Near-infrared integral-field spectrograph (NIFS): An instrument proposed for Gemini

Citation
Pj. Mcgregor et al., Near-infrared integral-field spectrograph (NIFS): An instrument proposed for Gemini, PUBL ASTRON, 16(3), 1999, pp. 273-287
Citations number
25
Language
INGLESE
art.tipo
Article
Categorie Soggetti
Space Sciences
Journal title
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
ISSN journal
1323-3580 → ACNP
Volume
16
Issue
3
Year of publication
1999
Pages
273 - 287
Database
ISI
SICI code
1323-3580(199912)16:3<273:NIS(AI>2.0.ZU;2-R
Abstract
In late 1998 the International Gemini Project Office identified a need for a low cost, near-infrared spectrograph to be commissioned on the Gemini Sou th telescope on the shortest possible timescale. In response, the Research School of Astronomy and Astrophysics of the Australian National University proposed to design, construct, and commission a near-infrared, integral-fie ld spectrograph on Gemini. The science drivers and novel design of the Near -infrared Integral-Field Spectrograph (NIFS) are described in this paper. N IFS will achieve significant economies in cost and schedule in several ways : By addressing targeted science with high efficiency. NIFS will primarily ta rget velocity measurements in galaxies to study the demographics of black h oles in galactic nuclei and the evolution of structural properties in high redshift galaxies. However, NIFS will also be applied to a wide range of ge neral astronomical topics, but these will not dictate the instrument design . By adopting a largely fixed-format design. A 3.2" x 3.2" 'stair-case' integ ral field unit (IFU) will feed a near-infrared spectrograph with four fixed -angle gratings mounted on a single grating wheel. A single, fixed-format c amera will form the spectral image on a 2048 x 2048 Rockwell HgCdTe HAWAII- 2 array. Two-pixel spectral resolving powers of similar to 5400 will be ach ieved with complete wavelength coverage in each of the J, H, and K photomet ric bands through 32 optimally sampled 0.1" wide slitlets. The velocity res olution of similar to 55 km s(-1) will be sufficient to achieve the targete d science objectives, and will allow software rejection of OH airglow lines . By packaging the NIFS instrument within a duplicate of the Near-infrared Im ager (NIRI) cryostat. The NIRI cryostat, On-Instrument Wavefront Sensor (OI WFS), detector focusing mechanism, control system, and EPICS software will all be duplicated with only minimal change. Construction of the duplicate N IRI cryostat, OIWFS, and control system will be done by the University of H awaii.