George Brims
University of California, Los Angeles
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Astronomical Telescopes and Instrumentation | 1998
Ian S. McLean; Eric E. Becklin; Oddvar O. Bendiksen; George Brims; John Canfield; Donald F. Figer; James R. Graham; Jonah Hare; Fred Lacayanga; James E. Larkin; Samuel B. Larson; Nancy G. Levenson; Nick Magnone; Harry I. Teplitz; Woon Wong
The design and development of NIRSPEC, a near-IR echelle spectrograph for the Keck II 10-meter telescope is described. This instrument is a large, facility-class vacuum-cryogenic spectrometer with a resolving power of R equals 25,000 for a 0.4 inch slit. It employs diamond-machined metal optics and state-of-the-art IR array detectors for high throughput, together with powerful user-friendly software for ease of use.
Proceedings of SPIE | 2014
James E. Larkin; Jeffrey K. Chilcote; Theodore Aliado; Brian J. Bauman; George Brims; John Canfield; Andrew Cardwell; Daren Dillon; René Doyon; Jennifer Dunn; Michael P. Fitzgerald; James R. Graham; Stephen J. Goodsell; Markus Hartung; Pascale Hibon; Patrick Ingraham; Christopher A. Johnson; Evan Kress; Quinn Konopacky; Bruce A. Macintosh; Kenneth G. Magnone; Jérôme Maire; Ian S. McLean; David Palmer; Marshall D. Perrin; Carlos Quiroz; Fredrik T. Rantakyrö; Naru Sadakuni; Leslie Saddlemyer; Andrew Serio
The Gemini Planet Imager (GPI) is a complex optical system designed to directly detect the self-emission of young planets within two arcseconds of their host stars. After suppressing the starlight with an advanced AO system and apodized coronagraph, the dominant residual contamination in the focal plane are speckles from the atmosphere and optical surfaces. Since speckles are diffractive in nature their positions in the field are strongly wavelength dependent, while an actual companion planet will remain at fixed separation. By comparing multiple images at different wavelengths taken simultaneously, we can freeze the speckle pattern and extract the planet light adding an order of magnitude of contrast. To achieve a bandpass of 20%, sufficient to perform speckle suppression, and to observe the entire two arcsecond field of view at diffraction limited sampling, we designed and built an integral field spectrograph with extremely low wavefront error and almost no chromatic aberration. The spectrograph is fully cryogenic and operates in the wavelength range 1 to 2.4 microns with five selectable filters. A prism is used to produce a spectral resolution of 45 in the primary detection band and maintain high throughput. Based on the OSIRIS spectrograph at Keck, we selected to use a lenslet-based spectrograph to achieve an rms wavefront error of approximately 25 nm. Over 36,000 spectra are taken simultaneously and reassembled into image cubes that have roughly 192x192 spatial elements and contain between 11 and 20 spectral channels. The primary dispersion prism can be replaced with a Wollaston prism for dual polarization measurements. The spectrograph also has a pupil-viewing mode for alignment and calibration.
Proceedings of SPIE | 1993
Ian S. McLean; Eric E. Becklin; George Brims; John Canfield; Suzanne Casement; Donald F. Figer; Frank Henriquez; Anthony Huang; W. Timothy Liu; Bruce A. Macintosh; Harry I. Teplitz
This paper describes a new infrared imaging system being developed at UCLA for use on both the Lick Observatory 3-m telescope and the W.M. Keck 10-m telescope. The instrument has a relatively wide field of view on each telescope and is intended for infrared surveys and deep imaging. To enhance efficiency, the new instrument incorporates a dichroic beam splitter to provide two simultaneous imaging systems, one short-wave (SW) from 1 - 2.5 micrometers and one long-wave (LW) from 2 - 5 micrometers . Each wavelength channel is independently optimized. The SW channel contains a Rockwell NICMOS3 256 X 256 HgCdTe array and the LW channel has an SBRC 256 X 256 InSb array. The thermal design employs a closed cycle cooler. A control and data acquisition system based on transputers and high speed analog electronics is being developed to handle the high data rates.
