Quasars and Galaxies at the Highest Redshifts Richard
- Slides: 59
Quasars and Galaxies at the Highest Redshifts Richard Mc. Mahon Institute of Astronomy University of Cambridge, UK Crafoord Symposium, Stockholm, Sep 2005 Crafoord Symposium, Sept 2005 1
Some Background Information • Main motivation is that objects at high redshift are ‘young’ due to the light travel time. e. g. we can ‘see’ objects that existed in the Universe before the Earth formed. • Quasars are the most luminous members of the Active Galactic Nuclei (AGN) family. – MB< -23 ; AGN light exceeds energy from host galaxy stellar light. • Quasars are intrinsically luminous bright beacons that are easier to observe that ‘normal’ galaxies like the Milky Way. Also ‘illuminate’ intervening material. i. e. IGM • Energy source is accretion of matter onto a super-massive black hole (107 to 109 Msol ) – Rees, 1984, ARA&A, 22, 471, ‘Black Hole Models for Active Galactic Nuclei’ • Recent observations have shown that most massive galaxies in the local Universe host super-massive black holes. The BH mass is correlated with the stellar bulge mass implies that the formation and evolution of BH and the stellar component in galaxies related (Magorrian et al, 1998; Ferrarese & Merrit, 2000; Gebhardt etal, 2000) – Rees, 1989, Rv. MA, 2, 1, ‘Is There a Massive Black Hole in Every Galaxy? ’ • Radiative feedback from quasars may play a major role in formation and evolution of galaxies. Crafoord Symposium, Sept 2005 2
Look Back Time matter, , H 0 = 0. 3, 0. 7, 70 Formation of Solar System: ~5 Billion year ago (5 Gyr) Redshift Look back Time (Gyr) Age of Universe 0 0. 0 13. 5 Gyr 0. 5 5. 0 8. 5 1. 0 7. 7 5. 7 Gyr 3. 0 11. 4 2. 1 Gyr 6. 0 12. 5 915 Myr 8. 0 12. 8 630 Myr 10 13. 0 460 Myr 30 13. 4 97 Myr 100 13. 45 16 Myr 1000 13. 46 0. 42 Myr Crafoord Symposium, Sept 2005 3
Highest Redshift History Quasars Galaxies Crafoord Symposium, Sept 2005 4
Highest Redshift History “Gunn” Quasars Galaxies Crafoord Symposium, Sept 2005 5
The Observational Challenges in surveys for high redshift objects • Experimentally difficult because: – Distant objects are very faint. – Rest frame UV radiation is red-shifted to regions of observed sky spectrum where night-time sky is bright. – Foreground objects are much more numerous so the experimental selection technique has to be very efficient. – May be undetectable, in a ‘reasonable’ amount of time using current technology; i. e. may need to wait or develop the technological solution. Crafoord Symposium, Sept 2005 6
Basic observational principles in optical surveys for higher redshift quasars and galaxies • UV ‘drop-out’ due to: – Intrinsic or Intervening Neutral Hyrogen ‘Lyman limit’ at 912Å. – Intervening Lyman-a forest ( <1216Å) • Emission line searches based on Lyman ( rest=1216Å) emission from ionized Hydrogen. Crafoord Symposium, Sept 2005 7
3 C 273 and z=3. 62 comparison Crafoord Symposium, Sept 2005 Evolution of HI: 3 C 273 spectrum from HST/FOC z=0; z=3. 6 QSO HIRES/Keck spectrum from M. Rauch 8
z=4 Model Quasar +SDSS filter set Crafoord Symposium, Sept 2005 9
Lyman- ( rest=1216Å) Lyman- Forest Quasars at z 5 C, N, O, Si. z = 4. 90, Schneider, Schmidt, Gunn, 1991, AJ, 98, 1951 z = 5. 0, Fan with Guun, Lupton et al. 1999 (SDSS collaboration) Crafoord Symposium, Sept 2005 11
z=5 quasar with SDSS filters Crafoord Symposium, Sept 2005 12
z=6 quasar with SDSS filter set Crafoord Symposium, Sept 2005 13
SDSS Surveys for z>5 Quasars Fan, et al. • Color selection of i-drop out quasars – At z>5. 5, Lyα enters z-band quasars have red i-z colour • Technical Challenges: – Rarest objects • One z~6 quasar every 500 deg 2 • Key: contaminant elimination – Major contaminants are L and T type Brown Dwarfs additional IR photometry Crafoord Symposium, Sept 2005 14
