ver.2017-03-28

Overview

Contact : winered-contact@cc.kyoto-su.ac.jp

WINERED (Warm INfrared Echelle spectrograph to Realize Extreme Dispersion and sensitivity) is anear-infrared high-resolution spectrograph developed by LiH. WINERED is a PI-type instrument, and is installedin the 3.58-meter New Technology Telescope (NTT) from 2017. WINERED has three distinctive features: warm
optics (no cold stop), wide spectral coverage (0.90−1.35 μm), and high sensitivity. WINERED has three observing

modes: “WIDE” (R=λ/ΔλFWHM=28,000) and “HIRES-Y&J” (R=68,000); the latter employs a specially designed
high-blazed echelle grating. HIRES-Y&J modes are going to be in science operation by the middle of 2017.

“Laboratory of Infrared High-resolution spectroscopy” (LiH) was established at the Koyama Astronomical
Observatory, Kyoto Sangyo University, in collaboration with the University of Tokyo and other domestic institutes/industries, forpursuing astrophysics, astrochemistry, astrobiology and planetary sciences as well as instrumentation, based on high-resolution
spectroscopic techniques in infrared wavelength region.
ModeCoverage‡

Throughput

λ/1

WINERED50%HIRES-Y&J

WIDE

Wavelength
coverage
GIANO (TNG)
IGRINS (McD)

WIDE

VINROUGE†

30%

IGRINS(McD)
APOGEE(SDSS)

10%

IRCS
(Subaru)

20K

WINEREDVINROUGE†

IRCS (Subaru)

iSHELL(IRTF)NIRSPEC(Keck2)

GIANO
(TNG)

HIRES-Y

HIRES-J

0.90 – 1.35 μm

0.96 – 1.11 μm

1.14 – 1.35 μm(z, Y, J bands)(Y band)(J band)Spectral resolution(R ≡ λ/ΔλFWHM)

28,00068,000†Throughput> 50 %> 35 %

Reflective echelle grating

Mosaicked high-blazed echelle grating

Main disperser

HIRES mode
HIRES-Y&J

APOGEE (SDSS)

Array

1.7 μm cut-off HAWAII-2RG

Size

1.75m(L) x 1.07m(W) x 0.50m(H)† : In the engineering observation on NTT, λ/ΔλFWHM ~ 55,000.

NIRSPEC (Keck2)

λ/10

iSHELL (IRTF)

CRIRES+(VLT)

60K
100K
Spectral Resolution

CRIRES+ (VLT)

WIDE

Telescope

20K

For commissioned instruments as of Y2015 (open circles show instruments close to commissioning).
† : VINROUGE is a high-resolution 2-5 μm spectrograph with Ge immersion grating, under development by LiH. First light is expected in Y2018.
‡ : Coverage is a wavelength range obtained simultaneously with a single grating setting, normalized with the center wavelength of the range.

60K
100K
Spectral Resolution

WIDE

HIRES

Slit width

0.54, 0.76 and 1.08 arcsec

Slit length

16.34 arcsec

Pixel scale

0.27 arcsec / pix

J-band limiting
magnitude†

15.6

15.9

16.2

14.2

14.6

14.8

(0.54 arcsec)(0.76 arcsec)(1.08 arcsec)(0.54 arcsec)(0.76 arcsec)(1.08 arcsec)† : S/N = 30, integration time = 8 hrs, magnitude per pixel.

ver.2017-03-28Instrumental Facts

Contact : winered-contact@cc.kyoto-su.ac.jp

Warm optics with no cold stop
1. Optics are at room temperature except for the infrared camera system (camera lenses and an infrared array).
2. Beneficial to reduce time and cost for development, alignment, and maintenance.

Wide spectral coverage
Achieved by a combination of decent optical design with a cross-dispersed echelle and a large format infrared array (2k x 2k).

