An optical and near-infrared multipurpose instrument
HONIR
Kiyoshi Sakimotoa , Hiroshi Akitayab , Takuya Yamashitac , Koji S. Kawabatab , HidehikoNakayac , Hisashi Miyamotod , Tatsuya Haraoa , Ryosuke Itoha , Risako Matsuia , Yuki
Moritanib , Asami Nakashimae,c , Takashi Ohsugib,a , Mahito Sasadaf , Katsutoshi Takakia ,Issei Uenoa , Takahiro Uia,c , Takeshi Uranoa , and Michitoshi Yoshidaba Department of Physical Science, School of Science, Hiroshima University, Kagamiyama

1-2-1, Higashi-Hiroshima 739-8526, JAPAN;
b Hiroshima Astrophysical Science Center, Hiroshima University, Kagamiyama 1-2-1,

Higashi-Hiroshima 739-8526, JAPAN;
c National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588,

JAPAN;
d Molex Japan Co., Ltd., Fukami-Higashi 1-5-4, Yamato, Kanagawa 242-8585, JAPAN;
e Department of Astronomy, Graduate School of Science, The University of Tokyo, Hongo

7-3-1, Bunkyo-ku, Tokyo 113-8656, JAPAN;
f Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto

606-8502, JAPANABSTRACT
We have developed an optical-infrared instrument HONIR (Hiroshima Optical and Near-InfraRed camera) to
be attached to the 1.5-m Kanata telescope at Higashi-Hiroshima Observatory, Hiroshima University. HONIR
is a three color (one optical and two near-infrared bands among 0.5–2.4 µm) simultaneous imager and spectrograph with a polarimetry function. The ﬁeld of view of the imaging mode is 10 arcmin square with a spatialsampling of 000 .29. Among the planned multipurpose functions, a two color (0.5–1.0 µm and 1.15–2.40 µm)
simultaneous imaging function has been installed and operated so far. The remaining functions, spectroscopy
and polarimetry, and the second near-infrared band arm, are under development and will be installed in thenear future.
Keywords: optical, infrared, imaging, spectroscopy, polarimetry

1. INTRODUCTION
We have developed a new instrument HONIR (Hiroshima Optical and Near-InfraRed camera) to be attachedon the Kanata telescope at Higashi-Hiroshima Observatory.
The Kanata telescope is a 1.5-m diameter Ritchy-Cretien telescope at Higashi-Hiroshima Observatory
managed by Hiroshima Astrophysical Science Center, Hiroshima University. On the telescope, three focal
ports, one Cassegrain port and two Nasmyth ports, are available (Table 1). We have operated sophisticatedinstruments on the telescope: TRISPEC1 capable of imaging, spectroscopy, and polarimetry, at three bands
among optical and near-infrared wavelengths simultaneously, and HOWPol2 capable of optical imaging, spectroscopy, and Stokes Q-U simultaneous polarimetry. By use of these instruments, with a tight collaboration
with high-energy satellites, we have published many observational results especially on variable objects suchas blazers, super novae, and gamma-ray bursts.3–7

Further author information: (Send correspondence to H. Akitaya)
H. Akitaya : E-mail: akitaya@hiroshima-u.ac.jp, Telephone: +81 82 424 5765, Fax: +81 82 424 5765

Table 1. Basic parameters of the Kanata telescope.

Type
Primary mirror diameter
Focal number
Plate scale
Field of view
Focal ports: Instrument

Ritchy-Cretien
1.5 m
F/12.311.148 arcsec/mm
15 arcmin
Cassegrain (with an instrumental rotator): HONIR
Nasmyth #1 (with an instrumental rotator): HOWPol
Nasmyth #2: High-speed camera, etc.

