AGN FEEDBACK AND QUENCHING OF STAR FORMATION:A MULTIWAVELENGTH APPROACH

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

EURO-VO AIDA

Research Initiative

Call for P

roposals

massive ( M* > 1010 MSUN ) galaxies

significant bulge

AGN SMBH

feedback

SF quenched

galaxies move onto the red sequence

Bell (2008)SDSS DR20.02 ≤ z ≤ 0.06

bulgeless quenched central galaxiesdo not exist

Bell (2008)SDSS DR2

bulgeless quenched central galaxiesdo not exist

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

... QUESTIONS...

? how common are bulgeless galaxies with SMBHs ?

? how red and dead are they ?

ANSWERS

multiwavelength data

time and $$ diverse analysis tools

large sample of galaxies

VOVO

VO VO

GOAL 1

red galaxies

no SF or 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. arXiv0801.3286to the SDSS colors

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)

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)

GOAL 4

Estimate MSMBH

- Via LBOL, AGN (Satyapal et al. 2007)

- Via Sérsic index n (Graham & Driver 2007), with n estimated by Blanton et al. (2003) for the SDSS DR2

GOAL 5

Estimate MHALO and exploreMSMBH ↔ MHALO correlation

Lr

M*

of host galaxy MHALO (Yang et al. 2007, SDSS, Yang et al. 2005, 2dFGRS)

complete sample(~6000 objs.)NYU-VAGC

0.02 < z < 0.06inclination b/a > 0.5log (M*/MSUN) > 10

Sérsic index n < 1.5(g-r) > 0.57 + 0.0575 log (M* / 108 MSUN)

test sample(~20 objs.)

SDSS SPECTRUMPARAMETERS- analyse spectra information- select sub-samples

obtain radio & X-ray imagesat arcsec resolution

FLUXES- build and analyse SED- select sub-samples

IMAGES- analyse optical/NIR images- select sub-samples

for dusty SED objs.analyse color images

for tricky morphological typesget optical/NIR high-res images

get all availablereduced data

TOPCAT

TOPCAT

TOPCAT

TOPCAT

GALFITALADIN

ALADINVIZIER

VO DESKTOP

VOSED? YAFIT?TOPCAT

ALADINMERLINimager

CIAO

SDSS J144322.25+010553.2

H-band / R-band consistent with NLAGN (Franceschini et al. 2005)

fRADIO / fOPTICAL => radio-quiet

“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)