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HETDEX:AGN-galaxy clustering at 2<z<3.5
Andreas Schulze
Kavli Institute for Mathematics and Physics of the Universe (Kavli IPMU)The University of Tokyo
Workshop "Clustering Measurements of Active Galactic Nuclei"Garching, Germany, 14-18 July 2014
Hobby-Eberly Telescope Dark Energy Experiment
⇒ blind, large-scale spectroscopic survey with VIRUS at HET⇒ 300 square degrees (60 square degrees with spectra) over 3 years
⇒ about 0.75 million redshifts from 1.9 < z < 3.5 (Lyα emitters)⇒ about 1 million redshifts from 0 < z < 0.5 (OII emitters)
⇒ Timeline: 2015-2017
Andreas Schulze (Kavli IPMU) HETDEX 2 / 16
Hobby-Eberly Telescope (HET)
McDonald Observatory, Texasfixed elevation-axis designsegmented primary mirror11.1 x 9.8 m (9.2 m effectiveaperture)
HETDEX⇒ HET upgraded to 22 arcmin
field of view⇒ in progress
⇒ new instrument VIRUS⇒ construction complete byend of 2014
Andreas Schulze (Kavli IPMU) HETDEX 3 / 16
VIRUS instrument
Visible Integral-Field ReplicableUnit Spectrograph (VIRUS)
75 IFUs feeding 150spectrographseach IFU contains 448 fibers(33 600 spectra per shot)3500− 5500 Å at R∼750Line flux limit:3.5× 10−17 erg/cm2/sand mAB ∼ 22
Andreas Schulze (Kavli IPMU) HETDEX 4 / 16
Survey Design
⇒ Spring field:42x7 deg2 with1/4.5 fill factorcentered on13hr, +53deg
⇒ Fall field:28x5 deg2
centered on1.5hr, 0deg
⇒ Fall field with ancillary data in optical (grizy, DES), near-IR (K,NEWFIRM), mid-IR (Spitzer-SHELA), far-IR (Herschel-HeRS)
Andreas Schulze (Kavli IPMU) HETDEX 5 / 16
Constraining Dark Energy with HETDEX
⇒ measure power spectrum of ∼ 800,000 LAEs
⇒ measure H(z = 2.3) and DA(z = 2.3) to 0.9%⇒ constrain evolution of dark energy (wa)⇒ most precise measurements at z > 2
Andreas Schulze (Kavli IPMU) HETDEX 6 / 16
AGN in HETDEX
fully blind IFU spectroscopic survey data from HETDEX enablesmultitude of ancillary science, including AGN
⇒ no preselection required⇒ detection through characteristic emission lines in spectra
type-2 AGN hard to identify([Ne V]3426 line, X-ray, mid-IR, ...)type-1 (broad line) AGN easy to distinguish from LAEs and [OII]emitters⇒ several lines detectable (MgII, CIII], CIV, Lyα) up to z = 3.5⇒ unambiguous redshift identification at z > 1.3
Andreas Schulze (Kavli IPMU) HETDEX 7 / 16
simulated type 1 AGN spectra
⇒ z = 1
4000 4500 5000 5500wavelength λ
400
600
800
1000
counts
g=21
4000 4500 5000 5500wavelength λ
200
300
400
500
600
counts
g=22
4000 4500 5000 5500wavelength λ
100
200
300
400
counts
g=23
⇒ z = 2
4000 4500 5000 5500wavelength λ
500
1000
1500
counts
4000 4500 5000 5500wavelength λ
100
200
300
400
500
600
700
counts
4000 4500 5000 5500wavelength λ
0
100
200
300
400
counts
⇒ z = 3
4000 4500 5000 5500wavelength λ
500
1000
1500
2000
counts
4000 4500 5000 5500wavelength λ
200
400
600
800
1000
counts
4000 4500 5000 5500wavelength λ
0
100
200
300
400
500
600
counts
Andreas Schulze (Kavli IPMU) HETDEX 8 / 16
HETDEX AGN selection
16 18 20 22 24g−band magnitude
100
101
102
103
104
cum
ula
tive
num
berN
(<g)
allz<1.01.0<z<1.9z>1.9
