highlights of recent sdss sciences by jpg
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Highlights of Recent SDSS Sciences by JPG. Yasushi Suto Department of Physics, The University of Tokyo. JPG (Japan Participation Group). Joined SDSS from the beginning Major contributions construction of the mosaic CCD camera fabrication and test of the urgiz filters, electronics, etc. - PowerPoint PPT PresentationTRANSCRIPT
Yasushi SutoDepartment of Physics, The University of Tokyo
Highlights of Recent SDSS Highlights of Recent SDSS Sciences by JPGSciences by JPG
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JPG (Japan Participation JPG (Japan Participation Group)Group)
Joined SDSS from the beginningJoined SDSS from the beginning Major contributionsMajor contributions
construction of the mosaic CCD cameraconstruction of the mosaic CCD camera fabrication and test of the urgiz filters, electronics, fabrication and test of the urgiz filters, electronics,
etc.etc. establishing photometric reference systemsestablishing photometric reference systems Simulation and verification of the photometric Simulation and verification of the photometric
pipelinepipeline Current members (14 in total)Current members (14 in total)
Univ. of Tokyo:Univ. of Tokyo: M.Doi, M.Fukugita, S.Okamura, M.Doi, M.Fukugita, S.Okamura, K.Sato, K.Shimasaku, Y.Suto, N.YasudaK.Sato, K.Shimasaku, Y.Suto, N.Yasuda
Tohoku Univ.:Tohoku Univ.: T.Ichikawa T.Ichikawa Nagoya Univ.:Nagoya Univ.: S.Ikeuchi, T.Matsubara S.Ikeuchi, T.Matsubara National Astron. Obs. of Japan:National Astron. Obs. of Japan: S.Ichikawa S.Ichikawa Others:Others: M.Hamabe, M.Sekiguchi, M.Watanabe M.Hamabe, M.Sekiguchi, M.Watanabe
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A slice of the universe: A slice of the universe: galaxy distribution from SDSS galaxy distribution from SDSS
DR1DR1http://www.sdss.org/dr1/
from Japanese TV program “Science ZERO” (NHK)
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Outline of the talkOutline of the talk
1. Morphology and luminosity dependence of clustering of SDSS galaxies; two-point and three-point correlation functions (Kayo et al.)
2. Topology of large-scale structure from the Minkowski functional analysis of SDSS galaxies (Hikage et al.)
3. Phase correlation of SDSS galaxies (Hikage et al.)
4. SDSS QSO lens survey (Inada, Oguri, et al.)5. Constraining the departure from Newtonian
gravity using SDSS galaxy power spectrum (Shirata et al.)
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major contributors of the major contributors of the results presented in this talkresults presented in this talk
Issha KayoIssha Kayo (Nagoya Univ.) (Nagoya Univ.) 2pt and 3pt galaxy clustering2pt and 3pt galaxy clustering
Chiaki HikageChiaki Hikage (Nagoya Univ.) (Nagoya Univ.) topology and non-Gaussianity of galaxy clusteringtopology and non-Gaussianity of galaxy clustering
Naohisa InadaNaohisa Inada (Univ. of Tokyo) and (Univ. of Tokyo) and Masamune OgMasamune Oguriuri (Univ. of Tokyo & Princeton Univ.) (Univ. of Tokyo & Princeton Univ.) QSO lens surveyQSO lens survey
Akihito ShirataAkihito Shirata (Tokyo Inst. Technology) (Tokyo Inst. Technology) constraining deviation from Newtonian gravityconstraining deviation from Newtonian gravity
Kazuhiro YahataKazuhiro Yahata (Univ. of Tokyo) (Univ. of Tokyo) QSO clusteringQSO clustering
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Part 1Part 1
Morphology and luminosity Morphology and luminosity dependence of clustering of SDSS dependence of clustering of SDSS
galaxies;galaxies; two-point and three-point correlation two-point and three-point correlation
functionsfunctions
Kayo et al. PASJ 56 (2004) 415
77
SDSS DR1 galaxies: SDSS DR1 galaxies: morphology dependent morphology dependent
clustering clustering
from Japanese TV program “Science ZERO” (NHK)
Late-types Late-types in bluein blue
Early-types Early-types in redin red
Density-Density-morphology morphology relation is relation is barely barely visiblevisible
88
Morphology-dependence of galaxy bias from SDSS magnitude-limited
sample
Galaxy bias is fairly scale-independent
Clear morphology dependence with respect to ΛCDM (computed semi-analytically over light-cone) Kayo et al.