HONIR is a brand-new instrument for the Kanata telescope that takes over and upgrades multipurpose
capabilities of the previous instrument TRISPEC. It is designed as an imager and spectrograph with a polarimetry function that obtains three band information among optical-infrared wavelengths of 0.5–2.4 µm
simultaneously with a ﬁeld of view of 10 arcmin square.
We started its development in early 2007 and conducted the ﬁrst test operation on the telescope with one
near-infrared imager in 2009. In the recent observational runs from October 2011, we installed a function of
two bands (one optical and one near-infrared) simultaneous imaging and started its operation.
In the near future, functions of spectroscopy and polarimetry (imaging polarimetry and spectro-polarimetry)
will be installed. In addition, another near-infrared arm will be also appended, which enables us to perform
three (one optical and two near-infrared) bands simultaneous observation.
In this paper, we introduce a concept of the instrument. We also report the current status and initialaccomplishments that had been performed in the recent observational runs with the existing function of twoband simultaneous imaging.

2. DESIGN AND SPECIFICATIONSHONIR is to be attached on the Cassegrain focus of the Kanata telescope. HONIR is designed to obtain
images of three wavelength bands (ranges of 0.5–1.0 µm, 1.15–1.35 µm, and 1.45–2.40 µm) simultaneouslywith a ﬁeld of view of 10 arcmin by 10 arcmin. In addition to imaging, spectroscopy and combination useof polarimetry are also available. All of the optical components in the instrument after the entrance optical
window are mounted on the optical bench cooled down to around 60–70 K in a vacuum chamber.
Among the planned functions in the design, that of two bands (wavelength ranges of 0.5–1.0 µm and 1.15–
2.40 µm) simultaneous imaging has been installed so far. The remaining functions (spectroscopy, polarimetry,
and the second near-infrared band arm) will be added in the near future. The basic speciﬁcations of the
instrument are summarized in Table 2.

2.1 Optical Design and Layout
The basic concept of the optics design of HONIR is a reimaging optical system with three branched arms
split by two dichroic mirrors, which simultaneously produces three images of diﬀerent wavelength ranges. The
layout of the optics and its picture are shown in Fig. 2–3.
A convergent ray from the telescope, passing through a CaF2 entrance window of the vacuum chamber, isfocused on the telescope focal plane, at which one of the focal masks (a square aperture for imaging, a narrowslit for spectroscopy, etc.) in the rotating turret is placed. An actual size of the whole ﬁeld of view of 100 × 100
at the telescope focal plane is 53.8 mm by 53.8 mm. It is followed by a common collimator lens unit and acold stop. The consequential collimated beam incidents a series of dichroic mirrors (Table 3) so that the beamis split into three passes with diﬀerent wavelength ranges: the optical arm at 0.5–1.0 µm, the IR arm #1 at
1.45–2.40 µm, and the IR arm #2 at 1.15–1.35 µm. Each arm has a camera lens that refocuses a demagniﬁed
ﬁeld image on a detector. We use diﬀerent types of detector between optical and near-infrared wavelengths:
a CCD with a pixel size of 15 µm and a HgCdTe detector with that of 20 µm (See section 2.3). Focal lengths

of the camera lenses and consequent magniﬁcation factors of reimaging are tuned so that an image of thewhole ﬁeld of view of 100 × 100 is focused at a pixel scale of 0.29 arcsec/pixel on both the detectors. Each of
the collimator lens unit and camera lens units consists of six or seven spherical lenses made of several glassmaterials and with anti-reﬂection coating. The properties of the lenses are summarized in Table 4.
It is planned to install three arms ﬁnally, however, the IR arm #2 components including its dichroic mirror
has not been installed yet. Therefore, the optical arm for 0.5–1.0 µm and the IR arm #1 for 1.15–2.40 µm
are available so far.
The optics is designed for operation at 85 K. In the design, an 80% encircled energy is achieved at a radiusof < 17 µm at H and Ks bands, < 12 µm at J band, and < 5.4 µm at optical wavelengths, over the whole
imaging area on a detector. Distortion of an image on a detector is less than 0.18 % at H and Ks bands, lessthan 0.19 % at J band, and less than 0.06% at optical wavelengths.
In the near future, the optical components for spectroscopy and linear polarimetry will be installed.
For spectroscopy, a slit mask on the telescope focal plane and grisms in the collimated beam at each arm
are inserted. A set of grisms and a slit mask of 0.2 mm (or 2.2 arcsec) width have been designed for low
dispersion spectroscopy (R ∼ 350), which are in the process of production (Table 5). In addition, we are alsoplanning to add grisms with a higher dispersion (R ∼ 700) and lower dispersion (R ∼ 30).
The forthcoming polarimetry will be performed by use of a rotatable super-achromatic half-wave plate
mounted just above the entrance optical window, an appropriate focal mask or slit at the telescope focal
plane, and a Wollaston prism as a polarization beam splitter at the pupil plane. A Wollaston prism splits an
incoming beam into two separated ones which are perpendicularly polarized.
We designed the Wollaston prism to satisfy the following requirements: an eﬃcient beam splitting angle(namely a large birefringence of the material and a large wedge angle of the wedge components) to split a