SDSS compilation z>5. 7 quasars Crafoord Symposium, Sept 2005 16
‘Edited’ Quasar compilation (pre-SDSS) Crafoord Symposium, Sept 2005 17
Quasar compilation (now with SDSS) ? DR 3 QSO 50, 000 quasars Crafoord Symposium, Sept 2005 18
Higher Redshift Quasar Surveys • Need to work in Infra-Red – Different detector technology – Sky ‘brightness’ problem • Two relevant projects – UK Infra Red Deep Sky Survey (UKIDSS) • WFCAM on UKIRT • Survey started in May 2005 • Pipeline Data processing centre(Cambridge+Edinburgh) – VISTA (will be an ESO telescope) (Surveys will start in early 2007? ) Crafoord Symposium, Sept 2005 19
The Night Sky Problem Broad band sky gets brighter as you go to redder wavelengths Waveband Central Wavelength (Angstroms) ‘Dark’ Sky Brightness Redshift Lyman- (1216Å) B 4400 22. 1 2. 6 V 5500 21. 3 3. 5 R 6000 20. 4 3. 9 I 7500 19. 0 5. 2 Z 8900 18. 0 6. 4 Y 10, 300 17. 0 7. 5 J 12, 500 16. 0 9. 3 H 16, 500 14. 0 12. 6 K 22, 000 13. 0 16. 3 Crafoord Symposium, Sept 2005 20
z=6 quasar (SDSS filter set) Crafoord Symposium, Sept 2005 21
z=7 quasar (SDSS filter set) Crafoord Symposium, Sept 2005 22
z=8 quasar (SDSS filter set) Crafoord Symposium, Sept 2005 23
z=6 quasar (SDSS filter set + WFCAM) Crafoord Symposium, Sept 2005 24
z=7 UKIDSS/VISTA Filters Crafoord Symposium, Sept 2005 25
z=8 UKIDSS/VISTA Filters Crafoord Symposium, Sept 2005 26
z=9 UKIDSS/VISTA Filters Crafoord Symposium, Sept 2005 27
z=10 UKIDSS/VISTA Filters Crafoord Symposium, Sept 2005 28
UK Infra Red Telescope (UKIRT) Wide Field Camera (WFCAM) 3. 6 m telescope Mauna Kea, Hawaii 4 x 2048 Hawaii II arrays 0. 4 arcsec pixels 0. 21 sq. degs / exposure • Not contiguous Filters: • Z, Y, J, H, K, H 2 -S(1), Br-g Crafoord Symposium, Sept 2005 29
UKIRT Wide Field Camera on Telescope Simulator WFCAM cryostat Asembled WFCAM cryostat Crafoord Symposium, Sept 2005 30
UKIDSS overview 5 elements of UKIDSS(5 -7 year duration) Sub-Survey Bands Limit (K) Area deg 2 night s Large Area Survey LAS YJHK 18. 4 4000 262 Deep Extragalactic Survey DXS JK 21. 0 35 118 Ultra Deep Survey UDS JHK 23. 0 0. 77 296 Galactic Plane Survey GPS JHK 19. 0 1800 186 Galactic Clusters Survey GCS JHK 18. 7 1600 84 Crafoord Symposium, Sept 2005 31
UKIDSS Science goals Cool Universe - Y brown dwarfs Obscured Universe - Galactic plane - reddened AGN, starbursts, EROs High-redshift Universe - 4000 A break z>1; high redshift galaxy clusters - Quasars at z>6. 5 Crafoord Symposium, Sept 2005 32
Current Status of WFCAM+UKIDSS • Instrument started commissioning on-sky phase in Nov, 2004 • Science Verification started in April 2005 • UKIDSS Survey started in May, 2005 • Instrument taken off telecope in June, 2005 – As planned • Survey restarted end of Aug, 2005 • Should have 100 deg 2 of data by end of 2005 Crafoord Symposium, Sept 2005 33
Visible and Infrared Survey Telescope for Astronomy • 4 -m wide field survey telescope at European Southern Observatory (ESO) , Paranal near the VLT site. • Initially Infra Red camera only. (i. e. an IR SDSS) • 75% time for “large surveys”. (e. g. Southern SDSS) • UK project (consortium of 18 Universities; funded in 1999) – Principal Investigator Jim Emerson (QMUL, London) • Now part of UK ESO ‘late joining fee’. • Will become ESO facility on completion of construction and commissioning in late 2006. Crafoord Symposium, Sept 2005 34
The ‘Heart of VISTA’; the IR focal plane: • 16 IR arrays, each 2048 x 2048; sparse filled mosaic; • 0. 60 deg 2 covered by detectors • 0. 34 arcsec/pix. - 6 consecutive ‘offset’ pointings give a continuous region - 1. 5 deg by 1. 0 deg i. e. 1. 5 deg 2 - every pixel covered by 2 pointings.
