Discovery of massive galaxies at high redshifts

Transcription

1 Discovery of massive gaaxies at high redshifts A ink with back hoe growth? A puzzing question for numerica simuations? B. Rocca-Vomerange Institut d Astrophysique de Paris Université Paris-Sud rocca@iap.fr Coaborations Guiaume Drouart (PhD student*), Caros De Breuck (ESO), Joe Vernet (ESO), Miche Fioc and the HzRG consortium Warm Dark matter Cooque Chaonge 2013

2 Outine I. The cosmoogica frame Gaaxy formation modes II. Principes of gaaxy evoution modes Modeing High-z gaaxies with the code PEGASE.3 Gaaxy counts and individua types III. The Hubbe diagram K-z IV. Od gaaxies and merging in two exampes of extreme (z=4) radio gaaxies 4C TN J , Rocca-Vomerange et a. 2013, MNRAS V Impications on theories Warm -- Dark Concusions matter Cooque Chaonge 2013

3 Recent striking observationa discoveries Modes are required to fit a data and to disentange cosmoogy and evoution Warm Dark matter Cooque Chaonge 2013

4 New concept: The tempate starburst M82 But the prototype of starburst Embedded in an eiptica gaaxy Reveaed by the IR Sateite IRAS As ULIRG (Utra Luminous Infra red Gaaxies) from dust emission Winds are supposed from expoding Supernovae LERMA, 27Janvier2013

5 Main Observations : ULIRGs : Starburst and AGN seem not evoved gaaxies LERMA, 27Janvier2013

6 Discovery of massive(10**9mθ) back hoes at z>4 Redshift distribution of the back hoe masses Of the QSOs sampe from SDSS DR3 Vestergaard eta. 2008, ApJ, 674, L1 Reation with the Gaaxy properties Merritt et a, 2006, Margorrian et a, 2004 LERMA, 27Janvier2013

7 Deeper and deeper muti- surveys (X, UV, optica,nir, FIR, radio ) An exampe In the optica: Hubbe Deep Fied-N Counts N(m), N(z), N(coor) by bin of z

8 And the convergence to spendid numerica simuations

9 Hierarchica merging or not? Cosmic time Mso T=14Gyr, z=0 z= Mso T=0, z>1000

10 Among the most recent simuations: The incorporation of the back hoe growth During gaaxy mergers into the semi-anaytic mode Based onλcdm by Baugh et a. An exampe of Hierarchica merging with back hoe growth (Durham group, Mabon et a, 2007, MNRAS)

11 Or based on the Jeans mass in an expanding universe The Jeans mass is the stabiity imit: when a density perturbation wi grow once it becomes instabe. The reativistic effects can be important. The expansion is considered as adiabatic, as ong as no energy sources is present ) ( 3 4 ) 2 ( 3 4 = = c P G n m n m M H J H J s v n: tota baryon number densi : mass density v s : adiabatic sound speed G: gravitation constant P/c 2 = radiation pressure (reativistic)

12 T THE JEANS MASS EVOLVES WITH COSMIC TIME Versus Temperature K M J 10 6 Versus Cosmic time t cosmic Before recombination M J After the recombination M 9.10 **15 Ms **6 Ms

13 And Evoution of sef-gravitating gas coud with dissipation Rees & Ostriker, time-scaes are in competition the free_fa time scae (dynamics) the cooing time scae (radiation) fonction L(T G ) is the cooing function depending on atomic properties 1 t ff = G cooing ( T 2 régimes are possibe. They depend on the cooing function t ff > tcooing coud fragmentation t ff < tcooing quasi-static evoution of the coud t 1 = L G

14 FRAGMENTATION

15 Temperature T K veocity t coo <t ff Sequenc t coo =t ff t coo >t ff Density

16 Cosmoogy pattern z Cosmic time 1.2Gyr Gyr Warm Dark matter Cooque Chaonge Gyr Gyr Gyr

17 Redshift z CosmicTime Redshift z CosmicTime Redshift z CosmicTim z=0 t=t 0 k+e corrections Looking-forward time zobs t obs Gaaxy age z formation t for BB Reation Redshift z- temps cosmique t(z) in Gyr Ho=72km.s-1Mpc-1, Ω L = 0.7, Ω M =0.3 1 z H t( z) LERMA, 27Janvier = 0 (1-2q 0 2 q x 0 ) dx

