MOONS - Multi Object Optical and Near-infrared Spectrograph for the VLT

MOONS will be a multi-objects spectrograph mounted at a Nasmyth focus at the VLT. It will have ~1000 fibers deployable over a field of view of ~500 square arcmin. The total wavelength coverage is from 0.6 micron to 1.8 micron, and it will have a low resolution and a medium resolution mode. In the medium resolution mode (R~4,000-6,000) the entire wavelength range 0.65-1.8 micron is observed simultaneously, while the high resolution mode covers simultaneously two selected spectral regions: one around the CaII triplet (at R~9,000) to measure radial velocities, a second at  R~20,000  in the H-band, for detailed measurements of chemical abundances.

 

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Principal Investigators  Michele Cirasuolo (ESO), Jose Afonso (Portugal), Marcella Carollo (Switzerland), Chris Evans (UK), Hector Flores (France), Roberto Maiolino (UK), Ernesto Oliva (Italy), Stephane Paltani (Switzerland), Leonardo Vanzi (Chile)
Project Manager  Alasdair Fairley (UK ATC)
Project Engineer
 Phil Rees (UK ATC)
Consortium
ESO Project manager  Peter Hammersley (phammer@eso.org)
ESO Project scientist
 Vincenzo Mainieri (vmainier@eso.org)
ESO Project Engineer  Gerald Hechenblaikner (ghechenb@eso.org)
Project Status  FDR
Location  Nasmyth focus at UT1, VLT
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MOONS at the Nasmyth platform

Milestones

  • Preliminary Design Review (PDR) – March 2016
  • Final Design Review (FDR) – March 2017
  • Start of scientific operations - end 2020

Instrument Description

MOONS will be a fibre-fed multi-object spectrograph covering from 0.65 micron till 1.8 micron operating from UT1. The instrument consists of a rotating part, which will be mounted on the VLT Nasmyth rotator, and the spectrographs that will be mounted on the Nasmyth platform. The fibre assemblies provide the connection between the rotating part of the instrument and the two static spectrographs.

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The rotating part of the instrument and the cable wrap will collectively be known as the rotating front-end (RFE) of the instrument. It consists of:

  • Field corrector
  • RFE structure and cable wrap
  • Calibration module
  • Acquisition camera module
  • Fibre pick-off module
  • Metrology camera module
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After the setup of the observations by the astronomer, the instrument will move the fibre positioners into the correct position within their own patrol field. The concept of the fibre positioners is two rotating mechanisms, one on the top of the other. The length of the arms has been chosen to maximise the field coverage such taht there are no gaps on the field. The location of the arms can then be verified using a set of cameras placed around the outside of the RFE. The plate must be retracted from the observing position in order to allow space for the camers to work.  

 

 

 

 

 

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Two spectrographs are required due to the large number of fibres. A single cryostat will contein both of them, in order to reduce the overall mass and volume of the instrument. Each spectrographs will simultaneously obtain spectra in the three wavebands, namely RI, YJ and H. A pair of dichroic filters is used to split the light into the three bands. In each band the light will be dispersed and then imaged through a camera onto its associated detector. A CCD detector will be used for the shortest waveband (RI), while Teledyne Hawaii 4RG detectors will be used for the two longer wavebands (YJ and H). The baseline design consists of two optically identical spectrogrphs. Each slit connects to 512 fibres, with a slit length of 200 mm.

 

 

 

 

Baseline Specification

Requirement Baseline Specification
Field-of-View   500 arcmin2
Fibre multiplex per pointing 1000
Smallest target separation <10″
Sky projectsd diameter of each fiber
1.0 arcsec
Wavelength coverage
0.65 - 1.8 micron
Observing modes
medium resolution (MR) and high resolution (HR)

 

Observing Mode / Band Spectral coverage R (at central lambda) Comment
MR-RI 0.647 - 0.955 4,100  Simultaneous in MR mode
MR-YJ 0.934 - 1.350 4,300
MR-H 1.452 - 1.800 6,600
 
HR-I 0.765 - 0.898 9,200  Simultaneous in HR mode
MR-YJ 0.934 - 1.350 4,300
HR-H
1.521 - 1.641 18,300
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Scientific Objectives

MOONS will be a versatile instrument that will provide ESO and the astronomical community with the observational power necessary to tackle a wide range of Galactic, extragalactic and cosmological studies. Some of the main science cases that are driving the MOONS design are the following:

  • Galactic archeology. The study of the resolved stellar populations of the Milky Way and other Local Group galaxies can provide us with a fossil record of their chemo-dynamical and star-fomation histories. MOONS will provide a crucial follow-up for the Gaia mission and for Galactic surveys with the VISTA telescope, delivering accurate radial velocities, metallicitites and chemical abundances for several million stars. The near-IR coverage of MOONS will allow to investigate the nature of the heavily-obscured regions of the Galactic bulge.
  • The growth of galaxies. Tracing the assembly history of galaxies over cosmic time remains a primary goal for observational and theoretical studies of the Universe. Exploiting the large multiplex and wavelength coverage of MOONS will allow for the first time to obtain high quality spectra for a statistically significant number of galaxies (~1 million) at z>1.
  • The first galaxies. The light from the first galaxies, just a few handred million years after the Big Bang is of great importance to understand the cosmic reionization. The unique combination of the 8m VLT aperture, wide-area coverage, and near-IR spectroscopy offered by MOONS will provide accurate distances, relative veleocities and emission-line diagnositcs for statistical samples of z>7 galaxies.

Finally, MOONS will provide the essential deep spectroscopic follow-up of current and future optical and near-IR imaging surveys (e.g. VISTA, VST, Pan-STARRS, LSST) and space mission (e.g. WISE, Athena).

 

References and external links