The cluster environment of high redshift FRI radio galaxies

1. Collaborators: Marco Chiaberge (STScI, INAF-IRA Bologna, JHU), Annalisa Celotti (SISSA), Colin Norman (JHU, STScI), Ranieri Baldi (SISSA) The cluster environment of high redshift FRI radio galaxies Gianluca Castignani (SISSA)

2. Radio morphologies, Fanaroff & Riley (1974) FRIs FRIIs Zirbel (1996) • FRI: Jet decelerates to v << c at ~1kpc • FRII: Relativistic jet on scales ~100 kpc up to ~1Mpc • FRI / FRII divide: L178 MHz<2 x 1026 W Hz-1 Zirbel, 1996 • FRI: Jet decelerates to v << c at ~1kpc • FRII: Relativistic jet on scales ~100 kpc up to ~1Mpc • FRI / FRII divide: L178 MHz<2 x 1026 W Hz-1

3. FRIs Locally: • “starved quasar”: faint optical nuclear emission (Chiaberge et al. 1999, Leiptzki et al. 2009, Baldi et al. 2010) • Host galaxy: mainly giant elliptical (cD) with the most massive BHs (Donzelli et al. 2007, Zirbel & Baum 1997) • ~70% of them in rich clusters, at variance with FRIIs (Hill & Lilly 1991; Zirbel 1997; Wing & Blanton 2011) At high redshift: • Two FRIs at z~1 (Snellen & Best 2001) • ~30 FRI candidates at z~1-2(Chiaberge+09)

4. FRIs at z~1-2. Why? Clusters • Beacons for HIGH REDSHIFT CLUSTERS • Link between z>~2 protoclusters and clusters • Formation and evolution of the red sequence AGN • Cosmological evolution unknown • Hints for strong evolution up to z~0.7 (Sadler et al., 2007) • Formation and evolution of the most massive galaxies and Bhs • Feedback: BH accretion - environment

5. The sample FRIscandidates at z~1-2, Chiaberge et al., 2009 (C09) COSMOS (2sq degrees) Mainly based onradio (FIRST) and optical selection, NOT on redshifts FRIscandidates sample z~1-2, Chiaberge et al., 2009 (C09) COSMOS field (2sq degree) Mainly based onradio (FIRST) and optical selection, NOT on redshifts Redshifts Accurate redshifts (Baldi et al., 2013) are required to redefine the sample in radio power Few spectroscopic-z: zCOSMOS, Lilly et al., 2007; Magellan, Trump et al., 2007 Photo-z: SED modeling stellar population(s) and dust component(s) Redshifts • Accurate redshifts(Baldi et al. 2013) are required toredefined the sample in radio power • Few spectroscopic-z: zCOSMOS bright (Lilly et al. 2007) Magellan (Trump et al. 2007) • Photo-z: SED modeling stellar population(s) and dust component(s)

6. Clusters around LLRGs?Cluster candidates around Low Luminous Radio Galaxies? (FRIs) The C09 sample redefined in radio power • 21 LLRGs • 11 High Luminous Radio Galaxies (HLRGs)

7. Two cluster candidates Figure: Field of COSMOS-FRI 01, cluster from visual inspection RGB images. Red: Spitzer 3.6μm. Green: optical i-band. Blue: optical V-band Figure: Field of COSMOS-FRI 026, cluster?

8. Cluster search techniques • SZ effect, only a few at z>1 (e.g. Planck coll. XXIX 2013; Hasselfield et al. 2013, Reichardt et al. 2013) • X-ray (Rosati et al., 2002): B~(1+z)-4 • Photo-z and number counts (Eisenhardt et al. 2008; Knobel 2009, 2012; George et al. 2011) • Color selection (e.g. Gladders & Yee 2005; Papovich et al, 2008). Red-sequence is just forming between z~1-2 (Hilton et al. 2010; Fassbender et al. 2011; Santos et al. 2011) • Search around radio galaxies(Miley & De Breuck 2008, Galametz et al. 2012, Wylezalek et al. 2013) only FRIIs adopted