High sensitivity
High throughput• Gratings with high diffraction efficiency- WIDE mode: replica echelle grating by Newport Co. (~83%), VPH cross-disperser (~86%).
- HIRES-Y&J modes: high-blazed echelle gratings by Canon Inc. (>70%), VPH cross-dispersers (~90%).
• Extremely-low reflection BBAR： R < 0.5% per lens surface.
• The minimum number of optical elements： no-use of white pupil optics.
• High Q.E. of an array： 1.7μm cut-off HAWAII-2RG (~86% @1.23μm).
Low noise• Low readout noise: σr=5.3 e- (NDR=32). Low-dark noise: σd< 2 e- (900sec)• Suppressed ambient thermal background (0.05e- /sec/pix @280 K) with custom thermal-cut filters .

Left: The measured thermal background radiation reaching the array for various the ambient temperatures. The difference of plots shows different
season. The solid line is a predicted flux with an assumption that the ambient environment is the block body. The dashed lines is the level of measured
stray light in the cryostat.
Right: Wavelength coverages of all the WINERED modes superimposed on an atmospheric transmission curve.

PI-type spectrograph• Compact [1.8m(L) x 1.1m(W) x 1.0m(H)] and light weight [~250kg].
• Attachable to any telescopes with a Nasmyth focus (slower than f/11).

WIDE mode

HIRES-Y&J modes

VPH X-disperser

Mosaiced high-blazed echelle grating

Array

270 lines/mm
120 mm × 100 mm

Calibration system
Th-Ar lamp (for comparison)
halogen lamp (for fielding)blaze angle : 79.32 deggroove pitch : 90.38 μm

HAWAII-2RG
1.7μm-cut off

Room temp.

Camera lensf = 280 mm
Φ = 128.25 mm

Echelle grating
blaze angle：63.75 deggroove pitch： 31.6 μm

Collimator lensf = 770 mm
Φ = 70 mm

Slit mirror
100 μm × 3.12 mm
200 μm × 3.12 mm

VPH X-disperser
Au mirror

724.80 line/mm (HIRES-Y mode)
540.48 line/mm (HIRES-J mode)

CCD slit viewer
λ = 600 - 900 nm

ver.2017-03-28

Observationalfacts
Facts
Observational: winered-contact@cc.kyoto-su.ac.jp
ContactContact: winered-contact@cc.kyoto-su.ac.jp
Observation

Quality of spectra• The high-sensitivity of WINERED enables us to obtain NIR high-resolution spectra with high signal-tonoise ratio in much shorter time, or bring us to unexplored faint-end by NIR high-resolution spectroscopy.
For example, WINERED mounted on a 10-m telescope equipped with AO can be used for the study of theabsorption line systems of z > 6 QSOs or GRBs (J > 18 mag).

Data reduction pipeline• Observers can select one of the three modes (WIDE, HIRES-Y&J) depending on their priority on spectral
resolution1 and wavelength coverage.
• Three slits of 100 μm-width (2-pix sampling), 140 μm-width (2.8-pix sampling) and 200 μm-width (4-pixsampling) are available.
• A sophisticated user interface customized for WINERED enables efficient observations.
1. Note that the WIDE and HIRES-Y&J modes cannot be switched during the observing night to avoid any hardware trouble.

• We developed the WINERED data-reduction pipeline, which automatically produces 1D spectra from raw
data in less than 20 minutes/frame.
• Automatic correction for telluric absorption, which is mandatory for infrared spectroscopy, is underdevelopment and is planned to be incorporated into the WINERED data-reduction pipeline.

WIDE mode

HIRES-Y&J modes

WIDE mode

HIRES-J ENGINEERING

Araki Telescope

Arcturus (K1.5Ⅲ)

Infraredspectraw/ WINEREDon ArakiTelescope(R = R=28,30028,000)
Infrared
spectraw/WINERED
on theAraki Telescope
Normalized flux +const

Araki Telescope

87654321Rigel (B8Iab)Y−bandHeavy telluricJ−bandProcyon (F5IV −V)
dCephei (F5Ib −G2Ib)
zGemini (F7Ib −G3Ib)
Arcturus (K1.5III)
Betelgeuse (M2Iab)
mCephei (M2Ia)

R=28,000

01.00

1.05

1.10

1.15

Wavelength [mm]

1.20

1.25

1.30

Araki Telescope

Araki Telescope

Araki Telescope