4MOST - 4m Multi-Object Spectroscopic Telescope 4MOST Spectroscopic Surveys & Asteroseismology - Roelof de Jong (AIP) 4MOST PI
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4MOST – 4m Multi-Object
Spectroscopic Telescope
4MOST Spectroscopic Surveys &
Asteroseismology
Roelof de Jong (AIP)
4MOST PI
Reconstructing the Milky Way’s History,
1–5 June 2015, Bad Honnef www.4MOST.eu
1
4MOST: Wide-field, high-multiplex optical
spectroscopic survey facility for ESO
• Status:
– Preliminary Design Phase started Jan 2015
– ESO Council approval expected June 2015
– Operations start on VISTA telescope 2021 (at least 2x 5 year)
• Science:
– Cosmology, galaxy evolution, high-energy and Galactic science
– Complement large-area space missions: Gaia, eROSITA, Euclid, PLATO
– Complement ground-based surveys: VISTA, VST, DES, LSST, SKA, etc.
• Survey facility:
– Instrument, science operations, data products, science
– Run all-sky 5 year public surveys in parallel, with yearly data releases
– Key surveys organized by consortium in coordination with community
– Add-on surveys from community through ESO peer-reviewed
applications
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 2
Main science drivers
A 5 year 4MOST survey provides
• Euclid/LSST/SKA (and other surveys) complement:
!Cosmology!and!galaxy!evolu6on!
– Dark Energy & Dark Matter (BAO, RSD, lensing, Ly forest)
– !Euclid!
Galaxy evolution (groups & clusters)
– Transients (SNe Ia, GRB)
!VST/VISTA/LSST/SKA!(+other!all&sky!surveys)!
– >13 ×106 spectra of mV~20-22.5 mag LRGs & ELGs
!
• eROSITA complement:
!!– Cosmology with x-ray clusters to z~0.8
!High&energy!sky!
– X-ray AGN/galaxy evolution and cosmology to z~5
!eROSITA!
– Galactic X-ray sources, resolving the Galactic edge
!– 2 ×106 spectra of AGN and galaxies in 50,000 clusters
• !Gaia complement:
!Galac6c!Archeology!
! –– Chemo-dynamics of the Milky Way
Stellar radial velocities, parameters and abundances
!Gaia ! 6
!!– 13 ×10 spectra @ R~5000 of mV~15-20 mag stars
4MOST 2 ×106 spectra
– | Reconstructing @ R~20,000
the Milky Way’s of mV1–5
History, Bad Honnef, ~14-16 mag
June 2015 stars
| Roelof de Jong 3
Main science drivers
A 5 year 4MOST survey provides
• Euclid/LSST/SKA (and other surveys) complement: !
– Dark Energy & Dark Matter (BAO, RSD, lensing, Lyα forest) +!~15!million!
– Galaxy evolution (groups & clusters) spectra!for!
– Transients (SNe Ia, GRB)
community!
– >13 ×106 spectra of mV~20-22.5 mag LRGs & ELGs
proposals!
• eROSITA complement: !
– Cosmology with x-ray clusters to z~0.8 4MOST!is!a!
– X-ray AGN/galaxy evolution and cosmology to z~5 general!purpose!
– Galactic X-ray sources, resolving the Galactic edge spectroscopic!
– 2 ×106 spectra of AGN and galaxies in 50,000 clusters
survey!facility!
• Gaia complement: serving!many!
– Chemo-dynamics of the Milky Way astrophysical!
– Stellar radial velocities, parameters and abundances communi6es!
– 13 ×106 spectra @ R~5000 of mV~15-20 mag stars !