(2003)
)CDM(
)(
galaxies
b
early-typeaveragelate-type
Reds
hift-
spac
eR
eal-
sp
ace
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Morphology-dependence of galaxy bias in real space from SDSS magnitude-limited sample
Galaxy bias is fairly scale-independentGalaxy bias is fairly scale-independent Clear morphology dependence: Clear morphology dependence: b=1.2b=1.2~~ 1.5 1.5
for “early”-typesfor “early”-types and and b=0.7b=0.7~~ 0.9 for “late”-0.9 for “late”-typestypes with respect to ΛCDM with with respect to ΛCDM with 88=0.9 (computed =0.9 (computed semi-analytically using the light-cone average described semi-analytically using the light-cone average described before)before) Kayo, Suto, Fukugita, Nakamura, et al. (2003)
)CDM(
)(
galaxies
b
early-typeaveragelate-type
1010
Previous predictions from SPH Previous predictions from SPH simulations with “galaxy” simulations with “galaxy”
formationformation Simulated “galaxies” Simulated “galaxies”
formed earlier are formed earlier are more strongly biasedmore strongly biased
Recently formed Recently formed galaxies preferentially galaxies preferentially avoid high-density avoid high-density regionsregions
Quite consistent with Quite consistent with the morphology- the morphology- dependent galaxy dependent galaxy bias derived from the bias derived from the recent SDSS DR1 !recent SDSS DR1 !
Yoshikawa, Taruya, Jing & Suto (2001)
“Galaxies” formed before z=1.7
(early-types ?)
“Galaxies” formed after z=1.7
(late-types ?)
Dark matter
(r)
b(r) early-types
late-types
1111
Volume-limited samples of SDSS Volume-limited samples of SDSS galaxiesgalaxies
Mr Early Late-22 -21 5881 3897-21 -20 5115 5975-20 -19 1626 3965-19 -18 322 1703
Red Blue-22 -21 7949 8329-21 -20 8930 8155-20 -19 3706 3829
1212
Early > Late Morphological
dependence becomes weaker as galaxies become brighter
Morphology and luminosity dependence of 2PCF of SDSS
galaxies
1313
(all) More luminous, and stronger
(late-type) More luminous, and stronger
(early-type) Very weak luminosity dependence
Luminosity and morphology dependence of 2PCF of SDSS
galaxies
1414
Physical interpretation ?Physical interpretation ?
Biasing is determined by formation epoch + Evolution ??
Luminous galaxy .... Massive Host Dark Halo Luminosity dependence
Evolution of biasing!?
During their long lives, ellipticalsmove around inside dark halos followingdark matter potential of the dark halos. They may forget the original luminosity dependence.
Elliptical ~ bright spirals
Age of bright spirals might be old.
Physical picture of morphology and luminosity dependence remains to be
understood…
1515
Three-point correlation function
321312312
1212123
123
)],,(
)()()(1[
dVdVdVsss
sssndP
The simplest statistics to probe the non-Gaussianity (phase information)
Definite observational results (Groth & Peebles 1977) were obtained more than 25 years ago with no convincing theoretical explanation yet.
Very recent detailed nonlinear models (e.g., Takada & Jain 2003) on the basis of the halo approach
Gaussian
Non-Gaussian
Nonlinear gravity
Nonlinear bias
3
s121 2
s31 s23
1616
Physically expected shape-dependence of Q
large scale: filamentary structure
Q
Θ 1800small scale: spherical halo structure
Q
Θ 1800
1717
Expected scale-dependence of Q Expected scale-dependence of Q from 2PCF of SDSS galaxies (linear from 2PCF of SDSS galaxies (linear
bias)bias)If biasing is simple linear form,
Qg relates to Qm as
If biasing has non-linear form,such as
then
1818
Q ~ 0.5 – 1.5 Weak
dependence on scale of triangles(hierarchical ansatz is valid)
Weak dependence on Luminosity
Weak dependence on Morphology
)()()()()()(
),,(
133221
321
ssssss
sssQred
Three-point correlation functions in redshift space
equilateral triangles
1919
Summary of 3-point correlation Summary of 3-point correlation functions of SDSS galaxiesfunctions of SDSS galaxies
Hierarchical clustering relation holds (QHierarchical clustering relation holds (Q ~~ cconst.)onst.)
