GeminiFocus April 2018 - Page 17

son). We also achieved unprecedented performance during our first science run at sub-80-milliarcsecond-level per- formance in the J-band. Figure 4. Optical layout for IGRINS. All parts shown are within the cryogenic part of the instrument. For Gemini, the five optical elements between the dewar window and the slit were exchanged. The TOPTICA laser has considerably lessened our daytime work to prepare for a laser night, requiring only that we turn the key on a few hours before the night, and the Gemini Multi-conjugate adaptive optics System (GeMS) is ready to operate. The GeMS team looks for- ward to more regular laser windows now to operate GeMS at its best. — Gaetano Sivo 2018A Brings Outstanding Near-IR Spectroscopy to Gemini South Through the Visiting Instrument Program, Gemini users have access to a powerful new capability for the 2018A semester: the broad-band, high-spectral-resolution Im- mersion GRating INfrared Spectrometer (IGRINS). IGRINS is a collaboration of the University of Texas and the Korea Astrono- my and Space Science Institute (KASI). This cross-dispersed near-IR spectrometer has a resolving power of R = 45,000 covering the H and K windows (from 1.45 to 2.5 microns, respectively) in a single exposure. As a visiting instrument, IGRINS is ideal be- cause it has a single observing mode and contains no moving parts (Figure 4). By ex- changing the input optics to accommodate Gemini, the IGRINS H and K echellograms will be unchanged between facilities. In March, the instrument team (Figures 5-7) will accompany IGRINS to Gemini South, where IGRINS has a strong track record of diverse and innovative science results, having spent over 350 nights at the 2.7-meter Harlan J. Smith Telescope at McDonald Observa- tory in Texas, and 200 nights at Lowell Ob- servatory’s 3.5-meter Discovery Channel Telescope in Arizona. Recent results span a range of topics including cold molecu- lar clouds, diffuse interstellar bands, T Tauri stars, systems containing multiple stars and/or planets, and even microquasars. The response to IGRINS at Gemini has been ex- tremely strong, resulting in many successful proposals for 2018A. April 2018 Figure 5. The IGRINS team (left to right respectively, back row: Gregory Mace, Jae Sok Oh, Chan Park; front row: Heeyoung Oh and Kimberley (Sokal). Mace shot this “selfie” in the IGRINS lab at UT Austin in February 2018. The new input optics for IGRINS at Gemini are shown in the background after installation. Credit: Gregory Mace (UT Austin) Figure 6. IGRINS team members Kimberley Sokal (left) and Ricardo Lopez at UT Austin packing the instrument for shipping. Credit: Gregory Mace (UT Austin) GeminiFocus 15