4C23.56, z=2.48 The Impact of High Redshi3 Radio Galaxies on Their Environments Nick Seymour (CASS) and the HeRGÉ CollaboraKon 1 12 September 2012 CSIRO ASTRONOMY & SPACE SCIENCE 1 Presented by Daniel Stern (JPL/Caltech) due to late Kme travel issues for NS.
4C23.56, z=2.48 The Impact of High Redshi3 Radio Galaxies on Their Environments Nick Seymour (CASS) and the HeRGÉ CollaboraKon1 12 September 2012 CSIRO ASTRONOMY & SPACE SCIENCE 1 Presented by Daniel Stern (JPL/Caltech) due to late Kme travel issues for NS.
Projet HeRGÉ (Herschel Radio Galaxy Evolution Project) Carlos De Breuck (ESO) Joel Vernet (ESO) Guillaume Drouart (ESO) Dominika Wylezalek (ESO) Daniel Stern (JPL/Caltech) Jason Rawlings (MSSL) Thomas Greve (UCL) Sabine Koenig (Dark Cosmology Center) Bjorn Emonts (CASS/CSIRO) Edo Ibar (UKATC/ROE) Rob Ivison (UKATC/ROE) Jack Mayo (UKATC/ROE) Audrey Galametz (Rome) Peter Barthel (Groningen) Martin Haas (Bochum) Nina Hatch (Nottingham) Matt Jarvis (Hertfordshire/UWC) Jason Stevens (Hertfordshire) Attila Kovacs (Minnesota) Matt Lehnert (Observatoire de Paris) Nicole Nesvadba (IAS, Orsay) Alessandro Rettura (JPL/Caltech) Huub Rottgering (Leiden) Brigitte Rocca-Volmerange (IAP) Arjun Dey (NOAO) Mark Dickinson (NOAO) Bruno Altieri (ESA) George Miley (Leiden) ESAC 2012 Nick Seymour Page 3
High Redshift Radio Galaxies PKS1138-262 at z=2.156 `The Spiderweb Galaxy (Miley et al. 2006; Hatch et al. 2008) Probably Massive (Proto-)cluster environment (see talks by J. Vernet and D. Wylezalek) Evidence of high SFR Most radio luminous sources in the Universe ESAC 2012 Nick Seymour Page 4
High Redshift Radio Galaxies PKS1138-262 at z=2.156 `The Spiderweb Galaxy (Miley et al. 2006; Hatch et al. 2008) Probably Massive (Proto-)cluster environment (see talks by J. Vernet and D. Wylezalek) Evidence of high SFR Most radio luminous sources in the Universe Archetypal obscured type 2 AGN ESAC 2012 Nick Seymour Page 5
K-z K-z or or Hubble Hubble diagram diagram for for radio radio galaxies galaxies 10 12 M Rocca-Volmerange et al. (2004) ESAC 2012 Nick Seymour Page 6
Spitzer High-z Radio Galaxy survey (SHzRG survey) 8 band imaging survey of 71 high-z radio galaxies (HzRGs: 1<z<5.2 and L 3GHz >10 26 WHz -1 ) Goal to obtain stellar masses (via rest-frame near-ir luminosities) and deconvolve the AGN component Later supplemented with IRS spectroscopy of a z~2 subset ESAC 2012 Nick Seymour Page 7
Stellar Masses of HzRGs <log(m/m )> ~ 11.3, but still time to grow a bit more (Seymour et al. 2007; De Breuck et al. 2010) ESAC 2012 Nick Seymour Page 8
AGN Mid-IR Power Seymour et al. (2007) De Breuck et al. (2010) ESAC 2012 Nick Seymour Page 9
AGN Mid-IR Power mid-ir strong for quasars (Ogle et al. 2006) Seymour et al. (2007) De Breuck et al. (2010) ESAC 2012 Nick Seymour Page 10
Mid-IR Spectroscopy Measure SFR and accretion from mid-ir spectra No correlation between AGN and SF power although both are high Rawlings et al. (2012) ESAC 2012 Nick Seymour Page 11
Torus and jet alignment edge-on Torus inclination face-on Drouart et al. (2012) Radio core dominance ESAC 2012 Nick Seymour Page 12
Projet HeRGÉ (Herschel Radio Galaxy Evolution Project) Five-band Cycle 1 Herschel photometry of all 71 SHzRGs (PI Seymour) Data 100% observed Students working hard Two papers accepted Two papers submitted Several more in prep. ESAC 2012 Nick Seymour Page 13
PKS1138-262 z=2.156 The Hungry Spider! Brandl starburst Mullaney AGN Seymour et al. (2012) ESAC 2012 Nick Seymour Page 14
PKS1138-262 z=2.156 The Hungry Spider! Brandl starburst L_IR AGN ~2e13L Acc ~0.2 Edd SFR ~1400 M /yr t_char ~0.8 Gyr t_jet ~5-25 Myr Mullaney AGN Seymour et al. (2012) ESAC 2012 Nick Seymour Page 15