2 ×106 spectra
– | Reconstructing
4MOST the Milky@ R~20,000
Way’s History, Bad of mV~14-16
Honnef, mag
1–5 June 2015 stars
| Roelof de Jong 4
Science Requirements
• 4MOST shall be able to obtain:
– Redshifts of AGN and galaxies (also in clusters)
• R~5000 spectra of 22 r-mag targets with S/N=5/Å with >3 targets in =2’
– Radial velocities of ≤2 km/s accuracy and
Stellar parameters of
4MOST instrument overview
Fibre positioner • New Wide-field Corrector, fibre
positioner and three spectrographs
• Spectrographs mounted on telescope
fork (gravitation invariant)
• Short fibre run (~15 m), prototype
shows very low FRD
Fibre Feed
Wide-Field Corrector
VISTA telescope
High-Res Spectrograph
Low-Resolution Spectrographs
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 6
Instrument Specification Specification Design value Field-of-View (hexagon) ~4.1 degree2 ( >2.5°) Multiplex fiber positioner ~2400 Medium Resolution Spectrographs (2x) R~5000–7000 # Fibres 1600 fibres Passband 390-930 nm Velocity accuracy < 2 km/s High Resolution Spectrograph (1x) R~20,000 # Fibres 800 fibres Passband 392-437 & 515-572 & 605-675 nm Velocity accuracy < 1 km/s # of fibers in =2’ circle >3 Fibre diameter =1.4 arcsec Area (first 5 year survey) >2h x 18,000 deg2 Number of science spectra (5 year) ~75 million of 20 min 4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 7
Wide-field corrector VISTA =2.5°
includes an ADC, A&G, and WFS
Development!AIP!responsibility!
1000nm
Field-edge position
Zenith Distance: 55 degree
Seeing: 0.7 arcsec
Fibre: 1.5 arcsec
=1.5”! 380 nm
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 8
Tilting Spine (Echidna) positioner
• ~2400 fibres
• Large, overlapping patrol areas
enables dense target packing and
special high-resolution fibres
• Closest separation ~15 arcsec
• Reconfiguration time
Dedicated HR and LR spectrographs
• Fixed configuration spectrographs, high throughput with
VPH gratings
4MOST HRS Status
• 3-arm designs with 6k x 6k detectors for both high- and
low-resolution
Optical Layout
HR:!LSW,!Heidelberg! LR:!CRAL,!Lyon!
Blue camera
VPHG
Red camera
Dichroics Corrector
Collimator
Fiber exit
Green camera
3D Layout
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 10Magnitude limits for typical science cases
abundances!
stellar!parameters!
radial!veloci6es!
2o min limit redshiZs! 2 hour limit
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 11How are we going to run 4MOST?
• Unique operations model for MOS instruments that
allows observations for most science cases
• 4MOST program defined by Public Surveys of 5 years
• Surveys will be defined by Consortium and Community
• All Surveys will run in parallel
– Surveys share fibres per exposure for increased efficiency
• Key Surveys will define observing strategy
– Millions of targets all sky
• Add-on Surveys for smaller surveys
– Small fraction fibers all sky
– Dedicated small area
– 103 to 106 targets
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 12How are we going to run 4MOST? • Consortium Surveys will ensure whole hemisphere covered with at least ~120 minutes total exposure time • Each exposure 20 minutes, repeats possible • Total exposures times per target between 20 and 120 min (and more) possible till required S/N • Areas with more targets get visited for more than 120 min • All decided at least ~2 days in advance. Current ESO operations models does not allow ToOs for 4MOST 4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 13
Science verification with full 4MOST
simulator: Design Reference Surveys
Surveys implemented with ~60M objects (coordination Feltzing & McMahon)
• Milky Way halo R>5000 (~3M objects) Helmi, Irwin
– Chemo-dynamics streams
• Milky Way halo R>20,000 (~ 0.2M objects) Christlieb
– Chemical evolution of accreted components
• Milky Way disks/bulge R>5000 (~25M objects) Chiappini, Minchev, Starkenburg
– Chemo-dynamics of bulge/disks
• Milky Way disks/bulge R>20,000 (~2.5M objects) Bergemann, Bensby
– Chemical evolution in situ components
• eROSITA galaxy clusters (~50,000 clusters, ~2.5M objects) Merloni (acting)
– Dark Energy and galaxy evolutions
• eROSITA AGN (~1M objects) Merloni
– Evolution of AGN and the connection to their host galaxies
• Galaxy evolution WAVES (~1.5M objects) Driver, Liske
– Dense magnitude/redshift limited galaxy survey
• Fundamental cosmology science (~23M objects) Kitaura
– Luminous red, blue galaxies, and AGN survey
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 14Simulate throughput, fibre assignment, survey
strategy and verify total survey quality
Targets!
