on the co- on the co- evolution of evolution of galaxies and their galaxies and their black holes black holes rac he l so me rville Max Planc k I nstitute fo r Astro no my, He ide lbe rg with thanks to E. Bell, X. Zheng, H.-W. Rix, & the GEMS team P. Hopkins, B. Robertson, T.J. Cox, L. Hernquist, Y. Li
mergers as drivers of galaxy and BH growth � trigge rs o f po we rful bursts o f star fo rmatio n? � re spo nsible fo r transfo rming disks into sphe ro ids? � drive rs o f gas into galac tic nuc le i, fe e ding the c e ntral BH, & pro duc ing an AGN?
questions � ho w signific ant are me rge rs in driving the c harac te ristic rise and fall o f the glo bal SF R and do wnsizing? � ho w signific ant are me rge rs in driving the c harac te ristic rise and fall o f BH ac c re tio n and do wnsizing? � are o bse rvatio ns o f me rge r rate s and QSO L F c o nsiste nt with the m be ing c lo se ly asso c iate d pro c e sse s?
COMBO-17 + GEMS + Spitzer � c o lo rs, pho to -z, ste llar masse s to z~1 fro m COMBO-17; HST imag ing fro m GE MS � Spitze r 24 � m data fro m the MI PS instrume nt te am (83 � Jy --> 3M � yr -1 at z~0.7) COMBO-17 and COMBO-17 and GEMS coverage GEMS coverage Spitzer image Spitzer image Rieke et al. 2004; data described in et al. 2004; data described in Papovich Papovich et al. 2004 et al. 2004 Rieke
Stellar mass function split by color Blue cloud Blue cloud Local MFs MFs Local Red sequence Red sequence Bundy et al. Bundy et al. Weak evolution Weak evolution 2006 2006 in MF of blue guys in MF of blue guys (~ disks) (~ disks) Strong evolution Strong evolution in red guys at in red guys at L<2L* at least L<2L* at least (~ spheroids) (~ spheroids) Borch et al. et al. Borch 2006 2006
global stellar mass evolution by color � ste llar mass de nsity in blue c lo ud ~c o nstant sinc e z~1 � ste llar mass de nsity in re d Red sequence Red sequence Chen et al. 03 Chen et al. 03 se que nc e has inc re ase d by a fac to r o f 2-3 sinc e z~1 Bundy et al. Bundy et al. Blue cloud Blue cloud 2006 2006 Borch et al. 2006 et al. 2006 Borch
which galaxies contribute to the UV luminosity density at z=0.7? 0.65<z<0.75 Wolf et al. 2005
contributions to global SFR budget by type at z=0.7 Wolf et al. 2004
the IR view at z=0.7: � Re d E / S0s are no n-star-fo rming � Mo st SF is in large spirals � 20-30% o f to tal SF at z=0.7 in manife stly inte rac ting syste ms Bell et al. 2005
U-V rest V
Most IR luminous galaxies in GEMS are relatively normal looking spirals LIRG, z = 0.33 ULIRG, z = 0.68 LIRG, z = 0.33 LIRG, z = 0.46 LIRG, z = 0.48 LIRG, z = 0.24
Evolution of IR LF Total Total IR LF very strongly IR LF very strongly Red Red evolving evolving Almost all SF is Almost all SF is in blue disks in blue disks Blue / disk Blue / disk Local Local Le Floc Floc’ ’h h et al. 2005 et al. 2005 Le Bell et al. 2005 Bell et al. 2005
SF and mass assembly split by color total � c o mpare inte grate d SF R with o bse rve d gro wth in ste llar blue mass � mo st star fo rmatio n is in blue s, but their mass de nsity do e s no t gro w! red � ne e d a pro c e ss that mo ve s galaxie s fro m blue Bell et al., in prep., Le Floc Floc’ ’h h et al. 2005 et al. 2005 Bell et al., in prep., Le to re d pile ...
