Ground-based and Airborne Instrumentation for Astronomy VIII最新文献

{"title":"The University of Tokyo Atacama Observatory 6.5m telescope: update of the Near-Infrared Echelle Spectrograph NICE as the first light instrument","authors":"K. Asano, Masuo Tanaka, H. Takahashi, H. Sameshima, A. Nishimura, T. Aoki, M. Doi, B. Hatsukade, N. Kato, T. Kamizuka, K. Kohno, M. Konishi, T. Minezaki, T. Miyata, T. Morokuma, Mizuki Numata, S. Sako, K. Motohara, T. Soyano, T. Tanabé, K. Tarusawa, S. Koshida, Y. Yoshii","doi":"10.1117/12.2561186","DOIUrl":"https://doi.org/10.1117/12.2561186","url":null,"abstract":"The Near-Infrared Cross-dispersed Echelle spectrograph (NICE) is a first light instrument for the TAO 6.5 m telescope. The instrument covers a wavelength range of 0.9 to 2.4 µm and has a resolving power of λ/∆λ ~2,600. NICE was first used on the 1.5 m infrared telescope at the National Astronomical Observatory of Japan from 2001 to 2005 and on the 1.6 m Pirka telescope in Japan from 2009 to 2018. We are now upgrading the cryogenics and computer system for the installation of NICE on the TAO telescope. Here we report on the current status and future schedules of instrumentation updates, control system, and modified specifications of NICE for its transfer to the TAO 6.5 m telescope.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"28 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116241312","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Keck-FOBOS spectroscopic facility: conceptual design","authors":"K. Bundy, K. Westfall, N. MacDonald, R. Kupke, C. Poppett, T. Miller, J. Lawrence, Celestina Saavedra Lacombea, R. Yan, M. Goodwin, M. Kassis, J. O’Meara, D. Masters, J. Burchett, B. Williams, R. Rich, V. Villar, N. Sandford, Y. Ting, P. Hinz, C. Schafer, R. Mandelbaum, Marina Huang, J. Prochaska, P. Guhathakurta","doi":"10.1117/12.2562914","DOIUrl":"https://doi.org/10.1117/12.2562914","url":null,"abstract":"The Fiber Optic Broad-band Optical Spectrometer (FOBOS) is a high-priority spectroscopic facility concept for the W. M. Keck Observatory. Here, we provide an update on the FOBOS conceptual design. FOBOS will deploy 1800 fibers across the 20-arcminute field-of-view of the Keck II Telescope. Starbugs fiber positioners will be used to deploy individual fibers as well as fiber-bundle arrays (integral field units, IFUs). Different combinations of active single fibers or IFUs can be selected to carry light to one of three mounted spectrographs, each with a 600-fiber pseudoslit. Each spectrograph has four wavelength channels, enabling end-to-end instrument sensitivity greater than 30% from 0.31-1.0 µm at a spectral resolution of R ~ 3500. With its high fiber density on a large telescope and modest field-of-view, FOBOS is optimized to obtain deep spectroscopy for large samples. In single- fiber mode, it will deliver premier spectroscopic reference sets for maximizing the information (e.g., photometric redshifts) that can be extracted from panoramic imaging surveys obtained from the forthcoming Rubin and Roman Observatories. Its IFUs will map emission from the circumgalactic interface between forming galaxies and the intergalactic medium at z ~ 2–3, and lay the path for multiplexed resolved spectroscopy of high-z galaxies aided by ground-layer and multi-object adaptive optics. In the nearby universe, its high sampling density and combination of single-fiber and IFU modes will revolutionize our understanding of the M31 disk and bulge via stellar populations and kinematics. Finally, with a robust and intelligent target and program allocation system, FOBOS will be a premier facility for follow-up of rare, faint, and transient sources that can be interleaved into its suite of observing programs. With a commitment to delivering science-ready data products, FOBOS will enable unique and powerful combinations of focused, PI-led programs and community-driven observing campaigns that promise major advances in cosmology, galaxy formation, time-domain astronomy, and stellar evolution.