PAUcam

PAUcam
Enrique Gaztañaga
ICE, IEEC/CSIC Barcelona
for the PAU Survey
Valencia 4 June 2013
1
The PAU@WHT Project in a Nutshell
•
Camera for WHT with 18 (2k*4k)
CCDs covering 1 deg ∅ FoV.
•
42 filters 130Å-wide covering
4300-8600 Å in 6 movable filter
trays, which also include standard
ugrizY filters (+8 UV: 3500-4300)
•
As a survey camera, it can cover
~2 deg2 per night to i~23 in all NB
filters (and i~24 for all ugrizY)
•
low-resolution spectra (Δλ/λ ~ 2%,
or R ~ 50) for >30000 galaxies,
5000 stars, 1000 quasars, 10
galaxy clusters, per night.
•
Expected galaxy redshift resolution
with NB: σ(z) ~ 0.003(1+z) to i~ 23
•
•
Data Management (community)
Science pipeline (end-to-end)
2
PAU@WHT Personnel
PI : E. Fernández (UAB/IFAE)
Co-­‐Is: E. Sánchez (CIEMAT), E. Gaztañaga (IEEC/CSIC), R. Miquel (IFAE/ICREA), J.García-­‐Bellido (IFT/UAM), M. Delfino (PIC)
PAU Camera PI: F. Castander
Project Manager: C. Padilla. Systems Engineer: L. Cardiel
DAQ: J. de Vicente. Mechanics: F. Grañena. Control: O. Ballester. OpLcs and integraLon: R. Casas, J. Jiménez
PAUdm & Science PI: E. Gaztañaga SimulaLons: F. Castander. OperaLons: N. Tonello. Data ReducLon: S. Serrano. QA & ValidaLon: I. Sevilla
The Survey Team
D. Alonso4, J. Asorey2, O. Ballester3, A. Bauer2, C. Bonnett2, A. Bueno4, J. Campa1, L. Cardiel3, J.
Carretero2, R. Casas2, F. Castander2, J. Castilla1, M. Crocce2, M. Delfino5, J.F. de Vicente1, M.
Eriksen2, S. Farrens2, E. Fernández3, P. Fosalba2, J. García-Bellido4, E. Gaztañaga2, F. Grañena3, A.
Izard2, J. Jiménez2, C. López2, L. C. López3, F. Madrid2, M. Maiorino3, P. Martí3, G. Martínez1, R.
Miquel3, C. Neissner5, L. Ostman3, A. Pacheco5, C. Padilla3, C. Pio3, A. Pujol2, J. Rubio4, E. Sánchez1,
D. Sapone4, S. Serrano2, I. Sevilla1, P. Tallada5, N. Tonello5.
1 2 3 4 5
Photometric Redshifts
• Measure relative flux in
multiple filters:
track the 4000 A break
• Estimate individual galaxy
redshifts with accuracy
σ(z) < 0.1 (~0.02 for clusters)
• Precision is sufficient
for 2D Dark Energy probes,
provided error distributions
well measured.
• Good detector response
in z band filter needed to reach
z>1
Elliptical galaxy spectrum
Narrowband Filter System to do Cosmology
Benitez, Gaztanaga, Miquel, Castander, Moles etal ApJ 2009
(PAU and JPAS)
5
Limiting Magnitudes @ WHT (5σ)
g
u
Δz = 0.03
r
100 Mpc/h
i
10000Km/s
z
Δz = 0.003
Y
10 Mpc/h
1000Km/s
2 exposures of ~100 s. Total time: 2 x 4174 s
PAU Science
• Survey strategy produces two samples:
- “Spectroscopic” sample: excellent photo-z’s with NB filters to iAB < 22.7
- “Photometric” sample: medium photo-z’s with BB filters to iAB < 24.1
• Science case depends on amount of time available
• Current science case, assuming 100 nights WHT (200 deg2):
- Use bright sample for redshift-space distortions (typical of spectroscopic
surveys)
- Use faint sample for weak lensing magnification and/or shear (typical of
imaging surveys, e.g. overlap CFHTLS or KIDS North)
- Exploit the gains of cross-correlating both samples on the same area
see Gaztañaga et al. 2012, MNRAS 422 2904 (astro-ph/1109.4852)
A PAU Survey with 200 sqr.deg has 10 times more density or 200
times more area than any current or on/going Spectroscopic Surveys.
