1 / 26

Guzzo+13, Garilli+14

The Formation and Build-up of the Red-Sequence Since z=1.3 in VIPERS. Guzzo+13, Garilli+14. Alexander Fritz INAF-IASF Milano M. Scodeggio, O. Ilbert, and the VIPERS Team. Dubrovnik, Croatia May 15 th , 2014. CMR and RS Evolution of E/S0s. Local z < 0.1. Intermediate 0 < z < 2 .

akio
Download Presentation

Guzzo+13, Garilli+14

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. The Formation and Build-up of the Red-Sequence Since z=1.3 in VIPERS Guzzo+13, Garilli+14 Alexander FritzINAF-IASF MilanoM. Scodeggio, O. Ilbert,and the VIPERS Team Dubrovnik, Croatia May 15th, 2014

  2. CMR and RS Evolution of E/S0s Local z < 0.1 Intermediate 0 < z < 2 e.g. Fontana+04, Bell+04, Weiner+05, Cassata+07, Faber+07, Franzetti+07, Ruhland+09, Whitaker+10 e.g. Strateva+01, Hogg+02, Bell+03, Baldry+04, Peng+10,+13, Schawinski+14 EarlyRS Late BC Peng+10 Faber+07 Cattaneo+09 A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  3. RS Evolution at 0 < z < 2 Literature • Large scatter(low numbers, different filters, various selections, cosmic variance, incompleteness, etc) • Coherent picture? Motivation • When/how did RS form? • High statistics • Different selection criteria • Benchmark for futuresurveys, e.g. Euclid A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  4. 441 VLT hours, ~24 deg2 in W1 and W4 • IAB<22.5, LR Red, T=45’, z>0.5 gri selection • ~100,000 redshifts, >40% sampling Guzzo+13, Garilli+14 Sample selection and Analysis • 0.4 < z < 1.3, CL zflg  95% • UVgrizYHJK+Spitzer k-cor small • Total uncertainties: 4-14%(ZP, extrapolation, different templates, etc) • Calzetti (UV bump at 2175Å )and Prevot extinction curves Bolzonella et al. 2000 z = 0.73 NTOT=44982 NW1 =23210 NW4 =21770 A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  5. CMR of VIPERS Galaxy Types: E/S0 Sa/Sb Sc/Sd SB/Irr 0.3<z<2 Massive red E/S0s in place at z~1 No evidence for slope variation (U-V)CL=1.34 - 0.30×z Fritz+14 A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  6. Selection Criteria of E+S0s Methods: • Colour-bimodality(optical) • SED types (UV+optical+N/MIR) • NUVr’ selection(Arnouts et al. 2013) Bimodality z ≤ 1.3 (U-V)CB=1.1-0.3×z Fritz+14 A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  7. Selection Criteria of E+S0s Methods: • Colour-bimodality(optical) • SED types (UV+optical+N/MIR) • NUVr’ selection(Arnouts et al. 2013) Passivevs.Active:(NUV-r’)=1.25-(r’-K) Efficiently de-select face-on dusty galaxies Fritz+14 A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  8. Classic = 0.28  0.14m Bimodality = 0.30  0.15m SED = 0.30  0.15m NUVr´ = 0.33  0.15m Strong evolution W1 and W4 similar 0.4<z<1.3 = 0.28  0.14m0<z<1.3 = 0.44  0.18m RS Evolution Comparison with Literature Different Selection Criteria A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  9. SP Constraints on RS Evolution Modelling the RS • PEGASE Fioc & Rocca-Folmerange 1997 • SF burst at 1.5 < zf < 5.00.1 <  < 3 Gyr • Good agreement betweenmodel and data • VIPERS: 0.5 <  < 0.8 • Rapid build-up of RSat z~1 within ~2 Gyr Quenching 1.7  zt  2.3 fading and reddening dashed: zt=3 dotted: zt=2.5 A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  10. RS and Number Density Evolution Modelling the RS • PEGASE Fioc & Rocca-Folmerange 1997 • SF burst at 1.5 < zf < 5.00.1 <  < 3 Gyr • Good agreement betweenmodel and data • VIPERS: 0.5 <  < 0.8 • Rapid build-up of RSat z~1 within ~2 Gyr Quenching 1.7  zt  2.3 fading and reddening Passive Quenched SF A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  11. RS and Number Density Evolution • ALL: weak evolution z<0.8, faster for z>0.8 • RED: weak evolution z<0.7drop at z>0.7 by ~0.4 dex SF quenching at z=1.5 dashed: zt=3 dotted: zt=2.5 Passive Quenched SF A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  12. RS BC Colour-Mass Relation 0.5 < z < 0.7 0.7 < z < 0.9 0.9 < z < 1.3 • Most luminous blue galaxies are massive • BC: Highest-mass edge evolves with time • RS: Highest-mass edge frozen since z=1.3Build-up of RS tilt z<0.7 A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  13. RS BC Colour-Mass Relation 0.5 < z < 0.7 0.7 < z < 0.9 0.9 < z < 1.3 • Most luminous blue galaxies are massive • BC: Highest-mass edge evolves with time • RS: Highest-mass edge frozen since z=1.3Build-up of RS tilt z<0.7 • Morphologies: undisturbed, no companionspossible Seyfert 2  AGN quenching A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  14. z~1.3 z~0 High-Mno merger Low-M merger RS Formation Fritz et al. 2014, A&A, 563 A92 The Build-up of the RS • SP Models: Rapid RS build-up ~2 Gyr  supported by SF in high-z galaxies • Evolution of CMR scatter 0.5 < z < 1:  decreases by 0.06 mag for MV -21 but constant for Mv  -21 • Quenching of SF at z~1, limited mergers • Independent support by SF at z~1 and MF (Davidzon+13) • Lower-mass E+S0s: minor wet mergers  transformation in groups  quenching  residual SF  limited dry mergers  build-up of low- and intermediate mass end of CMR NASA / ESA / S. Toft A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  15. Summary Fritz et al. 2014, A&A, 563 A92 CMR • Massive blue and red galaxies exist at 0.7<z<1 • Environmental dependence: scatter decreases for MV-21 Selection criteria of E/S0s • Classical RS definition restricted to most luminous galaxies • Similar results of different methods, minor role of dust at z<1.3 The Build-up of the RS • Rise in E+S0s number density since z~1 • Rapid RS build-up ~2 Gyr  SF Quenching at z~1, limited mergers, independent support by SF at z~1 and MF (Davidzon+13) • Massive E+S0s: Strong evolution • Lower-mass E+S0s: minor wet mergers  transformation in groups  build-up of low- and intermediate mass end of CMR A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  16. http://vipers.inaf.it Hvala!

