Sigma QUick Infrared Camera User Manual

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MIRSI: a Mid-InfraRed Spectrometer and Imager
Lynne K. Deutsch
*
a,b
, Joseph L. Hora
b
, Joseph D. Adams
a
, Marc Kassis
a
a
Boston University,
b
Harvard-Smithsonian Center for Astrophysics
ABSTRACT
MIRSI (Mid-InfraRed Spectrometer and Imager) is a mid-infrared camera system recently completed at Boston
University that has both spectroscopic and imaging capabilities. MIRSI is uniquely suited for studies of young stellar
objects and star formation, planetary and protoplanetary nebulae, starburst galaxies, and solar system objects such as
planets, asteroids, and comets. The camera utilizes a new 320 x 240 Si:As Impurity Band Conduction (IBC) array
developed for ground-based astronomy by Raytheon/SBRC. For observations at the Infrared Telescope Facility (IRTF),
MIRSI offers a large field of view (1.6 arcmin x 1.2 arcmin) with a pixel scale of 0.3 arcsec, diffraction-limited spatial
resolution, complete spectral coverage over the 8-14 µm and 17-26 µm atmospheric windows for both imaging (discrete
filters and circular variable filter) and spectroscopy (10 and 20 µm grisms), and high sensitivity (expected one-sigma
point source sensitivities of 5 and 20 mJy at 10 and 20 µm, respectively, for on-source integration time of 30 seconds).
MIRSI successfully achieved first light at the Mt. Lemmon Observing Facility (MLOF) in December 2001, and will
have its first observing run at the IRTF in November 2002. We present details of the system hardware and software and
results from first light observations.
Keywords: infrared astronomy, infrared arrays, mid-infrared instrumentation
1. INTRODUCTION
The MIRSI
1,2
system (http://mirador.bu.edu/mirsi/mirsi.html) was designed for the study of a number of astrophysical
phenomena that require thermal infrared observations in order to penetrate their warm, dusty environments. The system
has the capability to acquire both spectra and high-resolution, multi-wavelength images. This makes it possible to
unambiguously correlate the spatial and spectral features observed in astrophysical sources and thereby reveal the key
physical and chemical processes at work.
The MIRSI instrument concept had to satisfy several requirements to meet our scientific goals:
Operation over the 8-14
µ
m and 17-26
µ
m wavelength ranges.
Large field of view.
Diffraction-limited imaging.
In
imaging mode,
provide spectral resolution of up to 1% bandwidth for imaging of spectral features.
In
spectroscopic mode
, provide resolution of ~200, sufficient to resolve broad spectral features and detect
narrow spectral features.
Quick and easy selection of observing mode, with the flexibility to change observing parameters in real time.
Efficient, high throughput optics.
Telescope control capable of commanding offset, chop, and beamswitch.
Simple, real-time data reduction and quick-look capability.
Our design addresses each of these requirements. The camera system is based on a Raytheon/SBRC Si:As IBC CRC774
array with 320 x 240 pixels and a spectral range of 2-28
µ
m. The array is designed for high-flux applications and is read
out through 16 parallel readout lines. The system is housed in a cryostat containing LN
2
and LHe reservoirs attached to
an outer LN
2
radiation shield and an inner LHe shield, respectively. The main camera characteristics are summarized in
*
[email protected]du; phone; 60 Garden Street, MS-65, Cambridge, MA 02138-1516
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Summary of Contents

Page 1 - 1. INTRODUCTION

MIRSI: a Mid-InfraRed Spectrometer and Imager Lynne K. Deutsch*a,b, Joseph L. Horab, Joseph D. Adamsa, Marc Kassisa aBoston University, bHarvard-Smi

Page 2

parameters. The observing modes include: grab (which defines an exposure as a single on-source image), chop (which takes on- and off-source images by

Page 3

our observations, with a resulting effective aperture of about only 20 inches, a total FOV of 7 x 5 arcmin, and a diffraction limited PSF with a FWHM

Page 4 - 3. OPTICAL DESIGN

Table 1, and the array characteristics are given in Table 2. Details of the optical system, dewar, electronics, computer control, system integration

Page 5 - 4. ELECTRONICS

Figure 1. MIRSI dewar, side view. This is the orientation when the telescope is pointed at zenith. The LHe reservoir is in the center, the LN2 res

Page 6

An L-shaped bracket holding the detector electronics box is bolted to the end of the optics box section and to the camera interface plate. 3. OPTI

Page 7

distortion over the field, which is largest in the corners (at about 2.5 pixels). The distortion is not noticeable during observing and can be correc

Page 8

also contains two driver boards for setting and driving the detector bias and clock voltages, respectively. Four DSP coadder boards containing four ch

Page 9 - 5. SOFTWARE

Consequently, as replacement for the preamps, we fabricated a new signal cable to carry the signals from the dewar to the coadder board connectors. We

Page 10 - 6. FIRST LIGHT

We chose to employ continuous operation of the ROIC readout, with non-destructive exposure sequences, under the assumption of greater stability in ROI

Page 11 - REFERENCES

7.75:1, requiring 31000 steps and 1.5 minutes to complete one rotation. The filter wheel gear ratio also sets the positional accuracy of the CVF at ~

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