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Extragalactic Astronomy and Cosmology at IfA Edinburgh

Extragalactic Astronomy and Cosmology at IfA Edinburgh. Timetable for the day. 11:00 Closed Panel session 11:30 Presentations Part-1 12:50 Lunch 13:40 Presentations Part-2 14:50 Q & A session 15:50 Closed Panel Session 17:00 End. Schedule of Talks.

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Extragalactic Astronomy and Cosmology at IfA Edinburgh

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  1. Extragalactic Astronomyand Cosmology at IfA Edinburgh

  2. Timetable for the day • 11:00 Closed Panel session • 11:30 Presentations Part-1 • 12:50 Lunch • 13:40 Presentations Part-2 • 14:50 Q & A session • 15:50 Closed Panel Session • 17:00 End

  3. Schedule of Talks 11:30 Andy Lawrence Introduction11:40 Jim Dunlop Overview talk-111:50 Philip Best High-z galaxy evolution12:05 Marek Kukula Host galaxies of quasars12:20 Omar Almaini Deep X-ray surveys and AGN12:35 Will Percival Modelling AGN evolution new bid LUNCH 13:40 John Peacock Overview talk-213:50 Alan Heavens Statistical methods for cosmology vacant14:05 Eelco van Kampen Simulating galaxy formation14:20 Avery Meiksin Simulating evolution of the IGM new bid14:35 Arjun Berera Observational tests of inflation new bid

  4. Key Points • Grant supports 9 academic-equivalent staff • main activity of 6, partial activity of 3 • Peacock, Taylor, Jimenez and Berera added as PIs • Talented and aggressive team of PDRAs • Case presented as clear projects • science a continuum but deliverables distinct • PDRAs nurtured but do cycle through • Hughes, Taylor, Jimenez all moved through

  5. Edinburgh context • Institute for Astronomy • 7 ac. staff; 4.5 senior research fellows (half of Berera) • Temporary Lecturer being recruited • 5 PDRAs on rolling grant support + 1 on Gemini grant • WFAU : 6.5 research staff, 4.5 tech/admin (2.2 research FTEs) • Astronomy Technology Centre • approx 11 active astronomers; 3.5 research FTEs • Astronomy elsewhere in University • 3 academic staff in Maths/Physics (Heggie/Ruffert/Shotter) • 0.5 senior research fellows in Physics (Berera)

  6. Current bid • Merges existing roller and Peacock PDRA • Focused on extragalactic and cosmology • star formation and low mass stars excluded • supported to some extent in ATC and WFAU • Baseline 5 PDRAs : bid for +3

  7. PDRA bid summary • Hi-z funded Y1-2 bid+2yr Best in place (Hughes left)Hosts funded Y1-2 bid+2yr Kukula in placeX-AGN funded Y1 bid+3yr Almaini in placeAGN evoln new line bid+4yr Percival in place (1 yr contract)Stat.cos. funded Y1-2 bid+2yr vacant (Taylor got AF)Sim.cos. funded Y1 bid+3yr Van Kampen in placeIGM new line bid+4yrInflation new line bid+4yr • Notes : Hughes left early + Kukula spell at STScI • unspent funds  1 year contract to Percival

  8. Part 1 4 named PDRAs (3 existing grant lines + 1 new one) • Linking themes: • Major multi-frequency surveys • Cosmological evolution of AGN, galaxies & clusters • Physical connections history of AGN activity history of star-formation activity black hole formation host spheroid formation

  9. Key issues History of black hole activity History of star-formation activity (Radio& X-ray)(Visible& Dust-enshrouded)

  10. Black-hole formation Host spheroid formation Radio Galaxies Sub-mm evolutioncontrasts with radio evolution especially at z > 2.5 (Archibald, Dunlop et al. 2000) But perhaps this makes sense…. Stars Big black holes are needed by z= 3 and hence perhaps also big bulges Dust Friaca/Jimenez models predict growth ofstarsand decline ofdust for formation redshift z = 5 Gas

  11. Philip Best • z distribution of the field sub-mm population • sub-mm - optical studies of radio galaxies and high z clusters • Marek Kukula • HST/Gemini/VLT studies of the hosts of quasars, z = 0 - 5 • VLA/Merlin studies probing the origin of radio loudness • Omar Almaini • Major X-ray surveys: - resolving the X-ray background, • new hard X-ray populations, AGN to z = 8, X-ray/sub-mm link • Will Percival • Analytical theory - evolution of compact activity in a cosmological context • The black-hole galaxy-formation link

  12. Philip Best High z Galaxy Evolution Marek Kukula Quasar Host Galaxies Omar Almaini Deep X-ray Surveys Will Percival Modelling Evolution

