Kilo-Aperture Optical Spectrograph

K.A.O.S. is a highly multiplexed prime focus wide-field multi-object fiber spectrograph concept for one of the state-of-the-art telescopes of the Gemini Observatory.  K.A.O.S. is conceived as a facility instrument that will enable the next generation of spectroscopic surveys.

NEW!!! The KAOS Purple Book describes the main scientific drivers for K.A.O.S. and its technical feasibility.

Main Science Drivers (Killer Applications and Other Science!)

I. Dark Energy 

KAOS can measure the equation of state of the dark energy by measuring the physical length scale of the acoustic oscillations in the galaxy power spectrum at high redshift (z~1 and z~3) and comparing this to the scale at the surface of last scattering (determined by WMAP and Planck). This is a direct metric measure which is largely independent of the sociological habits of galaxies, and provides a constraint on w(z) independent from that provided by supernovae or lensing.

II. Galaxy Genesis

KAOS can determine the primary physical mechanisms responsible for the formation of the thick disk and halo of the Milky Way and M31 by obtaining accurate kinematics and chemical abundances of a million stars.

III. Other Science

Galaxy evolution (0.3 < z < 6.0); large scale structure of galaxies and the IGM; QSO surveys; rare object searches; IMFs in galactic star clusters; dynamics, chemistry and star formation histories of local group galaxies; intracluster stars in Virgo; turbulence in the ISM; mapping the reionization epoch; etc., etc.

KAOS is conceived as a facility instrument: you can use it too!

Basic KAOS Specs

    Field of view 1.5 degree diameter
    Number of fibers
    4,000-5,000
    Resolution
    1,000-40,000

Why Do We Need KAOS?

KAOS is in a class of its own: it  will yield a nearly two order of magnitude gain in information gathering power over that provided by extant or planned facilities and will therefore uniquely position the Gemini community to construct the large spectroscopic samples required to address many key questions in astronomy at the start of the next decade. We can measure the gains resulting from KAOS in two ways: (1) the multiplex advantage resulting from the large number of fibers; and (2) the A-Omega advantage.

KAOS on one of the Gemini Telescopes
Model of KAOS on Gemini: cut-away showing the fiber route and the spectrograph pier lab.

The KAOS Purple Book

The Purple Book describes the main scientific drivers for K.A.O.S. and its technical feasibility.
 

The KAOS Exposure Time Calculator

The KAOS Science Team

Sam Barden (NOAO), Chris Blake (UNSW), Joss-Bland Hawthorn (AAO), Brian Boyle (AAO), Michael Brown (NOAO), Matthew Colless (MSO/ANU), Warrick Couch (UNSW), Len Cowie (IfA/UH), Arjun Dey (NOAO), Daniel Eisenstein (Univ. of Arizona), Ken Freeman (MSO/ANU), Karl Glazebrook (Johns Hopkins Univ.), Buell Jannuzi (NOAO), Francis Keenan (Queens University, Belfast), Rolf Kudritzki (IfA/UH), Eric Linder (Lawrence Berkeley Laboratory), Anna Moore (AAO), David Meyer (Northwestern Univ.), Jeremy Mould (NOAO), Joan Najita (NOAO), Robert Nichol (Carnegie Mellon Univ.), Knut Olsen (NOAO), John Peacock (ROE), Hee-Jong Seo (Univ. of Arizona), Thaisa Storchi-Bergmann (UFRGS, Brasil), Steve Strom (NOAO), Nick Suntzeff (NOAO), Alex Szalay (Johns Hopkins Univ.), Rosie Wyse (Johns Hopkins Univ.)

Are you interested in KAOS?

If you are interested in joining the KAOS science team and contributing to the Purple Book, please send e-mail to Arjun Dey (dey@noao.edu) or Brian Boyle (director@aaoepp.aao.gov.au).

Last updated 2003 Feb 18 by Arjun Dey & Alex Szalay