Integral-field spectroscopy at the resolution limit of large telescopes: the science program of OSIRIS at Keck

OSIRIS (OH-Suppressing InfraRed Integral-field Spectrograph) is a new facility instrument for the Keck Observatory. Starting in 2004, it will provide the capability of performing three-dimensional spectroscopy in the near-infrared z, J, H, and K bands at the resolution limit of the Keck II telescope, which is equipped with adaptive optics and a laser guide star. The innovative capabilities of OSIRIS will enable many new observing projects. Galaxies in the early Universe will be among the most interesting targets for OSIRIS, which will perform detailed studies of their stellar content and dynamical properties. In more exotic objects, such as quasars, radio galaxies, and more nearby active galactic nuclei, OSIRIS can elucidate the relation of the central black hole to the properties of the host galaxy, and the mechanism by which gas is fed into the central engine. In the center of our own Galaxy, it will be possible to search for signatures of interaction between the massive black hole and stars in its immediate vicinity. Closer to home, OSIRIS will perform spectroscopic observations of young stars and their environment, and of brown dwarfs. Imaging spectroscopy of the giant planets, their moons, and asteroids will shed new light on meteorology, mineralogy, and volcanism in the Solar System. OSIRIS observations of Kuiper Belt objects will provide sufficient sensitivity to establish their surface composition, which will contribute substantially to our understanding of the history of the Solar System.

[1]  Andreas Quirrenbach,et al.  Data Reduction Pipeline for OSIRIS, the new NIR Diffraction Limited Imaging Field Spectrometer for the Keck Adaptive Optics System , 2002, SPIE Astronomical Telescopes + Instrumentation.

[2]  Andreas Quirrenbach,et al.  Adaptive optics observations of molecular hydrogen toward T Tauri , 1997, Optics & Photonics.

[3]  Andreas Quirrenbach,et al.  The Nuclear Stellar Core, the Hot Dust Source, and the Location of the Nucleus of NGC 1068 , 1997 .

[4]  Alfred Krabbe,et al.  The Nuclear Cluster of the Milky Way: Star Formation and Velocity Dispersion in the Central 0.5 Parsec , 1995 .

[5]  Claire E. Max,et al.  Titan's atmosphere in Late Southern spring observed with adaptive optics on the W. M. Keck II 10-meter telescope , 2002 .

[6]  David Le Mignant,et al.  Adaptive optics developments at Keck Observatory , 2004, SPIE Astronomical Telescopes + Instrumentation.

[7]  D. S. Acton,et al.  Exploring the Structure of Distant Galaxies with Adaptive Optics on the Keck II Telescope , 2000, astro-ph/0008411.

[8]  A. Pickles,et al.  OBSERVATIONS OF THE OH AIRGLOW EMISSION , 1993 .

[9]  Andreas Quirrenbach,et al.  Stellar Content of the Galactic Starburst Template NGC 3603 from Adaptive Optics Observations , 1998 .

[10]  E. Pecontal,et al.  3D spectrography at high spatial resolution. I. Concept and realization of the integral field spectrograph TIGER. , 1995 .

[11]  A. Quirrenbach,et al.  Image Slicing with Infrared Fibers , 1999 .

[12]  A. Quirrenbach,et al.  Keck Adaptive Optics Observations of the Radio Galaxy 3C 294: A Merging System at z = 1.786? , 2001 .

[13]  Andreas Quirrenbach,et al.  Adaptive Optics Near-Infrared Imaging of R136 in 30 Doradus: The Stellar Population of a Nearby Starburst , 1996 .

[14]  Alfred Krabbe,et al.  The Dark Mass Concentration in the Central Parsec of the Milky Way , 1996 .

[15]  Andreas Quirrenbach,et al.  The Circumnuclear Starburst in NGC 7552: First Results from Near-Infrared Spectral Synthesis , 1997 .

[16]  D. S. Acton,et al.  First Light Adaptive Optics Images from the Keck II Telescope: A New Era of High Angular Resolution Imagery , 2000 .