Joint formation and evolution of SMBHs and their host galaxies:

1
Joint formation and evolution of SMBHs and their
host galaxies

• How do the Quasar-Spheroid correlations change
  with the Cosmic Time?

Marzia Labita
A. Treves Università dellInsubria, Como,
Italy R. Falomo INAF, Osservatorio Astronomico
di Padova, Italy R. Decarli Università
dellInsubria, Como, Italy J. Kotilainen Tuorla
Observatory, Piikkio, Finland M.
Uslenghi INAF-IASF, Milano, Italy
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SMBHs and host galaxies

• Most (if not all) nearby (early type) galaxies
  host a supermassive black hole (SMBH) at their
  centers
• - proper motion of stars (Milky Way)
• - rotation curves of gas clouds MASER (22
  objects)
• The host galaxies of low redshift quasars contain
  a massive spheroidal component
• (observative results see Dunlop et al. 2003,
  Pagani et al. 2003)

Elliptical galaxies ? SMBHs
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Joint formation of SMBHs and massive spheroids

• According to the hierarchical merging scenario,
  massive spheroids should be the products of
  successive merging events
• At low redshift, the central BH mass is strongly
  correlated to the properties of the host galaxy
  bulge (of both active and inactive galaxies)
• OUTSIDE THE SPHERE OF INFLUENCE!

Formation of Formation and fuelling Elliptical
galaxies of their active nuclei
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Quasar

• Nuclear luminosity
• Radio power (RLQ RQQ)
• Spectral shape
• BH mass determination and evolution

Host Galaxy

• Bulge luminosity
• (Stellar velocity dispersion, morphology, size)
• Host galaxy luminosity (mass) evolution

Quasar Host Galaxy connection

• Study the BH host mass correlation at low z and
  trace its cosmological evolution close and beyond
  the peak of the quasar activity

5
Quasar

• Nuclear luminosity
• Radio power (RLQ RQQ)
• Spectral shape
• BH mass determination and evolution

Host Galaxy

• Bulge luminosity
• (Stellar velocity dispersion, morphology, size)
• Host galaxy luminosity (mass) evolution

Quasar Host Galaxy connection

• Study the BH host mass correlation at low z and
  trace its cosmological evolution close and beyond
  the peak of the quasar activity

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The NIR to UV continuum of radio loud (RL) vs.
radio quiet (RQ) quasarsM. Labita, A. Treves,
R. Falomo, 2007, MNRAS, in press
(astro-ph/0710.5035)

• Understanding the nuclear engine of quasars
• Characterization of the Spectral Energy
  Distribution (SED)
• Distinction between RLQs and RQQs in the Unified
  Models of AGN
• (relativistic jet, BH spin?)
• compare and contrast the SEDs of RLQs and RQQs

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First step QSO sample selection

• Requirements
• Sample as large as possible
• Minimally biassed against the radio properties
  and the nuclear color of the QSOs
• Observations in multiple bands (from NIR to UV)
  to construct the SED
• Radio detection (RLQs vs. RQQs)
• Negligible host galaxy component
• SDSS quasar catalogue (u, g, r, i, z)
• 2MASS detection (J, H, K)
• FIRST observation area (20 cm flux)

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Distinction between RLQs and RQQs

• 91 of the objects are below the FIRST limit
• RLQ if radio to optical flux ratio gt10 RQQ
  otherwise
• We choose glt18.9, so that we can discriminate
  between RLQs and RQQs

Host galaxy contribution

• Host luminosity estimate based on radio power and
  redshift
• We require that host to nuclear flux ratio lt0.2

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The final sample

• 887 QSOs (774 RQQs and 113 RLQs)

R band absolute magnitude
redshift
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SED construction

• For each object, 8 datapoints log ? log (?Lv)
• from the u, g, r, i, z, J, H, K observations
• Construction of the restframe SEDs of single
  objects
• Normalization of the RLQs and RQQs subsamples at
  1014.8 Hz
• Construction of the average spectral energy
  distributions

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Average SEDs of RLQs and RQQs
log(vLv) relative
log(vLv) erg/s
RLQs
ALL
RQQs
log(v) Hz
log(v) Hz

• RLQs are more luminous and redder than RQQs
• Huge dispersion of the spectral indices
• POWER LAW FIT

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Color difference between RLQs RQQs

• RLQs are redder than RQQs in the NIR to UV region
  with ?a 0.2
• P(KS)gt99
• Redshift independence
• Luminosity independence
• (L z matched samples)

RLQs
RQQs
Spectral index
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SED shape a possible bias

• Request of 2MASS observation only redder objects
  at high z
• Both the SEDs result softer for high z objects
  (i.e. at high frequencies)
• Lets use 2MASS data only at low z!

