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The High-Resolution Coronal Imager, Flight 2.1Rachmeler, Laurel A.Winebarger, Amy R.Savage, Sabrina L.Golub, LeonKobayashi, KenVigil, Genevieve D.Brooks, David H.Cirtain, Jonathan W.De Pontieu, BartMcKenzie, David E.Morton, Richard J.Peter, HardiTesta, PaolaTiwari, Sanjiv K.Walsh, Robert W.Warren, Harry P.Alexander, CarolineAnsell, DarrenBeabout, Brent L.Beabout, Dyana L.Bethge, Christian W.Champey, Patrick R.Cheimets, Peter N.Cooper, Mark A.Creel, Helen K.Gates, RichardGomez, CarlosGuillory, AnthonyHaight, HarlanHogue, William D.Holloway, ToddHyde, David W.Kenyon, RichardMarshall, Joseph N.McCracken, Jeff E.McCracken, KennethMitchell, Karen O.Ordway, MarkOwen, TimRanganathan, JaganRobertson, Bryan A.Payne, M. JaniePodgorski, WilliamPryor, JonathanSamra, JennaSloan, Mark D.Soohoo, Howard A.Steele, D. BrandonThompson, Furman V.Thornton, Gary S.Watkinson, BenjaminWindt, DavidDOI: info:10.1007/s11207-019-1551-2v. 294174
Rachmeler, Laurel A., Winebarger, Amy R., Savage, Sabrina L., Golub, Leon, Kobayashi, Ken, Vigil, Genevieve D., Brooks, David H., Cirtain, Jonathan W., De Pontieu, Bart, McKenzie, David E., Morton, Richard J., Peter, Hardi, Testa, Paola, Tiwari, Sanjiv K., Walsh, Robert W., Warren, Harry P., Alexander, Caroline, Ansell, Darren, Beabout, Brent L., Beabout, Dyana L., Bethge, Christian W., Champey, Patrick R., Cheimets, Peter N., Cooper, Mark A., Creel, Helen K. et al. 2019. "The High-Resolution Coronal Imager, Flight 2.1." Solar Physics 294:174. https://doi.org/10.1007/s11207-019-1551-2
ID: 154524
Type: article
Authors: Rachmeler, Laurel A.; Winebarger, Amy R.; Savage, Sabrina L.; Golub, Leon; Kobayashi, Ken; Vigil, Genevieve D.; Brooks, David H.; Cirtain, Jonathan W.; De Pontieu, Bart; McKenzie, David E.; Morton, Richard J.; Peter, Hardi; Testa, Paola; Tiwari, Sanjiv K.; Walsh, Robert W.; Warren, Harry P.; Alexander, Caroline; Ansell, Darren; Beabout, Brent L.; Beabout, Dyana L.; Bethge, Christian W.; Champey, Patrick R.; Cheimets, Peter N.; Cooper, Mark A.; Creel, Helen K.; Gates, Richard; Gomez, Carlos; Guillory, Anthony; Haight, Harlan; Hogue, William D.; Holloway, Todd; Hyde, David W.; Kenyon, Richard; Marshall, Joseph N.; McCracken, Jeff E.; McCracken, Kenneth; Mitchell, Karen O.; Ordway, Mark; Owen, Tim; Ranganathan, Jagan; Robertson, Bryan A.; Payne, M. Janie; Podgorski, William; Pryor, Jonathan; Samra, Jenna; Sloan, Mark D.; Soohoo, Howard A.; Steele, D. Brandon; Thompson, Furman V.; Thornton, Gary S.; Watkinson, Benjamin; Windt, David
Abstract: The third flight of the High-Resolution Coronal Imager (Hi-C 2.1) occurred on May 29, 2018; the Sounding Rocket was launched from White Sands Missile Range in New Mexico. The instrument has been modified from its original configuration (Hi-C 1) to observe the solar corona in a passband that peaks near 172 Å, and uses a new, custom-built low-noise camera. The instrument targeted Active Region 12712, and captured 78 images at a cadence of 4.4 s (18:56:22 - 19:01:57 UT; 5 min and 35 s observing time). The image spatial resolution varies due to quasi- periodic motion blur from the rocket; sharp images contain resolved features of at least 0.47 arcsec. There are coordinated observations from multiple ground- and space-based telescopes providing an unprecedented opportunity to observe the mass and energy coupling between the chromosphere and the corona. Details of the instrument and the data set are presented in this paper.
