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SWIRE Science: Investigating the Active and Passive Universe on Large Scales

SWIRE Science: Investigating the Active and Passive Universe on Large Scales. Alberto Franceschini Padova University. "SWIRE Science Team Meeting". IPAC, December 17-19, 2001.

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SWIRE Science: Investigating the Active and Passive Universe on Large Scales

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  1. SWIRE Science:Investigating the Active and Passive Universe on Large Scales Alberto Franceschini Padova University "SWIRE Science Team Meeting" IPAC, December 17-19, 2001

  2. The SWIRE view on the Active Universe:AGN Contribution to the Infrared and X-ray Backgrounds[weighing the stellar vs. gravitational energy budget]

  3. Summary • The CIRB, recent results, comparison with XRB • Ultimate energy sources for the BKGs: stellar emission and gravitational energy • Physical properties of the CIRB sources: AGN vs. SB • The X-ray diagnostics: deep IR/X-ray surveys • Testing the origin of the XRB • Prospects for SWIRE

  4. The Global Background Radiation

  5. COBE Discovery of the Cosmic Infrared Background (CIRB) (Puget et al. 1996; Hauser et al. 1998) λ=100 μ

  6. COBE HST (IR)=40 nW/msr (opt)=17 nW/msr The Infrared and Optical Background Radiations

  7. ULTIMATE ENERGY SOURCES XRB => mostly gravitational CIRB => mostly stellar? A solid limit: mass in local Massive Dark Objects (MDO's): MMDO ~ 2 10-3 M* (M* : mass in spheroids Kormendy & Richstone) How much energy out of this? ηstellar~10-3 , εAGN~0.5 (limit) LAGN ~ 2 10-3 ε/η Lstar ~ Lstar However: ηstellar~ (1-5) 10-3 , εAGN~ (0.1-0.5) , MMDO ~ (2-5) 10-3 M* (Magorrian et al.)

  8. A) 99% of the gravitational energy might be undetectable in X-rays because absorbed and re-radiated in the IR ~50% or more of the CIRB might be due to AGNs Relevant for the history of stellar formation (SF) • B) XRBpeak at 30 keV Compton-thick emission, implies that the 1-10 keV range covered by CHANDRA & XMM might not be appropriate at all to sample accretion processes • Long-λ background critical for rather fundamental issues of cosmology: • history of barion transformations in stars • AGN unification, obscured quasar populations

  9. Similarities of the CIRB/OPT. spectral shape and the typical StarBurst spectrum M82 broad-band spectrum Log L() (erg/s) Log() []

  10. 6.9x6.4 arcmin 19 sources above 3.5 mJy SCUBA 850  survey of the CFRS 1415h field (Eales et al. 2000)

  11. LW3 z=0 Typical source spectra 0.5 1 1.5 2 LW3 15 LW2 6.7  K-corrections

  12. (Fadda et al. 2000)

  13. 15  differential counts (Euclidean normalized) by Elbaz et al. (1999) Contribution of faint ISO sources to the diffuse mid-IR background light

  14. HDF-North image overlayed by the ISOCAM LW3 15  contours by Aussel et al. 1999 2 arcmin

  15. 2.7 arcmin ISOCAM 15 μ image overlayed to the FORS2/VLT R-band image on the FIRBACK UDS field

  16. IR-starbursts UV-optical galaxies Optical & X-ray AGNs Evolution of the comoving luminosity density (Franceschini et al. 2001)

  17. Correlations of the MIR and FIR fluxes => the global IR spectrum (Elbaz et al. 2001)

  18. Bolometric luminosities of the faint ISO sources => only 30% are ULIRGs (Lbol>1012 Lo)

  19. The faint sources detected by ISO at 15  are responsible for the bulk of the CIRB background

  20. ISO : tentative way to resolve the CIRB • Appropriate z (z ~ 1) • Easyly identified sources • Good sampling of the part of the LF making the • CIRB • Large samples available • Well-known z-distributions

  21. First characterization of the CIRB sources LOW-RESOLUTION ISAAC OBSERVATIONS OF Ha+NII (Rigopoulou et al. 2000)

  22. To summarize: • 18 galaxies observed with • H=19-22.5 • H detected in 15 (low-res) • SFR(H) = 10 M/yr • SFR(FIR) = 100 M/yr

  23. HST I-band image HDF- South source 27 M=3 1012 Mo (Ho = 60 Km/s) d=36 kpc

  24. X-ray, IR and optical diagnosis of AGN vs. Starburst emission (Bassani et al. 2000)

  25. CHANDRA SCUBA CHANDRA SCUBA X-ray vs. mm vs. optical (maps of A1835 and A2390) X-ray: CHANDRA optical: I-band mm: SCUBA 850  scale: 10 arcsec (Fabian et al. 2000)

  26. Severgnini et al. (2000) => Sub-mm and X-ray emissions as two unrelated penomena

  27. Modelling the IR SEDsof AGNs Radiative transfer modelling

  28. IR spectra of a typical AGN (NGC 1068) with those of typical starbursts (M82, Arp220, Arp 244) and a mixed AGN/SB (NGC 6240) Elbaz et al. (2002)

  29. NGC 1068 [Floch et al. 2001] [ISO CVF]

  30. Entirely different spectral shapes for galaxies and Active Galactic Nuclei in the Mid-Infrared

  31. IR SEDs of Active Galactic Nuclei Models based on radiative transfer solutions Granato, Danese, Franceschini (1997)

  32. M82 IR spectrum fitted by AGN model

  33. Image at 15 μ by ISO of the Lockman Hole (Fadda et al. (2001) Large square: shallow survey (0.7x0.7 deg.), small square: deep survey (20x20 arcmin) Inset: overlay of ISO and XMM (circle) on an I image

  34. The problem of the origin of the flux: starburst or AGN ?

  35. CHANDRA observation of the Hubble Deep Field North Brandt et al. (2001) (see Mushotzky et al. 2000, Hornschemeier et al. 2000) S0.5-2>5 10-17 (erg/cm2/s)

  36. ISO & CHANDRA sources in the HDFN (Fadda et al. 2001)

  37. Cross-correlation between ISO and CHANDRA in the HDFN

  38. A JOINT ISO/XMM Deep Investigation in the Lockman Hole

  39. XMM image by Hasinger et al. (2001) ISO image by Fadda et al. (2001)

  40. IR and X-ray dapths in the Lockman and HDFN

  41. STATISTICS ON ISO/XMM SOURCES IN THE LOCKMAN HOLE

  42. X-ray vs. IR flux diagnostics

  43. High X-ray luminosities =>>> they are type-II QSO

  44. X-ray to IR spectral index as a function of the X-ray flux

  45. AGN contribution to the CIRB: the ISO guess (<20%)

  46. Contribution of ISO galaxies to the CIRB C CIRB140 = 25(+/-7) W/m2/sr at λ= 140 μ IGL15: contribution to CIRB in W/m2/sr at λ= 15 μ IGL140: contribution to CIRB in W/m2/sr at λ=140 μ R: ratio of νSν at 140 and 15 μ

  47. New AGN statistics based on the mid-IR selection • Assuming that unclassified X-ray sources are type-2 (supported by these data): • 7 AGN type-1 • 12 AGN type-2

  48. ISO & XMM sources in common in the Lockman Hole area: type-II QSO originating the XRB Franceschini et al. (2001)

  49. X-ray luminosity vs. optical color X-ray hardness ratio vs. optical color

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