Figure 1. HONIR attached on the Kanata telescope (left) and its closeup (right).

Figure 2. Optical design and layout of HONIR.

Figure 3. Optical components mounted on the optical bench (left) and its bottom side (right).

Table 2. Basic specifications of HONIR.

Property
Optical0.5a–1.0
10 ×10

Wavelength coverage (µm)
Field of view (FOV) (arcmin)
Plate scale (arcsec/mm)c
Size of the whole FOV (mm)c
Sampling rate (arcsec/pix)d0.29
Size of the whole imaging area (mm)d30.7 ×30.7
Filters
Ba, V, RC , IC , z’, Y
Detector
Type
CCD
VendorHamamatsu Photonics
Format (pixels)
2048 ×4096f
Pitch (µm)
15Size (mm)30.72 ×61.44

Arm
IR #1
1.45(1.15)b–2.40
10 ×1011.14853.8×53.8
0.29
40.9 ×40.9
Y, J, He, Kse
HgCdTe (VIRGO)
Raytheon
2048 ×2048
2040.96 ×40.96

IR #2 (in future)
1.15–1.35
TBD

TBD
TBD
H, Ks
TBD
TBD
TBD
TBD
TBD

a

Partially transparent at 0.4–0.5 µm (B-band).
Until the future installation of the IR arm #2.
c
At the telescope focal plane.
dOn the detector.
e
To be moved to the IR arm #2 after its installation.
f
A half of the area is actually used for imaging.
b

Table 3. Specification of the dichroic mirrors.

Dichroic mirror#1 (optical–IR splitting)#2 (J–H splitting)Wavelengths (µm)
0.50–1.00
1.00–1.15
1.15–2.40
1.15-1.35
1.35–1.45
1.45–2.40

Eﬃciency> 90% reﬂectancetransition> 90% transmittance> 85% reﬂectancetransition> 90% transmittancestellar image eﬃciently on the detector, a small color dispersion (a small wavelength dependency of a refractive
index), a wide range transmittance for all of the wavelengths of 0.5–2.4 µm that HONIR measures, and a small
diﬀerence of coeﬃcients of thermal expansion between two diﬀerent optical axes to avoid destruction owing
to its cooling. A size constraint is also rigid because of the crowded optical layout. Thus, we have selected
LiYF4 (YLF)8, 9 as the best material among candidates and designed the Wollaston prism as shown in Table
6 and Fig. 4. The collimated beam is split into two inclined beams with orthogonal linear polarization modes
at a separation angle of 0.74–0.77 degrees depending on the wavelength. Consequently, dual stellar images of
two linear polarization modes are focused on the detector separated by 46–48 arcsec each other. We also use
a focal mask with a series of long rectangular apertures of 60000 × 4500 placed at a 93 arcsec pitch along thedirection of the beam separation, which truncates a half of the whole image area discontinuously as a shapeof a barred lattice. As a result, we obtain pairs of orthogonally polarized rectangular images without theiroverlap. Obtaining a series of polarized images with rotating the half-wave plate at a 22◦ .5 step, we ﬁnallymeasure the linear polarization distribution in the image. In addition, using an appropriate focal slit mask
and grisms together, spectro-polarimetry is also capable. We intend to achieve a polarimetric accuracy of
better than 0.1 percent.

Table 4. Construction of the lens units.