predicted numbercountsmain field: ∼ 20 000 AGN> 10 000 AGN at z > 1no preselection
Predicted HETDEX AGNselection function
21 22 23 24 25
g magnitude (AB)
1
2
3
redsh
iftz
Andreas Schulze (Kavli IPMU) HETDEX 9 / 16
AGN demographics
⇒ excellent sample for statistical studies of type 1 AGN
AGN luminosity function and evolution from 0 < z < 3.5
Evolution of active BH mass function and Eddington ratiodistribution function
AGN-Galaxy clustering
Andreas Schulze (Kavli IPMU) HETDEX 10 / 16
AGN Luminosity function
-8
-7
-6
-5
log
Φ[M
pc−
3m
ag−
1]
z=0.49 z=0.87 z=1.25
-30-25-20MB [mag]
-8
-7
-6
-5
log
Φ[M
pc−
3m
ag−
1]
z=1.63
-30-25-20MB [mag]
z=2.01
-30-25-20MB [mag]
z=2.40
-30-25-20MB [mag]
-8
-7
-6
-5
log
Φ[M
pc−
3m
ag−
1]
z=2.80
-30-25-20MB [mag]
z=3.25
predicted AGN LF for HETDEX mainsurvey (SDSS, VVDS, HETDEX)
AGN Luminosity functionconstrain faint end of AGNLF between z = 2 andz = 3.5 down to g ∼ 24,without preselection
Andreas Schulze (Kavli IPMU) HETDEX 11 / 16
Black hole mass and Eddington ratio distributionfunction
⇒ MBH estimates frombroad lines up toz = 2.5
⇒ determine AGNevolution as functionof MBH and Lbol/LEdd
⇒ probe BH massdownsizing between0 < z < 2.5
-28-26-24-22-20
Mi(z=2) [mag]
-10
-8
-6
-4
log
Φ
7 8 9 10
log M • [M¯]
-8
-6
-4
log
Φ•
-2 -1 0
log λ
-8
-6
-4
log
Φλ
z=1.6z=0.0
0.5 1.0 1.5 2.0 2.5z
-9
-8
-7
-6
-5
-4lo
gΦ
log LBol
44.044.545.045.546.046.547.0
0.5 1.0 1.5 2.0 2.5z
log M •
7.07.58.08.59.09.510.0
0.5 1.0 1.5 2.0 2.5z
log λ
−2.0−1.7−1.4−1.1−0.8−0.5−0.2
Schulze+(in prep.)based on SDSS+VVDS+zCOSMOS
Andreas Schulze (Kavli IPMU) HETDEX 12 / 16
AGN-Galaxy clustering
⇒ within 1.9 < z < 3.5 HETDEX will probe 104 AGN and 106
galaxies (LAEs) in the same volume
⇒ excellent sample for AGN-galaxy clustering at z > 2⇒ construct AGN-LAE 2-point cross-correlation function
(100× increase in power over AGN auto-correlation function)
Ross et al. (2009)
Andreas Schulze (Kavli IPMU) HETDEX 13 / 16
AGN-Galaxy clustering
large scale clustering:⇒ AGN bias factor⇒ relation to DM halos (typical DM halo masses)
small scale clustering:⇒ reach below 1/h Mpc separation => nonlinear regime⇒ Halo occupation distribution (HOD) => constrain AGN fueling and
feedback
good statistics to bin in AGN luminosity, BH mass,. . .
⇒ HETDEX will provide the precise probe of AGN-galaxy clusteringat z > 2
Andreas Schulze (Kavli IPMU) HETDEX 14 / 16
AGN-Galaxy clustering: The MHalo −MBH relation
MHalo from clusteringMBH from spectra
⇒ MHalo −MBH relation at2 < z < 2.5
Current estimate at 1.5 < z < 3based on small samples
Adelberger & Steidel (2005)
Andreas Schulze (Kavli IPMU) HETDEX 15 / 16
Conclusions
HETDEX will start first half 20153 year, massive, blind spectroscopic survey in two fields over300+150 deg2
powerful AGN survey (20000 type 1 AGN in main field)AGN demographics: AGNLF, BH mass and Eddington ratiodistribution function, AGN-galaxy clusteringwithin 1.9 < z < 3.5 104 AGN and 106 galaxies in the samevolume
⇒ HETDEX will provide unique probe of AGN-galaxy clustering atz > 2
Andreas Schulze (Kavli IPMU) HETDEX 16 / 16