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IGRINS at the Discovery Channel Telescope and Gemini South
Author(s): Gregory Mace; Kimberly Sokal; Jae-Joon Lee; Heeyoung Oh; Chan Park; Hanshin Lee; John Good; Phillip MacQueen; Jae Sok Oh; Kyle Kaplan ; Ben Kidder; Moo-Young Chun; In-Soo Yuk ; Ueejeong Jeong; Soojong Pak; Kang-Min Kim; Jakyoung Nah; Sungho Lee; Young-Sam Yu; Narae Hwang; Byeong-Gon Park; Hwihyun Kim; Brian Chinn; Alison Peck; Ruben Diaz; Rene Rutten; Lisa Prato; George Jacoby; Frank Cornelius; Ben Hardesty; William DeGroff; Edward Dunham; Stephen Levine; Larissa Nofi; Ricardo Lopez-Valdivia; Alycia J. Weinberger; Daniel T. Jaffe
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Paper Abstract

The Immersion GRating INfrared Spectrometer (IGRINS) was designed for high-throughput with the expectation of being a visitor instrument at progressively larger observing facilities. IGRINS achieves R∼45000 and > 20,000 resolution elements spanning the H and K bands (1.45-2.5μm) by employing a silicon immersion grating as the primary disperser and volume-phase holographic gratings as cross-dispersers. After commissioning on the 2.7 meter Harlan J. Smith Telescope at McDonald Observatory, the instrument had more than 350 scheduled nights in the first two years. With a fixed format echellogram and no cryogenic mechanisms, spectra produced by IGRINS at different facilities have nearly identical formats. The first host facility for IGRINS was Lowell Observatory’s 4.3-meter Discovery Channel Telescope (DCT). For the DCT a three-element fore-optic assembly was designed to be mounted in front of the cryostat window and convert the f/6.1 telescope beam to the f/8.8 beam required by the default IGRINS input optics. The larger collecting area and more reliable pointing and tracking of the DCT improved the faint limit of IGRINS, relative to the McDonald 2.7-meter, by ∼1 magnitude. The Gemini South 8.1-meter telescope was the second facility for IGRINS to visit. The focal ratio for Gemini is f/16, which required a swap of the four-element input optics assembly inside the IGRINS cryostat. At Gemini, observers have access to many southern-sky targets and an additional gain of ∼1.5 magnitudes compared to IGRINS at the DCT. Additional adjustments to IGRINS include instrument mounts for each facility, a glycol cooled electronics rack, and software modifications. Here we present instrument modifications, report on the success and challenges of being a visitor instrument, and highlight the science output of the instrument after four years and 699 nights on sky. The successful design and adaptation of IGRINS for various facilities make it a reliable forerunner for GMTNIRS, which we now anticipate commissioning on one of the 6.5 meter Magellan telescopes prior to the completion of the Giant Magellan Telescope.

Paper Details

Date Published: 6 July 2018
PDF: 18 pages
Proc. SPIE 10702, Ground-based and Airborne Instrumentation for Astronomy VII, 107020Q (6 July 2018); doi: 10.1117/12.2312345
Show Author Affiliations
Gregory Mace, The Univ. of Texas at Austin (United States)
McDonald Observatory (United States)
Kimberly Sokal, The Univ. of Texas at Austin (United States)
McDonald Observatory (United States)
Jae-Joon Lee, Korea Astronomy and Space Science Institute (Korea, Republic of)
Heeyoung Oh, Korea Astronomy and Space Science Institute (Korea, Republic of)
Chan Park, Korea Astronomy and Space Science Institute (Korea, Republic of)
Hanshin Lee, The Univ. of Texas at Austin (United States)
McDonald Observatory (United States)
John Good, The Univ. of Texas at Austin (United States)
McDonald Observatory (United States)
Phillip MacQueen, The Univ. of Texas at Austin (United States)
McDonald Observatory (United States)
Jae Sok Oh, Korea Astronomy and Space Science Institute (Korea, Republic of)
Kyle Kaplan , The Univ. of Texas at Austin (United States)
Ben Kidder, The Univ. of Texas at Austin (United States)
Moo-Young Chun, Korea Astronomy and Space Science Institute (Korea, Republic of)
In-Soo Yuk , Korea Astronomy and Space Science Institute (Korea, Republic of)
Ueejeong Jeong, Korea Astronomy and Space Science Institute (Korea, Republic of)
Soojong Pak, Kyung Hee Univ. (Korea, Republic of)
Kang-Min Kim, Korea Astronomy and Space Science Institute (Korea, Republic of)
Jakyoung Nah, Korea Astronomy and Space Science Institute (Korea, Republic of)
Sungho Lee, Korea Astronomy and Space Science Institute (Korea, Republic of)
Young-Sam Yu, Korea Astronomy and Space Science Institute (Korea, Republic of)
Narae Hwang, Korea Astronomy and Space Science Institute (Korea, Republic of)
Byeong-Gon Park, Korea Astronomy and Space Science Institute (Korea, Republic of)
Hwihyun Kim, Gemini Observatory (Chile)
Brian Chinn, Gemini Observatory (Chile)
Alison Peck, Gemini Observatory (United States)
Ruben Diaz, Gemini Observatory (Chile)
Rene Rutten, Gemini Observatory (Chile)
Lisa Prato, Lowell Observatory (United States)
George Jacoby, Lowell Observatory (United States)
Frank Cornelius, Lowell Observatory (United States)
Ben Hardesty, Lowell Observatory (United States)
William DeGroff, Lowell Observatory (United States)
Edward Dunham, Lowell Observatory (United States)
Stephen Levine, Lowell Observatory (United States)
Larissa Nofi, Lowell Observatory (United States)
Univ. of Hawai'i, Manoa (United States)
Ricardo Lopez-Valdivia, The Univ. of Texas at Austin (United States)
Alycia J. Weinberger, Carnegie Institution for Science (United States)
Daniel T. Jaffe, The Univ. of Texas at Austin (United States)


Published in SPIE Proceedings Vol. 10702:
Ground-based and Airborne Instrumentation for Astronomy VII
Christopher J. Evans; Luc Simard; Hideki Takami, Editor(s)

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