18 Modes of evoutionary SEDs 11. Instantaneous starburst: SSP Singe Stear Popuation (with the adopted IMF) Sum of SSPs = Gaaxy types (E, Sp, Im) Chemica evoution Z ( Graphite, siicates) Dust Evoution of Stear popuations, stear mass Gaaxy spectrum = SUM of stear spectra Gas content, ionized gas, etc Gaaxy Evoution -Doctora ectures March 2011

19 PEGASE.3 mode of Gaaxy evoution Accretion + outfows (winds) Gaaxy incuding HII regions Winds www2.iap.fr/pegas M baryon : (reservoir) Scenarios by type: Four Parameters Star Formation aw SFR(t) Infow time-scae Extragaactic winds IMF Gas Infow + RADIATIVE TRANSFER Dust absortion and emission LERMA, 27Janvier2013 M gaaxy

20 INFALL,WINDS=f(t) Initia GAS RESERVOIR Star Formation Law IMF, Zinit EEEEEv Evoutionary Tracks age Stear evoution Compete spectra ibrary SYNTHETIC SPECTRAL ENERGY DISTRIBUTION AND COLORS = Death of stars SN, PN, gas enrichment Metaicity Z=f (age) LERMA, 27Janvier2013 Dust mass =f (age) Nuceosynthesis yieds Residua gas= f (age) Mass of Stars, = f (age)

21 I. STELLAR EVOLUTIONARY TRACKS:1<M/M <25 L= F( Teff, age) Many Groups from Padova Genova Yaes Isomass Isochrones Log T eff LERMA, 27Janvier2013

22 A variety of scenarios fitting z=0 tempates by type in the coor-coor diagram Compared to the statistica SDSS survey (SLOAN) Tsamantsa et a, 2007, 2009 (Consortium GAIA) E Spira Irr Quenched Compact dwarfs? PEGASE.2 SCENARIOS by types ARE ALSO ROBUST IN THE UV/OPTICAL/NIR 1. Phot- z / spectro z ( Le Borgne, Rocca-Vomerange, Fioc, 2002) (code Z-PEG on LERMA, 27Janvier <z<2 Muti-λ faint gaaxy counts (Fioc & Rocca-Vomerange, 1999)

23 A puzze for Dark Matter modes : Eiptica gaaxy Spira Gaaxy SFR ELLIPTICAL time-scae of star formation <1Gyr SPIRAL time scae of star formation > 10Gyrs Possibe succession of mergers (ampitude, number, etc) Accretion/infa during a few 100 Myr Extra gaactic winds at 1 to 3 Gyr Star Formation time scae short ~1Gyr for E and ong for Spiras

24 + New constraint with Dust (farir) The new version PEGASE.3 Passive and active stear emission + nebua emission (HII regions) + chemica enrichment dust emission Dust mass (t, type) fitted on Metaicity enrichment (by types in particuar C and SI, from SN and evoved supergiants/agb Grain modes (Draine ) scattering/absorbing by Draine s grain popuation, Heated from Lyman cont. photons (N_Lyc) Star Formation RATE Factor for dense media): 2 media: diffuse ISM and HII regions (Zubko et a, 2004) Radiative transfer (adapted from Varosi &Dwek, 1999) 2 Geometries (disk/sab, spheroid)

25 Extinction Modeing Extinction A (z) (magnitude) depends on time foowing dust mass, metas and gas content. Optica depth = n10 2,5 A ( z) ( z) n10 A =. 2,5 A V ( z). E A V B-V ( z). E B-V N H ( z). N H Possibiity to increase the gas density StearPop._IAP_June2012 NHI = K. NHI(ISM) with K=1 to 10