9. Poisson Probabiliy Method (PPM)Castignani et al., in prep • Existing methods seem to be less efficient at z>~1.5 (only 9 spectroscopically confirmed z>~1.5 clusters, see Tozzi et al. 2013) • Methods based on photo-z and number counts (Scoville+2013 and and ref. therein)affected by: 1) low number counts 2) increasing photo-z uncertainties 3) photo-z catastrophic failure at z~1.5 (redshift desert)

10. PPM, how does it work?

11. PPM, how does it work? > 2sigma > 3 sigma > 4sigma

12. PPM plots 3.5σ detection (LLRG)

13. PPM plots 3.9σ detection (LLRG)

14. PPM plots 2.5σ detection (LLRG)

15. Papovich (2008) method • 1.6 μm bump in the SED of red galaxies (opacity of the H− ion in atmospheres of cool stars, John 1988) Galametz et al. (2012)

16. Papovich (2008) method • Red galaxies are selected ([3.6]-[4.5])AB> -0.1 mag (SPITZER-COSMOS) • The overdensity is evaluated as a number excess of red galaxies with respect of the COSMOS mean number density • Seven >2σ orverdensities are detected • All of them are also found with the PPM • The Papovich (2008) test does not find our z~1 clusters • ...and some of our z≈2 candidates (e.g. 05, 226, also suggested in Chiaberge et al. 2010). Are they blue clusters?

17. Simulated clusters Two z~1X-ray rich groups (M500≈ 6e+13Msun - Finoguenov et al. 2007) moved at higher z • Cluster membershipbased on: 1) PPMprojected and redshift information 2) sources with the lowest(K-I)ABare selected • Statistical Photo-z redshift uncertaintiesincluded • IAB<25 selection (according to Ilbert et al. 2009)

18. Simulated clusters The groups are detected up to z=1.5

19. Simulated clusters The groups are detected up to z=1.5

20. Simulated clusters The groups are detected up to z=1.5

21. Simulated clusters Spherically symmetric simulated groups - Richness (Nc = 10, 50, 100, 200, 300) -Redshift (zc = 1.0, 1.5, 2.0) - Comoving size (Rc = 1.0, 1.5, 2.0Mpc) • Rich groups(Nc≥100) are always detected • Groups with Rc = 1Mpc andNc = 10 are detected at zc≥1.5 • Groups detected up to an offset of ~100 arcsec from the position of the cluster

22. Overdensity detections • Gaussian filter to remove noisy patterns from the plot • Overdensities selected at∆z=0.28 (i.e. 2σ photo-z uncertainty at z~1.25 for i+AB~24 galaxies) • Peak finding algorithm to detect each overdensity in the field • The overdensities found within the FRI redshifts uncertainties are associated with the radio galaxy. • LLRGs: 14/21 • HLRGs: 8/11 • ...in agreement with what found locally 69%

23. Gravitational arc in the field of COSMOS-FRI 01!! Figure: HST ACS image of the field of COSMOS-FRI 01

24. Stacked weak lensing analysis • Clusters around LLRGs only • NFW+stars (George et al. 2012) • Signal compatible with rich groups: M200~1013.3Msun WORK in progress... Courtesy of Matthew George (University of California – Berkley)

25. Conclusions • FRIs plus PPM → z∼1-2 cluster search around FRIs candidates • ~70% cluster detection success • high redshift FRIs are in dense environment, as found locally Future work... • Weak lensing signal from the stacking of our (LLRGs) cluster candidates (in progress...) • CM plots, red sequence?? • PPM and wide field surveys, e.g. SDSS Stripe 82, LSST: • ∼1000 or more FRIs expected • PPM needs beacons and good photo-z FRIs plus PPM → z∼1-2 cluster search around FRIs candidates • ● ~70% cluster detection percentage • ● high redshift FRIs are in dense environment, as found locally • Future work... ● Weak lensing signal from the stacking of our (LLRGs) • cluster candidates (in progress...) • ● CM plots, red sequence?? • ● PPM can be applied to wide field surveys, e.g. SDSS • ● stripe 82, Chandra Deep field(s) North/South : • ●∼1000 or more FRIs expected • ● PPM needs targets (e.g. FRIs) and good photo-z