mergers? � direc t measure o f merger frac tio n fro m c lo se pair frac tio n in COMBO � agrees fairly well Bell et al. 06 Bell et al. 06 with o ther results Patton et al. 2002 Patton et al. 2002 * * fro m mass- Bundy et al. 2004 Bundy et al. 2004 Le Le Fevre Fevre et al. 2000 et al. 2000 Conselice Conselice et al. 2003 et al. 2003 se le c te d samples; Somerville et al. in prep. Somerville et al. in prep. SAM Bell, Phelps, rss et al. 2006
Mergers? � implied ‘transfo rmatio n’ rate is highe r, and ste e pe r, than the ‘dire c t’ e stimate s o f me rge r rate Bell et al. 06 Bell et al. 06 � n.b. ke e p in mind me rge r rate s are Patton et al. 2002 Patton et al. 2002 * * Bundy et al. 2004 Bundy et al. 2004 Le Le Fevre Fevre et al. 2000 et al. 2000 hard to me asure by Conselice et al. 2003 Conselice et al. 2003 any means! Somerville et al. in prep. Somerville et al. in prep. Bell, Phelps, rss et al. 2006
co--evolution of global accretion rates diamonds = accretion rate based on hard X-ray LF x � BH (z=0)/ � *,sph (z=0) ~2000 Zheng, Bell, rss, Rix, Jahnke et al. in prep
co-evolution in mass and accretion rate accretion onto massive BH SFR in all assuming distribution of galaxies is L/L Edd from too much... Kollmeier et al. SFR in (all) massive galaxies is about right Zheng et al. in prep SFR in massive spheroids not enough
co-evolution by mass and accretion rate � take L F o f o ptic al QSOs. � c o nve rt L o bs to L bo l using standard bo lo me tric c o rre c tio ns. � L bo l --> ac c re tio n rate assuming e ffic ie nc y o f c o nve rsio n o f re st mass to e ne rg y o f 10% � c o nve rt L bo l to M BH using distributio n fro m K o llme ie r e t al. 2006 base d o n line widths (<L bo l / L dd >~0.25, � ~0.3 de x) E � plo t ac c re tio n rate c o ntribute d by BH abo ve a g ive n mass limit
open circles: black hole mass limit accretion filled: star formation mass & SF limit Zheng, Bell, rss, Rix, Jahnke et al. in prep.
AGN host morphologies in GEMS: -4/15 appear to be mergers -2/15 have exponential profiles (n<2.5) -majority have deV-like (n>2.5) profiles Sanchez et al. 2004
colors of star forming galaxies vs. AGN hosts AGN galaxies z=0.7 1.5 0 r o spirals l o c V - U Sanchez et al. 2004 mergers Bell et al. 2005 V-band magnitude
Hydrodynamic simulations of galaxy mergers including black hole growth and feedback -sub-grid model of SF in multi-phase ISM -Bondi accretion onto central BH -thermal energy from stars and AGN returned to ISM di Matteo, Springel & Hernquist Springel, di Matteo & Hernquist Robertson et al. Hopkins et al.
characteristic QSO lightcurves -QSO accretes at << L edd over most of its lifetime -’visibility time’ much longer at faint luminosities -obscuration is largest during peak of accretion -optical QSO becomes visible during ‘blowout’ phase Hopkins et al. 2005
parameterization of lightcurves differential time spent in a given logarithmic luminosity interval: dt/dlog(L) = t Q (L/L Q ) � exp[-L/L Q ] where L Q propto peak lum or final BH mass, � ~const Hopkins et al. 2005
mapping the observed merger LF and QSO LF � we c an use the se parame te rizatio ns o f starburst & QSO lightc urve s to c o mpute statistic al mappings be twe e n QSO lumino sity func tio ns, L F o r mass func tio n o f me rging galaxie s, galaxy-galaxy me rge r rate , ho st lumino sity, e tc . Hopkins, rss, Hernquist, Cox, Robertson & Li 2006
observations: hard X-ray QSO LF (Ueda et al. 2003) merger LF at z=0.2 from 2MASS (Xu et al.) & z=0.7 from GEMS z=0.2 z=0.7 merger LF from inferred (gas rich) QSO LF predicted from merger mass function observed QSO LF observed merger LF Hopkins, rss, Hernquist, Cox, Robertson & Li 2006
star formation rate function of mergers GEMS mergers predicted from QSO LF
mergers contribute ~1% to the global SFR at z=0, 15-25% at z~1, 30-50% at z~2 Hopkins, rss et al. 2006
primordial power spectrum merger tree, sub-halo merging photo-ionization squelching collisional heating radiative cooling BH formation, AGN feedback star formation SN feedback chemical enrichment stellar populations galaxy galaxy dust absorption & emission observables observables
the need for AGN feedback in cosmological models � o verc o o ling pro blem: to o large a frac tio n o f gas c o o ls into galaxies; huge exc ess o f ultra-massive/ lumino us blue galaxies at z~0 � inverted c o lo r-magnitude relatio n & mass-age relatio n; dearth o f massive red galaxies at high redshift � weak o r no c o lo r bimo dality � dec rease in number density o f lumino us QSOs; AGN ‘ do wnsizing’
AGN feedback mechanisms I � during pe rio ds o f e ffic ie nt fe e ding (asso c iate d w/ me rge r?) we pro duc e a lumino us AGN/ QSO � the rmal c o upling o f AGN e ne rgy with I SM is pro bably fairly we ak (5%?), and duty c yc le sho rt � BH gro wth se lf-re gulate d (pro duc e s M BH - � re latio n) � AGN c an drive a wind that ‘ swe e ps up’ galaxy Di Matteo, Springel & Hernquist 2005
AGN feedback mechanisms II � perio ds o f lo w ac c re tio n e ffic ie nc y (ADAF ?) asso c iate d with je t fo rmatio n � ene rgy c o uple s with QuickTime™ and a decompressor gas ve ry e ffic ie ntly are needed to see this picture. (~100%?) and duty c yc le is lo ng � resulting bubble s lo o k similar to tho se se e n in Chandra image s o f so me c luste rs Bruggen, Ruszkowski & Hallen 2005
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