8
XTalks in Galaxy Clustering
1. Galaxy Clustering 2pt: 3D, all info but biased
2. Galaxy Clustering 3pt: 3D (bias can be measured)
3. Weak Lensing: 2D (unbiased but degenerate & few 2D modes)
4. Redshift Space Distortions (unbiased but few radial 1D modes)
5. BAO: 1.5 D (unbiased but 1.5D)
Combine (cross-correlate) Photometric &
Spectroscopic Surveys
and all different probes (XTalks)
and all systematics (bias, photo-z, IA)
astro-­‐ph:1109.4852
Photometric Sample i ~ 24
2D lensing
Δz = 0.03
100 Mpc/h
10000Km/s
measure bias
recover full 3D info from 2D+3D
Δz = 0.003
10 Mpc/h
Spectroscopic Sample i ~ 23
1000Km/s
Forecast: Planck+SNII priors
5000 sq.deg. DES depth
WL
RSD
+
BAO
Photometric
DES (i<24)
Spectroscopic
eBOSS+ (i<22.5)
Combine both as
Independent
Shear-Shear
+
GalaxyShear
+
GalaxyGalaxy
WLxG
+
RSD
+
BAO
+
(BIAS IS KNOWN)
RSD+
WLxG+
magnitudes
(eg 3pt)
no lensing/no shear
(eg 3pt)
RSD+
WLxG
0.6
2.4
6
PAU: Cross
Correlated over same
Area
+
(BIAS IS KNOWN)
11 (45)
4/7
5000 sq.deg.
WLxG: shear-shear, galaxy-shear, galaxy-galaxy (including MAG from
counts or MAG from magnitudes and counts)
1.5 (5.3)
200 sq.deg.
astro-­‐ph:1109.4852
William Herschel Telescope (WHT)
• Located in the ORM, La Palma
• Used by UK, Netherlands & Spain
• Highly oversubscribed
• High scientific output so far
• Diameter: 4.2 m
• Prime focus: 11.73 m
• Focal ratio: f/2.8
• FoV: 1 deg ∅, 40’ unvignetted
• Scale: 17.58’’/mm ⬄ 0.26”/pixel
7
(RADIUS)
PAUCam
PAUCam will be mounted
at the prime focus of the
WHT:
Strong limitation in
weight: max. 235 kg
Focal Plane
• Fill the available FoV as densely as
possible
• Use CCDs with the highest QE available
in the whole λ range from u to Y
L. Cardiel-Sas
8
PAUCam Filter System
• 42 (+8 UV) narrow-band filters
• FWHM = 130 Å (100 Å steps)
• Spectral range: λ=4300-8600 Å
• Rectangular transmission profile
• 6 broad-band filters
• ugriZY (SDSS & DES)
10
PAUCam Detectors
Hamamatsu new CCDs:
• 18 4k x 2k 15 µm pixels
• Excellent sensitivity across the entire
wavelength range from 0.3 to over 1 µm.
• 20 delivered, being characterized at
CIEMAT and IFAE
28
PAUCam Filter Trays
Cut-out showing filter-tray movable system
PAUCam
Body of camera made of carbon fiber, shaped to minimize wall thickness
Complete mold (in-house build)
Camera lid mold
20
Camera body in carbon fiber (Teruel-Spain)
Camera lid mold
5e-5mBar
on first test!
Oct 25h
22
PAU$Cam$“telescope$Simulator”$
Jukebox$Installed$
–  Alignment$work$
done$
Simulate$
movements$in$
different$posi@ons$
–  Torques$are$ok$
23
Cristobal$Padilla$J$Ins@tut$de$Física$d'Altes$
4/13$http://www.youtube.com/watch?v=owuRLSnov0Y&feature=youtu.be
Energies$
22$
Op#cal'Bench'
• 
• 
• 
Calibrated'op#cal'path''
Fully'automated'for'CCDs'characteriza#on'tests'(LabVIEW).'
