Yasushi SutoDepartment of Physics, The University of Tokyo

Highlights of Recent SDSS Highlights of Recent SDSS Sciences by JPGSciences by JPG

22

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

33

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)

44

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.)

55

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

66

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

99

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

2222

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

42

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

43

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