Astronomical Telescopes and Instrumentation | 2003
A. Mainzer; Ian S. McLean; Ted Aliado; Eric E. Becklin; George Brims; John Goulter; Evan Kress; Nick Magnone; John Milburn; Gunnar Skulason; Michael Spencer
Preliminary test results are reported for FLITECAM, the First Light Camera for SOFIA. This instrument is designed to perform imaging from 1 to 5 μm over the entire 8 arcmin field of view of SOFIA with 0.47arcsec pixels. The detector is a 1024 × 1024 InSb array, and large refractive optics are used for collimation and re-imaging. FLITECAM also has a pupil-viewing mode optimized for 3.5 mm and can accommodate grisms for slit spectroscopy. The instrument has passed Critical Airworthiness Design Review and has received the first part of its certificate of conformity. Ground-based tests of the finished instrument are planned for later in 2002 at the Lick Observatory 3-m Shane Telescope to verify that the point spread function meets its required FWHM of 1 arcsec over the full field and wavelength range. FLITECAM will be used to test the image quality and background of the SOFIA telescope, as well as for science applications.
Proceedings of SPIE | 2014
Emily C. Martin; Michael P. Fitzgerald; Ian S. McLean; Sean M. Adkins; Ted Aliado; George Brims; Christopher A. Johnson; Ken Magnone; Eric Wang; Jason Weiss
NIRSPEC is a high-resolution near-infrared (1-5 micron) echelle spectrometer in use on the Keck II telescope. We are designing an upgrade to the spectrometer, and here we present modeling for the expected performance of the upgraded system. The planned upgrade will (1) replace the Aladdin III science detector with a Teledyne H2RG, (2) update the slitviewing camera (SCAM) detector to an H1RG and replace the optics, and (3) upgrade the instrument control electronics. The new spectrometer detector has smaller pixels but a larger format, and its improved noise characteristics will provide a dramatic increase in sensitivity, especially between OH lines in H-band and shorter wavelengths. Optical modeling shows that the upgraded system is expected to achieve higher spectral resolution and a larger spectral grasp. Also, preliminary modeling of the SCAM optical design aims to permit operation from 1-5 μm, overcoming a limitation with the existing system.
Proceedings of SPIE | 2012
Ian S. McLean; Charles C. Steidel; Harland W. Epps; Nicholas P. Konidaris; Keith Y. Matthews; Sean M. Adkins; Theodore Aliado; George Brims; John Canfield; John Cromer; Jason Fucik; Kristin R. Kulas; Greg Mace; Ken Magnone; Hector Rodriguez; Gwen C. Rudie; Ryan F. Trainor; Eric Wang; Bob Weber; Jason Weiss
New Astronomy Reviews | 2006
James E. Larkin; Matthew Barczys; Alfred Krabbe; Sean M. Adkins; Ted Aliado; Paola Amico; George Brims; Randy Campbell; John Canfield; Thomas M. Gasaway; Allan Honey; Christof Iserlohe; Christopher A. Johnson; Evan Kress; David Lafrenière; Ken Magnone; Nick Magnone; Michael W. McElwain; Juleen Moon; A. Quirrenbach; Gunnar Skulason; Inseok Song; Michael Spencer; Jason Weiss; Shelley A. Wright
Proceedings of SPIE | 2006
James E. Larkin; Matthew Barczys; Alfred Krabbe; Sean M. Adkins; Ted Aliado; Paola Amico; George Brims; Randy Campbell; John Canfield; Thomas M. Gasaway; Allan Honey; Christof Iserlohe; Christopher A. Johnson; Evan Kress; David Lafrenière; James Edward Lyke; Ken Magnone; Nick Magnone; Michael W. McElwain; Juleen Moon; A. Quirrenbach; Gunnar Skulason; Inseok Song; Michael Spencer; Jason Weiss; Shelley A. Wright
Proceedings of SPIE | 2010
Ian S. McLean; Charles C. Steidel; Harland W. Epps; Keith Matthews; Sean M. Adkins; Nicholas P. Konidaris; Bob Weber; Ted Aliado; George Brims; John Canfield; John Cromer; Jason Fucik; Kristin R. Kulas; Greg Mace; Ken Magnone; Hector Rodriguez; Eric Wang; Jason Weiss
Astronomical Telescopes and Instrumentation | 2003
James E. Larkin; A. Quirrenbach; Alfred Krabbe; Ted Aliado; Matthew Barczys; George Brims; John Canfield; Thomas M. Gasaway; David LaFreniere; Nick Magnone; Gunnar Skulason; Michael Spencer; David Sprayberry; Jason Weiss