!Science!case! !S/N!!/!Å! rAB&mags! (Millions)!
MW!halo!HR! 140! 12–15.5! 0.07!
MW!halo!LR! 10! 16–20.0! 1.5!
MW!disk/bulge!HR! 140! 14–15.5! 2.1!
MW!disk/bulge!LR! 10–30! 14–18.5! 10.7!
X&ray!galaxy!clusters! 4! 18–22.0! 1.4!
X&ray!AGN! 4! 18–22.0! 0.7!
BAO+RSD!galaxies! 4! 20–22.5! 12.8!
MPE,!Garching,!Boller,!Dwelly!et!al.!
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong
Total! 15>29!Cosmology surveys (~15M objects)
• Dark Energy and General Relativity constraints by measuring
cosmic expansion history and growth of structure:
• Weak Lensing: Photo-z calibrations and characterize the foreground lensing
populations for KIDS, DES, LSST and Euclid. Same sky cross-correlation of
foreground density field & lensing improves constraints 2–4x
• Galaxy Clusters: Redshifts and velocity dispersions of Galaxy Clusters provides
strong constraints on growth rate of structure.
• SNe Ia: Follow-up DES Sne Ia host galaxies and later LSST transients to measure
expansion. 10s of LSST transients per pointing -> 100k transients/year
• BAO and RSD: Use different populations (LRGs, ELGs, AGN, Lα forest) and their
cross-correlation to measure expansion and structure growth
• Concentrate on redshifts zConstraints!on!Dark!Energy!(DE)!&!Modified!Gravity!(MG)!!
Combined!Spectroscopic!and!Deeper!Imaging!surveys
5 2
photo−z ee FoM = 1.6 Spec−z nn FoM = 0.6
spec−z nn FoM = 0.9 Photo−z ee MGFoM = 0.3
4 photo−z + spec−z ee + nn FoM = 7.2 1.8 Photo−z + Spec−z ee + nn MGFoM = 50.1
photo−z x spec−z ee ne nn FoM = 27.8 Photo−z x Spec−z ee ne nn MGFoM = 112.7
3 1.6
2 1.4
1 1.2
Q0(1+R0)/2
wa
0 1
−1 0.8
−2 0.6
−3 0.4
−4 0.2
−5 0
−2 −1.8 −1.6 −1.4 −1.2 −1 −0.8 −0.6 −0.4 −0.2 0 −4 −2 0 2 4 6
w Q0
• Full combination including cross-correlations using same sky
• Same-sky benefit substantial: x4 for DE, x2 for MG vs different hemispheres
• For 15,000 deg2 LSST+4MOST FOM=54 (DE), 383 (MG)
(Kirk, Private Communication)
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 17The Wide Area VISTA Extra-galactic Survey (WAVES)
The WAVES survey of ∼2m galaxies to rAB < 22 mag will be one of the VISTA/4MOST flagship surveys,
Galaxy+DM evolution (WAVES)
and if this LIEF bid is successful it will be led by Australian-based astronomers. The current survey design
consists of two interleaved studies: DEEP-WAVES optimised to probe evolutionary effects and WIDE-WAVES
optimised to probe deep into dark matter halos.