The High-Resolution Coronal Imager (Hi-C)Kobayashi, KenCirtain, JonathanWinebarger, Amy R.Korreck, KellyGolub, LeonWalsh, Robert W.De Pontieu, BartDeForest, CraigTitle, AlanKuzin, SergeySavage, SabrinaBeabout, DyanaBeabout, BrentPodgorski, WilliamCaldwell, DavidMcCracken, KennethOrdway, MarkBergner, HenryGates, RichardMcKillop, SeanCheimets, PeterPlatt, SimonMitchell, NickWindt, DavidDOI: info:10.1007/s11207-014-0544-4v. 2894393–4412
Kobayashi, Ken, Cirtain, Jonathan, Winebarger, Amy R., Korreck, Kelly, Golub, Leon, Walsh, Robert W., De Pontieu, Bart, DeForest, Craig, Title, Alan, Kuzin, Sergey, Savage, Sabrina, Beabout, Dyana, Beabout, Brent, Podgorski, William, Caldwell, David, McCracken, Kenneth, Ordway, Mark, Bergner, Henry, Gates, Richard, McKillop, Sean, Cheimets, Peter, Platt, Simon, Mitchell, Nick, and Windt, David. 2014. "The High-Resolution Coronal Imager (Hi-C)." Solar Physics 289:4393– 4412. https://doi.org/10.1007/s11207-014-0544-4
ID: 133157
Type: article
Authors: Kobayashi, Ken; Cirtain, Jonathan; Winebarger, Amy R.; Korreck, Kelly; Golub, Leon; Walsh, Robert W.; De Pontieu, Bart; DeForest, Craig; Title, Alan; Kuzin, Sergey; Savage, Sabrina; Beabout, Dyana; Beabout, Brent; Podgorski, William; Caldwell, David; McCracken, Kenneth; Ordway, Mark; Bergner, Henry; Gates, Richard; McKillop, Sean; Cheimets, Peter; Platt, Simon; Mitchell, Nick; Windt, David
Abstract: The High-Resolution Coronal Imager (Hi-C) was flown on a NASA sounding rocket on 11 July 2012. The goal of the Hi-C mission was to obtain high-resolution (˜ 0.3 - 0.4''), high-cadence (˜ 5 seconds) images of a solar active region to investigate the dynamics of solar coronal structures at small spatial scales. The instrument consists of a normal-incidence telescope with the optics coated with multilayers to reflect a narrow wavelength range around 19.3 nm (including the Fe xii 19.5-nm spectral line) and a 4096×4096 camera with a plate scale of 0.1'' pixel-1. The target of the Hi-C rocket flight was Active Region 11520. Hi-C obtained 37 full-frame images and 86 partial-frame images during the rocket flight. Analysis of the Hi-C data indicates the corona is structured on scales smaller than currently resolved by existing satellite missions.
The design, development, and implementation of a solar environmental simulator (SES) for the SAO Faraday Cup on Solar Probe PlusCheimets, PeterBookbinder, JayFreeman, MarkGates, RichardGauron, ThomasGuth, GioraKasper, JustinMcCracken, KennethPodgorski, WilliamDOI: info:10.1117/12.2024051v. 8862
Cheimets, Peter, Bookbinder, Jay, Freeman, Mark, Gates, Richard, Gauron, Thomas, Guth, Giora, Kasper, Justin, McCracken, Kenneth, and Podgorski, William. 2013. "The design, development, and implementation of a solar environmental simulator (SES) for the SAO Faraday Cup on Solar Probe Plus." In , https://doi.org/10.1117/12.2024051
MMT and Magellan Infrared SpectrographMcLeod, Brian A.Fabricant, DanielNystrom, GeorgeMcCracken, KenAmato, StephenBergner, HenryBrown, WarrenBurke, MichaelChilingarian, IgorConroy, MaureenCurley, DylanFuresz, GaborGeary, JohnHertz, EdwardHolwell, JustinMatthews, AnneNorton, TimPark, SangRoll, JohnZajac, JosephEpps, HarlandMartini, PaulDOI: info:10.1086/669044v. 1241318–1335
McLeod, Brian A., Fabricant, Daniel, Nystrom, George, McCracken, Ken, Amato, Stephen, Bergner, Henry, Brown, Warren, Burke, Michael, Chilingarian, Igor, Conroy, Maureen, Curley, Dylan, Furesz, Gabor, Geary, John, Hertz, Edward, Holwell, Justin, Matthews, Anne, Norton, Tim, Park, Sang, Roll, John, Zajac, Joseph, Epps, Harland, and Martini, Paul. 2012. "MMT and Magellan Infrared Spectrograph." Publications of the Astronomical Society of the Pacific 124:1318– 1335. https://doi.org/10.1086/669044
ID: 114270
Type: article
