An Extragalactic X-ray Surveys

X-ray Surveys with Space Observatory

Khyung Hee UniversityKim MinBaePark Jisook

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

Contents

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.

Why X-ray Survey?

Chandra & XMM-Newton

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

Chandra Deep Field South1Ms 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) 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 coun-terparts (optical/near-IR/IR/radio)

CDFS

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)

AEGIS-X

AEGIS-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)

STRIPE82-X

(Urry et al. 2013)

XMM-COSMOS RA 23h29m18.4s Dec -54deg40’33.6’’ (center),

2deg² 322 sources of AGN, 60% of to-

tal 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)

COSMOS field

The ultimate XMM-Newton extragalac-tic 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/south-ern field) : Optical, UV, NIR, mid-, far-IR, radio

XXL

XMM-Newton – Blanco Cos-mology 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)

XMM-BCS

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.

eROSITA

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

eROSITA

eROSITA

eROSITA planned survey area versus flux in comparison to existing sur-veys

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

ASTRO-H