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An Extragalactic X-ray Surveys

An Extragalactic X-ray Surveys. X-ray Surveys with Space Observatory. Khyung Hee University Kim MinBae Park Jisook. Contents. Why X-ray Survey? Chandra & XMM-Newton Survey with Chandra X-ray Observatory Survey with XMM-Newton eROSITA ASTRO-H. Why X-ray Survey?.

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An Extragalactic X-ray Surveys

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  1. An Extragalactic X-ray Surveys X-ray Surveys with Space Observatory KhyungHee University Kim MinBae Park Jisook

  2. Contents • Why X-ray Survey? • Chandra & XMM-Newton • Survey with Chandra X-ray Observatory • Survey with XMM-Newton • eROSITA • ASTRO-H

  3. Why X-ray Survey? • 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.

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

  5. CDFS Chandra Deep Field South 1Ms Survey (Giacconi etal. 2002) 2Ms Survey (Luo et al. 2008) 4Ms Survey (Xueet al. 2012) Main Chandra Source Catalog • RA 3h32m28.0s Dec -27deg48’30.0’’ (J2000) 464.5 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)

  6. AEGIS-X 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)

  7. AEGIS-X

  8. STRIPE82-X • 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)

  9. COSMOS field XMM-COSMOS • RA 23h29m18.4s Dec -54deg40’33.6’’ (center), 2deg² • 322 sources of AGN, 60% oftotal • 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)

  10. XXL • 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 : 18000 (out to z~4) • Multi-wavelength(northern field/southern field) : Optical, UV, NIR, mid-, far-IR, radio

  11. XMM-BCS • 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 > 2000 • Clusters: 45 • Optical, near-IR (SZE)

  12. eROSITA • eROSITA will be launched In 2015. (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.

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

  14. eROSITA eROSITAplanned survey area versus flux in comparison to existing surveys

  15. ASTRO-H • ASTRO-H will be launched In 2015. (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

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