The Cluster Environments of High

Redshift Radio GalaxiesJaron Kurk

MPIA Hauscolloquium12 5 2006

MPIA Hauscolloquium12 5 2006

Prof George Miley Dr Huub Röttgering

JKPhD May 2003

Bram VenemansPhD April 2005

Roderik OverzierPhD May 2006

Other Leiden PhDs involved: Laura PentericciCarlos De BreuckMichiel Reuland

Leiden students and postdocs: Andrew ZirmHuib Intema

Others:Chris Carilli,Wil van Breugel,Adam StanfordSteve CroftG. De LuciaT. HeckmanH. Ford

P. McCarthy

Leiden HzRGCluster Program

Thesis defense: May 30

Outline of Talk

• Introduction– Clusters– HzRGs– HzRG-Cluster Program

• Some examples– 1138 at z = 2.2– 1338 at z = 4.1

• Program Results– Line emitters– Distant clusters

Importance of Distant Clusters

Distant clusters are of interest because• their presence constrains cosmological parameters (e.g. Eke et al. 1996)• their galaxies provide unique reservoir to investigate

galaxy evolution

– clusters at z ~ 0.5 contain more blue galaxies (Butcher & Oemler 1984)

– scatter in colour-magnitude relation constrains formation mode– central brightest cluster galaxies do not fit on LF

But difficult to find because of• contamination by foreground galaxies• cosmological surface brightness dimming of extended X-ray

emission

Most distant clusters found to date• at z = 1.11 by X-rays (Stanford et al. 2002)• at z = 1.26 by X-rays and NIR imaging (Rosati et al. 1999,

Stanford et al. 1997)

Properties of HzRGs

Indirect evidence that HzRGs are located in (forming) clusters

• Radio galaxies observed in clusters or over-densities of galaxies

– Half of powerful RGs at z ~ 0.5 inhabit rich clusters (Hill & Lilly 1991, Yates et al. 1989), strong correlation with redshift as at z < 0.15 RGs avoid clusters (Prestage & Peacock 1989)

– Nearby example of Cygnus A (Owen et al. 1997)– Over-density of K band galaxies in 3CR fields (Best 2000, 2003)

and other z ~ 1 RG and QSO fields (Hall et al. 2001, Barr et al. 2004)– Over-density of EROs and sub-mm galaxies near 4C41.17 (Ivison et al. 2000)

• Radio galaxies observed in dense ambient gas

– High (> 1000 rad m-1) radio RMs (Carilli et al. 1997, Pentericci et al. 2000)

• Hosts of HzRGs resemble brightest cluster galaxies

• HzRGs are amongst the most massive galaxies up to z ~ 5 (De Breuck et al. 2002)

Properties of HzRGs

De Breuck et al. (2002)HzRGs are amongst the most massive galaxies up to z ~ 5

K-z diagram

Powerful AGN massive black hole massive galaxy (Magorrian relation)

Example HzRG: 1138-262 at z = 2.2

ACS/HST 20 orbits g+i

100 kpc

• Elements of both hierarchical and monolithic formation

• Morphological types that dominate the faint population in the UDF (chains, tadpoles and clump-clusters)

• Star formation in two modes: LBG-like (50%) and diffuse (50%)

Pentericci et al. (2002), Kurk (2003), Miley et al. (in prep.)

Example HzRGs: emission line halos

1338 at z = 4.1VLT line emissionACS continuumZirm et al. (2005)

1138 at z = 2.2VLT line emissionRadio 8 GHz continuumKurk (2003)

The Leiden HzRG Cluster Program

• Use HzRGs as beacons of forming clusters– HzRGs have properties of forming BCGs– Seem to live in dense environments at z ~ 1– Most massive galaxies at any z and therefore found in most massive DM halos

• Use Ly emitting galaxies as tracers of galaxy overdensities– Strongest (intrinsic) emission line– LAEs occupy faintest accesible part of LF– Spectroscopic confirmation relatively easy

• VLT Large Program– Eight radio galaxy fields at 2.2 < z < 5.2– Twenty nights with FORS/VLT (and twenty hours LRIS/Keck)

– Narrow band imaging of 33 Mpc2 fields and MOS spectroscopy

Line emitting galaxies at high redshift

• Primordial galaxies should emit 3-6% of their bol. lum. in Ly, resulting in EW0 = 100-200 Å (Charlot & Fall 1993)

• Ly is resonant, so large extinction can occur: only 25% of LBGs have EW0 > 20 Å (Shapley et al. 2003)