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"46 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116690327","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"New narrow-band filter system for the IRSF 1.4m telescope","authors":"K. Morihana, T. Nagayama, M. Tsujimoto, M. Yamagishi, K. Ebisawa","doi":"10.1117/12.2576307","DOIUrl":"https://doi.org/10.1117/12.2576307","url":null,"abstract":"","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"55 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121488071","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Performance of Kitt Peak’s Mayall 4-meter telescope during DESI commissioning","authors":"A. Meisner, B. Abareshi, A. Dey, C. Rockosi, R. Joyce, D. Sprayberry, R. Besuner, K. Honscheid, D. Kirkby, H. Kong, M. Landriau, M. Levi, Ting S. Li, B. Marshall, P. Martini, A. Ross, D. Brooks, P. Doel, Y. Duan, E. Gaztañaga, C. Magneville, F. Prada, M. Schubnell, G. Tarlé","doi":"10.1117/12.2574776","DOIUrl":"https://doi.org/10.1117/12.2574776","url":null,"abstract":"In preparation for the Dark Energy Spectroscopic Instrument (DESI), a new top end was installed on the Mayall 4-meter telescope at Kitt Peak National Observatory. The refurbished telescope and the DESI instrument were successfully commissioned on sky between 2019 October and 2020 March. Here we describe the pointing, tracking and imaging performance of the Mayall telescope equipped with its new DESI prime focus corrector, as measured by six guider cameras sampling the outer edge of DESI’s focal plane. Analyzing ~500,000 guider images acquired during commissioning, we find a median delivered image FWHM of 1.1 arcseconds (in the r-band at 650 nm), with the distribution extending to a best-case value of ~0.6 arcseconds. The point spread function is well characterized by a Moffat profile with a power-law index of β ≈ 3.5 and little dependence of β on FWHM. The shape and size of the PSF delivered by the new corrector at a field angle of 1.57 degrees are very similar to those measured with the old Mayall corrector on axis. We also find that the Mayall achieves excellent pointing accuracy (several arcseconds RMS) and minimal open-loop tracking drift (< 1 milliarcsecond per second), improvements on the telecope’s pre-DESI performance. In the future, employing DESI’s active focus adjustment capabilities will likely further improve the Mayall/DESI delivered image quality.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"23 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125140226","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"SDSS-V focal plane robot positioning metrology","authors":"C. Jurgenson, Michael Engelman, R. Pogge, T. O'Brien, D. Pappalardo, Nicholas Clawson, M. Derwent, Christopher Brandon, J. Mason, Julia Brady, Jon Shover","doi":"10.1117/12.2562492","DOIUrl":"https://doi.org/10.1117/12.2562492","url":null,"abstract":"The Sloan Digital Sky Survey V (SDSS-V) is an all-sky spectroscopic survey of ≥ 6 million objects, designed to decode the history of the Milky Way, reveal the inner workings of stars, investigate the origin of solar systems, and track the growth of supermassive black holes across the Universe.1 The robotic Focal Plane System (FPS)2 will carry 500 robots each with three fibers for science and metrology. The science fibers feed the BOSS3 and APOGEE4 spectrographs, while the metrology fibers are back illuminated to aid in robot positioning. Blind initial x/y positional precision of the robots is expected to be better than 50µm. The robots must position the fibers to better than 5µm in order to meet the science requirements. The FPS fiber viewing camera (FVC) consists of optomechanical components that look back through the telescope optics at light from back-lit fiducial and metrology fibers to measure the positions of the robots in the telescope focal plane. The FVC takes an image of the robots in the telescope focal plane, measures their positions to an accuracy of better than 3µm, and then feeds back error commands to the robot control system to meet the 5µm positional requirement. This paper details the optomechanical design, and initial results of an engineering run on the du Pont telescope.