1. DESpec survey strategy : realistic mock catalogue and target selection Stephanie Jouvel, Filipe Abdalla, Huan Lin, James Annis, Richard Kron 22 jun 2011

2. PLAN : Investigate DESpec survey strategy Build realistic Mock Catalogues of the DES + VISTA survey Derive spectrograph/fibers sensitivities for ground-based observation Investigate redshift distribution and galaxy density for DESpec science Which tragetting strategy ? What criterion in photoz or color-color space ?

3. 3 Galaxy Properties from Deep Surveys the VVDS “Deep” survey VIMOS/VLT deep spectroscopic survey on ~0.5 sq.deg ~9000 spectra from 0<z<5 down to I AB ~24 (magnitude selected)‏ the COSMOS survey 2deg 2 (representative)‏ 30 photometric bands from UV to IR with HST, Galex, Spitzer, Subaru, VLA, NOAO HST/ACS I band observation: galaxy sizes & shapes zCosmos spectroscopic survey Le fèvre et al. 2005 Koekemoer et al. 2007

4. 4 Building Mock Catalogues GOODS Luminosity Function catalogue COSMOS Mock catalogue COSMOS catalogue (position, size, photometry)‏ 1 million galaxies Photoz, SED, emission lines Photometry in DE mission filter sets + Photometric errors DE Forecast Simulated Catalogue based on GOODS LF(z,type)‏ COSMOS size distribution, emission lines Jouvel et al. 2009 Jouvel et al 2010 GOODS LF from Dahlen et al. 2005 COSMOS photoz from Ilbert et al. 2009 Stephanie Jouvel - Realistic redshift distribution, - Realistic size distribution, - Emission line fluxes catalogue Use this catalogue

5. 5 COSMOS Mock Catalog (CMC)‏ Construction using the properties of the COSMOS-ACS WL catalog using : - realistic photometric redshift distribution 30 photometric bands calibrated with spectroscopic redshift : > zCOSMOS bright (I~22 AB) > zCOSMOS faint (I~25 AB) > MIPS-spectro-z sample - best-fit template from this photoz distribution - galaxy size measured by Sextractor from Leauthaud et al 2007 Validation of the CMC using : - GOODS N&S visible - UDF visible + jh band - VVDS Ks band + spectro-z - GOODS-MUSIC Ks band

6. 6 COSMOS Mock Catalogue(CMC) Stephanie Jouvel We want precision cosmology  Need for realistic mock catalogues to test photoz codes : - Realistic redshift distribution  Impacts DE FoM from WL - Realistic distribution of galaxy sizes in redshift and magnitude => Realistic noise distribution impact photoz results -Emission line catalogue  Create spectroscopic catalogue to study photoz calibration

7. 7 COSMOS Mock Catalog (CMC)‏ : Validation Emission line prediction : Kennicutt et al. 1998 : UV-OII relation Validation of the redshift distribution and emission line fluxes using the VVDS-DEEP I~24 AB (Lamareille et al 2008)‏ Jouvel et al. 2009

8. 8 Spectroscopic Success Rate (SSR) : Validation using VVDS Validation : reproducing the VVDS SSR SSR : galaxy rate for which we will be able to measure a redshift Jouvel et al. 2009

9. 9 PhotoZ Calibration Survey (PZCS): Spectroscopic Success Rate (SSR)‏ WIDE NIR photometric calibration (BAO–RD survey)‏ template calibration: - DEEP-visible-NIR - DEEP-NIR Jouvel et al. 2009 In the context of the JDEM survey we simulated different spectroscopic surveys :

10. 10 SSR Forecast for PZCS Forecast : -DEEP-NIR space survey (PZCS)‏ DEEP-NIR : I~27 0.5<z<3.5 35gal/arcmin2 Jouvel et al. 2009

11. 11 DEEP-vis-NIR : I~27 0<z<3.5 60gal/arcmin2 SSR forecast for PZCS Forecast : DEEP-visible-NIR space survey (PZCS)‏ Jouvel et al. 2009

12. 12 WIDE-NIR : H ~22 0.5<z<1.5 5gal/arcmin2 SSR Forecast for PZCS Forecast : WIDE-NIR space survey (BAO like)‏ Jouvel et al. 2009

13. DESpec survey strategy : 1. Mock catalogue and photoz

14. DES+VISTA photometric redshift ANNz training with 10000 galaxies Le Phare with COSMOS templates

15. DESpec survey strategy : 2. Target selection

16. Line sensitivities from Huan Lin - Sensitivities for 30 mins exposure time on 2 arcsec ø fibers (70% light fraction) - Resolution R=2500 at 0.9um. - Calculation include DES throughput + sky noise and atmospheric lines from Hanuschik (2003)

