Guzzo+13, Garilli+14

Guzzo+13, Garilli+14

Alexander FritzAlexander FritzINAF-IASF MilanoINAF-IASF Milano

M. Scodeggio, O. Ilbert,M. Scodeggio, O. Ilbert,and the and the VIPERS TeamVIPERS Team

The Formation and Build-up of The Formation and Build-up of the Red-Sequence Since z=1.3 in the Red-Sequence Since z=1.3 in

VIPERSVIPERS

Dubrovnik, CroatiaDubrovnik, Croatia May 15May 15thth, 2014, 2014

CMR and RS Evolution of E/S0sCMR and RS Evolution of E/S0sCMR and RS Evolution of E/S0sCMR and RS Evolution of E/S0s

e.g. Fontana+04, Bell+04, Weiner+05, Cassata+07,

Faber+07, Franzetti+07, Ruhland+09, Whitaker+10

Intermediate 0 < z < 2e.g. Strateva+01, Hogg+02, Bell+03,

Baldry+04, Peng+10,+13, Schawinski+14

Local z < 0.1

Peng+10 E

arl

yEarl

y

RS

RS

Lat

Lat

e

e

BC

BC

Cattaneo+09

Faber+07

A. Fritz (INAF-IASF Milano) May 15th, 2014, Dubrovnik, Croatia

RS Evolution at 0 < z < 2RS Evolution at 0 < z < 2RS Evolution at 0 < z < 2RS 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

441 VLT hours, ~24 deg441 VLT hours, ~24 deg2 2 in W1 and W4in W1 and W4

IIABAB<22.5, LR Red, T=45’, z>0.5 <22.5, LR Red, T=45’, z>0.5 grigri selection selection

~100,000 redshifts~100,000 redshifts, , >40% sampling>40% samplingGuzzo+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

z = 0.73NTOT=44982NW1 =23210NW4 =21770

Bolzonella et al. 2000


CMR of VIPERSCMR of VIPERSCMR of VIPERSCMR of VIPERS

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

Galaxy Types:

E/S0

Sa/Sb

Sc/Sd

SB/Irr


Selection Criteria of E+S0sSelection Criteria of E+S0sSelection Criteria of E+S0sSelection 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


Selection Criteria of E+S0sSelection Criteria of E+S0sSelection Criteria of E+S0sSelection Criteria of E+S0s

Methods:

• Colour-bimodality(optical)

• SED types (UV+optical+N/MIR)

• NUVr’ selection(Arnouts et al. 2013)

Passive vs. Active:(NUV-r’)=1.25-(r’-K)

Efficiently de-select face-on dusty galaxiesFritz+14


RS EvolutionRS EvolutionRS EvolutionRS Evolution

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 0.14m

0<z<1.3 = 0.44 0.18m

Comparison with Literature

Different Selection Criteria


SP Constraints on RS EvolutionSP Constraints on RS EvolutionSP Constraints on RS EvolutionSP Constraints on RS Evolution

dotted: zt=2.5

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


RS and Number Density EvolutionRS and Number Density EvolutionRS and Number Density EvolutionRS and Number Density Evolution

Passive

Quenched SF


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

RS and Number Density EvolutionRS and Number Density EvolutionRS and Number Density EvolutionRS and Number Density Evolution

dotted: zt=2.5

dashed: zt=3

• ALL: weak evolution z<0.8, ALL: weak evolution z<0.8, faster for z>0.8faster for z>0.8

• REDRED: weak evolution z<0.7: weak evolution z<0.7drop at z>0.7 by ~0.4 dexdrop at z>0.7 by ~0.4 dex

SF quenching at z=1.5

Passive

Quenched SF



Colour-Mass RelationColour-Mass RelationColour-Mass RelationColour-Mass Relation

RS

BC

• 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

0.5 < z < 0.7

0.7 < z < 0.9

0.9 < z < 1.3


Colour-Mass RelationColour-Mass RelationColour-Mass RelationColour-Mass Relation

RS

BC

• 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

0.5 < z < 0.7

0.7 < z < 0.9

0.9 < z < 1.3

RS FormationRS FormationRS FormationRS Formation

z~1.3z~0

High-Mno merger

Low-M merger

Fritz et al. 2014, A&A, 563 Fritz et al. 2014, A&A, 563 A92A92

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

NA

SA

/ E

SA

/ S

. Toft


SummarySummarySummarySummary

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

Fritz et al. 2014, A&A, 563 Fritz et al. 2014, A&A, 563 A92A92

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


Hvala!Hvala!

http://vipers.inaf.it

Environmental QuenchingEnvironmental QuenchingEnvironmental QuenchingEnvironmental Quenching

Fritz et al. 2014

Cosmic varianceCosmic varianceCosmic varianceCosmic variance

CompletenessCompletenessCompletenessCompleteness

VIPERS PDR-1VIPERS PDR-1VIPERS PDR-1VIPERS PDR-1

Guzzo+13, Garilli+14

VIPERS in a VIPERS in a NutshellNutshell 0.5 < z < 1.30.5 < z < 1.3

grigri selection z>0.5 selection z>0.5

PDR-1 (Sep PDR-1 (Sep 2013):2013):Guzzo+13, Guzzo+13, Garilli+14Garilli+14

Aera: 10.32 degAera: 10.32 deg22

Science ResultsScience Results::Bel+13, Bel+13, Davidzon+13, Davidzon+13, de la Torre+13, de la Torre+13, Fritz+14, Fritz+14, Malek+13, Malek+13, Marulli+13, Marulli+13, Cucciati+14 Cucciati+14

New benchmark New benchmark atatz=0.8 with N=10z=0.8 with N=1055

Garilli+14

LF of VIPERSLF of VIPERSLF of VIPERSLF 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

RED dominate

RED dominate

Massive

…... Local


LF ComparisonLF ComparisonLF ComparisonLF Comparison

All RED

- 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)

Statistical WeightsStatistical WeightsStatistical WeightsStatistical Weights

CSR: z=0.6: Red/Blue ~94%/97%

z=0.5: Red/Blue ~82% z=0.45: Red/Blue ~70%

Spectral Properties of RS GalaxiesSpectral Properties of RS GalaxiesSpectral Properties of RS GalaxiesSpectral 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

Completeness and Contamination Completeness and Contamination Completeness and Contamination 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

Documents

Guzzo+13, Garilli+14