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High Redshift Quasar Survey

Survey Science Group Workshop, 2013 High1 Resort. High Redshift Quasar Survey. Yiseul Jeon, Myungshin Im, W.-K. Park, J. H. Kim, M. Karouzos, J.-W. Kim, S.-K. Lee, H. Jun, C. Choi, D. Kim, D. Kim, J. Hong, M. Hyun, and Y. C. Taak

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High Redshift Quasar Survey

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  1. Survey Science Group Workshop, 2013 High1 Resort High Redshift Quasar Survey Yiseul Jeon, Myungshin Im, W.-K. Park, J. H. Kim, M. Karouzos, J.-W. Kim, S.-K. Lee, H. Jun, C. Choi, D. Kim, D. Kim, J. Hong, M. Hyun, and Y. C. Taak Center for the Exploration of the Origin of the Universe (CEOU), Astronomy Program, Dept. of Physics & Astronomy, Seoul National University

  2. Contents • Introduction • History of our Universe • High Redshift Quasars • Method of Study • Multi-wavelength Data • Color Selection • Current Status • Summary

  3. I. Introduction

  4. History of our Universe BB Dark Age Reionization Galaxy Formation Robertson et al. 2010 Neutral Hydrogen Recombination First Star/First Galaxy/First SMBH z ~ 20 Reionization z ~ 10 Galaxy Formation

  5. High Redshift Quasars • Quasar • - An energetic active galactic nucleus • - Powered by an accretion disc • High Redshift Quasar • - One of the brightest objects • - Useful for investigating the early universe • >50 quasars at z>5 discovered Artist's impression of quasar GB1508+5714 (z=4.3) • Intrinsic Properties of early SMBHs Mass Growth of SMBHs & Evolution of QLF • Environmental Effect due to Quasars Reionization of IGM

  6. 1. Growth of Super Massive Black Holes

  7. 1. Growth of Super Massive Black Holes 1) SMBH at z~7 SMBH of 109M⊙ already exists age ~0.8 Gyr

  8. 1. Growth of Super Massive Black Holes 1) SMBH at z~7 First SMBH already exists age < 1 Gyr → must have formed at very early time. 2) Redshift Desert at 5<z<6 Due to limitations of current selection technique 109M⊙ z~6  1010M⊙ z~5 ←z=5.5 ←z=5.2 i-z x10 increase during 0.5Gyr Chiu et al. 2005 r-i

  9. 1. Growth of Super Massive Black Holes 1) SMBH at z~7 First SMBH already exists age < 1 Gyr → must have formed at very early 2) Redshift Desert at 5<z<6 Due to limitations of current selection Cause of SMBH Growth unknown  More samples required

  10. 2. Reionization of Intergalactic Medium BB Dark Age Reionization Galaxy Formation Robertson et al. 2010 IGM attenuation (Madau 1996) ↓

  11. 2. Reionization of Intergalactic Medium Robertson et al. 2010 Gunn-Peterson trough z=6.13 Fan et al. 2006 Fan et al. 2006 z=5.93 z=5.83

  12. 3. Evolution of Quasar Luminosity Function ? Robertson et al. 2010 At z>10: First stars (e.g., Kashlinsky et al. 2005) At z<2.5: mostly by AGNs (e.g., Haardt & Madau 1996) Quasar Luminosity Function at z~6 Willott et al. 2010 At z~6: Star Forming Galaxy vs. Quasar ◇ SDSS main △ SDSS deep stripe ● CFHQS

  13. SMBH Mass Growth HI Fraction in IGM QLF at z~6 Redshift Redshift M1450 • Limitations of Previous Studies • Redshift Desert at 5<z<6 and Discovery of z~7 Quasar •  New selection technique • Various Luminosity Range •  Deep Survey Data • Larger Sample Size •  Wide Survey Data → New technique with New Deep/Wide survey data

  14. II. Method of Study

  15. Quasar candidate selection • e.g.) z~7 quasar (blue) • z Drop-out • Bluer Y-J than Brown Dwarf(green) • Power-law SED i z Y J H K 3.6 4.5 + Quasars Δ Model Brown Dwarfs + Star-forming galaxy + Passive Evolving Galaxy

  16. Quasar candidate selection • Match multi-wavelength catalogues • Select quasar candidates using color-color diagram • Remove spurious objects by eyeball rejection • Do photometry on original images • Imaging follow-up • Spectroscopy of remaining candidates

  17. Quasar candidate selection - Multi-wavelength catalogues (a) 3 mag deeper than SDSS z-band (b) available only for CEOU (c) only accessible to UKIDSS collaboration

  18. On-going High-z Quasar Survey of CEOU

  19. Quasar Selection at 5<z<6 Redshift gap at 5<z<6: due to the limitations of current filter system

  20. Quasar Selection at 5<z<6 <McDonald 2.1m> • Camera for QUasars in EArly uNiverse (CQUEAN) with custom designed Is and Iz filters at McDonald 2.1m ←CQUEAN • Spectroscopic Follow-up Observation • 2.5 nights at KP-4m (2012B) • 3 nights at KP-4m (2013A) • 3 nights at NTT (2013A)

  21. Quasar Selection at 5<z<6 • 2.5 nights at KPNO 4-m telescope <KPNO 4-m Jan. 2013 >

  22. Quasar Selection at z~7 Mauna Kea @May 2009

  23. Quasar Selection at z~7 • The most distant known quasar at z=7.085 (Mortlock et al. 2011) • Ongoing & Future Optical/Near-IR Surveys Willott et al. 2010 Intermediate-widemedium-deep survey is needed. UKIRT NIR Survey !

  24. IMS Fields

  25. Quasar Selection at z~6

  26. Quasar Selection at z~6 (1) From SEGUE data confirmed by HET and follow-up NIR spec. at IRTF (2) From UKIDSS LAS dataconfirmed by Magellan Color-Color Diagram NIR spectrum by IRTF, SpeX

  27. Quasar candidate selection - Spectroscopy of candidates • Confirm as Quasar! • Calculate redshift by identifying redshifted Lyman break and UV emission lines • Measure SMBH mass using UV emission lines such as CIV λ1549 • Investigate Lyman alpha forest to understand the ionization state of IGM

  28. III. Summary

  29. III. Summary • Limitations of Previous High-z Quasar Survey 1. Growth of SMBH 2. Reionization of IGM 3. Evolution of quasar LF • Deep/Wide Survey Data with New selection technique • SMBH evolution • IGM ionization process • CQUEAN/UKIRT • Thank you

  30. On-going High-z Quasar Survey of CEOU *assuming continuous density evolution of the high-z quasar LF (Willott+10)

  31. SMBH Mass Growth • < First SMBH > • Accretion from Seed BH • If BH mass increases by accretion with Eddington rate, • where tEdd = 0.45 Gyr and ε is the radiative effiency • From seed mass of 102M⊙, it takes 0.9 Gyr. • And From 105M⊙, 0.5 Gyr. (Volonteri10) •  Not enough for 109M⊙ at z~7 • By Galaxy Merger •  Possible from SAM in ΛCDM (Li+07) • < Vigorous growth at 5<z<6 > • Existence of the most massive SMBH Redshift

  32. SMBH Mass Growth HI Fraction in IGM • Abrupt transition? • (Fan+06) • Continuous process? • (Becker+07) Redshift Redshift

  33. SMBH Mass Growth HI Fraction in IGM QLF at z~6 Also, QLF of 5<z<6 and z~7 Redshift Redshift M1450 → Our research will contribute towards the understanding of the evolution of SMBHs and the IGM ionization state at the early Universe.

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