Lens unit
Collimator lens
Focal length (mm)312.0
Magniﬁcation factora–
Plate scale (arcsec/mm)b–
Number of lenses
7
Lens materials
S-FPL53, S-TIH53,
S-FTM16, S-FPL51
Eﬀective diameter (mm)80abOptical camera lens
178.0
0.570519.55
5
CaF2 , S-FPL53,
S-FTM16, S-FPL51
75

IR camera lensa
237.2
0.7603
14.67
5
CaF2 , S-FPL53,
S-FTM16, S-FPL51
75

The same conﬁguration for both the IR #1 arm and IR #2 arm.
On the detector as a combination with the collimator lens.
Table 5. Design of the grisms for low dispersion spectroscopy.

Arm
Wavelength coverage
Slit width (arcsec)
Resolution (R = λ/∆λ)Wavelength of the maximum eﬃciency (µm)
Material
Wedge angle (degrees)
Grooves (gr/mm)
Blaze angle (degrees)
Groove pattern typeb
Size (mm)Eﬀective diameter (mm)ab

Optical0.41–0.97
330
0.683
BK7
21.5
300
23.0
54-039R
51×51×2147

IR #1
1.50–2.40
2.2a
371
1.933
S-FTM16
22.5
120
26.7
54-831R
59×59×26
55

IR #2
1.07–1.43
354
1.232
BK7
23.5
180
23.9
54-870R
59×59×27
55

0.2mm at the telescope focal plane.
Model number of Richardson Gratings, Newport Corporation.

2.2 Cryogenics
Almost all of the principal components of HONIR are enclosed in a vacuum chamber and cooled down tosuitable temperatures to suppress thermal background radiation from the instrument itself and thermal noiseof the detectors.
The vacuum chamber is a large box, measuring 960×960×630 mm, built up by welding boards and framesof aluminum base alloy. It was manufactured by TAIYO NIPPON SANSO Corp.
The chamber contains an optical bench, on which lens units, optical elements, and detector containers
are mounted. The optical bench is attached to the chamber wall through four non-rigid supports made ofglass epoxy and metal plates and enclosed by a radiation shield box for its thermal isolation from the ambientchamber walls. Following evacuation of the chamber by a pressure of ∼ 10−3 − 10−4 Torr, the optical bench
is cooled down to and kept at 60–70 K with a refrigerator directly connected to the optical bench. A single
stage Giﬀord-McMahon cycle refrigerator RF-471 by AISIN SEIKI Co.,Ltd., with a cooling power of 140 W
at 70 K, is used.
The detectors (CCD and HgCdTe detector) in their container are placed on a cold plate connected tothe cooled optical bench through a narrow thermal path. The temperature of each detector is stabilized at
the appropriate level for its operation (173 K for the CCD and ∼ 75 K for the HgCdTe detector) by use ofa platinum thermometers and a resistance heater on the cold plate controlled by a temperature controller(model 331 by Lake Shore Cryogenics, Inc.).
In the recent operation of the instrument at ambient temperatures ranging from -5 to +15 degrees C, it
took 100 hours to cool the optical bench from room temperature to 60 K, following 38 hours evacuation of theTable 6. Design of the Wollaston prism.

Material
Number of components
Size (mm)Eﬀective aperture diameter
Wedge angle
Beam splitting angle
Image separation on the detector
Operating temperature
Wavelength range
Wavefront error
Other features

LiYF4 (YLF)
2
34×34×1230 mm
16◦ .39◦
0 .7685 (0.47 µm)–0◦ .7381 (2.4 µm)
4700 .80 (0.47 µm)–4500 .90 (2.4 µm)
80 K
0.5–2.4 µm
λ/2
Optical contact or adhesive (TBD)

Figure 4. Design of the Wollaston prism.

chamber by a pressure of 2 × 10−3 Torr. The temperature of the optical bench and pressure in the chamber
had been kept at 60–70 K and ≤ 10−5 Torr, respectively, for 36 days at least. In addition, further improvementof the cryogenic performance is planned by installing additional radiation shields and a sorption pump on thecold head of the refrigerator.