Comparison of IR camera field sizes Moon! Crafoord Symposium, Sept 2005 36
Dome – May 05 Crafoord Symposium, Sept 2005 37
Summer 2005 Crafoord Symposium, Sept 2005 38
Highest Redshift Galaxies Crafoord Symposium, Sept 2005 40
Searches for higher redshift quasars and galaxies • UV ‘drop-out’ technique survey technique due to: – Intrinsic or Intervening ‘Lyman limit’ 912Å. – Intervening Lyman-a forest ( <1216Å) • Emission line searches based on Lyman- emission from ionized Hydrogen. Crafoord Symposium, Sept 2005 41
Highest Redshift History Quasars Galaxies Crafoord Symposium, Sept 2005 42
High Redshift Lyman- emission lines surveys: Astrophysical principles for Success Partridge and Peebles, 1967, Are Young Galaxies visible? Minimum Flux limit • Previous surveysin the early 1990’s were based on the simple paradigm of a monolithic collapse. – expected star formation rates of 50 -500 Msol yr-1 – i. e. the SCUBA/FIR Population? • Assume SFR detection limits more appropriate to a slowly forming disc or sub -galactic units in a halo – i. e. 1 -3 Msol yr-1 Þ 1. 0 -2. 0 10 -17 erg s-1 cm-2 at z=4 Minimum Volume • search a comoving volume within which you expect to find the progenitors of around 10 L* galaxies. (. i. e. ~ Milky Way mass) – Local density 1. 4± 0. 2 10 -2 h 50 Mpc-3 (e. g. Loveday etal, 1992) Þ minimum is 1000 Mpc 3 Crafoord Symposium, Sept 2005 43
Potential Narrow band filter locations 5. 7 Crafoord Symposium, Sept 2005 6. 6 6. 9 44
z=5. 7 for Lyman- z=6. 6 for Lyman- Crafoord Symposium, Sept 2005 45
Basic experimental principle • Basic principle is to survey regions where the sky spectrum is darkest in between the intense airglow. – “Gaps in the OH airglow picket fence” • Lyman-alpha redshifts of gaps in “Optical-Silicon” CCD regime – – 7400 Å; z=5. 3 8120 Å; z=5. 7; used extensively 9200 Å; z=6. 6; used extensively 9600 Å; z=6. 9; no results yet • CCDs have poor QE and sky relatively bright Crafoord Symposium, Sept 2005 46
Summary of known spectroscopically confirmed z>6. 0 galaxies Narrow Band Surveys • z>6. 0; n=13 – from Hu et al. 2002(1), Kodeira et al. 2003(2), Rhoads et al 2004(1), Taniguchi et al. 2005(9) – z(max)=6. 6 Other Surveys • 2 other z>6 emission line selected galaxies – Kurk et al, 2004(1); Stern etal, 2005(1) • Ellis etal, lensed search z=7 candidate (no line emission; photo-z) • i-drops Nagao et al, 2004(1); Stanway etal, 2004(1) • Quasars; SDSS n=5 (6. 0< z<6. 5) Crafoord Symposium, Sept 2005 47
(observed; Lyman- )=9190Å (rest; Lyman- )=1216Å Redshift=6. 558 Crafoord Symposium, Sept 2005 Hu, etal, 2002 48
z=6. 597 galaxy (Taniguchi et al, PASJ, 2005) Survey: • Subaru 8. 2 m • Suprimecam 34’ x 27’; 0. 2”/pixel • 132Å filter centred at 9196Å • Exposure time; 54, 000 secs (15 hrs) Results • 58 candidates • 9 spectroscpoically confirmed with z=6. 6 9235 Ang Crafoord Symposium, Sept 2005 redshift 6. 597 z. AB 26. 49 i-z >1. 72 49
Composite spectrum of z=5. 7 candidate galaxies [OIII]4959 z=0. 6; unresolved and 4959 line [OIII](5007Å) z=1. 2; note resolved doublet [OII](3727Å) n=18 galaxies z=5. 7; note asymmetry Lyman- (1216Å) Hu, Cowie, Capak, Mc. Mahon, Hayashino, Komiyama, 2004, AJ, 127, 563 Crafoord Symposium, Sept 2005 50