HighEvacuum'cryostat'(<10E6'mbar)'with'low'temperature'error'(±'10'mK)'customized'for'CCDs.''
Op#cal'Path'Layout'
Flat'Field'NonEUniformity'<'2%'
25/04/13'
Cristobal'Padilla'E'Ins#tut'de'Física'd'Altes'
Energies'
24
Op#cal'Bench'
28'
3d#Metrology#bench#
Needed to measure the CCD planarity and in the focal plane
25/04/13#
Cristobal#Padilla#;#Ins=tut#de#Física#d'Altes#
Energies#
25
31#
PAUCam Electronics
Proposed%Final%Version%
%Based%on%AD8066/LT1801%
(Under%Test)%
First%Prototype%
(LMH6552)%
%
Test%Setup
• 
• 
Main%Electronics%Features:%
•  Differen3al%configura3on%
•  Low%noise%(<%27.5uVrms%equivalent)%
•  High%shielded%board%%
•  Even%low%power%consump3on:%
%%%%%LT1801%<%280mW/board%
%
High%Vacuum%Compa3ble:%
•  Gold%coa3ng%
•  No%silkscreen,%stencils%and%protec3on%paint%
•  Low%outSgassing%components%
25/04/13%
Cristobal%Padilla%S%Ins3tut%de%Física%d'Altes%
Energies%
%
26
33%
Lab Infrastructure for DES/PAU
3D metrology bench
Clean room class 10K, 1K, 100
CCD test station
Fully computerized machining tool (lathe)
Addi$onal)Components)
•  The)shu3er)is)fully)
designed)
–  Will)go)into)
produc$on)soon)
•  The)camera)
window)is)delivered)
•  Clean)room)for)
assembly)is)
opera$onal)
25/04/13)
Cristobal)Padilla)E)Ins$tut)de)Física)d'Altes)
Energies)
28
35)
PAUCam Control System
Telescope
Control
System
TCS Int
er
fa
Guider
ObservaUon Control System
ce
Alarms
Image View
and Quality Analysis
GUI
Focal
Plane
Data AcquisiUon
System
5-day
Storage
Transfer
Slow Control
Instrument
Control
System
to PAUdm
Science Data Flow
One computer already installed at the WHT. Tests of interface are taking place. PAU Camera Construction
Many other elements of the camera are either ready:
• Mechanics, vacuum and cryogenics challenges understood.
Final commission in progress
• Optics (entrance window): INAOE done!
• Shutter: design ready, under construction.
• Assembly done in house.
• Electronics is produced
• CCDs in hand and on specs, finishing characterization.
• Filters ordered (some recieved)
• Control system hardware in hand, software integrated.
• Transportation, instal and test tools design and in construction
Data Management System
P.#Tallada#
PAU data management
data management
Status
Goals Achieved
✓ Nightly Processing Pipeline with broad and narrow band photo-calibration
✓ Pixel Simulation Pipeline with main instrumental & atmospheric effects
✓ Community Pipeline able to run in any Unix system (Personal or Cluster)
✓ PAU Archive, Database and Data Transfer protocol
✓ Operation & Orchestration in GRID with ~500 processors in parallel
✓ Web Interface for monitoring, analysis and data distribution
Under work
๏ Multi-Epoch & Multi-Band Pipeline with Global Calibration
๏ Data Transfer monitor & integration tests with PAUcam
๏ Quality Control & Assurance System (and integration with the portal)
๏ Integration of PAU Science codes in operation Framework
System & Pipelines
Commissioning
Pipeline
data management
Web Portal
PAU data management
to
science
Nightly Processing Pipeline
Level 1
products
RAW
Analysis
Pipeline
Pixel Simulation
Pipeline
Storage
& GRID
Data Base
Data Transfer
data
arrival
MEMBA
Multi-Epoch & Multi-Band
Analysis
Level 2
products
d a t a c e n t re
PAU data management
data management
Pixel Simulation of PAUCam (filter z)
Pixel Simulation
Zoom In
PAU data management
Nightly Detrending
Algorithms
Schedule
data management
Quality Control
PAU Pixel Simulation
Nightly Calibration
Global Calibration
MEMBA
Grid Execution
Operation
Commissioning
NFS liberation
Storage Management
Transfer
Data Base
Web portal & data access
Service Operation
DC0
201
DC1
201
DC2
201
DC3
201
DC4
now
more?
