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Review of Radio Observations

Galaxy Evolution and Environment. Review of Radio Observations. Tiziana Venturi tventuri@ira.inaf.it. Bologna, 5 Novembre 2009. Outline. Radio emission in galaxies: - AGN, starburst, HI Same cosmic epoch: - Local radio luminosity function for rich and poor environments

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Review of Radio Observations

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  1. Galaxy Evolution and Environment Review of Radio Observations Tiziana Venturi tventuri@ira.inaf.it Bologna, 5 Novembre 2009

  2. Outline • Radio emission in galaxies: • - AGN, starburst, HI • Same cosmic epoch: • - Local radio luminosity function for rich and poor environments • - Radio galaxies in dense environments • Radio source evolution with the cosmological epoch: • - Radio luminosity functions for AGNs and starbursts compared to the local RLF • - Relation with the environment • - Steep spectrum radio galaxies and search for protoclusters • Present and future available radio facilities

  3. Radio Loud AGNs Radio galaxies are associated with elliptical galaxies. The radio emission is non thermal (synchrotron) and it origins in the galaxy nucleus.

  4. The radio emission takes the form of (a)symmetric jets and a central component (core) coincident with the optical nucleus. The local environment shapes the radio lobes Head Tail FRII FRI Symmetric double Wide angle tail Radio galaxies are classified as low power (FRI) and high power (FRII), the divide being P(1.4 GHz)~ 1024.5 W/Hz The two FR classes also differ in morphological details

  5. Starburst Galaxies Non thermal radio sources whose radio emission is dominated by supernova remants and radio supernovae (P1.4GHz < 1021.5 -22 W/Hz) M82 z=0.000677 Arp 299 z=0.0103 NGC 253 Z=0.000811 Perez-Torres et al. 2009

  6. HI emission in spiral galaxies VIVA project (VLA) THING Survey - VLA Detailed study of HI emission possible only in the very local Universe (z<0.1) HI emission in spirals is known to be strongly affected by the environment (field, groups, clusters, merging clusters): morphology & HI deficiency (Vollmer 2009, Virgo) Dependance of HI on cosmological epochs (up to z~0.25) only recently started (Catinella et al.)

  7. AGN and Starbust radio emission Environment … Same redishift: local environment

  8. AGN and Starbust radio emission … & Evolution Different redshift: evolution

  9. Local Universe and role of the environment on the radio emission I. Statistical properties of radio galaxies and cluster environment - High galaxy density in clusters compared to the field - galaxy-galaxy interaction - Large scale interaction (cluster merger) Does this affect the radio luminosity function for AGN and starburst galaxies?

  10. The dense cluster environment does not seem to influence the RLF for AGN, whose main dependance is on the optical magnitude Field galaxies Galaxies in the 6dFG sample Cluster galaxies Ledlow & Owen 1996 Auriemma et al. 1977 Mauch & Sadler 2007 But analysis on individual merging clusters seem to deviate in opposite directions: A2255 “Universal” RLF A3558 A3562 Comparison sample A3556 SC A3558 Shapley complex Venturi et al. 2000 Mauduit & Mamon 2007 Miller & Owen 2003

  11. Same conclusions on the radio emission from starburst galaxies Faint end of the RLF includes starbusts A2255 higher than the comparison cluster sample Miller & Owen 2003 Shapley galaxies and re-analysis of MO03 do not show significant enhancement of startburst emission in merging custers Giacintucci et al. 2004

  12. Local Universe and role of the environment on the radio emission II. Radio galaxies at cluster centres: morphology, feedback and cycles of radio emission A large fraction of brightest cluster members (BCG) is radio loud (~60%) Their radio morphology can be broadly divided into two classes: Abell 2052 Abell 400 WATs and extended with radio power close to the FRI/FRII divide Both in cooling and non cooling clusters Core-Halo radio galaxies Only in cooling clusters Mittal et al. 2009

  13. Radio emission and ICM at the cluster centres know of each other Pcav(1042 erg/s) 1 1 McNamara & Nulsen (2007, ARAA 45, 117) Lradio(1042 erg/s) LICM(1042 erg/s) Feedback from the central AGN may stop the cooling - Cavities in the ICM filled by radio lobes from the central galaxies prove the role of the central AGNs. HPBW 18’’ , f.c. 0.15 mJy/b GMRT 610 MHz current burst HPBW 22’’ f.c. 0.7 mJy/b SE cold front Steep spectrum emission not obviously connected with the central galaxy: old radio emission? NGC5044 GMRT 240MHz Same old burst? α> 1.6 Giacintucci et al 2009

