1 / 30

Science with FMOS The UDS perspective Omar Almaini (Nottingham)

Science with FMOS The UDS perspective Omar Almaini (Nottingham). Update on UKIDSS UDS The UDS redshift survey ( UDSz ) Opportunities with FMOS. The need for deep infrared surveys. Optical selection samples rest-frame UV at high- z. 1. Miss galaxies heavily obscured by dust

zeno
Download Presentation

Science with FMOS The UDS perspective Omar Almaini (Nottingham)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Science with FMOSThe UDS perspectiveOmar Almaini (Nottingham) • Update on UKIDSS UDS • The UDS redshift survey (UDSz) • Opportunities with FMOS

  2. The need for deep infrared surveys Optical selection samples rest-frame UV at high-z 1. Miss galaxies heavily obscured by dust 2. Miss galaxies with old stellar populations 3. Provide poor estimate of stellar mass Deep IR surveys vital for a complete census

  3. The UKIDSS Ultra-Deep Survey Depths achieved so far: (AB, 5, 2" apertures) DR3: K=23.6, H=23.5, J=23.8 (104 hours) 0.88 deg. DR5: K=24.0, H=23.8, J=24.2 (178 hours) 2012:K=25.0, H=25.2, J=25.5 (~1700 hours) Already deepest IR survey over this area…

  4. The Subaru/XMM Deep Field Optical: B=28.2, V=27.6, R=27.5, i’=27.2, z’=26.5, U=27.0 X-ray: XMM-Newton 100ks + 6x50ks Radio: VLA 12 Jyrms 1.4Ghz Spitzer: Spitzer SWIRE 3.6-160m (NEW: Legacy survey to ~24 AB at 3.6, 4.5m) Submm: SHADES 8mJy (850m) + SCUBA2 from 2010 RA = 02 18 00, Dec = -05 00 00

  5. Evolution in colour bimodality to KAB=23 0.25 < z < 0.75 0.75 < z < 1.0 1.0 < z < 1.25 (u-b)rest 1.75<z<2.25 1.5 < z < 1.75 1.25 < z < 1.5 MK Cirasuolo et al. (2009)

  6. Clustering evolution with redshift and luminosity (passivevsstarforming) Hartley et al. (2009)

  7.  = 0.03 Photometric redshifts (U, B, V, R, i’, z’, J, H, K, 3.6, 4.5) Cirasuolo et al. (2007)

  8. The UDS Redshift Survey(UDSz) Omar Almaini (PI), Rob Chuter, SebastienFoucaud, Will Hartley, Emma Bradshaw (Nottingham) Jim Dunlop, Ross McLure, Michele Cirasuolo, Henry Pearce, Rob Ivison (Edinburgh) Chris Simpson (LJM), Ian Smail (Durham), Malcolm Bremer (Bristol) + many other Co-Is

  9. UDSz ESO Large Programme (~60% complete) 93 hours VIMOS142 hours FORS2

  10. 0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 4.5 5.0 photo-z ESO Large Programme: UDSz •K-selected sample to KAB<23 over 0.6 sq degrees• Primary sample pre-selected with zphot>1 • Sampling 1/6 galaxies (~4000)

  11. Selection Criteria VIMOS (Red+Blue) i’<24 or V<25.5 i’<25 & V>25.0 FORS2 (300I) + extras (e.g. z>5 LBGS, SCUBA gals)

  12. FORS2 5.5 hours 300I VIMOS 2.6 hours red 4.5 hours blue

  13. BzK galaxies observed with VIMOS Rob Chuter (Nottingham)

  14. EROs (R-K>5.5) observed with FORS2 Henry Pearce (Edinburgh)

  15. First confirmed UDS galaxy at z>6 Ly-α at z=6.05 (FORS2)

  16. Early estimate of redshift completeness: 77% VIMOS + FORS2

  17. First public release of UDSz early 2010 • Observations ~60% complete • Reduction and redshift determination ongoing • Anticipate ~3000 reliable redshifts • First public release early 2010

  18. The need for FMOS • Ideally suited for spectroscopy in the redshift desert (1.4<z<2.5) • … and for optically-faint galaxies (i>25) • With FMOS: Hα/NII 0.5<z<1.6 • Hβ/OIII 1.2<z<3.4 • OII 2.0<z<3.6 • MgII 2.7<z<5.0 • Ca H+K 1.6<z<3.5 • => SFR, age of stellar population, AGN prevalence, outflows, • studies of environment, clustering, halo occupation • Is it feasible? • Line: Hα limit in 5 hours ~ 3 x10-17 cgs=> SFR of 3 Myr-1 (z=1.5) • Continuum: ~7 hours to reach S/N=5 to J~22, H~21

  19. 5000 4000 3000 2000 1000 0 count z > 1 z < 1 FMOS? 20 22 24 26 28 i Challenge for FMOS: the optically faint population (i>24.5)

  20. 1.0< z< 1.5

  21. 1.0< z< 1.5 i<24.5 i>24.5

  22. 1.0< z< 1.5 i<24.5 i>24.5 J<22, H<21

  23. 1.5< z< 2.5

  24. 1.5< z< 2.5 i<24.5 i>24.5

  25. 1.5< z< 2.5 i<24.5 i>24.5 J<22, H<21

  26. The need for FMOS • Ideally suited for spectroscopy in the redshift desert (1.4<z<2.5) • … and for optically-faint galaxies (i>25) • With FMOS: Hα/NII 0.5<z<1.6 • Hβ/OIII 1.2<z<3.4 • OII 2.0<z<3.6 • MgII 2.7<z<5.0 • Ca H+K 1.6<z<3.5 • => SFR, age of stellar population, AGN prevalence, outflows, • studies of environment, clustering, halo occupation • Is it feasible? • Line: Hα limit in 5 hours ~ 3 x10-17 cgs=> SFR of 3 Myr-1 (z=1.5) • Continuum: ~7 hours to reach S/N=5 to J~22, H~21

  27. Fin

More Related