X-ray Surveys with Space Observatory Khyung Hee University Kim MinBae Park Jisook

 Why X-ray Survey?  Chandra & XMM-Newton  Survey with Chandra X-ray Observatory  Survey with XMM-Newton  eROSITA  ASTRO-H

 To detect X-ray emission from very hot regions of the Universe.  The minimizing quasar and galaxy photometric redshift errors and extending the sample to higher redshift.  The X-ray Surveys make to find obscured AGNs and other AGNs with weak optical signatures.  Multi-wavelength follow-up of detected X-ray sources is crucial to understand the properties of the observed objects.

Two powerful and active X-ray missions. ⊲ NASA : Chandra X-Ray Observatory ⊲ ESA : X-Ray Multi-Mirror (XMM) Newton

Chandra Deep Field South 1Ms Survey ( Giacconi et al. 2002) 2Ms Survey (Luo et al. 2008) 4Ms Survey (Xue et al. 2012) Main Chandra Source Catalog  RA 3h32m28.0s Dec -27deg48’30.0’’ (J2000) arcmin², 3.872Ms  740 sources (75% AGN)  300 new sources (2Ms->4Ms) (65%: AGN,35%: normal & starburst galaxies,1% stars)  0 < z < 8  97% have multi-wavelength counterparts (optical/near-IR/IR/radio)

All-wavelength Extended Groth strip International Survey X-ray catalogue for AIGES (Laird et al. 2009)  The Extended Groth Strip (EGS: RA=14h 17m, Dec= +52deg 30’, small region in the constellation Ursa Major), 0.67deg², 1.8Ms  1325 sources  Optical(76%), IR(94%, DEEP2,CFHTLS, Spitzer/IRAC surveys of the EGS)

 The Celestial Equator in the Southern Galactic Cap (“Stripe 82”) ( 20h24’< RA < 04h08’, -1.27deg < Dec< 1.27deg, total 300deg²)  2073, 607, 2079 (soft, hard, full)  16.5 deg² for Stripe 82-X - Chandra 7.4deg² (LaMassa et al. 2013a) - XMM 10.5deg² (LaMassa et al. 2013b) (overlaps 1.5 deg²)  3362 sources  high luminosity source (L_x≥ 10^45 erg/s) : 657 sources, 125 AGN sources are z > 2,  UV(GALEX), Near-IR(UKIDSS, WISE), ugriz-band(SDSS), radio(FIRST) (Urry et al. 2013)

XMM-COSMOS  RA 23h29m18.4s Dec -54deg40’33.6’’ (center), 2deg²  322 sources of AGN, 60% of total  Redshift of AGN : 0.4 < z < 4.25  UV(GALEX), U-band(CFHT), BVRiz(Subaru), K-band(CTIO/Kitt peak), radio(VLA), mid-IR(Spitzer), i-band(HST) C-COSMOS (Elvis et al. 2009)  1760 source in 0.8 deg², 200ks  COSMOS-Legacy (for 2 deg²)

 The ultimate XMM-Newton extragalactic survey  2011~ 2013  Two extragalactic regions of each 25 deg² - 1. CFHTLS W1 region : RA 2h23m, Dec -4deg30’ (J2000), 25 deg² - 2. BCS region : RA 23h30m, Dec-55deg00’ (J2000), 25 deg² - each,10~>40ks  Galaxy cluster : 600~1400(out to z~1.5-2) AGN : (out to z~4)  Multi-wavelength(northern field/southern field) : Optical, UV, NIR, mid-, far-IR, radio

 XMM-Newton – Blanco Cosmology survey project  RA 23h29m18.4s, Dec - 54deg40’33.6’’ (center), 14 deg²  Initial 6 deg² (Suhada et al. 2012) - Point sources > Clusters: 45  Optical, near-IR (SZE)

 eROSITA will be launched In (German+Russian)  eRASS (eROSITA All-sky survey)  The expection of 3 million AGNs in soft band - To detect the hot intergalactic medium of 50~100 thousand galaxy clusters and groups and hot gas in filaments between clusters to map out the large scale structure in the universe for the study of cosmic structure evolution - To study in detail the physics of galactic X-ray source populations, like pre-main sequence stars, supernova remnants and X-ray binaries.

(M.J.Freyberg, R.Egger (1999), "ROSAT PSPC All-Sky Survey maps completed“)

eROSITA planned survey area versus flux in comparison to existing surveys

 ASTRO-H will be launched In (JAXA+ US) - To explore the structure and evolution of Universe - The most sensitive wideband observation over an energy range from 0.3 to 600 keV  Instruments - Hard X-ray: Telescope, Imager - Soft X-ray: Telescope, Imager, Spectrometer - Gamma-ray: detector