17 ABSTRACT We present data products from 300 ks (NEP) deep field. This field has a unique set 9-band infrared pho- tometry covering 2–24 µm Infrared Camera, including mid-infrared (MIR) bands not covered by Spitzer. is one deepest ever achieved at ∼15 µm, far widest among those with similar depths MIR. makes this MIR-selection AGN z ∼ 1. design detection procedure, which performs joint Maximum Likeli- hood PSF fits on all our 15 mosaicked pointings an area 0.34 deg . procedure been highly optimized tested simulations. provide point catalog photometry Bayesian-based 90 per cent confidence upper limits 0.5–7, 0.5–2, 2–7, 2–4, 4–7 keV bands. contains 457 sources spurious fraction estimated to be ∼1.7 cent. Sensitivity flux maps are provided as well. search optical MIR counterparts central 0.25 , where Sub- aru Suprime-Cam multiband images exist. Among 377 detected there, ∼80 have ∼60 also mid-IR counterparts. cross-match MIR-selected Hanami et al. Around 30 that MID-IR SEDs purely explain- able activity strong Compton-thick candidates. Key words: methods: analysis – surveys galaxies: active X-ray: galaxies. E-mail: mkrumpe@ucsd.edu c RAS INTRODUCTION absorbed (CT) quantification their contribution total accretion