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Feb/19/2008
A Demography of Galaxiesin Galaxy Clusters
with the Spectro-photometric Density Measurement.
Joo Heon Yoon 윤주헌 Sukyoung Yi 이석영
Yoon et al. 2008 ApJS in press
(astro-ph/0712.1054)
Dept. of Astronomy Yonsei Univ.
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Environment Effect
Check individual clusters of galaxies.
Require homogeneous catalogue.
I. Motivation
II. Method
III. Result
J. H. Yoon
K. Schawinski
S. K. Yi
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Incompleteness of SpectroscopyI. Motivation
II. Method
III. Result
1. Classical cluster catalogue (e.g. Abell) Based on eye-inspection. Projection effect, time-consuming…
2. Massive database (SDSS, 2dF, …) Systematic Search! Redshift – 3D distribution! (e.g. C4)
Fiber collision!!
Spectroscopy is incomplete!!
In a dense cluster,
fspec. ~ 65%
Incompleteness Problem!!
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1. SDSS DR5 spectroscopic and photometric survey galaxies.
2. 0.05 < z < 0.1
3. Volume limited samples, r<17.77, Mr < -20.54
DataI. Motivation
II. Method
III. Result
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How do we add galaxies missed by spectroscopic survey?
Galaxies in a cluster have Color-Magnitude Relation.
Cluster Member Selection via CMRI. Motivation
II. Method
III. Result
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Cluster Finding with spec.+phot. data
Measure local density of galaxies
where 3σ=1Mpc, and σv = velocity dispersion
2
2
1 1( ) exp
22a
s
r
22
13 3a z
v
r r
For galaxies
with spectra.
For galaxies
without spectra.
Select red-sequence galaxies in CMR2
2
1 1( ) exp
22a
p
r
2
13ar
s p Finding the
Maximum Density Galaxy!!
Finding Galaxy Cluster!!
I. Motivation
II. Method
III. Result
spectro-photometric density
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Cluster Finding with spec.+phot. data
From SDSS
I. Motivation
II. Method
III. Result
Yoon, Schawinski, Sheen, Ree, & Yi, 2008 ApJS in Press (astro-ph/0712.1054)
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Efficiency of the New Measurement
From SDSS
I. Motivation
II. Method
III. Result
CTIO observation supports our method.
92% of completeness by CTIO obs.
New density
Spec. density
CTIO density
missing
A2670
Our new method.
Minimize the incompleteness.
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Galaxy ClassificationI. Motivation
II. Method
III. Result
From SDSS
1. Consider spectroscopic members
2. Visual Inspection- SDSS optical combined images- Self-consistency- fracdev_r
3. Color Classification
4. Non-cluster Galaxies ρ = 0
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Color & Luminosity vs. RadiusI. Motivation
II. Method
III. Result
From SDSS
Color & Luminosity
No clustocentric dependence.
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I. Motivation
II. Method
III. Result
From SDSS
Color & Luminosity vs. Radius
Color & Morphology
Clustocentric dependence < R200
MDR is intrisic. The morphology-density relation
Stronger in Denser cluster
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Why the Brightest Cluster Galaxy?I. Motivation
II. Method
III. Result
From SDSS
von der Linden et al. 2007 : BCG & non-BCG difference
Liu et al. 2007 : Different scaling relations. Quillen et al. 2007 : Star formation in BCGs.
Secondary of environmental effect?
BCGs in simulation Extremely huge Continuously growing BCGs are so special.
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The BCGs vs. DensityI. Motivation
II. Method
III. Result
From SDSS
Denser Brighter BCGs
As well as 2nd BCGs & 3rd BCGs
No difference in their density dependence.
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I. Motivation
II. Method
III. Result
From SDSS
BCGs, 2nd BCGs, & 3rd BCGs are redder
than Non-cluster galaxies.
They are different population.
The BCGs vs. NCGs
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I. Motivation
II. Method
III. Result
From SDSS
CMR of ETGs
Cluster ETGs are optically red.
Non-cluster ETGs have a blue tail.
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I. Motivation
II. Method
III. Result
From SDSS
Environmental Dependence
Gomez et al. 2003
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I. Motivation
II. Method
III. Result
From SDSS
Environmental Dependence
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I. Motivation
II. Method
III. Result
From SDSS
ρ vs. Rclustocentric
R/R200ρ
Red/B
lue
Red/B
lue
g -
r
g -
r
R/R200ρ
Galaxy position
in clusters
Local density effect
on galaxy colors>
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Conclusion
New density measurement. minimize the incompleteness. A better tool for environment study.
New homogenous cluster catalogue. Color radial dependence Morphology-Density relation. Denser Environment Stronger MDR Denser Brighter BCGs Cluster Galaxies Redder than Non-cluster Galaxies. They are
different each other. BCGs and other cluster galaxies.
show the same Mr-density relation. Local galaxy density > Position in cluster
New density measurement. minimize the incompleteness. A better tool for environment study.
New homogenous cluster catalogue. Color radial dependence Morphology-Density relation. Denser Environment Stronger MDR Denser Brighter BCGs Cluster Galaxies Redder than Non-cluster Galaxies. They are
different each other. BCGs and other cluster galaxies.
show the same Mr-density relation. Local galaxy density > Position in cluster
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All color logos
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All color logos
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All color logos
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Measuring Density (Schawinski et al. 2006)
DEC
RA z
DEC
RA z
Line of Sight
1Mpc
I. Motivation
II. Method
III. Result
3 X σ v
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A Demography of Cluster GalaxiesI. Motivation
II. Method
III. Result
From SDSS
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Efficiency of the New Measurement
From SDSS
I. Motivation
II. Method
III. Result
BCGs are generally in centers.
BCG & MDG separation smaller, better.
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Efficiency of the New Measurement
From SDSS
I. Motivation
II. Method
III. Result
CMR efficiency test with spectroscopic, early-type (fracdev_r > 0.95) member galaxies.
Completeness= Purity =
# of members in red-sequence100
# of all members
# of members in red-sequence100
# of all red-sequence
90% cover
15% contamination
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Efficiency of the New Measurement
From SDSS
I. Motivation
II. Method
III. Result
Our new density parameter
Good tracer of cluster size and mass.
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From SDSS
Spectrum analysis Line indices, SFR, etc. ― Clustocentric radius
SH’s SAM clusters with Khochfar’s semi-analytical model vs. Observed clusters Constrain SAM.
Future Study