Fibres - Institut d`Astrophysique de Paris

Two projects of 4-m telescope Optical Multi-Object Spectrograph
WEAVE
4 MOST
Carine Babusiaux
Piercarlo Bonifacio
Vanessa Hill
PNCG Atelier Grand relevés
28 Avril 2014, Paris
4-MOST
4-metre Multi-Object Spectroscopic Telescope
www.4most.eu
PI: Roelof de Jong (Allemagne)
Telescope: VISTA (4m, South)
all-sky public (consortium & community) surveys
large mutiplex, LR & HR, Full optical wavelength coverage, Large FoV
Conceptual Design study for ESO completed 1 Feb 2013
4MOST & MOONS both recommended for next phases
but 4MOST delayed to delta-phase A
2
Main science drivers
•
Gaia follow-up:
Chemo-dynamical structure of the Milky Way
Stellar radial velocities, parameters and abundances (15 < mG < 20 mag)
Chemical tagging (mG < ~16 mag)
•
eROSITA follow-up:
Cosmology with x-ray clusters of galaxies
X-ray AGN/galaxy evolution to z~5
Galactic X-ray sources, resolving the Galactic edge
•
Euclid/LSST/SKA (and other surveys) follow-up:
Dark Energy
Galaxy evolution
Transients
3
Instrument
Wide Field
Corrector
Specification
Concept Design
Field-of-View (hexagon)
2
>4.0 degree (⌀>2.5°)
Multiplex fiber positioner
~2400
Med Resolution Spectrographs
R~5000-8000
# Fibres
1600 fibres
Passband
390-930 nm
High Resolution Spectrographs
Tilting spine
positioner
Fibre
Feed
R~20,000
# Fibres
800 fibres
Passband
395-456 nm & 587-673 nm
High-Res
Spectrographs
Med-Res
Spectrographs
4
Consortium
• Instrument Institutes:
AIP, MPE, LMU, ZAH (D), IoA?, RAL (UK), NOVA/Astron ? (NL), AAO (AU), ESO (EU)
GEPI (F, phase A seulement: design du spectrograph HR),
CRAL (F, en pourparler pour phase B: spectrograph LR),
• Science Institutes
Universities of Lund, Uppsala (S), Groningen (NL)
5
Performances (1h exposure)
stellar
abundances
stellar parameters
stellar radial velocities
galaxy redshifts
6
Planned Surveys
Science case
S/N
rAB-mags
Targets
(Millions)
per Å
MW halo HR
140
12–15.5
0.07
MW halo LR
10
16–20.0
1.5
140
14–15.5
2.1
MW disk/bulge HR
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 galaxies
4
20–22.5
12.8
Total
•
Seven science cases
fully simulated
with observations in parallel
•
More than 30% fibres free for
other ESO community projects
>27
in 5 years (dedicated telescope)
7
Next steps
•
Now:
Preparation for the next development phases
Consortium evolution.
En France: le GEPI se désengage, le CRAL est en discussion pour
prendre la fabrication des spectrographes LR.
•
Early 2014:
Official start of Preliminary Design phase
•
Dec 2015:
Detailed designs finalized
•
Aug 2018:
Full system integrated and verified at AIP, preliminary acceptance Europe
•
Jul 2019:
Delivery and installation at telescope, preliminary acceptance Chili
•
Aug 2019 – Jul 2024:
First science survey of 4MOST, all consortium surveys public,
about 30% of fibres available for the community
8
WEAVE
http://www.ing.iac.es/weave/
PI: Gavin Dalton (RAL, UK)
co-PI FR: Piercarlo Bonifacio (GEPI)
Telescope: WHT (4m, North)
large mutiplex & FoV, LR & HR & IFU, Full optical wavelength coverage
Between phase B & C
9
Science cases
●
Complément au sol pour Gaia:
- Vr haute précision: relevé à R=5,000 d'étoiles 15<V<20
- Abondances chimiques détaillées: relevé à R=20,000 d’étoiles 12<V<17
●
Evolution des Galaxies :
- Relevé WEAVE-APERTIF (Integral-Field-Unit): évolution et propriétés
cinématiques des galaxies
- Relevé WEAVE-LOFAR: évolution des galaxies à formation d’étoiles,
accrétion par les trous noirs centraux, ...
●
Cosmologie:
- Relevé WEAVE-LOFAR: BAO et distorsions dans l’espace des
redshifts, croissance des structures et de l’Univers
10
Instrument overview
11
Specifications
Telescope, diameter
WHT, 4.2m
Field of view
2
2º diameter (3.1degree )
Number of fibers
1000
Fiber size
1.3”
Number of small IFUs, size
~25, 9”x12” (1.3” spaxels)
Large IFU size
~1.5’x1’ (2.6” spaxels)
LR resolution
5 000 (at band center)
LR wavelength coverage
370–1000 (nm)
HR resolution
20 000 (at band center)
HR wavelength coverage
388-435, 600–678 (nm)
12
Low resolution : R = 5 000
σ(vr)<3 km/s at V=20
in 1hr of dark time (V=19 in bright time)
→ full complementarity with Gaia
→ chemo-dynamics
13
High resolution : R = 20 000
S/N>80 / resolution element
at V=17 in ~2 hours
→ abundances to ~0.1
dex
→ chemical labelling
14
Nominal Survey Plan
15
Consortium
PI: G. Dalton (RAL, Oxford, UK)
RAL (UK), NOVA (NL), IAC (ES), ING, INAF(I)
France:
GEPI : Système fibres
Lagrange : Correcteur de champ (Phase A seulement)
16
Timeline
• Phase A kickoff Sept. 2011
• Preliminary Design Review completed: March 2013
• Final stage mid-term review: Feb. 2014
• Final Design Review: July 2015
• MAIT 2013-2017 (blanks commandés)
• Comissioning: July-December 2017
• Survey 2018-2022 (80-100% of telescope time for > 5 years)
17
Costs
18
Two 4-m telescope Optical Multi-Object Spectrograph
4MOST
WEAVE
Telescope
VISTA
WHT
Hemisphere
South
North
FoV
2°.5
2°
Fibres
2400
1000
Modes
Status
Summary
LR : 5 000
HR : 20 000
-
IFU
Phase A/B
Phase B/C
19