Observation of Planetary Atmosphere and Magnetosphere from the Haleakala Observatories in Hawaii

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1 Observation of Planetary Atmosphere and Magnetosphere from the Haleakala Observatories in Hawaii 2/21/2014 M. Kagitani 1, T. Sakanoi 1, T. Obara 1, M. Yoneda 2, S. Okano 2,Y. Kasaba 1 and H. Nakagawa 1 1: PPARC, Tohoku Univ. 2: IfA, Univ. Hawaii ATST (4.2m) IfA 0.5m Tohoku 0.4m

2 Investigation of the Planetary upper atmosphere /magnetosphere Spacecraft / Space-based In-situ measurements of plasma and fields Remote sensing free from the atmospheric window (X-ray, EUV, FUV, IR-MIR, Radio freq., ENA) Ground-based Less restriction for the instruments => higher resolution (spectral, temporal) with latest technology HST H2 aurora (HST/FUV) EUV aurora (EXCEED) Jupiter H2 aurora (SUBARU w/ao) (from Uno 2013)

3 Continuous monitoring of Jupiter Aurora It is difficult to get long-term machine-time for middle/large class telescope. B C Solar dynamic pressure CML:~160 IRTF 3 Jupiter H3+ aurora (away in red, toward in blue)

4 Mercury Sodium Exosphere We have been made continuous observation at Haleakala observatory in Hawaii using 40cm telescope and high-resolution spectrograph in visible for the following targets, - Mercury sodium exosphere - Jupiter plasma torus & neutral sodium clouds - Saturn s Enceladus torus Sodium intensity Proton flux Mercury s Na tail (Kameda et al., 2006)

5 Jupiter Watch Campaign on Jan Intensive Jupiter Watch Campaign was made with HST, EXCEED, and ground-baesed telescopes (KP4m, Gemini, IRTF etc.), The duration is 1-weeks. Haleakala 0.4m monitoring total flux tube contents of S+. It has its maximum at around DOY , then it is decreasing. The observation is ongoing (but has not been reduced yet.) Combining EXCEED/HISAKI observation (DOY ), we can indentify causes of this variation. [arbitrary unit] Total Flux-tube contents of S+ on the plasma torus 3 montes 3 montes Brightness of neutral sodium DOY 2013 DOY 2013

6 Plan for groundbased observation at Haleakala Observatory (1) Continuous observation by remote and (semi-)automatic control (2) using high-resolution spectroscopy in visible, IR and MIR. (3) with sufficient photon 0.6m, PLANETS 2m 2015-?? 0.4m, 2007-

7 Haleakala observatories Chicago building (PLANETS 2m) Baker-Nunn Building (Harrington 0.8m) Baker-Nunn Support Building (Tohoku 0.6m) Haleakala (El. 3000m) Manua Kea (El. 4200m)

8 Steps in the Progress of Tohoku 0.6m telescope project (0) Permit for relocoation of 0.6m telescope from Iitate Observatory in Fukushima from the president of IfA/UH, Gunther Hasinger on Dec Facility Use Agreement with IfA/UH Conservative District Use Permit from Department of Land and Natural Resources was issued on July To avoid the nesting season of Hawaiian petrel (seabird), the beginning of construction work was postponed until December Minor change on the existing building (no footprint change, a new volume should be <150% of the original building.) (3) Special Use Permit (and inspections) from Haleakala National Park Service (4) Environmental and Cultural Monitoring by Native Hawaiian. -Soil and lava are restricted to moved from the summit. -Compliance with summit work regulations

9 Construction Plan

10 Building and dome The dome construction will be on May-June 2014 The first light will be on July 2014

11 Layout of the instruments - Visible high-resolution spectrograph - Infrared Echelle spectrograph - Infrared heterodyne Spectrometer - Tip-tilt correction, easy switching for instruments above N VIS IR MIR

12 Visible high-resolution spectrograph with Integrated Field Unit telescope focal plane Re-imaging lens (1) 2.5 /fiber-pitch (2) 5.1 /fiber-ptich 2.5 /fiber (21x30 ) Spatial resolution (FOV) 5.1 /fiber (42x60 ) Spectral resolution 67,000 Wavelength mm Pre-disperser 590,630,670,(770,900) Jupiter (SII, SIII), Observing target Mercury (Na, K), Saturn (OI), etc. Input end of fiber with microlens array 2.5mm 3mm Entrance slit of spectrograph 96 (128) fibers 50 μm Spectrograph 12

13 Mid-infrared heterodyne super high-resolution spectrometer Wavelength 7-11 μm BlackBody Photomixer Resolving power > 10,000,000 Operating range Sensitivity Detector 8.0, 9.6, and 10.3 μm ~3,000 K(λ=10.3μm) MCT photo-diode Telescope Scanner mirror BeamSplitter Local osci - Bandwidth 3,000 MHz Back End FFT digital spectrometer - Bandwidth 2,000 MHz - Channels 16,382 (61 khz resolution) Field of View 1.7 arcsec (1.5m ϕ telescope) O3 (obs) Size, weight 1100 x 700 x 700 mm, 80kg 13

14 Infrared high-resolution echelle spectrograph Slit length 50 arcsec Spectral resolution 20,000 Wavelength 1 4 μm Imaging mode available size 800x500x400 mm Echelle grating drive mechanism Image spectrograph changer 14

15 Science targets & Requirement for Instruments Science Target Planets Wavelength [mm] FOV Instruments Atmospheric Escape (Mars, Venus and Mercury) Magnetosphere & Atmosphere of Giant planets (Jupiter / Saturn) Mars, Venus (O nm, N2+ 391nm, CO 2 + ~289nm, etc.) Mercury (NaD 589nm, K 766nm) Jupiter torus (SII 672nm, SIII 631nm / 953nm, OI 630, OII 733nm etc.) Saturn torus (OI 630nm) VIS , ~20Rv, ~20Rj Spectroscopy R > 50,000 (with image slicer) & Occultation mask Jupiter & Saturn: Aurora (H / 3.9 um, H 2 2.1um) IR 2-4 Spectroscopy R > 20,000 Atmospheric Minor Constituent & Dynamics (Mars, Venus) Mars (H 2 O 2, CH 4, etc.) Venus (CO 2, SO 2, etc.) MIR ~2Rj Spectroscopy R > ~1,000,000

16 Summary Continuous observations from the ground with high-resolution are needed for the investigation of planetary upper atmosphere and magnetosphere as well as the space-based observations (EXCEED, HST, MESSENGER, Cassini, Juno, BepiColombo, Akatsuki, etc.). 0.6m telescope with three instruments will be installed in the Haleakala observatory by July 2014 for the purpose of long-term monitoring of planetary atmosphere and magnetosphere, Visible ( micrometer) high-resolution spectrograph with IFU IR (2-4 micrometer) high-resolution echelle spectrograph MIR (7-10 micrometer) ultra high-dispersion Heterodyne spectrograph