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AGN FEEDBACK AND QUENCHING OF STAR FORMATION: A MULTIWAVELENGTH APPROACH

AGN FEEDBACK AND QUENCHING OF STAR FORMATION: A MULTIWAVELENGTH APPROACH. EURO-VO AIDA Research Initiative Call for Proposals. Sonia Antón ( CICGE/SIM-IDL , Portugal) Bruno Coelho (FCUP/CAUP, Portugal) Catarina Lobo (CAUP, Portugal) Isabel Márquez (IAA, Spain)

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AGN FEEDBACK AND QUENCHING OF STAR FORMATION: A MULTIWAVELENGTH APPROACH

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  1. AGN FEEDBACK AND QUENCHING OF STAR FORMATION:A MULTIWAVELENGTH APPROACH EURO-VO AIDA Research Initiative Call for Proposals Sonia Antón(CICGE/SIM-IDL, Portugal) Bruno Coelho(FCUP/CAUP, Portugal) Catarina Lobo (CAUP, Portugal) Isabel Márquez(IAA, Spain) Josefa Masegosa(IAA, Spain) Evanthia Hatziminaoglou:EURO-VO scientist

  2. massive ( M*> 1010 MSUN ) galaxies significant bulge AGN SMBH feedback SF quenched galaxies move onto the red sequence

  3. bulgeless quenched central galaxies do not exist Bell (2008) SDSS DR2 0.02 ≤ z ≤ 0.06

  4. bulgeless quenched central galaxies do not exist Bell (2008) SDSS DR2 BUT ... - Spitzer MIR spectroscopy unveiled optically eluded AGN in bulgeless galaxies(Satyapal et al. 2007, 2008) 8 AGN / 23 late-type gals MSMBH> ≈ 106 MSUN

  5. ... QUESTIONS... ? how common are bulgeless galaxies with SMBHs ? ? how red and dead are they ? large sample of galaxies multiwavelength data VO VO ANSWERS diverse analysis tools time and $$ VO VO

  6. GOAL 1 red galaxies no SFor dust enshrouded ? - Identify dusty systems: - IR excess in the SED (eg. Vega et al. 2008) - B-I images (eg. Kotilainen & Ward 1997) - Use extinction corrections proposed by Maller et al. arXiv0801.3286 to the SDSS colors

  7. GOAL 2 bulgeless galaxies correctly classified? - Review morphological classification (Sérsic (1968) index n, by Blanton et al. 2003 for the DR2) for these more “problematic” systems: => higher resolution images (HST...) => NIR images (especially for dusty & edge-on systems)

  8. GOAL 3 frequency and characterization of AGN ? - radio: - compact core morphology - flat spectrum (eg. Nagar et al. 2005, Falcke et al. 2000) - radio loudness:fRADIO/ fOPTICAL(Kellerman et al. 1989) - X-rays: - hard unresolved nuclear source (eg. González-Martín et al. 2006, Cappi et al. 2006) - high fX-RAYS / fOPTICAL(Ho 2008) - B-R and B-I bluer cores (Antón et al. 2002, 2008, Kotilainen & Ward 1997)

  9. GOAL 4 Estimate MSMBH - Via LBOL, AGN(Satyapal et al. 2007) - Via Sérsic index n(Graham & Driver 2007), with nestimated by Blanton et al. (2003) for the SDSS DR2

  10. GOAL 5 Estimate MHALO and explore MSMBH ↔ MHALO correlation Lr M* of host galaxy MHALO(Yang et al. 2007, SDSS, Yang et al. 2005, 2dFGRS)

  11. complete sample (~6000 objs.) NYU-VAGC 0.02 < z < 0.06 inclination b/a > 0.5 log (M*/MSUN) > 10 TOPCAT Sérsic index n < 1.5 (g-r) > 0.57 + 0.0575 log (M* / 108 MSUN) TOPCAT test sample (~20 objs.) ALADIN VIZIER VO DESKTOP get all available reduced data SDSS SPECTRUM PARAMETERS - analyse spectra information - select sub-samples TOPCAT FLUXES - build and analyse SED - select sub-samples • IMAGES • - analyse optical/NIR images • select sub-samples VOSED? YAFIT? TOPCAT TOPCAT ALADIN MERLINimager CIAO obtain radio & X-ray images at arcsec resolution for tricky morphological types get optical/NIR high-res images for dusty SED objs. analyse color images ALADIN GALFIT

  12. SDSS J144322.25+010553.2

  13. fRADIO/ fOPTICAL => radio-quiet H-band / R-band consistent with NLAGN (Franceschini et al. 2005)

  14. “The first steps into a new world are always the most difficult ones. The VO realm, with all its large potentialities and promises, makes no exceptions.” from the ESA-VO pages (on VOSpec)

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