• DEEP-WAVES will cover 100 sq.
deg. to rAB < 22 mag and ex-
tend the power of SDSS-like popu-
• Wide-WAVES
lation statistics out to (VST
z ∼ 1. KiDS
The ∼ area)
–1.2750 deg2will
m galaxies , 0.8M galaxies,
allow for the de-
zeROSITA complement
• German - Russian X-ray mission, Launch late-2015
• 8x all sky survey, 0.5 –10 keV, beam ~25”
• Mission goals: Dark Matter and Energy, growth of structure
• 105 galaxy clusters with >20 redshifts per cluster
• 106 AGN, 106 Galactic sources
• A Stage IV DE experiment
Strong cosmology constraints by cross-calibrating different tracers
• AGN evolution and Galaxy-Black Hole connection
- X-ray (eROSITA
- Redshift determ
- Mass calibration
up)
- Cluster Mass fun
- Cluster Power S
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 19Gaia needs spectroscopic follow-
up to achieve its full potential
• Gaia astrometric mission
launched Dec-2013
– paralaxes and proper motions
for ~1 billion stars to mG1!million!in!the!blue!!
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 20Testing cosmology with Milky Way
dynamics
• Obtaining R~5000 spectra of
>106 stars at |b|>30° allows us to:
– Determine the Milky Way 3D
potential from streams to ~100kpc
– How is DM reacting to baryons:
• has there been significant adiabatic Cooper+ (2010)
contraction?
• is there a disk-like DM component?
• does the DM respond to the bar?
– Determine the mass spectrum of
Dark Matter 103–105 M halo
substructure by the kinematic
effects on cold stellar streams Yoon+ (2011)
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 21HR: Milky Way halo
Yong!et!al.!2013!!
• Observe ~100,000 halo stars with
HR spectrograph
• Metallicity distribution function
– Constraints on Pop III stars (IMF,
rotation)
• Chemo-dynamical substructure
– Identify stream of tidally disrupted
dwarfs
– Early chemical enrichment of
streams (depends on a few stars)
– Accreted versus in situ formation
• Include LMC & SMC + stream
Nissen!&!Schuster!2010!!
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 22
Roelof!de!Jong!|!4MOST! !Milky way bar creates moving
groups in velocity distribution
• So far only done out to
200 pc with Hipparcos
• Gaia combined with
4MOST can do this to
~10 kpc, i.e. in almost
half the Milky Way
Minchev et al. !
(2010)
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 23Milky Way bulge chemo-dynamics
• Two formation scenarios:
– Collapse/merging of proto-galaxies
– Bar instability, disk buckling
• Observe ~150,000 giants,
covering inner 1.5 kpc of the Milky
Way
• Full coverage to understand
effects of reddening and
substructure
• Bulge-halo-thick disk connection?
• Search for chemo-dynamical
substructures
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 24Galaxia based mock catalogues
• Gaia based selection
• Cover all MW components
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 25Observing TESS/PLATO bright sample
• 4MOST saturates for a 10th mag star in a default 20 min
exposure in High Res Spectrograph (HR)
• With 2 min exposures we could cover 7.5th-11th mag stars in HR
– Target densities ~10s-600 per pointing
– ~15 exposures/hour
– 11th-13th mag stars in parallel LR, on average 400 stars/pointing
• PLATO FoV 2250 deg2 = ~600 4MOST pointings = ~40 hours =
~4 bright nights (early release?)
• Entire sky in 40 bright nights
– Can be done in one year using only the 4 nights around full moon
– ~1M HR, ~2M LR objects to 13th mag
• Are repeats useful if we have velocity accuracy of 1 km/s? What
if 400m/s, or 100 m/s?
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 26TESS/PLATO
g. 4. Same as Fig. 3 for the B passband.
stars in twilight?
10!
• 20+ min at
Astronomical!twilight!
Nau6cal!twilight!
V&band!Surface!brightness!(V&mag!arcsec &2)!
beginning and end
of night for bright
15! sample?
• ~8 exps/night ->
Full!moon!
full sky in 30!min!
95! 100! 105! 110!
