MOSAIC for the ESO-ELT Franois Hammer (see - - PowerPoint PPT Presentation

MOSAIC for the ESO-ELT

François Hammer (see http://www.mosaic-elt.eu)

Also: Heidelberg/Göttingen, Stockholm/Lund/Uppsala, Helsinki/Turku, Madrid Complutense/IAA, Roma/Arcetri, Vienna, Lisboa/Porto è Last newcomers: Geneva and Univ. of Michigan

Xavier Barcons; EWASS; Liverpool; 12 Avril 2018

Dr Adrian Russell Director of Programmes Phone +49 89 320 06955 arussell@eso.org 25 May 2018 Dear Francois I am writing to confirm that the MOSAIC project has held the Phase A review and the Review Board congratulated the team for the excellent work. As you know there are a number of actions which need to be completed in order to fully define which version of MOSAIC will be

• implemented. These pre-phase B activities are necessary in order to close out on the science

trade-offs and set the final top-level requirements of the instrument. This has been driven by a number of factors, not least is the fact that ESO no longer has the budget to pay for the MOSAIC hardware. We are taking a proposal to the June 2018 Council to allow MOSAIC to be funded externally in return for GTO. Assuming this proposal is met positively then we hope to move rapidly to confirm the top-level requirements and the target budget for fundraising (the two are related of course). Further (joint) work will also be required to define fully the interface to the telescope and help define the requirements of the PFS for Nasmyth B. ESO is still working on the assumption that these pre-Phase B activities will continue smoothly into a GTO funded Phase BCD to completion starting in early 2019 and keep the MOSAIC team fully engaged without any major hiatus. I therefore encourage you to plan the effort availability

• f the team accordingly.

Best wishes Dr Adrian Russell ESO Director of Programmes Cc: Dr Mark Casali Prof François Hammer

Observatoire Paris-Site de Meudon GEPI 5 Pl Jules Janssen 92195 Meudon Cedex France

• 1. Finalize trade-offs
• Comparison with other instruments: to

be complimentary with Harmoni

• Multiplex depends on

mass/volume/budget

• 2. Interfaces with the telescope
• Mass/volume finalized by ESO
• 3. Proposal to ESO Council
• To exchange GTO against FTE &

hardware budget

• Possibility of Public Surveys

Pre-Phase B activities

MOS ‘Principle’

1.

exploits the telescope collecting surface

1.

a moderately good image quality

èTo perform exceptional & unique science advances in 2020s

16 existing ten meter class telescopes: Total surface area = that of the E- ELT!

François Hammer, MOSAIC for ELT, Comité de Suivi

Telescope coating severely limits performance in B, and in the VIS; optimized for METIS. Contract for coating M1 has been cancelled. This justifies limiting VIS to l > 450 nm

Science and final TLRs for MOSAIC

Finalize Trade-offs after comparison with other facilities in the 2020s:

• We have already limited the MOS capabilities mostly because of

(1)Telescope performances (background: no K band, < 1.8 micron, mirror coating: l> 450nm) and (2) Other instruments (comparison with Harmoni shows MOS better for galaxies; fine-tuning of the HDM pixel size)

• Mass/budget imposes us to limit to:

4 NIR Spectrographs + 2 VIS Spectrographs

4 prioritized Science Cases

Inventory of matter (incl. mass assembly) First-light galaxies Extragalactic stellar populations Evolution of dwarf galaxies

Cf Phase A Science Description

Essential to vs. Benefitial to

WEBSIM-COMPASS simulator

HMM=High Multiplex Mode (mono- aperture fibers) HDM=High Definition Mode (IFUs)

http://websim-compass.obspm.fr/

Puech, SPIE, 2016

Physical parameter space Instrument parameter space Observational parameter space

Exploring all the parameter space(s) (N>>10 parameters) for all SCs would be prohibitive in (calculation & human) time

VLT & HST E-ELT & JWST The reionisation of the Universe: first objects

Example: z~9 LAEs/LBGs

z=9 mJ=28 10 hr

z ~ 9 10 hrs z ~ 7 20 hrs Most distant galaxies: MOSAIC, follow-up of JWST imagery: Higher spectral resolution, search for popIII?

IFUs: unbeatable for the best sky subtraction

JAB=28 JAB=26

Simulations: Disseau et al.

From Vanzella et al. 2014

Collecting surface ensures MOSAIC without competitors for faintest sources in NIR

INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE

ILLUSTRIS-TNG

INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE

IGM TOMOGRAPHY

19 March 2018 François Hammer, MOSAIC for ELT, Comité de Suivi

Lyman forest: targets at z=3.5, AB=24.5-25.5 (2-10 hrs) Metallic lines (missing baryons): targets at z= 3.5, AB=24.5-25.5 Simulations: Rahmani et al. (in prep.) AND Simulations: Japelj et al.

