Binary Quasars: Does the Halo Occupation Distribution ... · Always roll credits before the movie 2. Clustering of Photometrically Classiﬁed Quasars Clustering on small scales from

A Large Sample of 25 kpc h-1

Binary Quasars: Does the Halo Occupation Distribution

Evolve Over 0.6 < z < 2.3?

A Cosmic Rendezvous, Trieste, April 2012, Adam Myers

Adam Myers, University of Wyoming

Outline1. Credits

Always roll credits before the movie

2. Clustering of Photometrically Classified Quasars Clustering on small scales from a half-million quasars

3. The Halo Occupation Distribution for Quasars And what it implies for angular clustering

4. A New Sample of Binary Quasars And the largest sample on scales of 17.8 kpc h-1–37.3 kpc h-1

5. Future Prospects for Samples of Binary Quasars Can we do even better?


Credits

• Wayne Barkhouse, Jo Bovy, Suchetana Chatterjee, TJ Cox, George Djorgovski, Sareh Eftekharzadeh, Eilat Glikman, Joseph Hennawi, Ryan Hickox, Ashish Mahabal, Daisuke Nagai, Gordon Richards, Jonathan Richardson, Yue Shen, Martin White, Zheng Zheng

Outline1. Credits







Richards et al. (2009)• Using u-g, g-r, and

two other colors r-i and i-z, about 600,000 quasars classified from the Sloan Digital Sky Survey at redshift < 2.5 over one-fifth of the sky

• Classification efficiency >95%

u-g g-r

u-gr-ig-

ir-ig-

ri-z


Photometric Quasar Catalogs

SDSS-1 (DR6/DR7) with Kernel Density Estimation (~500,000 z < 2.5 quasars

in NGC)


Quantifying Structure: Clustering Measurements

• Red Points are, on average, randomly distributed, black points are clustered

• Red points: ω(θ)=0

• Black points: ω(θ)>0

• Varies with (angular) distance, θ (blue circles)

• Red: ω(θ)=0 on all scales

• Black: ω(θ) is larger on smaller scales


Quasar ClusteringMyers et al. (2006, 2007)

Clustering of dark matter

expected at redshift ~1.5

• Used just DR4 imaging

• Shape here is (exquisitely) consistent with cold dark matter, dark energy

• Data is well above black line because quasars are highly biased tracers of large-scale structure

Rprop = 14.7 kpc h-1

R = 35.2 kpc h-1

θ (arcmin)

ωb q

Outline1. Credits







Angular Clustering of DR7 Photometrically Classified Quasars

~500,000 quasars can constrain

clustering on small scales very well without

spectroscopic confirmation

Rprop = 14.7 kpc h-1

R = 35.2 kpc h-1


But not so well split into 4

redshift bins (more on how to circumvent

this later)

0.01 0.10 1.00 10.00 100.00rp [h

-1 Mpc]

0.1

1.0

10.0

100.0

1000.0

10000.0

wp(r

p)

[h-1

Mp

c]

0.01 0.10 1.00 10.00 100.00rp [h

-1 Mpc]

0.1

1.0

10.0

100.0

1000.0

10000.0

wp(r

p)

[h-1

Mp

c]

0.61<z<1.31.3<z<1.61.6<z<1.9

1.9<z<2.27

Angular Clustering of DR7 Photometrically Classified Quasars


HOD constraints over 0.6 < z < 2.3

• Deprojecting and using Richardson et al. (2012)

• Satellites are rare and only found in the most massive haloes

• Jon found similar results using spectroscopicallyconfirmed samples

10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mpc]

10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mpc]

0.61 < z < 2.27

1012 1013 1014 1015

M [h-1 MO • ]

10-4

10-3

10-2

10-1

100

<N

(M)>

CentralSatellite

1010 1011 1012 1013 1014 1015

0.0

0.5

1.0

1.5

2.0

1010 1011 1012 1013 1014 1015

M [h-1 MO • ]

0.0

0.5

1.0

1.5

2.0

dp/d

logM

0.0 5.0 10.0 15.0 20.0fsat x 104

0

1000

2000

3000

dp/d

f sat


10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

0.61 < z < 1.3

1012 1013 1014 1015

M [h-1 MO • ]

10-4

10-3

10-2

10-1

100

<N

(M)>

CentralSatellite

1010 1011 1012 1013 1014 1015

0.0

0.5

1.0

1.5

2.0

1010 1011 1012 1013 1014 1015

M [h-1 MO • ]

0.0

0.5

1.0

1.5

2.0

dp

/dlo

gM

0.0 5.0 10.0 15.0 20.0fsat x 104

0

1000

2000

3000

dp

/df s

at



10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

1.3 < z < 1.6

1012 1013 1014 1015

M [h-1 MO • ]

10-4

10-3

10-2

10-1

100

<N

(M)>

CentralSatellite

1010 1011 1012 1013 1014 1015

0.0

0.5

1.0

1.5

2.0

1010 1011 1012 1013 1014 1015

M [h-1 MO • ]

