Download Gemini IFU Observations of Feedback from Radio

Gemini IFU Observations of Feedback
from Radio-Quiet Quasars at z~0.5
Black Hole Feedback 2012
Guilin Liu
JHU/CAS
Nadia L. Zakamska
JHU/CAS
Jenny E. Greene
Princeton
Nicole P. H. Nesvadba
Insitut d'Astrophysique Spatiale
Xin Liu
CfA/Hubble Fellow
Thirst for Quasar Feedback:
Galaxy luminosity function
Bright end needs mass-dependent quasar feedback to quench SF!
+ SNe
+ SNe + AGN
Croton et al. 2006 (as taken from
Guinevere Kauffmann's talk)
+ SNe + AGN +
Reionization
Thirst for Quasar Feedback:
BH mass-buldge correlation
• Fact
– BH masses in nearby galaxies
strongly correlate with many
galaxy properties
• Implication
– BH evolution has profound
effects on galaxy formation
MBH
• LBuldge / Msph / σc / re ...
• Puzzle
– Physical mechanism?
– masses / sptial scales vastly
different
– need galaxy-wide feedback
σ (km s-1)
Gultekin et al. 2009
Thirst for Quasar Feedback:
To reproduce BH-galaxy correlation...
• Thermal heating?
– 5% × quasar energy is sufficient
to expell gas and quench SF
– Hopkins et al. 2006, ClaudeAndre Faucher-Giguere's talk
• Momentum-driven?
– < 1% × quasar energy is
sufficient
– Zubovas & King 2012, J. Ostriker
and his group
• Radio jets?
– strong: radio galaxies / RL
quasars
– weak: NGC 3079 (?)
Hopkins et al. 2006
unobscured
(Type 1)
Radio-loud objects
Jets can do serious damage to galaxy
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obs pe 2
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Jet-driven winds induces bow-shock and
cocoon, deposit mechanic energy into
ISM/IGM
- both in observations and simulations
Urry & Padovani 1995
Geibler 2011
Radio-loud objects
Jets can do serious damage to galaxy





turbulent outflows detected at z~2
emision regions follow the jet
physical scales are tens of kpc
velocity ~ 1000 km/s, dispersion ~ 1000 km/s
kinetic energy ~1060 erg
Nesvadba et al. 2006, 2008
Standard wisdom
Stockton & MacKenty found
 ~30% RL quasars have
"extended emission line
regions" (~50 kpc)
 RQ quasars don't have
them
 photoionized by nucleus
 galaxy-scale winds driven
by radiation?
But only ~10% quasars are radio-loud...
Stockton & MacKenty 1987
Our Gemini IFU Observations
11 SDSS RQ (+3 RL)
quasars that are:
– obscured (type 2)
– highly luminous
• Lbol~1047 erg/s or
higher
• mass dependent
feedback expected
– from Zakamska et al.
(2003) and Reyes et
al. (2008) catalogs
Integral field
spectroscopy @
Gemini
– FoV: 5"×7"
– seeing 0.4"-0.6"
– spectral resolution
~50 km/s
Credit: Durham Univ.
[O III] 5007Å
Intensity
Maps
Radio-Quiet
Quasars
extended ionized
nebulae seen in
EVERY case;
regular and round
morphology
physical extents of
20-40 kpc
All objects
are
spatially
resolved
Radio-Loud
Quasars
Liu et al, in prep
RQ
Quasars
Zakamska et
al, in prep
Well-organized velocity fields, signature of outflows (| Δv| ≤ 100
km/s)
[O III] 5007Å Radial Velocity Maps
Radial Velocity
FWHM
duoL- oi da R
Nesvadba et al. 2008
RQ vs. RL Quasar
Outflows
• Comparable
outflow extent:
– 20 - 40 kpc
• Similar velocity
dispersion:
– up to ~1000 km/s
ei u Q- oi da R
• RQ quasars
have larger
opening angles
Zakamska et al, in prep
RQ vs. RL Quasar Nebulae
• 3 RL objects at
z=2-3
– Nesvadba et al.
2008
• Size
– similar at z~0.5
– smaller than
z=2-3 RLs
• Ellipticity
– RQ: ε < 0.25
– RL: ε > 0.25 or
irregular
– one exception
Liu et al, in prep
Galaxy-Wide Outflowing Gas
Ionized Gas vs. Host Galaxy
• Size: [OIII] > continuum
• Ellipticity: ~ same
– only one exception
– [OIII] ~ 2.1 × Continuum
– regular and round
– ε ~ 0.1
Liu et al, in prep
Size-Luminosity Relation
isophotal radius
at 10-15/(1+z)4
erg/s/cm2/□"
 power index = 0.24 ± 0.02
 theoretical expectation: 0.5
 matter-bounded?
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Liu et al, in prep
RQ quasar outflow: Why not observed before?
• Sensitivity?
– narrow-band imaging shallower than
long-slit spectroscopy and IFU
• Luminosity dependence?
– Villar-Martin, Humphrey et al. found
<20% at lower luminosities
– 0.8 dex increase in [OIII], detection
fraction changes <20% to >50%
• Viewing angle?
– type 2's more favorable?
• Fooled by long-slit data?
– limited spatial information
Humphrey et al, 2010
Next Steps
• Go for unobscured quasars
– Evolution?
• Gemini IFU (PI: Liu) - approved
• Continue observing low-z high-L obscured quasars
– star formation:
• Herschel (PI: Zakamska) - approved
– molecular outflow:
• ALMA (PI: Greene) - approved
– weak jets?
• Karl G. Jansky VLA (PI: Liu) - approved
• Probe higher redshifts
– newly identified obscured quasars at z=2-3 from BOSS
• HST (PI: Michael Strauss) - approved
• ALMA (PI: Zakamska) - pending
Summary
 Galaxy-wide quasar feedback will save theorists
 Jets from RL objects are seen to have strong effect on
ISM/IGM
 RL objects are rare, what about RQ quasars?
 RQ quasars at highest luminosity commonly have
outflows that are galaxy-wide, round, and likely
energetic