Sun!Zenith!Distance!(deg)!
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 27Other Science feasible with surveys with thousands to millions of objects • High resolution spectroscopy survey of Open Clusters • Radial velocities time series of low mass binary systems • Star formation history of the Milky Way from 100,000 White Dwarfs • Nature of peculiar variable stars discovered by Gaia, LSST, Euclid • Chemo-dynamics of Magellanic Clouds and other satellites • Follow-up of LSST and Euclid variables/transients • Repeats on deep fields • Reverberation mapping of AGNs • Support Euclid photometric redshift calibrations (for z
Consortium
• Facility Institutes
– Leibniz-Institut für Astrophysik Potsdam (AIP) (D)
– MPI für Extraterrestrische Physik, München (D)
– Zentrum für Astronomie, Univ. of Heidelberg (D)
– MPI für Astronomie, Heidelberg (D)
– Institute of Astronomy, Cambridge University (UK)
– Australian Astronomical Observatory (AU)
– Centre de Recherche Astrophysique de Lyon (F)
– NOVA/ASTRON (NL)
– ESO, Garching (EU)
• Science Institutes
– University of Lund (S)
– University of Uppsala (S)
– University of Groningen (NL)
– L’Observatoire de Paris, GEPI, Paris (F)
– University of Hamburg (D)
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 29Schedule and Milestones
Title Given Planned # Prede Expected Start 2011 2012
!
Duration cessors
!
08 09 10 11 12 01 02 03 04 05 06 07 08 09
• Jan 2015
4MOST concept design
Project Kickoff 5 days
1/9/11
5/9/11
!
– Start Preliminary Design phase
Definition Phase 12/9/11
Refine science requirements 58 days 12/9/11
Determine operational constraints 58 days 12/9/11 Phase!B!
• May 2016:
Prepare sub-component performance estimates 58 days 12/9/11
Implement basic survey simulator 58 days 12/9/11
– Preliminary Design Review, all concepts tested, evaluated, and costed
Prepare requirements and operations documents 58 days 12/9/11 !
Definition Review Meeting 2 days 1/12/11
!
• Dec 2017:
Prelimiary Selection Phase 2 5/12/11
Refine survey simulator 60 days 5/12/11
Define baseline design 40 days 5/12/11
Phase!C!
– Final Design Review, detailed designs finalized
Refine sub-component performance estimates 40 days 5/12/11
Downselect telescope, positioner and spectrograph 5 days 30/1/12
!
• Jan 2020:
Complete reiview documents
Mid-term review and feedback
20 days
5 days
6/2/12
5/3/12 !
Final Selection Phase 9 12/3/12
– All subsystems manufactured, assembled, integrated and verified
Refine survey simulator 75 days 12/3/12
!
Detail selected sub-component study 35 days 12/3/12
• Oct 2020:
Complete selected sub-component technical designs
Perform cost/performace trade studies
35 days
40 days
12/3/12
30/4/12 !
– Full system integrated and verified at AIP, preliminary acceptance Europe
Complete final performance and operations documents 40 days 30/4/12
Final tradeoff review 5 days 25/6/12 Phase!D!
Consolidation Phase 16 2/7/12
• Jun 2021:
Finalise design details
Complete and deliver review documents
20 days
45 days
2/7/12
2/7/12
!
– System delivered and installed on telescope, preliminary acceptance Chili !
!
• Jun 2021 – Jun 2026: !
– First science survey of 4MOST, about 30% of targets determined by Phase!E!
community surveys
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 30Wide-field, high-multiplex optical
spectroscopic survey facility for ESO
• Status:
– Project approved by ESO, PD phase started, operations 2021 (2x 5 year)
• Science:
– Cosmology, galaxy evolution, high-energy and Galactic science
– Complement large area space missions: Gaia, eROSITA, Euclid, PLATO
– Complement ground-based surveys: VISTA, VST, DES, LSST, SKA, etc.