2.3 Detectors and Readout Electronics
HONIR equips two detector arrays and their controller systems for the optical arm and the IR arm #1 atpresent. The block diagram of the detector system is shown in Fig. 5.
For the optical arm, a fully-depleted back-illuminated CCD array with 2048×4096 pixels at a 15 µm pitch,
manufactured by Hamamatsu Photonics K. K.,10 is placed. Readout operation is conducted by the integrated
control system Messia 5,11 and the front-end electronics MFront2.12, 13 The detector temperature is stabilized
at 173 K by the cryogenic system. The active detector area has a 1:2 ratio rectangular shape, however, only
a half of the area is actually used for the imaging. Signals on pixels in four separated areas are read out inparallel at 133 kHz. A frame readout rate is 17.4 sec/frame for reading the whole pixels including prescan
and overscan pixels. A conversion factor is in a range of 1.54–2.15 electrons/ADU depending on the read out
ports. The readout noise is ∼8 electrons rms at the above readout rate.
For the IR #1 arm, one HgCdTe VIRGO-2K focal plane array with 2048×2048 pixels at a 20 µm pitch,
manufactured by Raytheon Company, is installed at present. The detector is cooled to around 75 K. Its
readout is also operated by the Messia 5 control system, with the multi-array control system MACS2 14 as afront-end electronics. The signals from four separate areas on the detector are read out in parallel at a rate of
236 kHz, and consequently a frame rate becomes 4.5 sec/frame to read out 2072×2050 pixels in total including
six reference pixels for each row and two reference rows. A conversion factor derived by measuring a photontransfer curve in a laboratory environment is 3.4 electrons/ADU. The signal response against incident light is
not deviated from an ideal linear relation by 1 % until 130,000 electrons accumulation. The dark current is
at a negligible level of lower than 0.1 electrons/sec. However, the readout noise is at very high level: 24–78
electrons rms (depending on reading ports) at a laboratory and 170–210 electrons rms on the telescope atpresent. This signiﬁcant readout noise has restricted detecting faint objects, and should be suppressed.
We are now developing a new readout electronic system for the VIRGO detector to replace the current
system. Its design is based on the Kiso Control Array operated on a newly developed Kiso Wide Field
Camera15 at Kiso Schmidt Telescope. The new system will have a function of 16 ports parallel readout, which
reduces a frame rate by 1.2 sec/frame and improves eﬃciency of data acquisition. The reduction of the readout
Cold Box

MFront2
MF2̲PRECCD

MF2̲SIG
Linux PC

CCD

ADC

MF2̲BIAS
clock, bias

Messia 5 CMC #1

MF2̲IF

Messia 5 CMC #2
DSP Board #2
Messia 5 system

Photo Isoliation

PCI Bus

DSP Board #1
ADC

preamp

CLOCK
MACS2

Figure 5. Block diagram of the detector system.

VIRGO

noise is also expected. In the near future, another set of an infrared detector and a readout system will bealso installed for the planned additional IR arm #2.

2.4 Mechatronics Design
HONIR has four rotating turrets to change optical elements inserted into the optical path. A focal mask turretis at the telescope focal plane, a cold stop mask turret is at the pupil plane just after the collimator lens in
the collimated beam, and two ﬁlter turrets in the collimated beam section in each branched arm.
Each of the turrets has bump switches for detecting its ﬁducial position angles and a stepping motor for its
rotation. We modiﬁed stepping motors P430-258-005 (Portescap) to be applicable for vacuum and cryogenic
use by replacing their oiled ball bearings with MoS2 -sputtered dry ball bearings (NTN Corp., Japan).1
All of the devices are operated by the integrated control system Motionnet (Nippon Pulse Motor Co., Ltd.),
which consists of a “Center Board” (PPCI-L112) as the main controller on a Windows PC and motor drives(MNET-BCD4020FB), one for each turret unit, cascadingly connected to each other.
In the future extension of the instrument, grism turrets for existing two arms, and a ﬁlter and grism turretpairs for another IR arm will be appended.