Authors: McLeod, Brian A.; Fabricant, Daniel; Nystrom, George; McCracken, Ken; Amato, Stephen; Bergner, Henry; Brown, Warren; Burke, Michael; Chilingarian, Igor; Conroy, Maureen; Curley, Dylan; Furesz, Gabor; Geary, John; Hertz, Edward; Holwell, Justin; Matthews, Anne; Norton, Tim; Park, Sang; Roll, John; Zajac, Joseph; Epps, Harland; Martini, Paul
Abstract: The MMT and Magellan infrared spectrograph (MMIRS) is a cryogenic multiple-slit spectrograph operating in the wavelength range 0.9--2.4 ?m. The refractive optics of MMIRS offer a 6.9" × 6.9" field of view for imaging with a spatial resolution of 0.2 arcsec pixel-1 on a HAWAII-2 array. For spectroscopy, MMIRS can be used with long slits up to 6.9" long, or with custom slit masks having slitlets distributed over a 4.9" × 6.9". A range of dispersers offer spectral resolutions of 800--3000. MMIRS is designed to be used at the f/5 foci of the MMT or Magellan Clay 6.5 m telescopes. MMIRS was commissioned in 2009 at the MMT and has been in routine operation at the Magellan Clay Telescope since 2010. MMIRS is being used for a wide range of scientific investigations from exoplanet atmospheres to Ly? emitters.
Minimizing the mirror distortion for subarcsecond imaging in the Hi-C EUV telescopePodgorski, William A.Caldwell, DavidMcCracken, KennethOrdway, Mark P.Cheimets, Peter N.Korreck, KellyGolub, LeonCirtain, JonathanKobayashi, KenDOI: info:10.1117/12.930610v. 8502
Podgorski, William A., Caldwell, David, McCracken, Kenneth, Ordway, Mark P., Cheimets, Peter N., Korreck, Kelly, Golub, Leon, Cirtain, Jonathan, and Kobayashi, Ken. 2012. "Minimizing the mirror distortion for subarcsecond imaging in the Hi-C EUV telescope." Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series 8502:https://doi.org/10.1117/12.930610
ID: 115719
Type: article
Authors: Podgorski, William A.; Caldwell, David; McCracken, Kenneth; Ordway, Mark P.; Cheimets, Peter N.; Korreck, Kelly; Golub, Leon; Cirtain, Jonathan; Kobayashi, Ken
Abstract: NASA/MSFC and SAO have developed a High Resolution EUV Solar Coronal Imaging telescope (Hi-C). The scientific objective of the mission is to determine, at higher spatial resolution than previously available, the geometric configuration and topology of the structures making up the inner corona. The Hi-C telescope launched on a rocket in early July 2012. It acts as a technology pathfinder for future satellite based missions. Key technology features of the Hi-C telescope are: (1) A 23.9 meter focal length, allowing for 0.1 arc-second pixels (2) Extremely high quality optics (3) Single wavelength multi-layer coating over the entire surface of each optic (4) Low distortion approach to mounting the primary into the telescope. The low distortion approach to mounting the primary mirror into the telescope is discussed in this paper. In previous solar EUV telescopes (TRACE, AIA, IRIS) the primary mirror is first bonded into a flexured mirror cell that is then bolted into the telescope. Techniques for bonding the mirror into the mirror cell have been well developed. If done properly, these techniques produce minimal distortion in the optic. Experience has shown, however, that bolting of the cell into the telescope produces distortions, typically in the form of astigmatism. The magnitude of the astigmatism may be acceptable for lower resolution missions, but as we approach ever higher resolutions, these astigmatisms contribute significantly to the error budget. In the Hi-C mission the mirror mounting hardware was completely assembled into the telescope tube prior to bonding the mirror to the mount. This final operation was done with the telescope tube vertical and the primary mirror surface facing up. This approach minimizes the "bolt-up" distortions typically seen, thus improving resolution.