KMOS
Science goals:
KMOS is a near-infrared multi-object integral-field spectrometer for one of the ESO Very Large Telescopes. This second-generation instrument will be an invaluable tool to investigate the physical and environmental processes which shape the formation and evolution of galaxies over cosmic time. In fact, its high multiplex capability (up to 24 sources observed simultaneously) is ideal to follow-up large statitistical samples of distant galaxies. The synergy between multi-wavelength imaging surveys and KMOS deep, near-IR integral field spectroscopy will be essential to map the variations in star-formation history, spatially resolved star-formation properties, merger rates and dynamical masses of galaxies at z>1 across a wide range of environments, allowing us to delineate the mass assembly history of galaxies as a function of redshift.
The instrument:
KMOS is being designed and built by a consortium including the Max-Planck Institut für extraterrestrische Physik, the Universitätssternwarte München, the UK ATC, the University of Durham, the University of Oxford and the University of Bristol.
The instrument design employs 24 configurable arms that position pick-off mirrors at user-specified locations in the Nasmyth focal plane. The light collected by these pick-off arms is then fed to 24 advanced image slicer integral-field units (IFUs) and then dispersed by three cryogenic grating spectrometers which generate 14x14 spectra for each of the 24 independent sub-units. The patrol field of the pick-off arms is 7.2 arcmin in diameter, which is the diameter of the unvignetted field at the VLT Nasmyth focus. Each IFU has a square field of view of 2.8x2.8 arcsec, large enough to allow local sky-subtraction for compact high-redshift targets, doubling the effective multiplex gain over systems which require beam-switching. In addition to observing multiple individual sources, KMOS has the capability for integral field mapping of contiguous areas (~1.0 sq. arcmin) in a 24-point dither pattern. This mode would be useful for very extended sources or blank-field surveys for emission-line sources (e.g. Ly alpha at z>7). The spectral resolution of R~3500 provides velocity resolution for studies of low-mass objects and is optimal for OH-avoidance in the J & H bands. Lower resolution modes are also possible and would allow simultaneous coverage of two adjacent bands.
Status and UK-ATC involvement:
The instrument has successfully passed the Final Design Review and entered an advanced assembly phase with final commissioning expected in late 2011. The UK-ATC has a major role in the KMOS project, being responsible among others for the construction of the cryostat, the robotic pick-off arms, the cable co-rotator and the final assembly of the various sub-systems. There are more images available on the Lightbox.
Contacts:
Title |
Name |
Telephone |
|
Project Manager |
Alasdair Fairley |
+44(0)1316688286 |
alasdair.fairley@stfc.ac.uk |
Systems Engineer |
Phil Rees |
+44(0)1316688296 |
phil.rees@stfc.ac.uk |
Instrument Scientist |
Michele Cirasuolo |
+44(0)1316688283 |
ciras@roe.ac.uk |
Quality Manager |
John Murray |
+44(0)1316688251 |
john.murray@stfc.ac.uk |
Lead Mechanical Engineer |
Paul Jeffers |
+44(0)1316688347 |
paul.jeffers@stfc.ac.uk |
Pick-Off Arm Designer |
Richard Bennett |
+44(0)1316688239 |
richard.j.bennett@stfc.ac.uk |
Lead Electrical Engineer |
Naidu Bezawada |
+44(0)1316688235 |
naidu.bezawada@stfc.ac.uk |
Project Assistant |
Lynn Ritchie |
+44(0)1316688442 |
lynn.ritchie@stfc.ac.uk |
Specifications:
Baseline Specification |
|
| Optical Throughput | z>15%, J>20%, H>30%, K>30% |
| Wavelength coverage | 0.8 to 2.5 μm |
| Spectral Resolution | R~3400,3800,3800 (J,H,K) |
| Number of IFUs |
24 |
| Extent of each IFU | 2.8 x 2.8 sq. arc seconds (14 x 14 spatial pixels) |
| Spatial Sampling | 0.2 arc seconds |
| Patrol field |
7.2 arcmin diameter circle |
| Close packing of IFUs | 3 within 1 sq arcmin |
| Closest approach of IFUs | 2 pairs of IFUs separated by 6 arcsec |
| Sensitivity (5σ, 8 hrs, Vega) |
z≈21.0, J≈21.2, H≈21.0, K≈19.2 |
For more information about KMOS please contact Michele Cirasuolo or visit the University of Durham KMOS website.
Applications of Astronomy
13-15 October 2010
This conference will give an overview of technologies and techniques developed in astronomy, highlight the solutions they offer for solving commercially relevant issues, and provide information and guidance on how academics and industry can collaborate to develop future applications.
The conference will include a public lecture from Will Whitehorn, President of Virgin Galactic, on the evening of the 13th October.