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X-rays from the First Massive Black Holes

Brandt, Vignali, Schneider, Alexander, Anderson, Bassett, Bauer, Fan, Garmire, Gunn, Lehmer, Lopez, Kaspi, Richards, Strateva, Strauss. X-rays from the First Massive Black Holes. Are early black holes feeding and growing in the same way as local ones?. Chandra 4-10 ks snapshots (>100)

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X-rays from the First Massive Black Holes

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  1. Brandt, Vignali, Schneider, Alexander, Anderson, Bassett, Bauer, Fan, Garmire, Gunn, Lehmer, Lopez, Kaspi, Richards, Strateva, Strauss X-rays from the First Massive Black Holes Are early black holes feeding and growing in the same way as local ones? Chandra 4-10 ks snapshots (>100) z > 4.8 SDSS, Opt. bright, RLQs, Exotic High detection fraction ROSAT, Chandra, XMM-Newton archives Additional z > 4 detections Supporting samples at z = 0-4 Deep X-ray surveys www.astro.psu.edu / users / niel / papers / highz-xray-detected.dat

  2. X-ray Versus Optical Fluxes X-ray and optical fluxes correlated. Fluxes generally low; X-ray spectroscopy challenging even for XMM-Newton.

  3. X-ray Spectroscopy at z > 4 XMM-Newton spectroscopy possible for a few of the X-ray brightest quasars. Joint fitting can place respectable average X-ray spectral constraints. PSS 1326+0743 z = 4.17 XMM-Newton PSS 0121+0347 z = 4.13 XMM-Newton Vignali et al. (2004) Also see Ferrero et al. (03), Grupe et al. (04)

  4. X-ray Spectral Comparisons at Low and High Redshifts Significant intrinsic scatter at all redshifts, but no systematic trend. Inner-disk coronae stable. No X-ray reflection “humps” detected. No X-ray absorption detected. Vignali et al. (03)

  5. X-ray Contribution to Spectral Energy Distribution Combine high-redshift sample with well-defined, lower-redshift samples to constrain X-ray evolution. Want broad lum. and z coverage to break degeneracies High-detection fraction (pattern censoring issues) Reliable separation of RQQ and RLQ Good BAL removal / control New sample of ~ 152 SDSS and PSS quasars spanning z = 0.02-6.28 Partial correlation analyses indicate luminosity effect is primary. No highly significant trend with redshift. Also see Vignali, Brandt, & Schneider (2003)

  6. New X-ray Constraints on z > 4 Radio-Loud Quasars 12 high-redshift RLQs with flat radio spectra and moderate-to-high R. Fill X-ray observation gap between RQQs and blazars. Representative of majority of RLQs. Bassett et al. (04) Blazars Lopez et al. (04) New RLQ targets 100% detection rate with some bright objects great for XMM-Newton. Small-scale, jet-linked X-ray component (SSC) consistent at z > 4 and z ~ 0. Degree of X-ray enhancement vs. RQQs X-ray spectral shape Suggestive evidence for X-ray absorption. Radio quiet

  7. Rarity of X-ray Luminous Jets at z > 4 One “favored” model for X-ray jet emission is IC/CMB. Need bulk relativistic velocities on kpc scales. If true, X-ray jets can outshine cores at z > 4. Use Chandra’s imaging to search for such X-ray luminous jets. We do not detect X-ray jets in any of our 12 RLQs (including objects similar to 3C 273 and PKS 0637-752). Physical sizes < 10-15 kpc. Such X-ray luminous jets are rare. Perhaps synchrotron with multiple electron populations? Following Rees & Setti (1968) etc.

  8. X-ray Survey Constraints on z > 4 AGN Probe moderate-luminosity, typical AGN at z > 4 Minimize absorption bias (rest-frame 2-40 keV) High-redshift sources and candidates in central Chandra Deep Field-N Find or constrain sky density exploiting Lyman break. Alexander et al. (01), Barger et al. (03), Cristiani et al. (04), Koekemoer et al. (04) Constraints on reionization. Vignali et al. (02)

  9. Ongoing Chandra and XMM-Newton Surveys 21 Ongoing Deep Surveys 18 Ongoing Wide Surveys ~ 3.5 sq. degrees in total Lists above available from astro-ph/0403646

  10. Constraining Lower Luminosity AGN at High Redshift X-ray Stacking of Large Lyman Break Galaxy Samples from GOODS z ~ 3.0 z ~ 3.8 Lehmer et al. (04) 468 U-dropouts from GOODS-N Effective exposure = 0.8 Gs ~ 25 yr 338 B-dropouts from GOODS-N, S Effective exposure = 0.4 Gs ~ 13 yr Also tight constraints on V, i dropouts at z ~ 5, 6 Observed X-ray emission plausibly from X-ray binaries and supernova remnants – no need to invoke numerous lower luminosity AGN. Also see Moustakas & Immler (04), Wang et al. (04)

  11. General Conclusions AGN at z ~ 4-6 and z ~ 0-2 have reasonably similar X-ray and broad-band spectra. No hints of different accretion/growth mechanisms. (After controlling for luminosity effects) Small-scale X-ray emission regions insensitive to strong large-scale environmental differences from z ~ 0-6. X-ray emission universal. X-ray surveys giving significant demographic constraints on mod.-lum. AGN at highest redshifts.

  12. Some Future Prospects Improve coverage at z = 5 - 6.5 + Other selection methods – minimize bias IR, submm, mm Minority populations Weak-line quasars, BALQSOs, RLQs Better X-ray spectral and variability studies Chandra can go significantly deeper with best positions for ~ 20 years. Both Chandra and XMM-Newton can go wider.

  13. Long-Term Prospects – Proto-Quasars and Black Holes from the First Stars 1 Chandra count per 35 yr

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