• LAE surveys fashionable– Hu et al. (1998), Rhoads et al. (2000),

Stiavelli et al. (2001), Ouchi et al. (2002),Hu et al. (2004), Tapken et al. (2006),Steidel et al. (2000)

– Little evolution of UV continuum with z– Controversy about red colours and high

equivalent widths– Clustering observed in large fields

• LAEs are currently redshift record holders

Intermezzo I - LAE at z = 6.5

• FORS2/VLT slitless spectroscopy combined with a medium band filter

• One LAE emitter found at z = 6.518 with flux of 210-17 erg s-1 cm-2

• Comparison of LFs at z = 5.7 and z = 6.5 shows little evolution and therefore reionization earlier than z = 6.5 (Malhotra & Rhoads 2004)

Kurk et al. (2004)

The NB Imaging Technique

Kurk (2003)

Individual HzRG Fields

• PKS 1138-262 at z = 2.16– Pilot VLT project (first VLT visitor observations, in 1999)

– Lowest redshift of sample– Indications of dense environment– Suitable redshift for H narrow band imaging– Chandra X-ray , NICMOS, MOIRCS observations– Main subject of my thesis my favourite object!

• TN J1338-1942 at z = 4.10– One of the brightest (in Ly line and radio continuum)

– Most overdense field (in terms of LAEs)– Drop-out imaging with ACS and Suprime-Cam

1138 Imaging

Imaging: 0.5 hr B band, 4 hr narrow band- Fifty LAEs with EW0 > 20 A and F > 210-19 erg s-1 cm-2 A-1

Spectroscopy: 6, 5.5, 4 hr for each FORS1 mask- Fifteen confirmed (out of 27)

Kurk et

al. (2000)

1138 Spectroscopy results

Spectroscopic confirmation of 15 LAEs- Single line rules out [OII],

[OIII], Hβ- One QSO: FWHM ~ 5800 km s-1, CIV emission

Pentericci et al. (2000)

1138 Spectroscopy results

Spectroscopic confirmation of 15 LAEs- LAE redshifts centered on radio

galaxy- Probability redshifts drawn from random distr. < 0.4%- Redshifts seem to be distributed in two groups

Kurk et al. (2004)

σv = 385, 205 km s-1

σv = 900 km s-1

Actual redshift distribution

Monte Carlo Simulation

2

3

• Two 2.5’2.5’ ISAAC fields– HAEs have 5 higher density within 0.66’ radius compared with outside 1.0’ radius

– No blank field HAE surveys deep enough to compare with

1138 H imaging

-Kurk et al.

(2004)

1138 H spectroscopyTwo nights of ISAAC spectroscopy confirmed redshifts nine HAEs, including one QSO, v = 360 km s-1

-Kurk et al.

(2004)

Intermezzo II - Wide field H survey

• Finally NIR detectors with large FoV available• WFCAM survey at z = 2.2 of 1.5 deg2 (on-going, P.I. Smail)• VISTA survey at z = 0.8 of 1.6 deg2 (proposed, P.I. Fynbo)• LF of H emitting galaxies, good estimate of (global) SFR at

z > 2• Comparison with HzRG fields (also other emission lines)

• Chandra imaging (40 ksec) reveals– apart from RG 17 serendipitous sources in FORS field

– about 50% more soft sources with flux > 10-15 erg s-1 cm-2 than in CDF (1.5 significance)

– coincidence with 3 LAEs, 1 HAE, 1 ERO– optical/X-ray ratios indicate AGN– four X-ray sources and RG roughly aligned

1138 X-ray sources

-Pentericci et al. (2002),

Croft et al. (2005)

1138 SCUBA companions

Field of 1138 is second densest in sample of seven HzRG fields (Stevens et al. 2003) with three companions, two of them aligned E-W

1138 NICMOS CMD

RG Lya HaUDF/HDFN

Factor nine overdensity in red sequence galaxies (1.3 < J-H < 2.1) in six NICMOS fields near 1138

Zirm et al. (in preparation)

1138 Subaru CMD

Red sequence Lya Ha

Red sequence galaxies (J-K > 2.3) in 4’7’ MOIRCS field (Kodama et al., in prep.)Subaru NIR MOS and VLT optical MOS proposed

(Vega)

1338 ACS imaging

-Miley et al.

