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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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slide1

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

slide2

massive ( M*> 1010 MSUN ) galaxies

significant bulge

AGN SMBH

feedback

SF quenched

galaxies move onto the red sequence

slide3

bulgeless quenched central galaxies

do not exist

Bell (2008)

SDSS DR2

0.02 ≤ z ≤ 0.06

slide4

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

slide5

... 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

slide6

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

slide7

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)

slide8

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)

slide9

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

slide10

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)

slide11

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

slide13

fRADIO/ fOPTICAL => radio-quiet

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

slide14

“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)