19 March 2018 François Hammer, MOSAIC for ELT, Comité de Suivi

z ~ 0.1 Werk et al. 2014 COS-HALO with HST

Distant background galaxy z~3.5 Circumgalactic medium (CGM) ~ 200-300 kpc Adapted from Distant background galaxy z~ 3.5

z ≥ 3

MOSAIC@E-ELT can provide a full understanding

• f the evolution of the

warm/cold gas surrounding galaxies Distant background galaxy

4500 9000

INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE

ILLUSTRIS-TNG

INV INVENT ENTORY OF M MATTER I IN T THE D DISTANT U UNIVERSE

DARK MATTER FROM ROTATION CURVES

GENZEL+17

19 March 2018 François Hammer, MOSAIC for ELT, Comité de Suivi

High definition mode: dark matter evolution from well-sampled rotation curves up to z=4

MOAO is required to provide at least 5 to 7 resolution elements per rotation curve side

Simulations of a z=3.6 L* galaxy with EW=50, 200A, pixel scale =80 to 160 microns Simulations: Wang, Puech et al. IFU ~ 2hrs

Survey speed: MOSAIC will be 8 times faster than HARMONI in doing rotation curves

Puech, Evans et al. SPIE, 2018

A more stringent requirement on multiplex is necessary in the early Universe where galaxies are mostly peculiar, meaning that for 10 galaxies we may expect only 1-4 rotating disks, depending on mass/redshift

Local Universe: the Universal rotation curve had required tens of galaxies in each mass bin (e.g. Salucci et al. 2007)

Stars Cool gas Warm-hot Hot Total baryons 17 100

% Fraction of matter in the local Universe

4500 9000 Redshifted lines (A, z=3.5)

in the distant Universe (%) z=3-3.5

83%

VLT, KECK ELT

At z > 6: witnessing the elaboration of the first super massive black holes

19 March 2018 François Hammer, MOSAIC for ELT, Comité de Suivi

Bright emissions: “dithering” may improve spatial resolution by ~ 2

NGC 55

MOSAIC performance

S/N ~25 S/N ~65 S/N ~140 S/N ~240 S/N >400

MOSAIC performance

Mass, volume & cost issues

MOSAIC multiplex depends first on mass/vol./cost

Full MOSAIC (5 NIR + 5 VIS spectrographs):

• Too heavy (42 tons instead of 40 tons available)
• Too expensive, 32M€ without contingencies!
• Could the Consortium be enlarged?
• ESO limits on GTO would imply 25M€ as a limit for hardware cost
• Would it be better to keep maximal the space of discovery?

MOSAIC multiplex depends first on mass/vol./cost

Full MOSAIC (5 NIR + 5 VIS spectrographs):

• Too heavy (42 tons w/o contingencies, instead of 40 tons available)
• Too expensive, 32M€ without contingencies!
• Could the Consortium be further enlarged?
• ESO limits on GTO would imply 25M€ as a limit for hardware cost
• Would it be better to keep maximal the space of discovery?

Science and final TLRs for MOSAIC

Finalize Trade-offs and comparison with other facilities in the 2020s:

• Mass/budget imposes us to limit to:

4 NIR Spectrographs + 2 VIS Spectrographs

• Very simplified modes (3) for a very powerful instrument:
• Keep High Definition Mode: 8 IFUs in NIR (10 as a goal)

+ High multiplex in both VIS: 80 & NIR: 80+80 (goal: 80 è 100)

IFUs & high multiplex modes

• 80 point like objects in VIS, 160 in NIR (or 80 with 80 sky fibers)
• 8 IFUs with MOAO in NIR (High Definition Mode)
• VIS could be observed simultaneously with HMM-NIR or HDM

Distribution & Operation of observing modes

Fibre link & system complexity

Complexity/risk vs GIRAFFE: + : Adaptive Optics, number of spectrographs, more demanding in sky subtraction

• : less functions in spectrographs (same slit), larger plate scale

Conclusions

• This year 2019: finalize TLRs and prepare the Phase B design
• Budget for hardware almost closed, still few new partners in contact
• Prepare the Consortium: up to 15 countries, 40 Institutes!!!
• Negotiations necessary with ESO for acceding to the telescope
• Both MOS/HIRES are classified as Phase 2 instruments (lower

priorities)

• Also 2019: starting of the survey preparation (130 to 150 GTO nights)
• Requires (young) scientists willing to simulate science of the 2020-30