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Interpretation of the color difference

• Is there an enhanced dust extinction in RLQs?
• Difference of the thermal components?
• Big blue bump superposition of black body
  emission from an accretion disc
• Color difference ? Temperature difference
• Is there a real temperature difference?
• Is the color difference related to spinning?
• Difference of the non-thermal components?
• Is there synchrotron contamination from the
  relativistic jets in RLQs?

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1. Is there an enhanced dust extinction in RLQs?

• ?AV0.16mag would explain the difference
• Why RLQs are more extinted?
• Different inclinations?
• Dust production related to radio emission?

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2. Is there a real temperature difference?

• TdiskMBH-1/4
• BHs of RLQs are supposedly more massive
• RQQs are expected to be hotter (and bluer)

3. Is the color difference related to spinning?

• Radio emission is usually ascribed to faster
  spinning
• Spinning BHs (RLQs) have a shorter last stable
  orbit radius and then a hotter disk ? NO!

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4. Is there synchrotron contamination from the
relativistic jets in RLQs?

• In pole-on radio sources there is a significant
  chance of synchrotron contamination from the
  relativistic jets
• Radio selected samples suffer from a bias towards
  pole-on radio sources (relativistic beaming) but
  in our sample does not!
• ?The color difference between RLQs and RQQs is
  probably due to a real temperature difference of
  the accretion disks.
• NEXT STEP quantify this effect!

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Quasar

• Nuclear luminosity
• Radio power (RLQ RQQ)
• Spectral shape
• BH mass determination and evolution

Host Galaxy

• Bulge luminosity
• (Stellar velocity dispersion, morphology, size)
• Host galaxy luminosity (mass) evolution

Quasar Host Galaxy connection

• Study the BH host mass correlation at low z and
  trace its cosmological evolution close and beyond
  the peak of the quasar activity

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First step BH mass determinations at low z

• Dynamical BH mass determinations
• VIRIAL THEOREM
• Local Universe
• stars orbiting around the SMBH ? only inactive
  galaxies
• Higher redshift
• gas regions emitting the broad lines BLR ?
  Type I AGN!
• v f line-width (Doppler Effect) UV?
  Optical? f ?
• R ? L?a (from reverberation mapping) FWHM?
  s-line?

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Hß broad emission of low-redshift quasars Virial
mass determination and the geometrical
factor(Decarli R., Labita M., Treves A., Falomo
R., 2007, submitted to MNRAS)

• AIM Solid base at low z to study nuclear-host
  connection
• beyond the peak of the nuclear activity
• (see also Labita et al. 2006, MNRAS, 373, 551)
• Are BH mass determinations from Hß and from CIV
  consistent?
• Which is the better estimator?
• FWHM or s-line?
• ? SOLID RECEIPT FOR BH MASS DETERMINATION
• ? HINTS ON THE BLR GEOMETRY
• Do the known correlations between the properties
  of QSOs and their host galaxies hold up to z0.5?

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The Sample

• Quasars, zlt0.7, reliable host galaxy luminosity
  determination, elliptical galaxy
• ?About 40 quasars at ltzgt0.3 of which

25 ASIAGO dedicated observations
UV
29 HST archive spectra
9
2
9
0
12 SDSS catalogue spectra
optical
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Data reduction, measurements and analysis

• Standard IRAF procedure
• Subtraction of the FeII contamination (zero-order
  correction)
• Monochromatic luminosity measurement (power-law
  fit)
• Line-width measurements
• Narrow component subtraction
• 2-gaussian fit of the broad
• component
• FWHM and s-line measurements
• s-line is strongly dependent
• on the line wings

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CIV vs. Hß line shapes and line-widths