• Survey facility:
– Instrument, science operations, data products, science
– Run all-sky 5 year public surveys in parallel with yearly data releases
– Key surveys organized by consortium in coordination with community
– Add-on surveys from community through ESO peer-reviewed applications
• Instrument specifications:
– High multiplex: 1600 fibres to R~5000 + 800 fibres R~20,000 in parallel
– Wavelength: LR: 390-930 nm, HR: 392-437 & 515-572 & 605-675 nm
– Large field-of-view on VISTA, 4m-class telescope: =2.7°
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 31Special message 4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 32
The Galaxy is BIG • America’s Galaxy is BIG • Africa’s Galaxy is BIG • Australia’s is BIG • Asia’s Galaxy is BIG • Europe’s Galaxy is BIG • Lot’s of work for all of us to do! 4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 33
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 34
Diagnostic tools 4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 35
Diagnostic tools
Fraction of completed targets by redshift bin
1
All
Fraction of targets in bin
0.8
0.6
0.4
0.2 Unobserved
Observed
Completed
0
0 1 2 3 4 5 6
Redshift
1
AGN
Fraction of targets in bin
0.8
0.6
0.4
0.2
0
0 1 2 3 4 5 6
Redshift
4MOST | 1Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong BAO 36Figure-of-Merit (FOM = Metric)
4FS - Survey FoM progress
1 AGN
BAO • Monitor relative
GalHaloLR
GalDiskLR progress to
Clusters
0.8
GalHaloHR
GalDiskHR
assign proper
weights
0.6
Goal!
FoM
0.4
0.2
0
0 200 400 600 800 1000 1200 1400 1600 1800
Day of survey
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 37
4MOST Facility Simulator - OpSimCosmology surveys (~15M objects)
DESI!!
DESI!! (ELG)!
(LRG)!
• Dark Energy and General Relativity constraints by measuring
cosmic expansion history and growth of structure using different
probes:
• Weak Lensing: Photo-z calibrations and characterize the foreground lensing
populations for KIDS, DES, LSST and Euclid. Same sky cross-correlation of
foreground density field & lensing improves constraints 2–4x
• Galaxy Clusters: Redshifts and velocity dispersions of Galaxy Clusters provides
strong constraints 4
onMgrowth
OST!(Lrate of structure.
• SNe Ia: Follow-up DES Sne Ia R G+Egalaxies
host LG)! and later LSST transients to measure
expansion. 10s of LSST transients per pointing -> 100k transients/year
F.!Kitaura!for!4MOST!
• BAO and RSD: Use different populations (LRGs, ELGs, AGN, Lα forest) and their
cross-correlation to measure expansion and structure growth
• Concentrate on redshifts zPlanned Simulation and Analyses Tools
• Consortium provides full forward modelling tools:
– Astronomer provides simulation with selection
observables
– Select targets as for real catalogue
– Create fields and observing schedule including
competition from other surveys
– Apply (simplified?) atmosphere and instrument model
– Apply (simplified?) data reduction and parameter
extraction model
• Is full MCMC modelling needed?