0.0

0.5

1.0

1.5

2.0

dp

/dlo

gM

0.0 5.0 10.0 15.0 20.0fsat x 104

0

1000

2000

3000

dp

/df s

at



10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

1.6 < z < 1.9

1012 1013 1014 1015

M [h-1 MO • ]

10-4

10-3

10-2

10-1

100

<N

(M)>

CentralSatellite

1010 1011 1012 1013 1014 1015

0.0

0.5

1.0

1.5

2.0

1010 1011 1012 1013 1014 1015

M [h-1 MO • ]

0.0

0.5

1.0

1.5

2.0

dp

/dlo

gM

0.0 5.0 10.0 15.0 20.0fsat x 104

0

1000

2000

3000

dp

/df s

at



10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

10-2 10-1 100 101 102

rp [h-1 Mpc]

10-1

100

101

102

103

104

wp(r

p)

[h-1

Mp

c]

1.9 < z < 2.27

1012 1013 1014 1015

M [h-1 MO • ]

10-4

10-3

10-2

10-1

100

<N

(M)>

CentralSatellite

1010 1011 1012 1013 1014 1015

0.0

0.5

1.0

1.5

2.0

1010 1011 1012 1013 1014 1015

M [h-1 MO • ]

0.0

0.5

1.0

1.5

2.0

dp

/dlo

gM

0.0 5.0 10.0 15.0 20.0fsat x 104

0

1000

2000

3000

dp

/df s

at


Outline1. Credits







Many Observations...

SDSS J1254+0846(Green et al. 2010)

Credit: TJ Cox


Complete on scales of

2.9’’< Δθ < 6’’

for redshifts of 1.2 < z < 2.3

80 SDSS DR7 Binary Quasars with Δθ < 10’’ to g < 21


80 SDSS DR7 Binary Quasars


80 SDSS DR7 Binary Quasars


Complete for 44 Binary Quasars


Clustering precision at ~25 kpc h-1

This sample: 0.6 < z < 1.3

0.8 < z < 2.5 (Hennawi et al. 2006)



0.8 < z < 2.5 (Hennawi et al. 2006)




0.8 < z < 2.5 (Hennawi et al. 2006)




0.8 < z < 2.5 (Hennawi et al. 2006)




0.8 < z < 2.5 (Hennawi et al. 2006)



Quasar Clustering Evolution at 25 kpc h-1


Quasar Clustering Evolution at 25 kpc h-1

Outline1. Credits







Photometric Quasar Catalogs

SDSS-1 (DR6/DR7) with Kernel Density Estimation (~500,000 z < 2.5 quasars)


Photometric Quasar CatalogsSDSS-1 with Kernel Density Estimation

(~500,000 z < 2.5 quasars)


Photometric Quasar CatalogsSDSS-1 with Kernel Density Estimation

(~500,000 z < 2.5 quasars)

State of the art, SDSS-IIIwith Extreme Deconvolution (~1,000,000 z < 3.5 quasars)


Bovy et al. (2012)

1234

P(z)

ugrizSDSS J025717.69−005614.8z=2.3i=19.7

1234

P(z)

+ GALEX UVNUV=25.4NUV SNR=0.3FUV SNR=0.4

1234

P(z)

+ IRK=19.2KSNR=14.2

0.5 1.0 1.5 2.0 2.5z

1234

P(z)

+ GALEX UV + IR

2468

10

ugrizLBQS 0021+0046z=1.6i=18.2

2468

10

+ GALEX UVNUV=19.8NUV SNR=11.6FUV SNR=0.4

2468

10

+ IRK=18.2KSNR=39.6

0.5 1.0 1.5 2.0 2.5z

2468

10

+ GALEX UV + IR

The f weights for counting, here, are calculated by the (comoving) overlap of the PDF and windows placed around each spectroscopic objects


An illustration of utilizing full probabilistic information. Measure the clustering of photometrically classified

quasars around spectroscopically confirmed

quasars

Each photometrically classified quasar is weighted by its overlap with a quasar

of known redshift.

1.0

2.0

3.0 z=1.90 z=2.12200h-1Mpc 200h-1Mpc

f11 = 0.23 f12 = 0.00

0.51.01.52.0

103 f(

χ) (h

Mpc

-1)

f21 = 0.16f22 =0.18

3200 3400 3600 3800 4000χ (h-1Mpc)

1.02.03.04.05.0

f31 = 0.03 f32 = 0.64

Pair Weighting

103 f

(χ) (

hMpc

-1)

χ (h-1Mpc)

Myers et al. (2009)

A Large Sample of 25 kpc h-1

Binary Quasars: Does the Halo Occupation Distribution

Evolve Over 0.6 < z < 2.3?


Adam Myers, University of Wyoming

Documents

Binary Quasars: Does the Halo Occupation Distribution ... · Always roll credits before the movie 2. Clustering of Photometrically Classiﬁed Quasars Clustering on small scales from