  13. High Redshift Galaxy Evolution Observational and theoretical study of the evolution of massive galaxies. Main themes: • Dust enshrouded starbursts at high redshift • SCUBA surveys & follow-up • HDF, 8mJy, cluster surveys • Galaxy evolution in clusters • Deep spectroscopic studies of HzRG’s • Age dating of stellar populations

  14. My previous work Radio, optical, IR & spectroscopic studies of HzRG’s

  15. The SCUBA 850-m HDF map Deepest SCUBA map 50 hours integration 100 arcsec radius Beam: 14.5’’ FWHM Noise: rms 0.45 mJy 5 strong sources

  16. HDF 850.1 Downes et al. astro-ph/9907139 IRAM 1.3-mm & VLA data needed to provide an accurate position. No consistent optical id. cf. such ULIRGs with optical SF gals (ratio ~ 5)

  17. Background structure: “normal” star-forming galaxies Subtract 5 brightest point sources (Peacock et al. 2000) Residual structure correlates with optical-UV selected star-forming galaxies

  18. 8 mJy survey Collaboration with Imperial College, Cambridge and UCL • Shallow wide-field survey to complement HDF • 400 sq. arcmins to S850mm= 8mJy (3-) • 8 SCUBA shifts allocated; 24 more long-term • z and T constraints from deep 175m ISO data • New PhD student (Suzie Scott) working on data reduction & source extraction

  19. Deep radio imaging (VLA time already awarded): identify sources with z < 2.5 z estimate from radio vs sub-mm spectral index isolates extreme z objects Multi-wavelength follow-up Essential for reliable identifications & redshifts of SCUBA sources. Will take several years. from Carilli & Yun, 2000

  20. mm interferometry, IRAM PdB • time awarded (collaboration, Dieter Lutz) • reliable positions for radio empty fields • brightest SCUBA source in Lockman hole region has been detected - but no optical/IR id • Deep optical - IR imaging • UKIRT time allocated • some sources will need Gemini • Spectroscopy • obtaining redshifts clearly requires 8m class telescopes

  21. High redshift cluster studies Why carry out deep radio / sub-mm studies of high redshift clusters? • SCUBA observes different population of star-forming objects than those from optical studies • Clusters at high z: • are young, possibly still forming • have high galaxy merger rates • are ideal testbeds of galaxy evolution • Good complement to field surveys / low-z clusters

  22. 2 projects: • Deep SCUBA and VLA studies of z~1 clusters • 8 shifts start-up SCUBA time allocated • 30 hrs VLA data on MS1054 taken in April • Initially targeting clusters with much optical-IR data • Imaging around z>3 radio galaxies • known regions of high overdensity (protoclusters?) • positive results from pilot study (4C41.17) • long-term status awarded for an extended study Both projects will require considerable follow-up.

  23. CL1604+43 (z=0.9), 850m Preliminary results (March 2000 data) 1 shift (2 more to come) - 3 clear detections - 2-3 marginal - much richer than blank field pointings

  24. MS1054-03 (z=0.8), 5GHz 30 hrs, 5 GHz, C-array (taken April 2000) - rms 5.7Jy - numerous detections - overlay with deep HST mosaic: most detections have secure id’s - Keck MOS data: many id’s at redshift of cluster.

  25. Galaxy evolution in clusters In addition to studies of cluster star formation, aim to push back cluster studies to earlier epochs • very deep optical / IR imaging around z>1.5 RGs • cross-correlation statistics • colour-magnitude diagrams • photometric redshifts • follow-up multi-object spectroscopy (Gemini) • evolution of cluster environments • age-dating of evolved elliptical galaxies (Jimenez) Just one massive cluster at this redshift has severe consequences for LSS and cosmological models.

  26. Conclusions Studies of SCUBA sources are rapidly advancing and provide key information about SF history of the Universe. Much follow-up work is required. Long-term goal is to couple this work with that on • Galaxy evolution in clusters • Deep spectroscopic studies of HzRGs • Age dating of stellar populations to obtain a consistent view of the evolution of “activity” in the Universe

  27. Philip Best High z Galaxy Evolution Marek Kukula Quasar Host Galaxies Omar Almaini Deep X-ray Surveys Will Percival Modelling Evolution

  28. Quasar Host Galaxies PDRA: Marek Kukula PI: James Dunlop Ground-based & HST observations of carefully constructed quasar samples Line-free imaging and off-nuclear spectroscopy of host galaxies Comprehensive study of local (z=0.2) quasar hosts now complete Recently extended out to z=2 with NICMOS Next phase: follow host galaxy evolution to z>4 with HST, VLT & Gemini

  29. Why study quasar hosts? HST studies of local (z < 0.3) quasars show that their hosts tend to be dominated by a massive spheroidal component. Very likely all large elliptical galaxies contain massive black holes and are potential quasar hosts. At z = 2.5 a significant fraction of all massive black holes were active. Quasar evolution and the starformation history of the universe share similar properties growth & fuelling of black holes is closely linked to the evolution of large-scale structure.