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 39Data release and publication policies
• All raw data immediately public
• All 1D spectra immediately available to all surveys
• 1D spectra released to external public in yearly DRs
• Higher level data products as agreed between individual surveys
and ESO, probably yearly data releases after 1-1.5 yr
• Publication policies similar to Sloan
– First announce science project and papers
– “Builders” (both facility and survey) have opt-in option on papers
– Surveys can have additional rules
• Valid for both Consortium and Community surveys
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 40Background: EU strategic docs
• A Science Vision for European Astronomy (ASTRONET)
– Extreme Universe (Dark Energy & Dark Matter, Black holes)
– Galaxy Formation & Evolution
– Origin of Stars and Planets
– Solar System
• ASTRONET Infrastructure Roadmap%
„A smaller project, but again of high priority, is a wide-field spectrograph
for massive surveys with large optical telescopes.“
• ESA-ESO Working Group on Galactic populations, chemistry and dynamics%
„Blue multiplexed spectrograph on 4 or 8m class telescope“
• Strategic Review on Europe’s 2-4m telescopes over the decade to 2020
(ASTRONET/OPTICON)
„Optical wide-field spectrograph on 4m telescopes (N+S)“
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 41Cosmological constraints by obtaining redshifts
A Stage
and velocity IV DEofexperiment
dispersions galaxy clusters
-•X-ray
X-ray(eROSITA)
(eROSITA) selection
selection -
- Redshift
Redshiftdetermination
determination
-•Mass
Masscalibration (dedicated follow
calibration
up) – (dedicated follow-up)
-•Cluster
ClusterMass function
Mass vs. zvs. z
function
-•Cluster
ClusterPower Spectrum
Power vs. z vs. z
Spectrum
DETF
FoM
(photo-z) 57
(spec-z) 103
174
263
Merloni et al. 2012
Pillepich
4MOST | Reconstructing the Milky Way’s et al. 2012
History,Wide-field Corrector can be inserted
into VISTA like IR camera
4MOST | Reconstructing the Milky Way’s History,Wide-field corrector VISTA =2.5°
includes an ADC, A&G, and WFS
Design!IoA,!King,!Parry,!Sun,!et!al.!
*
*
ADC doublets 401!kg
* *
* * ADC lens
310!kg
Design!AAO,!Gillingham!et!al.!
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 44Unique operational aspects
• All observation preparation including target catalogs,
survey strategy, observing block creation, calibrations
are shared between Surveys
• All data reduction up to 1D calibrated spectra is shared
• Consortium is performing these tasks for both
Consortium and Community Surveys
• We need to perform these tasks absolutely impartially to
avoid conflicts with Community
• ESO requests we perform this for the lifetime of
instrument (~10 years)
• GTO return on this effort (second 5 years) still under
negotiation with ES
– ESO proposes secondment at ESO for Science Operations
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 45Proposals
4MOST ESO
Phase 1 consortium community
Members ESO Public Survey Panel
Targets Members
Targets
Surveys, Priorities
Science
Phase 2 Team
Targets, Survey Strategy
OpSys
Observing Blocks
ESO OB database
Observing OBs valid for the night, Cal OBs
Night
Observation Tool
observer
OB to be executed
4MOST
ICS
Instrument
Raw data (science, calibration)
ESO data archive
Raw data, Observing information
Data Reduction
Spectral Reduction Data Analysis
Reduced spectra
Reduced spectra
Science
Reduction
4MOST archive
High-level products
Reduced spectra
Phase 3 High-level products
Science
Operations
ESO data archive Instrument Control
Data Management
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof deESO
Jong
/ other 46Advantage of the optical wavelength
range
EUCLID
R=250
!
4MOST | Reconstructing the Milky Way’s History,Proposed organisation breakdown
ESO
• Break work into Facility
and Science part ESO
ESO Public
Surveys Panel
• Science gets split
between Survey Teams 4MOST Facility Science
and Infrastructure 4MOST
Executive Board
Working Groups
• Science development Science & Technical 4MOST
4MOST
Science Coordination
overseen by the 4MOST Steering Committee Principal Investigator
Board
Science Coordination
Board (SCB)
4MOST
• ESO Public Survey Project Office Project Scientists
Panel approves all
4MOST Survey Facility Institutes Infrastructure
Coordination Board
proposals
ESO Community Survey Science Infrastructure
Teams Working Groups
Community
Consortium Survey
4MOST Consortium Teams
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 48Competitiveness: Low-Resolution
Informa6on/yr!!!
Area/yr!!!
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 49Competitiveness: High-Resolution
Informa6on/yr!!!
Area/yr!!!
4MOST | Reconstructing the Milky Way’s History, Bad Honnef, 1–5 June 2015 | Roelof de Jong 50You can also read