z~5. 7 Lyman- (1216Å) emitters Crafoord Symposium, Sept (Angstroms) 2005 Observed wavelength 51
z~1. 2 [OII]3727 doublet emitters Crafoord Symposium, Sept (Angstroms) 2005 Observed wavelength 52
The Night Sky Problem Broad band sky gets brighter as you go to redder wavelengths Waveband Central Wavelength (Angstroms) ‘Dark’ Sky Brightness Redshift Lyman (1216Å) B 4400 22. 1 2. 6 V 5500 21. 3 3. 5 R 6000 20. 4 3. 9 I 7500 19. 0 5. 2 Z 9000 18. 0 6. 4 J 12, 500 16. 0 9. 3 H 16, 500 14. 0 12. 6 K 21, 000 13. 0 16. 3 Crafoord Symposium, Sept 2005 53
Narrow band searches in the near Infrared • OH lines contribute 95% of sky background in 1. 0 -1. 7 m range; – i. e. 20 times the continuum emission. • Filters need to have widths of 10Å or 0. 1% to avoid OH lines. – c. f. 100Å in the optical • NB. Narrower band means you solve a smaller redshift range i. e. volume so wide field is needed. Some of the technical issues – Filter design and manufacture – Field angle shift of central wavelength – Out of band blocking; Crafoord Symposium, Sept 2005 54
Infrared OH Sky Observations: Mahaira etal, 1993, PASP GOOD NEWS The 1. 0 to 1. 8 micron IR sky is very dark between the OH lines which contain 95% of broad band background. THE NOT SO GOOD NEWS The narrowest gaps are narrower than in the optical; filter widths of 0. 1 per cent are needed compared with 1% filters in optical. THIS IS A TECHNICAL CHALLENGE WE HAVE SOLVED; see Ian Parry’s talk Crafoord Symposium, Sept 2005 55
DAZLE – Dark Age Z Lyman Explorer Mc. Mahon, Parry, Bland-Hawthorn(AAO), Horton et al IR narrow band imager with OH discrimination at R=1000 i. e. 0. 1% filter FOV 6. 9 arcmin 2048 Rockwell Hawaii-II 0. 2”/pixel Sensitivity: 2. 10 -18 erg cm-2 sec-1(5 ), 10 hrs on VLT i. e. ~1 M yr-1 at z=8; Sky emission and absorption spectrum around 1. 06 and 1. 33 microns showing DAZLE filter pairs for Lyman at z=7. 7, 9. 9; other gaps are Sept at 8. 8, Crafoord Symposium, 20059. 2 56
DAZLE: Digital state • 3 D CAD drawing of DAZLE Final Design on VLT UT 3(Melipal) Visitor Focus Nasmyth Platform. • UT 3 optical axis is 2. 5 m above the platform floor • grey shading shows the DAZLE cold room(-40 C)which is 2. 5 m(l) x 1. 75 m(w) x 3 m(h). • Blue Dewar at top contains the 2048 x 2048 pixel IR detector Crafoord Symposium, Sept 2005 57
Dazle in Cambridge Laboratory(Aug 2005) Refridgeration ‘Box’ Crafoord Symposium, Sept 2005 58
Highest Redshift History Quasars Galaxies Crafoord Symposium, Sept 2005 59
Quasar compilation (now with SDSS) ? DR 3 QSO 50, 000 quasars Crafoord Symposium, Sept 2005 60
Some Future ground based surveys for higher redshift Galaxies and Quasars z>7 galaxies • Dark Ages ‘Z’ Lyman- Explorer (DAZLE) on the VLT (to start Jan 2006) z>7 quasars • UKIDSS: UK Intra-Red Deep Sky Survey (started May 2005; 5 year survey project) – UKIRT (Hawaii) + WFCAM – ESO members; Public Access from late 2005); Worldwide +18 month • VISTA Surveys (to start early 2007) Crafoord Symposium, Sept 2005 61
FINAL SLIDE Crafoord Symposium, Sept 2005 62
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