The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. We will describe the extensive preparations of the Mayall telescope and its environs for DESI, and will report on progress-to-date of the installation of DESI itself.
We describe the design, construction and measured performance of the Kitt Peak Ohio State Multi-Object Spectrograph
(KOSMOS) for the 4-m Mayall telescope and the Cerro Tololo Ohio State Multi-Object Spectrograph (COSMOS) for
the 4-m Blanco telescope. These nearly identical imaging spectrographs are modified versions of the OSMOS
instrument; they provide a pair of new, high-efficiency instruments to the NOAO user community. KOSMOS and
COSMOS may be used for imaging, long-slit, and multi-slit spectroscopy over a 100 square arcminute field of view with
a pixel scale of 0.29 arcseconds. Each contains two VPH grisms that provide R~2500 with a one arcsecond slit and their
wavelengths of peak diffraction efficiency are approximately 510nm and 750nm. Both may also be used with either a
thin, blue-optimized CCD from e2v or a thick, fully depleted, red-optimized CCD from LBNL. These instruments were
developed in response to the ReSTAR process. KOSMOS was commissioned in 2013B and COSMOS was
commissioned in 2014A.
The Thirty Meter Telescope (TMT) project is a partnership between ACURA, AURA, Caltech, and the University of
California. The Telescope Control System (TCS) for TMT is comprised of many subsystems. The TCS Supervisory
Controller is responsible for pointing the telescope via an embedded pointing kernel, sequencing commands to the
telescope systems, responding to errors and alarms and interacting with the telescope safety system. This paper describes
the conceptual design for the Supervisory Controller and addresses the integration with the other TMT software systems.
The requirements are discussed in terms of producing a functional, usable, safe, reliable and maintainable system.
The Thirty Meter Telescope (TMT) is a collaborative project between the California Institute of Technology (CIT), the University of California (UC), the Association of Universities for Research in Astronomy (AURA) and the Association of Canadian Universities for Research in Astronomy (ACURA). Current activity is focused on the design and development phase (DDP) of all systems. For the TMT to achieve seeing and diffraction limited performance, the telescope-related software systems will have to work in concert to precisely control all 738 primary mirror (M1) segments along with the active secondary mirror (M2) and an articulated tertiary mirror (M3). In this paper we discuss the conceptual design of the software control systems for these surfaces and their integration into a cohesive whole.