PKS1138-262 z=2.156 The Gas-rich Spider! CO(1 0) in the Spiderweb Galaxy A. CO(1 0) A. 1637 +453 997 +123 +863 bleh +723 2937 16 kpc C. B. 867/ 1547 1587 1827 Flux (mjy/bm) Flux (mjy/bm) Flux (mjy/bm) B. C. MRC 1138 262 z = 2.161 5 0 # optical emitters Emonts et al. (2012) Velocity (km/s) ESAC 2012 Nick Seymour Page 16
PKS1138-262 z=2.156 Gas-rich companion HAE229 lies ~250 kpc away HST image with CO contours (blue) black contours = 3.6µm CO spectrum seen in (lower left) group of 4 galaxies, 2 confirmed as proto-cluster members strong PAH emission (Ogle et al. 2012) 30" MRC 1138 262 Emonts et al. (2012) v opt ESAC 2012 Nick Seymour Page 17
Mergers and feedback amongst starburskng radio galaxies Ivison et al. (2012) ESAC 2012 Nick Seymour Page 18
Mergers and feedback amongst starburskng radio galaxies Ivison et al. (2012) ESAC 2012 Nick Seymour Page 19
Environment of 4C41.17 Wylezalek et al. (2012) ESAC 2012 Nick Seymour Page 20
Conclusions (1) HzRGs are unique laboratories to study the formation of massive galaxies and clusters (2) HzRGs are massive, radio-loud, highly accreting starbursts probably triggered by gas rich major mergers (3) Projet HeRGÉ will provide a complete measure of their evolutionary state, and will test theories of how radioloud phase of AGN relates to galaxy formation ESAC 2012 Nick Seymour Page 21
Thank you CASS Nick Seymour Future Fellow t +61 293 724 284 e nicholas.seymour@csiro.au w hop://www.atnf.csiro.au/people/nick.seymour CSIRO ASTRONOMY & SPACE SCIENCE
Star Formation Rates of HzRGs Specific Star Formation Rates/Characteristic Time SFRs from SCUBA observawons specific Star FormaWon Rate (ssfr) = SFR/M (Gy - 1 ) = measurement of the current SFR relawve to past SFR needed to build up the stellar mass of the galaxy (Gy - 1 ) CharacterisWc Wme = inverse of ssfr (in units of Wme) = Wme to double mass at given SFR
Specific Star Formation Rates/Characteristic Time Seymour et al, 2007
Environments of HzRGs 24um selected sources (Mayo et al. 2012) Red IRAC selected sources (Galametz et al. 2012) Number galaxies within 1 Number of Sources in Cell 25 20 15 10 5 MRC2025 7C1805 LBDS53w069 6C0140, PKS0529 4C23.56, 6C0058 3C470, MRC0114, MRC0316, PKS1138 3C65, 3C266, 7C1756, MRC1017, WNJ0747 LBDS53w002 4C40.36, MRC0350, USS2202 MG2144, MRC0152, MRC0211, MRC2104, TXJ1908, USS1243 3 sigma 3C368.0, 4C41.17, 6C0032, B3J2330, MRC2048, MRC2224 3C239, 4C24.28, 4C28.58, LBDS53w091, MG1019, TNJ1338, USS1707 3C294.0, 4C60.07, 6C0132, 7C1751, 8C1435, MRC0406, TNJ2007, USS0943, USS1410 3C356.0, 6C1232, 6CE0905, TXS0211, WNJ1115 6C0930, 6CE0820, MRC0037, MRC0324, TNJ0924, WNJ1911 TNJ0205 TNJ0121 MRC0251, WNJ1123 3.0 2.5 2.0 1.5 1.0 0.5 Surface Density (N/sq. arcmin) Surface density (N/arcmin 2 ) 8 6 4 2 MRC0114-211 (z=1.41) PKS1138-262 (z=2.16) MRC0350-279 (z=1.90) 7C1756+6520 (z=1.42), 4C23.56 (z=2.48) ClGJ0218-0510 (z=1.62) 3C470 (z=1.65), MRC2025-218 (z=2.63) USS1425-148 (z=2.35) MRC0156-252 (z=2.02) USS1410, WNJ1115 MRC2224-273(z=1.68),MRC2139-292(z=2.55), CLJ1449-0856(z=2.07) MRC1324 6CE0620, USS1707 7C1805, MRC2048, MRC1017, MG2308 6C0132, TXS0211, LBDS53W002, MRC2104 3C266, LBDS53W091, MRC0152, USS1558, 4C28.58, MRC0406 6CE0905 6CE0901, 3C257, USS0828, MG1019 3C294, 4C40.36, 4C24.28, USS0943, MRC0324 MRC0211, 7C1751, WNJ0747 3C239, 5C7.269, 6C0930, PKS0529, USS2202 25 20 15 10 5 N (r < 1 arcmin) 0 10 20 30 % of SWIRE Cells # of HzRG fields 40 0 0 0 5 10 15 20 25 30 Percentage of cells Number of HzRGs HzRGs ASA 2012 Nick Seymour Page 25