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"490 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114253246","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Conceptual design of the Giant Magellan Telescope Commissioning Camera","authors":"J. Crane, A. Uomoto, P. Amram, S. Augusto, C. Birk, Antonio Braulio Neto, D. Faes, T. Hare, Patricio Jones, C. Oliveira, S. Shectman, Marco Antonio Furlan de Souza","doi":"10.1117/12.2560718","DOIUrl":"https://doi.org/10.1117/12.2560718","url":null,"abstract":"The Giant Magellan Telescope (GMT) Commissioning Camera (ComCam) is an all-refractive, focal reducing camera intended for the evaluation of telescope performance in both natural seeing and ground layer adaptive optics modes across a six arcminute field of view. As the first purpose-built, large imager for the GMT, it also provides unique public outreach functions and scientific research opportunities by enabling both narrowband and broadband imaging and photometric measurements at wavelengths between 360 and 950 nm. In addition to a discrete set of narrowband and broadband filters, inclusion of a deployable Fabry-Perot etalon will greatly enhance ComCam’s capabilities. With an image scale of 0.06 arcseconds per pixel, ComCam will be able to take full advantage of the GMT’s GLAO-corrected image quality under the best predicted conditions. ComCam has undergone a conceptual design review and is now under development in the preliminary design phase. Instrumental first light will be concurrent with that of the GMT.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"14 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127742336","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Multifocal station for the Wendelstein 2m Fraunhofer Telescope","authors":"Kerstin Krecker, M. Fabricius, R. Bender, Vanessa Fahrenschon, H. Gebler, C. Gössl, F. Grupp, O. Hans, M. Häuser, U. Hopp, H. Kellermann, F. Lang-Bardl, W. Mitsch, J. Richter, S. Rukdee, R. Saglia, Sami Wirthensohn","doi":"10.1117/12.2560940","DOIUrl":"https://doi.org/10.1117/12.2560940","url":null,"abstract":"The Wendelstein 2 m Telescope has been in regular science operation since 2013. It is equipped with a three channel camera and an Echelle spectrograph called FOCES on one of it’s two Nasmyth foci. FOCES is a wavelength comb stabilized instrument which aims at <1m/s precision. High stability and repeatability of the entire system, including its fiber feed, are required and fast exchange times, between imaging mode and radial velocity measurement, is desirable. We are in the advanced implementation phase of an automated multifocal exchange system to allow for stable and fast exchange between the three different science instruments, a wavefront sensor and a calibration system. We present the final optical design and discuss the mechanical design choices we made in particular with respect to the limited design volume. We will conclude with presenting results from first tests on the system’s optomechanical stability.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"32 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116133620","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Mechanical aspects of near infrared imager spectrometer and polarimeter","authors":"P. Kasarla, P. S. Patwal, H. L. Adalja, S. N. Mathur, D. Sarkar, A. Singh, A. Rai, P. Prajapati, S. Naik, Amish B. Shah, S. Ganesh, Kiran S. Baliyan Physical Research Laboratory, Ahmedabad, India., Indian Institute of Technology, Gandhinagar","doi":"10.1117/12.2561339","DOIUrl":"https://doi.org/10.1117/12.2561339","url":null,"abstract":"Near-infrared Imager Spectrometer and Polarimeter (NISP) is a camera, an intermediate resolution spectrograph and an imaging polarimeter being developed for upcoming 2.5m telescope of Physical Research Laboratory at Mount Abu, India. NISP is designed to work in the Near-IR (0.8-2.5 micron) using a H2RG detector. Collimator and camera lenses would transfer the image from the focal plane of the telescope to the detector plane. The entire optics, mechanical support structures, detector-SIDECAR assembly will be cooled to cryo-temperatures using an open cycle Liquid Nitrogen tank inside a vacuum Dewar. GFRP support structures would be used to isolate cryogenic system from the Dewar. Two layer thermal shielding would be used to reduce the radiative heat transfer. Molecular sieve (getter) would be used to enhance the vacuum level inside Dewar. Magnet-reedswitch combination are used for absolute positioning of filterwheels. Here we describe the mechanical aspects in detail.