201
Galaxy
Sampless & mask
LRG, ELG,c, L, qso
Galaxy
Catalog (SV-DES,
MICE, other)
WP1
Science Pipelines
WP3
loopback
loopback
Photoz
Measured
wij(𝚹), Cl(zi,zi), CIC
z-bin
definition
loopback
WP2
Likelihood
Model
p(ΩΩk) &
WP4
cosmological model
selection & priors p(Ωk)
loopback
WP5
F.Castander
M.Crocce
P.Fosalba
E.Gaztanaga
www.ice.cat/mice
Galaxy MICE simulaUons
DES-MICE v0.3r2.0
Components/Validations:
A very large and high resolution DM sim: clustering
Find halos: validate mass function & clustering of halos
Make Weak Lensing (WL) maps
Assing galaxies to halos (HOD)
Assing WL information to galaxies
38
Dark Matter vs Galaxy
All sky lensing maps
MICE simulations
•
Non-linear (resolution) effects in DM and
galaxy mocks (bias/HOD)
•
•
•
•
•
•
Weak lensing (tangential shear, magnification)
redshift space distortions (photo-z)
galaxy biasing (how light trace de mass)
BAO statistics
3pt-correlations
halo occupation, groups and clusters
Summary
• Construction of PAUCam is well under way.
-
Mechanical, vacuum and cryogenic challenges solved. Camera body in
carbon fiber being tested.
-
CCDs in hand, being characterized. Filters being ordered/delivered.
Control system hardware in hand, software being tested.
• Data managemen/Science Pipeline system developed.
• An MoU with ING was signed 2012.
-
MoU contemplates ample time allocation for the survey (for a price...).
• Compelling science case based on complementarity of
spectroscopic and imaging characteristics.
• Everything is on schedule to comission in late 2013. The survey will
start soon thereafter. The PAU camera at WHT will be the most
powerful imaging instrument at El Roque.
THE END
• Additional slides
43
PAU Survey Strategy
• Use 8 central CCDs to define the survey footprint, use the other CCDs
to increase S/N.
• Each central CCDs covers the whole survey area twice.
• 6 filters trays with 8 central filters (8 NB + 10 BB).
• Broad bands reach ~1.4 magnitudes deeper than narrow bands.
• Detect objects in the broad bands, and then get flux in the narrow
bands.
• Push to low signal to noise.
• Surveying capability: sample 2 deg2 / night to iAB < 22.7 mag in all NBs
and iAB < 24.1 in all BBs ➜ >30000 galaxies / night
• Exposure times depend on tray: ~100 s for bluest, ~250 s for reddest.
• No selection effects.
Photo-z Performance (Faint sample: 22.5 < iAB < 24)
Δz = 0.03(1+z)
100 Mpc/h
10000Km/s
Photo-z Performance (Bright sample: iAB < 22.5)
Δz = 0.003(1+z)
10 Mpc/h
1000Km/s
Redshi, Space Distor5ons (RSD)
Measure both bias and growth!
µ=0
π=0
1.0
Anna Cabré’s PhD Thesis arXiv:0807.3551
BAO: 0.5
FoMγ= 6 Crocce etal 2011
(Forecast for DES: Ross etal 2011)
0.0
radial H(z) H(z=0.34) = 83.8 ±3.0± 1.6
EG, Cabre & Hui (2009) -­‐0.1
Transverse cdz/H(z)
θ(z=0.34) = 3.90 ± 0.38
Carnero etal 2011
∫
19
RSD in 2D
Jacobo Asorey & MarUn Crocce
arXiv:1305.0934
48
Bias from 3-­‐point staUsUcs (2D/3D)
Kai Hoffman & Julien Bel
49