  30. Low-redshift quasar hosts R-band imaging with HST/WFPC2 0.1 < z < 0.25 Carefully matched samples: Radio-Quiet Quasars, Radio-Loud Quasars & Radio Galaxies R-band filter avoids contamination by quasar emission lines Awarded 34 orbits in Cycle 6 (completed 1999) Surface brightness profile Image Model 2-D modelling Galaxy Residual

  31. 2-D modelling of HST data: Analysis of HST images The hosts of all but the least luminous RQQs are massive elliptical galaxies

  32. Black Hole Masses For local inactive galaxies: M (bh) = 0.006 M (bulge) (Magorrian et al. 1998) Can now do the same for our quasar samples: Bulge luminosity Black hole mass RLQ RQQ 9 10 M (bh) ~ 10 - 10 M 0 Can estimate Eddington luminosities: quasars are radiating at ~10% Eddington 100% 10% 1%

  33. Off-nuclear spectroscopy Optical spectroscopy with the WHT Use image to select optimum slit position 5 arcsec off-nucleus Galaxy spectrum Spectrophotometric modelling Hosts dominated by an old (~12 Gyr) stellar population. Little on-going starformation (< 0.5 % by mass). Main result : at z = 0.2 all luminous quasars are in massive ellliptical galaxies - regardless of radio luminosity of the quasar

  34. Out to z=2 with NICMOS Define 3 new quasar samples at z = 0.4, 1 & 2 Choose quasars of the same intrinsic luminosity at each z Redshift/filter combination always samples the same region of the restframe spectrum 60 orbits with WFPC2 & NICMOS in Cycle 7 (to complete Nov. 2000)

  35. Results from NICMOS A first look at host galaxy evolution out to z=2 2-D modelling Image Surface brightness profile z=0.2 : massive elliptical galaxies z=2 : no large, luminous galaxies present z=1 : large, luminous elliptical galaxies large galaxies are still assembling? same as hosts at z=0.2 smaller galaxies, quasar fuelling more efficient? hosts fully-assembled by z=1

  36. Next phase: 2000 - 2004 Follow host galaxy evolution out to z > 4 Initial observations underway: HST Cycle 9 VLT near-infrared imaging (commencing 2000) (commencing 2000) Same highly successful strategy: carefully controlled samples line-free imaging Starting point for major study with new-generation instruments Work to date

  37. New observations New instruments will make detailed studies of high-z quasar hosts possible Edinburgh team extremely well-placed to exploit these new capabilities : HST Advanced Camera for Surveys : multi-colour optical imaging Gemini : NIR imaging (proposal submitted) Ground-based 8-m spectroscopy

  38. Philip Best High z Galaxy Evolution Marek Kukula Quasar Host Galaxies Omar Almaini Deep X-ray Surveys Will Percival Modelling Evolution

  39. Deep X-ray Surveys Omar Almaini Andy Lawrence, Jim Dunlop XMM

  40. Progress 1998-2000 • ROSAT/ASCA Surveys • ROSAT/ASCA Surveys Almaini et al 1998 Lira et al. (1999) Iwasawa et al. (2000) • Studies of dwarf AGN • Studies of dwarf AGN Fabian et al 1998 • X-ray/sub-mm link • X-ray/sub-mm link Georgantopoulos et al 1998 • X-rays from starbursts • X-rays from starbursts Natarajan & Almaini 2000 Boyle et al 1998 • QSO X-ray Variability • QSO X-ray Variability Blair et al 1999 Almaini, Gunn & Shanks 2000 Almaini et al. 2000 Almaini, Lawrence & Boyle 1999 Manners et al. (in preparation)

  41. The ELAIS/SCUBA X-ray Survey Chandra (150ks) XMM (150ks) PI: Almaini • ELAIS 7.5, 15, 90, 175µm • UK 8mJy SCUBA survey • Imaging to R=26, K=22 • VLA radio (0.1mJy)

  42. The Puzzle Of The X-ray Background

  43. Deep ROSAT Surveys 12 day exposure!

  44. Emission-line galaxies? ‘NELGs’ Broad-line QSOs Almaini et al. (1996)

  45. July 23, 1999

  46. The ELAIS/SCUBA X-ray Survey Chandra (150ks) XMM (150ks) PI: Almaini • ELAIS 7.5, 15, 90, 175µm • UK 8mJy SCUBA survey • Imaging to R=26, K=22 • VLA radio (0.1mJy)

  47. Chandra Soft X-ray Source Counts

  48. Chandra Hard X-ray Source Counts

  49. XMM

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