(2004)

ACS/HST FoV 3.4’3.4’gri imaging to detect g-

dropouts at z ~ 4Compare with cloned GOODS B-

dropoutsFactor 2.5 more g-dropouts than

expected, representing a 3 excess (i < 26)

More than 50% within 1 Mpc radius

Even stronger at i < 27Alternative of a cluster of z ~

0.5 Balmer break objects improbable

-g (4 orbits) r (4

orbits) i (5 orbits)

-LAE

-RG

-LAE

-LAE

Suprime-Cam FoV 25’24’BRI imaging to detect LBGs at

3.5 < z < 4.5 (6% cont.)874 LBGs with IAB < 26.5

125 LBGs with IAB < 25.0

Correl length r0 = 3.7 / 4.6 h-1 Mpc

Largest overdensity at pos of 1338

Size of ~ 2 Mpc includes 104 LBGs

7 coincide with confirmed LAEs28-35 LBGs associated with RGOverdensity 5-7Spectroscopy needed to trace

web

1338 Subaru imaging

-Intema et al.

(submitted)

Conclusions on Ly Emitters• In total ~ 300 LAEs of which ~ 150 confirmed

– spectroscopic confimation succes rate ~ 90%– AGN fraction < 10%, based on line widths (95% < 1000 km s-

1)• lines asymmetric, sometimes with absorption (M(HI) up to 5104 M)

– LLy < 1043 erg s-1, fainter than L* in UV continuum

– No evidence for zero metallicity (max EW0 < 240 A)

– Continuum colours are blueer ( = -1.7) than for LBGs ( = -1.1)

– SFRs in the range 1 - 10 M yr-1 (LBGs typically > 10 M yr-1)

– Low dust content (blue UV and consistent Ly and UV SFR)• extinction correction on Ly SFR << 2

– Ages < 100 Myr, in 16% < 10 Myr (from UV continuum)– Half light radii (~ 1.0 kpc) smaller than for LBGs in GOODS (~ 2.3 kpc, Ferguson et al. 2004)

Conclusions on Ly Emitters

Venemans et al. (in prep)

Large Program Results

Name of RG z IMG SPC

MRC 2048-272 2.06 10 3

MRC 1138-262 2.16 37 15

MRC 0052-241 2.86 57 37

MRC 0943-242 2.92 65 28

MRC 0316-257 3.13 77 31

TN J2009-3040 3.15 21 11

TN J1338-1942 4.10 54 37

TN J0924-2201 5.19 14 6

σv (km/s)N/A~900~980~715~640~515~265~305

Conclusions on Distant Clusters

• At least six out of eight fields show overdensity– surface overdensity on the order of 3-5

• Confirmed emitters are clustered in redshift space– width of vel. distr. 2-5 smaller than NB

• Estimated protocluster masses 2-91014 M

– assuming bias parameter b = 3-6 and certain volume V (Steidel et al. 1999)M = <>V(1+m), 1 + bm = C(1+gal), C = 1 + f - f (1 + m)1/3

where <> is mean density of universe and C redshift space distortions

• Velocity dispersion decreases with redshift• FoV too small to give reliable estimate of sizes

– but from second field near 1338 radius of ~ 2 Mpc seems correct

Venemans et al. (in prep.)

Conclusions on Distant Clusters

N-body modelling by G. De Lucia shows that– LAEs in protoclusters can

be identified with young (< 100 Myr) galaxies• luminosity or colour is

not enough– velocity distribution of

simulated clusters increases with decreasing redshift

– HAEs near 1138 lie within virialized core and may be older (as suggested by their brighter K-band continua)

Millenium simulation will improve results

Venemans et al. (in prep.)

RG proto-clustersSubgroupsSimulated clustersHubble Flow

Conclusions on Distant Clusters

Theory of linear spherical collapse predicts critical density at which structure will collapse, almost indendent of cosmology L = 1.686 (Peacock 1999)

Compare evolution of linear matter overdensity of protoclusters with this critical density

gal M L L(z) in CDM (Carroll et al. 1992)

1338 collapses at z ~ 0.51138, 0316, 0924 at z ~ 0

Overzier et al. (in prep.)

1138

13380316

0924

Intermezzo III - a QSO field at z = 6.3

• Overdensity of i-dropout galaxies in the field of QSO SDSS 1030+0524 at z = 6.28 (Pentericci et al., submitted)

• Follow-up spectroscopy (on-going, P.I. Walter)

Empty slide

RG PKS 1138-262

EROs: extremely redLAEs: purple

BIK FORS/ISAAC

Abbreviations used

• HzRGs: High Redshift Radio Galaxies• LAEs: Ly Emitters (Lyman- emitting galaxies)

• HAEs: H Emitters• EROs: Extremely Red Objects• ERGs: Extremely Red Galaxies (red distant galaxies)

• DRGs: Distant Red Galaxies (really red distant galaxies)

• LBGs: Lyman Break Galaxies (blue distant galaxies)