  17. Environmental Quenching Fritz et al. 2014

  18. Cosmic variance

  19. Completeness

  20. VIPERS PDR-1 VIPERS in a Nutshell • 0.5 < z < 1.3 • gri selection z>0.5 • PDR-1 (Sep 2013):Guzzo+13, Garilli+14 • Aera: 10.32 deg2 • Science Results:Bel+13, Davidzon+13, de la Torre+13, Fritz+14, Malek+13, Marulli+13, Cucciati+14 • New benchmark atz=0.8 with N=105 Guzzo+13, Garilli+14 Garilli+14

  21. LF of VIPERS Key Results: • ALF (Ilbert+05) • High statistics • Large sample + volume:complete log(M*)>11 Mo • Red galaxies dominatebright part of LF z>0.8 • More massive galaxies at 0.8 < z < 1.2 …... Local RED dominate  RED dominate  Massive A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

  22. LF Comparison All RED

  23. Statistical Weights • TSR (i’AB) =Nspec / Nphot • SSR (i’AB, z) = (Ngal – Nfail) / Ngal • CSR (z) = NVL / NTOT • No dependence z-completeness with galaxy types (1.0<z<1.3~4%) • Used in LF + MF, different wrt clustering (de la Torre+13, Guzzo+13) CSR: z=0.6: Red/Blue ~94%/97% z=0.5: Red/Blue ~82% z=0.45: Red/Blue ~70%

  24. Spectral Properties of RS Galaxies - Stacked Spectra • -22.5  MB  -23.0 • Low-z: 0.5 < z < 0.6High-z: 0.9 < z < 1.0 • Large number (100<N<180) • Weak [OII] 3727 emission CB: SFR=2.2 Mo yr-1 SED: SFR=1.3 Mo yr-1 NUVr´: SFR=1.9 Mo yr-1

  25. Completeness and Contamination Completeness • Fraction of SED E/S0s classified as E/S0s inparticular method Contamination • Fraction of E/S0s in methodclassified as late-type inSED type classification CB: CP ~ 85%CO z<0.8: ~10%, z>1: ~30% CL:CP z>0.7: <70%CO ~10% • NUVr´: CP ~ 75-80% all z’s, CO~5-10% lower than CB

More Related