• Hß profile is more gaussian (isotropic case)
  than CIV
• R(Hß)1.5 R(CIV) but FWHM(Hß)gtFWHM(CIV)
• The geometries of the Hß and CIV regions are
  intrinsically different

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BH mass host luminosity correlation

• CIV mass estimates are well correlated with MR
• Hß mass estimates are barely correlated with MR
• CIV line-width is a better velocity estimator
  than Hß
• We can constrain f by matching the mass estimates
  via the BH mass host luminosity correlation
• NO redshift dependence of this correlation

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BH mass host luminosity correlation

• CIV mass estimates are well correlated with MR
• Hß mass estimates are barely correlated with MR
• CIV line-width is a better velocity estimator
  than Hß
• We can constrain f by matching the mass estimates
  via the BH mass host luminosity correlation
• NO redshift dependence of this correlation

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Hints on the BLR geometry

• Isotropic model fv3/2 ruled out
• Thin disc model f(?min, ?max) ok for CIV clouds
• For Hß clouds?
• Hß shape
• R vs. FWHM
• Expected angles
• Isotropic component disc component
• Thick disc model

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• The next step QSOs at higher z
• Spectroscopical campaigns (ESO, TNG, NOT) are
  going on to collect the spectra of QSOs with a
  reliable bulge magnitude estimate
• In the meantime

ESO 3.6mEFOSC2
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Quasar

• Nuclear luminosity
• Radio power (RLQ RQQ)
• Spectral shape
• BH mass determination and evolution

Host Galaxy

• Bulge luminosity
• (Stellar velocity dispersion, morphology, size)
• Host galaxy luminosity (mass) evolution

Quasar Host Galaxy connection

• Study the BH host mass correlation at low z and
  trace its cosmological evolution close and beyond
  the peak of the quasar activity

PRELIMINARY!
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BH bulge mass correlation evolution with z
GMBH/Mbulge
log MBH
log G
x
redshift
MR
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BH bulge mass correlation evolution with z
GMBH/Mbulge
log MBH
log G
x
redshift
MR
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BH bulge mass correlation evolution with z
GMBH/Mbulge
log MBH
log G
x
G grows with z ? ?
redshift
MR
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Quasar

• Nuclear luminosity
• Radio power (RLQ RQQ)
• Spectral shape
• BH mass determination and evolution

Host Galaxy

• Bulge luminosity
• (Stellar velocity dispersion, morphology, size)
• Host galaxy luminosity (mass) evolution

PRELIMINARY!
Quasar Host Galaxy connection

• Study the BH host mass correlation at low z and
  trace its cosmological evolution close and beyond
  the peak of the quasar activity

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Host galaxy luminosity (mass) evolution
x
x
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Host galaxy luminosity (mass) evolution
x
x
35
Host galaxy luminosity (mass) evolution
x
x
?
Hint at z2.5 (peak of the nuclear activity),
well formed BHs are hosted by not completely
formed galaxies
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Summary and conclusions (I)

• The NIR to UV continuum of RLQs vs. RQQs
• For a sample of 1000 objects with SDSS 2MASS
  observations
• Average SED construction
• RLQs are more luminous than RQQs
• RLQs are redder than RQQs and this is independent
  on redshift or luminosity
• RQQs seem to be hotter due to smaller BH masses
  (???)
• FUTURE Try to understand better why RLQs are
  redder than RQQs

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Summary and conclusions (II)

• Joint formation and evolution of galaxies and
  SMBHs
• LOW REDSHIFT
• Receipt for BH mass determination
• Known correlations between BH host mass hold up
  to z0.5
• Labita M., Falomo R., Treves A., Uslenghi M.,
  2006, MNRAS, 373, 551
• Decarli R., Labita M., Treves A., Falomo R.,
  2007, submitted to MNRAS
• HIGH REDSHIFT
• Host luminosity (mass?) SEEMS to increases with
  Cosmic Time (???)
• Kotilainen J., Falomo R., Labita M, Treves A.,
  Uslenghi M., 2007, ApJ, 660, 1039
• G SEEMS to decrease with Cosmic Time (???)
• Hint at z2.5 (peak of the nuclear activity),
  well formed BHs are hosted by not completely
  formed galaxies (???)
• FUTURE What will the new observations at higher
  redshift tell us?