Almost no luminosity/morphology dependenAlmost no luminosity/morphology dependencece In contrast, 2-point correlation function is very sIn contrast, 2-point correlation function is very s
ensitive to bothensitive to both bb22 may be correlated with b may be correlated with b11
But redshift-space distortion effect makes sBut redshift-space distortion effect makes significant difference ignificant difference
2020
Part 2Part 2
Topology of large-scale structure from the Minkowski functional analysis
of SDSS galaxies
Hikage et al. PASJ 55 (2003) 911
2121
Topological analyses of LSS in SDSS using Minkowski Functionals (MFs)
A complete set of morphological descriptors d+1 functionals in d-dimensional pattern
In 3d spatial distribution, volume, surface area, mean curvature, and the Euler characteristic (genus)
Complementary statistics to the two-point correlation function (includes the phase information)
Analytic expressions known for Gaussian fields Probe of the non-Gaussianity:
Primordial non-Gaussianity in the initial condition the non‐linearity of the gravitational evolution the non-linearity of the galaxy biasing
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Topology of SDSS galaxy Topology of SDSS galaxy distributiondistribution
Topology of SDSS Topology of SDSS galaxy distribution galaxy distribution (measured with (measured with Minkowski Minkowski Functionals) is Functionals) is consistent with consistent with those originated those originated from the from the primordial primordial random-Gaussian random-Gaussian field in field in CDM CDM (Hikage, Schmalzing, (Hikage, Schmalzing, Buchert, Suto et al.Buchert, Suto et al. 20032003 PASJ).PASJ).
Volume fraction
Surface area
Euler characteristic (genus)
Integrated mean curvature
2323
Luminosity dependence of MFs is weakLuminosity dependence of MFs is weak
No significant luminosity dependence of MFs is detected so far
volumefraction
Surface area
mean
curvature
Euler
characteristic
2,nfluctuatiodensity;,/
-21<Mr<-20-20<Mr<-19-19<Mr<-18
2424
Morphological dependence of MFs is weakMorphological dependence of MFs is weak
2,nfluctuatiodensity;,/
volumefraction
Surface area
mean
curvature
Euler
characteristic
-21<Mr<-20
No significant morphological dependence of MFs is detected so far
2525
SDSS data represent a fair sample of the universe ?
Hikage et al. (2003)
volumefraction
Surface area
mean
curvature
Euler characteristic
volumefraction
Surface area
mean
curvature
Euler characteristic
Difference of MFs for two independent regions of SDSS Two regions in Sample 12 barely converge within the error bars from Mock samples. Encouraging, but larger samples are needed.
Sample 10 Sample 12
2626
Part 3Part 3Phase correlation of SDSS galaxies
(power-point file provided by C.Hikage)
Hikage, Matsubara & SutoApJ 600 (2004) 553
Hikage et al. in preparation
2727
Fourier phases of cosmological density
fluctuations
k
kx
Phase: not well studied inspite of its importance (difficult to quantify, mod. 2π)
kkk exp i
Amplitude: already extensively
discussed in two-point statistics,
i.e., two-point correlation function and power
spectrum
2828
Importance of phases in large Importance of phases in large scale structure of the universescale structure of the universe
Randomize the phases
Scale-independent amplitudes
Simulated density field on meshes
Correlation of Fourier-phases is also essential in the pattern of large scale structure of the
universe
2929
Difficulty of quantifying phase Difficulty of quantifying phase correlations in a direct mannercorrelations in a direct manner
22 cyclic propertycyclic property lose the information of the cumulative phase shift lose the information of the cumulative phase shift
experienced by (nonlinear) gravitational evolutionexperienced by (nonlinear) gravitational evolution Phases vary by the position of the origin in a giPhases vary by the position of the origin in a gi
ven coordinateven coordinate
Thus usually indirect statistics of phase correlThus usually indirect statistics of phase correlationsations higher-order correlation functionshigher-order correlation functions Minkowski functionalsMinkowski functionals
xkkk xxx
3030
Distribution function of phase sumDistribution function of phase sum(Matsubara 2003)(Matsubara 2003)
Phase sumPhase sum invariant by the position of origininvariant by the position of origin
