1 Palermo 20-22 nd May Looking ahead to MOONS William Taylor on behalf of the MOONS consortium.

1 Palermo 20-22nd May

Looking ahead to MOONS

William Tayloron behalf of the MOONS consortium


MOONS: Multi Object Optical and Near infra-red Spectrograph

Selected by ESO as third generation instrument for the VLT

Operational by 2019

PI: Michele Cirasuolo

Consortium•UK•France•Italy•Switzerland•Portugal•Chile

Primary science cases:

•Galactic Archeology•Galaxy Evolution


Instrument specifics

Parameter Specification

Field of view 25’ diameter (same as FLAMES)

Number of fibres ~1000

Wavelength range 0.8 – 1.8 μm

Throughput > 30%

Fibre diameter 1.05 arcsec

Resolution modes Just “Low” and “High”

Field reconfiguration time < 5 mins


MOONS current spectrograph baseline

4


Fibre positioners


Sky troublesRequire R > 4000 to get continuum between the sky lines

Rodrigues et al., 2012, SPIE

Sky subtraction tests with FLAMES

Proposed A-B-B-A observing strategy

Molecfit – Telluric absorption models

Smette et al., 2014


Galactic science case

Coordinators (past and present):Livia Origlia, Carine Babusiaux, Chris Evans, Lex Kaper

Loosely split into:•The bulge •The inner disc•Stellar clusters •Halo of globular clusters•The Magellanic systems•Dwarf galaxies in the local group?•Tidal streams in the MW?•and more…


Wavelength selection

IR to give:•penetrating power•for cool stars fewer absorption bands, easier to determine continuum (arguably)•potential to build-on (and learn from) APOGEE survey

Low-res mode:•Calcium Triplet commonly used for metallicity estimates•R>a-few-thousand, RSG abundance determination

High-res mode:•To determine different evolutionary processes need to sample certain species•Include a few DIBs•Windows also chosen to avoid strong telluric absorption


Galactic centreH < 15.5 at R~20,000 with a S/N ~ 30 in 1hr

Absorption (Av=0.7mag/kpc; Besancon model)


H<15.5 (MOONS R~20,000)

GAIA follow up

MOONS can access all the GAIA targets in the CaT window


Data setsGAIA, VISTA, UKIDSS, VPHAS, in the future LSST (?) etc.

From VISTA:

•VISTA Variables in the Vía Láctea (VVV)•VISTA Magellanic Clouds (VMC)


ClustersTo observe parameters such as:

•everything discussed in the last 48 hours!

Can do this in both:

•Embedded clusters

•Obscured clusters

Basically: a larger, possibly broader data set


VVV ‘new’ clustersBorissova et al., 2011, A&A

Considerations:

•Small spatial scales

•Cluster membership

•Target numbers

•Target density


S/LMC…Study kinematics and chemical

abundances of both Clouds to

learn about their interaction and

the impact on their evolution

Low metallicity clusters

…and beyondUse RSG as abundance tracers in nearby

local group galaxies


And finally…And finally… possible surveysAnd finally…

Inner Galaxy survey to obtain complete kinematic and chemical screening of the old stellar populations of the inner disc and bulge regions. 1-2 hrs per pointing at R=20,000 in the J- and H-bands (i.e. down to H<15.5 mag) + CaT at R=8,000 for free:

- 50 nights, spectra for ~250,000 stars

Wide-area Gaia survey to follow-up stars observed with Gaia in Thin and Thick disc, tidal streams, the field populations around halo and clusters. 0.5-1hr integration obtain CaT at R=8,000 and simultaneously near-IR low-resolution spectra in J & H-band (i.e. I<21) :

- 50 nights, spectra for ~500,000 stars

Thanks!

1 Palermo 20-22 nd May Looking ahead to MOONS William Taylor on behalf of the MOONS consortium.

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