26 Atas of synthetic gaaxies(optica-fir) LERMA, 27Janvier2013 Fioc, Rocca-Vomerange, Dwek, in preparation

27 To mode High-z gaaxies in the observer frame (avoiding anaysis in the rest-frame) 1. Buiding ibraries of tempates by types 2. defining types as z=0 oca tempates 3. Predicting tempates at z from: oca tempates + cosmoogy+ evoution

28 LERMA, 27Janvier2013 k- (expansion) corrections ) (0, ), ( ) ( 0 0 t M t z M z k i i i - = Computed with F i λ=synthetic fux from ibrary modes through the pass-band of the fiter λ e-(evoution) corrections ), ( ), ( ) ( 0 t z M t z M z e i z i i - = Rocca-Vomerange & Guiderdoni, 1988, AA A M m z e z k t z M t z m bo obs - = = ) ( ) ( ) ( ) 0, ( ), ( 0 Apparent magnitudes at z, t obs

29 k- (expansion) corrections - - = - ' ) ', ( ) (1 ' ) ), /(1 ( 2.5og ' 0 ' 0 ' d R t t F z d R t t z F k zfor i zfor i i F i λ=apparent fux from synthetic ibrairies R λ =pass-band of the fiter λ e-(evoution) corrections - - = - ' ) ), /(1 ' ( ' ) ), /(1 ' ( 2.5og ) ( ' 0 ' d R t t z F d R t t z F z e zfor i zfor z i i Rocca-Vomerange & Guiderdoni, 1988, AA

30 To mode high-z eiptica: the best targets are distant radio gaaxies : Loca massive eipticas are faint in the far Infrared They are dominated by the 1mu peak Xiouris et a, 2003 Loca E Xiouris et a., 2003,Temi et a, 2004 Not strong sources detected by the IR sateites (IRAS, ISO, Spitzer) Raeigh-Jeans distribution of the LERMA, K-M 27Janvier2013 stear popuation Minor 50K and 20K

31 Moreover high-z radio gaaxies (hosted by eipticas) revea activity of star formation Powerfu, utra distant 1<z<7, STELLAR, nebuar and AGN emissions But compex LERMA, 27Janvier2013

32 Extension of the Hα cocoon Of the FR-II radio gaaxy 3C171 (z=0.286) (Ø=140kpc*) Sharp Emission a cocoon boundarie Narrow couping With Radio LERMA, 27Janvier2013

33 The tempate distant radio gaaxy 4C41.17 (z=3.8) Huge Lyα Couds of kpc of ionized gas (cocoon) (Dey et a, 1997, Van Breuge et a, 1999, Reuand et a, 2003). HIGH-z RADIO GALAXIES are hosted by MASSIVE ELLIPTICALS (van Breuge et a, 1998, Penterricci et a, 2001) Stear ines are detected aong the radio axis (Dey et a, 1997), as WR starbursts Star formation aong the radio jet and south-east component, Bickne et a, 2000

34 LERMA, 27Janvier2013

35 The striking resut of the interpretation of the Hubbe K-z Diagram with the code PEGASE : eipticas are od, massive and red from z=4 and more powerfu radio gaaxies are the most massive gaaxies the sharp imit are Eipticas of Baryonic Mass 10** 12 MΘ M im = 10**12 M Θ from K mag Mim = M crit of fragmentation derived from Jeans mass and Cooing Function Rees & Ostriker, 1977, (Rocca-Vomerange, Le Borgne, De Breuck, Fioc, Moy, 2004, AA, 415, 931) Redshift z HUBBLE K-z diagram fitted by PEGASE

36 d 2 A j Modéisation des comptages ( m, z) = ( M ( z))(1 j j z) 3 dv dz dm Gaaxy Number density by apparent magnitude m and z bin of type j dz dv z k+e ( M j ( z)) j z=0 uminosity function by type j for fiter λ D dz m j ( z) = M j ( z = 0, t0 ) k j ( z) e j ( z) ( m - M ) k- and e- corrections are computed from synthetic spectra for a scenarii and a z Gaaxy Evoution -II Counts 2012 Doctora ectures

