1 / 16

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?.

will
Télécharger la présentation

An Extragalactic X-ray Surveys

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related