  14. Evidence of restarted activity in radio galaxies at the cluster centres further links the radio filled cavities with the central AGN Steep spectrum dominated by the diffuse emission 3C317 in A2052 VLBI Active nucleus Venturi et al. 2004

  15. Redshift Evolution Statistical properties of radio AGN and starburst galaxies - Evolution of the radio source population - Massive black hole formation and evolution with cosmic time - Star formation and its evolution with cosmic time - Relation with the environment radio luminosity functions in different redshift bins Samples of galaxies with radio and optical information (spectroscopic or photometric)

  16. Recent determinations of the Local Radio Luminosity Function 6dFGS D2+ NVSS SDSS + NVSS + FIRST Best et al. 2005 Mauch & Sadler 2007

  17. High power & low power radio galaxies Different evolution with cosmic time Strong evolution of powerful radio sources established long ago Low Power FRI High Power FRI Forlow power radio galaxies in the COSMOS field the evolution is much weaker than at high power (Smolcic et al. 2009) Evolution of powerful radio galaxies up to z=0.55 from SDSS+NVSS(Donoso et al. 2009) 0.1≤z≤0.35 0.35<z≤0.6 0.6<z≤0.9 0.9<z≤1.3 Dunlop & Peacock 1990

  18. Dependance on the environment AGNs in the SDSS z ≤ 0.55 RLF for central radio galaxies in the NEP sample (0.3<z<0.8) NEP clusters Radio loud AGN are more strongly clustered than control galaxies of the same mass and quasars at the same redshif Local RLF Possible evolutionary effects for the radio loud galaxy population(Branchesi et al. 2006) Adapted from Kauffmann et al. 2009

  19. Evolution of “passive” AGNs and star forming galaxies zCOSMOS field (0.1<z>0.9) Number of AGN over control sample vs local overdensity AGN Control sample Radio AGN SFG Radio-based AGN definition: Two classes of AGN, with “passive” and with star forming (non-passive) galaxy host Only “passive” AGN show environmental dependence: black hole masses or emission mechanism difference? Black Hole Masses distribution irrespective on environment ==> difference in feeding the black hole Triangles:High densities Points: low densities Only the red “passive” AGN show a density dependency In higher environments the ratio between stellar mass and emissivity is higher (signature of the cooling of the group or cluster) ==> Feedback No environmental effect on AGN hosted by star forming ==> trigger by secular (i.e. bars) phenomena (Bardelli et al. 2009) L1.4GHz Cooling flow of group/cluster L1.4GHz Mstar

  20. High redshift radio galaxies and the Early Universe Tracers of massive galaxy formation and protoclusters Miley & De Breuck, 2008 AARev 15,67 1.4 GHz VLA over Lyα 4C41.17 at z=3.8 Powerful (P500MHz >1027 W/Hz) steep spectrum (α> 1) radio galaxies at high redshift (z>2) Rare objects: 178 known to date PKS1138-282 - z=2.2 X-ray over radio MRC1182-262 proto cluster: host galaxy surrounded by giant Lyα halo in a 3 Mpc scale structure of M>2x1014 MSun

  21. Present and future radio facilities Wide fields and the “weak” Universe New and upgraded observational facilities over the whole radio window ready or to be operational over the next 12-16 months LOFAR 30-80 MHz 120-240 MHz eVLBI and MERLINfrom 1.6 to 22 GHz EVLA Complete frequency coverage from 1 to 50 GHz ALMA 10 bands from 35 to 850 GHz GMRT 1.4 GHz – 240 MHZ

  22. μJy sensitivity from 1 to 50 GHz at resolutions from milliarcsecond to arcsecond scale and from ~20 μJy to few mJy at the ALMA frequencies Sub-mJy to mJy sensitivity at the LOFAR frequencies GMRT

  23. … some examples … Low power end of the RLF for AGN Starburst galaxies locally and at high z Very distant radio galaxies HI at high z Starburst & starforming galaxies at high z HI dynamics in the Local Universe … and much more…

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