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