17. Redshift distribution from em lines Redshift distribution of emission line galaxies selected with : - I (DES) < 23 - 1 < photoz < 2 - at least one em line detected at 5 sigma Photoz with Le Phare (template fitting method) u DES+VISTA Can we select the emission line galaxies based on DES+VISTA photometry only ? Total of roughly 12000 gal/deg2

18. Multidimensional method based on NN selection

19. Use of NN to select em line galaxies We assign a value of : - 1 for targetted em line galaxies - 0 for non targetted galaxies We then use ANNz and train a NN on a sample of 10000 galaxies from the CMC (DES+VISTA) Results for i(DES) < 24

20. Which ANNz selection criterion ? Fig : Cumulated nbr galaxies/deg2 fct ANNz target probability We suggest a selection criterion of 0.8 yielding to : -7500 emission line galaxies / deg2 i(DES)<24 - and a contamination of 800 gal/deg2 i(DES)<24 0.8

21. Which ANNz selection criterion ? Solid : percentage of galaxies for which we will measure a redshift/total nbr gal & Dashed : SSR fct ANNz target probability We suggest a selection criterion of 0.8 yielding to : -7500 emission line galaxies / deg2 i(DES)<24 - and a contamination of 800 gal/deg2 i(DES)<24

22. Redshift distribution of ANNz sel 0.8

23. Redshift distribution / em lines gal

26. Line sensitivities from Huan Lin 0.6-1um - Sensitivities for 30 mins exposure time on 2 arcsec ø fibers (70% light fraction) - Resolution R=2500 at 0.9um. - Calculation include DES throughput + sky noise and atmospheric lines from Hanuschik (2003)

27. Use of NN to select em line galaxies We assign a value of : - 1 for targetted em line galaxies - 0 for non targetted galaxies We then use ANNz and train a NN on a sample of 10000 galaxies from the CMC (DES+VISTA) Results for i(DES) < 24 Using Huan Lin sensitivities cut between 0.6-1um

28. Which ANNz selection criterion ? Fig : Cumulated nbr galaxies/deg2 fct ANNz target probability We suggest a selection criterion of 0.8 yielding to : -7500 emission line galaxies / deg2 i(DES)<24 - and a contamination of 800 gal/deg2 i(DES)<24 0.8 Using Huan Lin sensitivities cut between 0.6-1um

29. Which ANNz selection criterion ? Solid : percentage of galaxies for which we will measure a redshift/total nbr gal & Dashed : SSR fct ANNz target probability We suggest a selection criterion of 0.8 yielding to : -7500 emission line galaxies / deg2 i(DES)<24 - and a contamination of 800 gal/deg2 i(DES)<24 Using Huan Lin sensitivities cut between 0.6-1um

30. Redshift distribution of ANNz sel 0.8 Using Huan Lin sensitivities cut between 0.6-1um

31. Photoz for the NN target galaxies

32. Can we do color-color cut ? g-r vs r-i r-i vs i-z It looks difficult to select the OII line in a coloc-color cut. We need a higher dimensional kind of cut such as photoz codes can provide

33. Conclusion We simulated a DES+VISTA catalogue using the CMC which include emission line fluxes. Huan Lin derived a fiber sensitivities including all instruments troughput and sky noise including astmospheric lines for a DESpec instrument. Using Huan Lin sensitivities we can select emission line galaxies from DES+VISTA photometry using ANNz. We suggest a selection criterion of 0.8 with a yield of 8000gal/deg2 for i(DES)<24 and a success rate of 93% or 5000gal/deg2 i(DES)<23 and a success rate of 95% (to verify). A color-color cut does not seem the optimal solution to select target for DESpec.

34. 34 COSMOS Mock Catalog (CMC): Validation Jouvel et al. 2009

35. 35 COSMOS Mock Catalogue(CMC) Stephanie Jouvel We want precision cosmology  Need for realistic mock catalogues to test photoz codes : - Realistic redshift distribution  Impacts DE FoM from WL - Realistic distribution of galaxy sizes in redshift and magnitude => Realistic noise distribution impact photoz results -Emission line catalogue  Create spectroscopic catalogue to study photoz calibration

36. Emission lines z = 0 H-a6563 A Ly-a1215 A OII3726-3729 A doublet H-b4861 A OIII4959A and 5007A z~2.5 : Ly-a 4250 OII 13000 z~3.5 : Ly-a 5460

37. Results from CMC : Photoz calibration 37 work with Gary Bernstein as part of the SNAP-WL group -Simulation of spectroscopic survey using forecast survey sensitivities for : optical/+NIR surveys, SHALLOW or DEEP. => No photoz calibration possible for z 1.6 galaxies. => Need of visible + NIR spectroscopy to cover the whole redshift range of future photometric surveys. Jouvel et al. 2009 Stephanie Jouvel

38. u* +0.019 g’ -0.079 r’ -0.002 i’ 0 Z’ -0.008 Photoz : Need for spectroscopic calibration Successful method to remove systematic trends Importance of the zero-point calibration Further improvement of the templates Ilbert et al.2006