2.5 Optical Shutter
The optical shutter unit for a CCD imaging is mounted over the optical entrance window of the vacuum
chamber (Fig. 7). The unit consists of a black aluminum shutter plate with a rectangular aperture of 151
mm by 97 mm. A linear actuator SACR-S6DH-350BE (SUS Corporation), which equips a linear encoder andan AC servomotor, drives the shutter plate. The shutter plate travels along the long side of the aperture in asingle direction at appropriate variable speeds so that the exposure time on the CCD becomes uniform andat intended duration at every positions on the detector. The stability of the exposure time is better than 0.1
msec at the shortest exposure time of 0.3 sec.

(b)

(a)

(c)

Figure 6. The focal mask turret unit. (a) An overview of the turret unit, (b) the stepping motor, and (c) the bumpswitch for detecting one of the fiducial position angles.

3. INITIAL OBSERVATIONAL RESULTS
In the most recent test observation of the instrument attached on the Kanata telescope between October 2011
and February 2012, we veriﬁed its imaging performance by obtaining images of celestial objects. Fig. 8 shows
samples of the images processed by pseudo-color composition. In the central region of an image, the best image
size obtained was ∼ 0.9 arcsec fwhm at near-infrared bands and ∼ 1.7 arcsec fwhm at optical bands, including
blurring by seeing eﬀect and telescope tracking error. They are in generally at acceptable level. In the outerregion of the ﬁeld of view, however, apparent blurring and elongation of stellar images were observed. We
concluded that this degradation is due to incomplete alignment of the optical elements in the instrument. We
are improving it by replacing the lens holding parts and careful adjustment of the optical elements in future.
As a sample of photometric observation, light curves of the young stellar object MM Mon for seven days
measured at J, H, and Ks bands are shown in Fig. 9. Every data point was obtained from ﬁve dithered framesof 60 sec exposure each. Distinct photometric variations are detected at a photometric precision of about 0.01
mag at J and H bands, and about 0.02 mag at Ks band.

4. SUMMARY AND FUTURE PROSPECTS
We have developed a brand-new instrument HONIR for the 1.5-m Kanata telescope at Higashi-Hiroshima
Observatory. HONIR is designed as an imager and spectrograph with a polarimetry function that obtains
information of three wavelength bands among optical and near-infrared ranges simultaneously. A imaging
function of two wavelength bands (0.5–1.0 µm and 1.15–2.40 µm) has been already installed and operated
successfully in general so far. The remaining functions (spectroscopy, polarimetry, and another infrared
band arm) are under development and will be added in the near future. By using the powerful, multipurpose
capabilities of HONIR, we will proceed our observational research on transient or variable astronomical objects
at the Kanata telescope further.

ACKNOWLEDGMENTS
We are grateful to S. Sato, S. Sako, K. Okita, Y. Hirahara, M. Kino and K. Yanagisawa for helpful comments
and kind cooperation. This research has been supported in part by the Grant-in-Aid for Scientiﬁc Research(23244030, 23340048) from the JSPS and MEXT, Japan. Y.M., R.I. and M.S. are supported through the
JSPS (Japan Society for the Promotion of Science) Research Fellowship for Young Scientists. Evaluation of
performance of the optical elements was supported by Advanced Technology Center, National Astronomical
Observatory of Japan.

Figure 7. The shutter unit (left) and the aperture on the shutter plate moving over the entrance window across thehorizontal direction of the picture (right).

(a) M42 (V, J, Ks )(b) NGC891 (V, RC , IC )(c) NGC891 (J, H, Ks )Figure 8. Pseudo-color (blue-green-red) composite images taken by HONIR. (a) M42 (90 .2 × 90 .8; V-band: 20 sec;
J-band: 210 sec; Ks -band: 510 sec), (b) NGC891 at optical wavelengths (60 .2 × 90 .5; V-band: 360 sec; RC -band: 360
sec; IC -band: 360 sec); and (c) NGC891 at near-infrared wavelengths (J-band: 1200 sec; H-band: 1080 sec; Ks -band:
1080 sec).

Ks (mag)

10.2
10.3
10.4
10.5

H (mag)

10.8
10.9
11.0
11.1

J (mag)

11.5
11.6
11.7
11.8
55950

55952

55954
MJD

55956

55958

Figure 9. Light curves of the young stellar object MM Mon at J, H, and Ks bands.

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