However, providing two superb telescopes is only part of the job. If Gemini is to attain this prominent role in astronomy, the telescopes must be operated in a fashion to allow the partner communities to effectively and efficiently carryout frontier observations, and the Gemini instrumentation capabilities have to continue to evolve to exploit new scientific opportunities and technology developments as they become available.

The capabilities of the initial complement of instrumentation (Table 1) will allow the Gemini communities to undertake the broad range of scientific programs identified in the Gemini Science Requirements Document. The on-going instrumentation program is intended to provide the key capabilities beyond those offered by the Phase I instrumentation that will keep the Gemini facilities at the forefront of astronomical research well into the 21st century.

Table 1. Gemini Phase I Instrumentation
Instruments		Wavelength Range	Array Format	Pixel Scale		FOV/Slit Length	Spectral Resolution	Other Capabilities	Upgrade Options
MAUNA KEA
Multi-Object Spectrograph (GMOS-N)		0.4 - 1.1µm	4k x 6k CCD	0.08"		5.5’ x 5.5’	R~1 k (3 pix) R~3k (3 pix) R~10k (3 pix)	~200 multi slits 0.2" pix IFU	1-1.5µm 0.1" pix IFU
								Imaging
Near IR Imager (NIRI)		1 - 5.5µm	1k x 1k InSb	0.02" 0.05 0.11		20" x 20" 50" x 50" 110" x 110"	Filters to R~100	R~700 grism Polarizing prism Near IR WFS (t/t) Coronagraph
Near IR Spectrograph (NIRS)		1 - 5.5µm	1k x 1k InSb	0.05" 0.15"		50" 100"	R=2k, 6k, 18k R=0.7k, 2k, 6k.	X Dispersion Polarizing Prism Near IR WFS (t/t)	1 - 2.5µm 0.05" pix IFU R~30k
Adaptive Optics System (AOS)		1 - 2.5µm 0.8 - 5.5µm (goal)				2' dia		natural guide star conjugation to alt. feed all inst. ports 0.5 - 2.5µm ADC	Laser Beacon
			SR=0.4 at 1.6 um, median seeing and bright guide stars
CERRO PACHON
Multi-Object Spectrograph (GMOS-S)	0.38 - 1.1µm		4k x 6k CCD		0.08"	5.5' x 5.5'	R~ 1 k (3 pix) R~3k (3 pix) R~10k (3 pix)	~200 multi slits 0.2" pix IFU	1 - 1.5µm 0.1" pix IFU
								Imaging
High Resolution Optical Spectrometer (HROS)	0.30 - 1.1µm		4k x 4k CCD			60"	30k - 80k	Cass mounted Prism X Dispersion	R= 120k Multi object Hi Stab Lab Feed Polarizing Prism
Mid-IR Imager	8 - 25µm		~256 x 256		0.13"	40" x 40"	Filters to R~100

In order to ensure the continuing relevance of the Gemini On-going Instrumentation Program, international scientific reviews will be held every two years, providing an opportunity to reevaluate the content and direction of the instrumentation program from a scientific and technical perspective, taking into account changing scientific opportunities, the evolution of technology opportunities, the status of the on-going instrumentation activities, and the availability of funds. The First of these International Gemini Instrumentation Workshops was held at Cosener's House, Abingdon, England on 18, 19 January 1997.

The Workshop assumed that the Gemini Phase I instrumentation program, which is currently in process, will be completed in full.

Section II summarizes the key scientific issues and opportunities identified by the Workshop. These are not intended to be comprehensive but rather to illustrate the type of programs judged to be high priority for Gemini, and are only a small subset of the potentially significant research areas for Gemini. Based on these scientific issues and opportunities, and the special characteristics of the Gemini Telescopes, instrument capabilities were derived, which together with the capabilities of the Phase I Instrumentation Program were judged to address the broad key issues in an effective fashion. Phasing of the instrumentation developments and location on Gemini-N/S were included in the considerations when appropriate. The resulting recommendations of capabilities are outlined in Section III. The recommendations include new instrumentation capabilities, upgrades to the baseline capabilities of the Phase I instrumentation and also instrumentation shared between the Gemini telescopes and other telescopes on the two sites.

The recommendations generated by the Workshop will be adopted as guidelines for formulating the Gemini on-going instrumentation program. Due to funding constraints and technological considerations it may not be possible to implement all these recommendations.