37 Muti-ambda modeing faint gaaxy counts: UV OPTICAL--NIR with evoution scenarios by types Fioc and Rocca-Vomerange, 1999, AA,344,393 b J BLUE U and 3000A UV 29 I K Gaaxy popuation fractions : ELLIPTICAL (26%) :Sa+Sb+Sbc (24%) Sc+Sd+Im (50%)

38 Confirmed by 9% of IR Utrauminous Eipticas THE ATYPICAL MID-IR EXCESS (RG and/or AGNs?) to expain the typica IR bump,a other gaaxies are norma Hubbe Sequence gaaxies Mode: Rocca-Vomerange, de Lapparent, Seymour, 2007 Seymour, Number Fioc, Type 2007, AA, Magnitude 475, 801 M* Fraction 9% utra-bright eipticas Norma % norma mode coor eipticas IRAS LF 24% Eary // Spiras 50% Late // Spiras IRAS LF Fu ine: k+e corrections, dashed LERMA, ine: 27Janvier2013 k- corrections, dot ine: comoving v

39 The gaaxy popuation IR excess and 24 um discovered in the ISO and Spitzer faint counts is due to 9% of IR Utra-Luminous massive 12 µm 24 µm (Rocca-Vomerange, Seymour, de Lapparent, 2007, AA) Fu ine: expansion + k + e corrections, dashed ine: expansion + k- corrections, LERMA, 27Janvier2013 Dotted ine: expansion Standard Cosmoogy (Ω M =0.3, Ω =0.7)

40 Buiding Continuous SEDs N. Seymour, C. De Breuck, D. Stern, B. Rocca-Vomerange co-authors, 2010, 2012) Optica + NIR (UV rest-frame) MIR Spitzer (IRAC, MIPS, IRS) De Breuck et a, 2010 Hersche (PACS and SPIRE) Wyezaek et a 2013, Drouart et a, 2013 Submm and radio Aperture corrections Fux-Caibrations Coors through Fiter pass-bands LERMA, 27Janvier2013

41 Two seected Radiogaaxies 4C41.17 and TN J (z=3.8) Faint AGN contribution Evidences of stear popuations Continuous fux-caibrated SEDs from Optica (UV rest-frame) Spitzer (K-band rest-frame) Hersche and submm (cod grain peak rest-frame) negigeabe synchrotron emission LERMA, 27Janvier2013

42 Synthetic synthesis method -LIBRARIES OF STARBURSTS at a ages, various IMF, -LIBRARIES OF ELLIPTICALS, SPIRALS and IRREGULARS - A c2 minimization method on the goba coverage of the SEDs - A seection of 2 radio gaaxies at the same z=3.8 - Faint radio power - Evidence of star formation - Observations Hersche + Spitzer + K and optica - Caibration and aperture checked OUTPUTs: c2 minimum, types, ages and masses of the 2 components LERMA, 27Janvier2013

43 z=3.8 One starburst component 25Myr + AGN Hersche+Submm optica LERMA, 27Janvier2013

44 4C41.17 : One eary type component Sa age 1.6Gyr + AGN Spitzer Hersche/submm optica LERMA, 27Janvier2013 Rocca-Vomerange et a, 2013

45 1st concusion ONE COMPONENT is not sufficient to fit z=4 SEDs Any eary type popuation does not fit the far-ir/submm Any starburst, even evoved, does not fit the mid-ir LERMA, 27Janvier2013

46 4C41.17: A sum of Two Stear Popuation components Starburst at age 30Myrs + Eiptica at age 700Myrs +AGN (600K) Exceent c2=0.96, huge masses 10 ^11 M0, ow Z Observations Are red points With error bars AGN mode : (dashed green) Pier& Kroik mode One od 0.7 Gyrs One young stear component of 30Myrs LERMA, 27Janvier2013 Rocca-Vomerange et a, 2013, MNRAS

47 TN J (z=3.8) Two stear components: + SO/Eiptica at age 1200Myrs Starburst at age 35Myrs AGN mode Pier & Kroik (dashed green) Od Eiptica At 1.2 Gyr (red ine) Pus A starburst At 35 Myrs (dark bue) Green arrows : Superior imits LERMA, 27Janvier2013 Rocca-Vomerange et a, 2013