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"2 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115254836","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The development status of the NIR Arm of the new SoXS instrument at the ESO/NTT telescope","authors":"F. Vitali, M. Aliverti, G. Capasso, F. D'Alessio, M. Munari, M. Riva, S. Scuderi, R. Z. Sánchez, S. Campana, P. Schipani, R. Claudi, A. Baruffolo, S. Ben-Ami, F. Biondi, A. Brucalassi, R. Cosentino, Davide Ricci, P. D’Avanzo, H. Kuncarayakti, A. Rubin, J. Achr'en, J. A. Araiza-Durán, I. Arcavi, A. Bianco, R. Bruch, E. Cappellaro, M. Colapietro, M. Valle, M. D. Pascale, R. D. Benedetto, S. D'orsi, D. Fantinel, A. Gal-yam, M. Genoni, M. Hernández, O. Hershko, J. Kotilainen, M. Landoni, G. Causi, S. Mattila, G. Pignata, K. Radhakrishnan, M. Rappaport, B. Salasnich, S. Smartt, M. Stritzinger, E. Ventura, D. Young","doi":"10.1117/12.2562147","DOIUrl":"https://doi.org/10.1117/12.2562147","url":null,"abstract":"We present here the development status of the NIR spectrograph of the Son Of X-Shooter (SOXS) instrument, for the ESO/NTT telescope at La Silla (Chile). SOXS is a R~4,500 mean resolution spectrograph, with a simultaneously coverage from about 0.35 to 2.00 μm. It will be mounted at the Nasmyth focus of the NTT. The two UV-VIS-NIR wavelength ranges will be covered by two separated arms. The NIR spectrograph is a fully cryogenic echelle-dispersed spectrograph, working in the range 0.80-2.00 μm, equipped with a Hawaii H2RG IR array from Teledyne. The whole spectrograph will be cooled down to about 150 K (but the array at 40 K), to lower the thermal background, and equipped with a thermal filter to block any thermal radiation above 2.0 μm. In this work, we will show the advanced phase of integration of the NIR spectrograph.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"42 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123300291","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Design requirements for the Wide-field Infrared Transient Explorer (WINTER)","authors":"Danielle Frostig, J. Baker, Joshua Brown, R. Burruss, Kristin E. Clark, G. FHur'esz, Nicolae Ganciu, Erik Hinrichsen, V. Karambelkar, M. Kasliwal, N. Lourie, A. Malonis, R. Simcoe, J. Zolkower","doi":"10.1117/12.2562842","DOIUrl":"https://doi.org/10.1117/12.2562842","url":null,"abstract":"The Wide-field Infrared Transient Explorer (WINTER) is a 1x1 degree infrared survey telescope under devel- opment at MIT and Caltech, and slated for commissioning at Palomar Observatory in 2021. WINTER is a seeing-limited infrared time-domain survey and has two main science goals: (1) the discovery of IR kilonovae and r-process materials from binary neutron star mergers and (2) the study of general IR transients, including supernovae, tidal disruption events, and transiting exoplanets around low mass stars. We plan to meet these science goals with technologies that are relatively new to astrophysical research: hybridized InGaAs sensors as an alternative to traditional, but expensive, HgCdTe arrays and an IR-optimized 1-meter COTS telescope. To mitigate risk, optimize development efforts, and ensure that WINTER meets its science objectives, we use model-based systems engineering (MBSE) techniques commonly featured in aerospace engineering projects. Even as ground-based instrumentation projects grow in complexity, they do not often have the budget for a full-time systems engineer. We present one example of systems engineering for the ground-based WINTER project, featuring software tools that allow students or staff to learn the fundamentals of MBSE and capture the results in a formalized software interface. We focus on the top-level science requirements with a detailed example of how the goal of detecting kilonovae flows down to WINTER’s optical design. In particular, we discuss new methods for tolerance simulations, eliminating stray light, and maximizing image quality of a fly’s-eye design that slices the telescope’s focus onto 6 non-buttable, IR detectors. We also include a discussion of safety constraints for a robotic telescope.","PeriodicalId":215000,"journal":{"name":"Ground-based and Airborne Instrumentation for Astronomy VIII","volume":"383 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124764820","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}