perturbation formula for the distribution perturbation formula for the distribution function of phase sum (Matsubara 2003)function of phase sum (Matsubara 2003)
)0kkk( 21kkk n21 n
23)3(5.1
cos4
1 pOpP 21212121 kkkkkkkk
sampsamp1
3 ~,
V
P
VPPP
Bp
221
21
kkkk
kk
n=3 Order parameter
(Hierarchical ansatz)
3131
Application to SDSS galaxy Application to SDSS galaxy distributiondistribution
5.17rm
5.14rm
Sample 12 (now calculating using sample 14)
Volume limited samples
3232
Mock catalogsMock catalogs
Same geometry as observation Same number density as observationConsidering redshift distortion using velocity information
N-body simulations (Jing & Suto, Kayo)
2563,Gaussian initial condition
Construct mock catalogs with
3333
Luminosity/model dependence of p(3)
Errors:
Sample variance of mock (LCDM) results
3434
Dependence on 8
3535
Summary of the current statusSummary of the current status First attempt to characterize the phase First attempt to characterize the phase
correlation of SDSS galaxies directly using correlation of SDSS galaxies directly using the phase sum distribution functionthe phase sum distribution function
So far the result in good agreement with So far the result in good agreement with CDM model (CDM model (88=0.9)=0.9)
Analysis with sample 14 is in progressAnalysis with sample 14 is in progress
3636
Part 4Part 4SDSS QSO lens survey
(power-point file provided by M.Oguri)
Inada, Oguri, Pindor, et al. Nature 426 (2003) 810
Oguri, Inada, Keeton, et al. ApJ 605 (2004) 78
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Gravitationally lensed quasar
telescope lens object(galaxy or cluster)
source(quasar)
Strong gravitational field around a galaxy or cluster will bend the light path (according to general relativity)A quasar behind a galaxy or cluster can be split into several images (gravitationally lensed quasar)
lensed images
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Number of target QSOs for lens survey
CFHT(Crampton et al.)CFHT(Crampton et al.)
HSTHST(Maoz et al.)(Maoz et al.)
CompoundCompound(Kochanek)(Kochanek)
JVASJVAS(Helbig et al.)(Helbig et al.) CLASSCLASS
(Myers et al.)(Myers et al.)
2dF (Miller et al.) 2dF (Miller et al.) SDSS (we are here)
SDSS (final, spec)
SDSS(final, photo)
exponential growth
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How to find lenses
1.0" < < 3.5" (marginally resolved)
> 3.5" (resolved)
Search stellar objects with similar colors to the quasar
search for extended quasars in the quasar catalog using:
galaxy profile (de-Vau and exp-disk) fitting likelihood PSF fitting likelihood
quasar
similar color object
60" radius
Inada et al, in preparation
Follow-up observations are needed to confirm if these candidates are really lenses or not !
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Current status: new lensed quasars
J1226(Magellan, i)
J0924(Magellan, i)
J1155(Keck, K)
J0903(ARC, i)
J1021(Keck, K)
J1335(Subaru, i)
J0246(Keck, K)
J1138(Magellan, i)
J1001(UH88, I)
J1206(UH88, I)
A
B
CD
J1004(Subaru, i)
A
BD
C
J1650(WIYN, I)
A
B
C
D
AB
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Summary of new SDSS lens (12)
SDSS J0924 Inada et al., AJ 126(2003)666SDSS J0903 Johnston et al., AJ 126(2003)2281SDSS J1004 Inada et al., Nature 426(2003)810SDSS J1155 Pindor et al., AJ 127(2004)1318SDSS J1335 Oguri et al., PASJ 56(2004)399SDSS J1226 Inada et al., AJ submittedSDSS J0246 Inada et al., to be submittedSDSS J1021 Pindor et al., to be submittedSDSS J1001 SDSS J1206SDSS J1138 Burles et al., in preparationSDSS J1650 Morgan et al., AJ 126(2003)2145
Oguri et al., to be submitted Pap
ers
by S
DS
S c
olla
bora
tion
Pap
er b
y n
on-S
DS
S
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Largest-separation lens: SDSS J1004
C
D
A B
C
D
A
B
HST (ACS, I)
HST(NICMOS, H)
First discovery of a quasar lensed by a cluster (and the LARGEST quasar lens discovered so far!)
Subaru (Sprime, gri)
SDSS (i band)
15"
Inada, Oguri, Pindor, et al., Nature 426(2003)810 Oguri, Inada, Keeton, et al., ApJ 605(2004)78
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Prospect for the lens statisticsExpected constrains from lens statistics of all SDSS spec quasars (~80,000 at 0.6<z<4.0)Constraints on M– and M–w (assuming a flat universe) planes Comparable to current SN surveys