Haleakala Observatories

Tohoku University Haleakala Observatories


Remote observatoy for long-term monitoring of tenuous emissions from planetary atmosphere and magnetosphere

Overview


The Tohoku University Haleakala observatories were first installed in March 2006, with the aim of continuous monitoring of faint emissions from exosphere/magnetosphere of planets (Jupiter, Mercury, Saturn, etc.) We employ two telescopes (T60 and T40) with several kinds of unique instruments. This program is in collaboration with UH/IfA PLANETS.
Haleakala Long-term Monitoring Program

T60


T60 is a 60-cm reflective telescope with Cassegrain and Coude foci. Daily operation is usually made remotely or semi-automatically. It has four kinds of instruments dedicated for various observing targets:

t60optical_design | Dimension of frange plate at Cassegrain focus

T40


T40 is a 40-cm Schmidt-Cassegrain telescope coupled to a high-resolution (R=67,000) echelle spectrograph with an integral field Unit (IFU). A wide field-of-view monochromatic imager is attached onto the telescope.


T60 / VISP(Visible Imager and SPectrograph with coronagraphy)

■ Specifications

Telescope D=600mm, f=14400mm (F24)
FOV imaging: 315″ circular,
Slit-A: 200″x2″ (60micro-m in width)
Slit-B: 200″x3.3″ (100micro-m in width)
CCD E2V CCD 47-10, 13 micro-m/pixel, 1024×1024
Spatial scale 0.52″/pixel
Observing Mode Mode 1: Narrow-band filter imaging
Mode 2: Mid-res. slit spectroscopy
Mode 3: High-res. slit spectroscopy
Mode 1
 NB Filters
 
[SII]6716+6731, NaD5890, etc.
Mode 2
 dispersion
 resolving power
 sensitivity
(Single order grating, 630nm blazed)
20.3pm/pixel
10,000
0.69E-3 cts/R/s @ 630nm
Mode 3
 dispersion
 resolving power
 sensitivity
(Echelle grating)
2.74pm/pixel
76,000
0.31E-3 cts/R/s @ 630nm

T40 / High-resolution echelle spectrograph with IFU


The integral field unit (IFU) consists of 96 optical fibers (AFS50/125Y low-OH fiber from Fiberguide Industries). The fibers are arranged in 8 by 12 array at the telescope focus corresponding to 41″ by 61″ with a spatial resolution of 5.1″ on the sky. A micro-lens array is attached on the input end of the IFU to inclease a fill-factor and to control the NA of input beam. The IFU was developped at ATRC in Maui under collaboration with IfA/UH. A pellicle beamsplitter and a guiding camera was installed in front of the IFU input end to make precise pointing and tracking.

■ Specifications

Optical layout Near-Littrow
Spatial platescale 5.1″/fiber
Wavelength platescale and Res.Pow. 4.4pm/pixel and 67,000
FOV 41″ x 61″
Wavelength coverage 4.4nm for 672nm

T40 / Wide-FOV Monochromatic Imager


■ Specifications

Spatial platescale 42arcsec/pixel
CCD Pixel number 384 x 576
Spatial coverage 6.91o x 4.61o
5895A filter center wavelength:589.5 nm, bandpath:1.7nm
6200A filter center wavelength:620.0 nm, bandpath:0.9nm