The Impact of High Redshi3 Radio Galaxies on Their Environments

Transcription

1 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.

2 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.

3 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

4 High Redshift Radio Galaxies PKS 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

5 High Redshift Radio Galaxies PKS 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

6 K-z K-z or or Hubble Hubble diagram diagram for for radio radio galaxies galaxies M Rocca-Volmerange et al. (2004) ESAC 2012 Nick Seymour Page 6

7 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

8 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

9 AGN Mid-IR Power Seymour et al. (2007) De Breuck et al. (2010) ESAC 2012 Nick Seymour Page 9

10 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

11 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

12 Torus and jet alignment edge-on Torus inclination face-on Drouart et al. (2012) Radio core dominance ESAC 2012 Nick Seymour Page 12

13 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

14 PKS z=2.156 The Hungry Spider! Brandl starburst Mullaney AGN Seymour et al. (2012) ESAC 2012 Nick Seymour Page 14

15 PKS 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

16 PKS z=2.156 The Gas-rich Spider! CO(1 0) in the Spiderweb Galaxy A. CO(1 0) A bleh kpc C. B. 867/ Flux (mjy/bm) Flux (mjy/bm) Flux (mjy/bm) B. C. MRC z = # optical emitters Emonts et al. (2012) Velocity (km/s) ESAC 2012 Nick Seymour Page 16

17 PKS 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 Emonts et al. (2012) v opt ESAC 2012 Nick Seymour Page 17

18 Mergers and feedback amongst starburskng radio galaxies Ivison et al. (2012) ESAC 2012 Nick Seymour Page 18

19 Mergers and feedback amongst starburskng radio galaxies Ivison et al. (2012) ESAC 2012 Nick Seymour Page 19

20 Environment of 4C41.17 Wylezalek et al. (2012) ESAC 2012 Nick Seymour Page 20

21 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

22 Thank you CASS Nick Seymour Future Fellow t e nicholas.seymour@csiro.au w hop:// CSIRO ASTRONOMY & SPACE SCIENCE

23 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

24 Specific Star Formation Rates/Characteristic Time Seymour et al, 2007

25 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 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, USS 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, WNJ Surface Density (N/sq. arcmin) Surface density (N/arcmin 2 ) MRC (z=1.41) PKS (z=2.16) MRC (z=1.90) 7C (z=1.42), 4C23.56 (z=2.48) ClGJ (z=1.62) 3C470 (z=1.65), MRC (z=2.63) USS (z=2.35) MRC (z=2.02) USS1410, WNJ1115 MRC (z=1.68),MRC (z=2.55), CLJ (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, USS N (r < 1 arcmin) % of SWIRE Cells # of HzRG fields Percentage of cells Number of HzRGs HzRGs ASA 2012 Nick Seymour Page 25