48 2d concusion A young popuation, evoved (age 30Myr) issued from the evoution of a very short (1Myr) Starburst In a dense medium 10^22-23 part/cm2 ( x10 NHI ISM) fitting simutaneousy the 2 peaks : the optica (UV rest-frame) from the stear photospheric (no absorbed) emission the far-ir/submm emission derived from absorption The starburst is from a neary primitive (or ow Z) metaicity The goba initia mass is roughy a few 10^11 M0, Better spatia resoution is needed. But this resut is robust: To increase absorption (or optica LERMA, depth) 27Janvier2013 wi increase the farir by decreasing UV em To decrease absorption has the opposite effect

49 3rd concusion An REVEALED eary-type popuation Formed at redshift z=10 is discovered in Spitzer data The SED is quite compatibe with the typica 1mum peak (rest-frame) of eary type gaaxies. A striking confirmation of the K-z od popuation (RV et a, 2004) 10^12 M0 stear masses the red passive sequence of giant stars Metaicity Z is O.OO5, compatibe with eary-type scenarios. Masses are derived from fitting LERMA, the 27Janvier2013 sum to the fux caibrated SED ~ 10 ^11-12 M0

50 4th concusion Because The 2 radio gaaxies are seected for their ow AGN activity, AGN mode is not constraining. The AGN peak domain is not we covered by observations For these two targets: AGN modes are therma (BB 600K), Or mode c of Pier & Kroic, 1992). LERMA, 27Janvier2013

51 AN od popuatio n at z=3.8 + a merging episode undergoing an episode of vigorous star formation These powerfu radio-oad gaaxies are ikey a sub popuation of radio-quiet gaaxies (Kriek et a, 2006, Stockton et a, 2008) LERMA, 27Janvier2013

52 Star formation by Merging or jet_coud interaction Issued from jet-coud interaction (Bickne t eet a, 2000) et a 2000) The formed stear mass Is too huge to form in a so narrow zone The most ikey process is a gas-rich merging of mass ratio ~1 to 1/10, triggering an extremey short starburst in a dense medium The intense star formation rate is >10^4 M0/yr during 1 Myr LERMA, 27Janvier2013 So short time scae woud correspond to the short time

53 Consequences on cosmic SF history (1) The star formation history is dominated by eipticas at eary epochs (z=10 or more). SF History (2) Rapid increase of SF for spiras 0<z<1, comparabe To CFRS resuts (Le Fevre et a, 1998): CFRS is seected on Sa spiras. (3) Dwarfs contribute to SFH at ow z Empty circes are data from CFRS, Deep survey seected on Spira Sa gaaxies These sources are not ULIRGs induced by gaaxies in LERMA, 27Janvier2013 interaction. A are compatbe with deep UV-optica-NIR counts z

54 Concusions Evoutionary synthesis: in the observer s frame: (cosmoogy + active and passive evoution) Loca tempates + distance + k+ e corrections Hubbe Sequence types + Starburst Evoutions Radio gaaxies are the most distant and massive gaaxies Confirmation of massive eary type gaaxy hosts In the K-z diagram ( Rocca-Vomerange et a, 2004) And the fragmentation imit 10^12 M0 LERMA, 27Janvier2013

55 Concusions (foowing) Two star formation time-scaes: Instantaneous ~1-Myr merging reveaed by dust from SN and AGB stars Cumuative ~1 Gyr possibe sum of hierarchica merging, the enveop is a mode. Star formation initiates at zfor> 4-10 or more, zfor < 4 is unikey for the most massive RG Evidences of star formation stear masses with back hoe growth is confirmed LERMA, 27Janvier2013

56 Near Future Evoutionary synthesis with the HERGE sampe G. Drouart s thesis Reation AGN-Starburst (ocaisation, intensity, respective time-scaes) Pegase. 3 avaiabe to the community (README on www2.iap.fr) Artice (Fioc, RV, Dwek, in preparation)