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Astronomy

Evolution of long wavelength astronomy sensors

End-user demands continue to push the state of the art and evolution of large format, impurity-band conductor detectors for both space- and ground-based telescopes.
28 June 2011, SPIE Newsroom. DOI: 10.1117/2.1201106.003786

Astronomers have been interested in performing observations in the very long wavelength infrared band (5–28μm) for decades. IR telescopes are useful to detect very cold or distant objects, so they are important for studying star formation regions, cold stars and extragalactic objects, among others. To this purpose, both ground- and space-based observatories have to be equipped with specific sensors that can collect infrared radiation. These so-called impurity band conductor (IBC) sensors have a sensitivity adequate to detect light in the desired spectral range (see Figure 1). They use impurities in the semiconductor to convert long-wavelength photons into an electrical current.

We have been manufacturing IBC detectors for many decades.1 These arrays, in multiple formats, can be found in numerous space and ground-based instruments. For example, NASA's Spitzer Space Telescope's Infrared Array Camera, for example, uses two IBC detectors and two InSb (Indium antimonide) detectors. Observers used this early instrument for a wide range of astronomical research programs and produced images such as those in Figure 2.

The success of Spitzer encouraged the use of large format (wider field of view) IBC arrays. With these devices, astronomers benefit from increased sky coverage and improved sensitivity, thereby decreasing observation time. For instance, we recently delivered 1k×1k IBC mid-infrared detectors to the Jet Propulsion Laboratory (JPL) for the Mid-Infrared Instrument. This device is expected to be on board the planned James Webb space telescope (JWST), successor of the famous Hubble telescope. JPL performed qualification testing and characterization of dark current (the excess current present when a detector has no incoming photons) and noise on these detectors, and both should be minimal for higher performance. While the results delivered by these new IBC arrays will have to wait until the launch of the JWST mission (now delayed by several years), tests showed that the devices met or exceeded key requirements such as noise and dark current.2


Figure 1. Spectral sensitivity of impurity band conductor (IBC) focal planes is well suited for space and ground based astronomy (the photon response to infrared light from 5 to 28μm is excellent).

Figure 2. Infrared images from the Spitzer Space Telescope. The image on the left shows the region in visible and short infrared, with most of the internal structure of the astronomical object obscured at these wavelengths. On the right, using long wavelength IBC detectors, much more of the internal structure is seen and can be analyzed. Infrared light at 4.5μm is represented in orange while light at 8.0μm and 24μm is represented in red (Courtesy NASA/JPL-Caltech).

In the meantime, ground-based telescope requirements have also been changing. Several instruments have used an IBC detector array mated to a custom integrated circuit that ‘reads out’ the individual pixel information, which is called a read-out integrated circuit (ROIC). The first ROIC custom-designed to operate with an IBC detector—CRC-774 (the 774th circuit produced by the Carlsbad Research Center)—consists of 320 columns × 240 rows of unit cells, each 50×50μm in size, with 16 or 32 selectable outputs arranged in blocks of 20 columns each. This particular design of IBC has been integrated into several instruments, including the Cooled Mid-infrared Camera and Spectrometer on the National Astronomical Observatory of Japan Subaru Telescope. This instrument demonstrates the power of IBC sensors to reveal complex dust structures in the mid-infrared wavelength band (see Figure 3).

Presently, the state-of-the-art IBC detector for ground-based telescopes is Aquarius-1k, a device we developed in collaboration with the European Southern Observatory (ESO). It is a 1024×1024, 30μm high-performance array featuring high quantum efficiency IBC detectors, low noise, low dark current, and on-chip clocking for ease of operation. The Aquarius-1k was designed and delivered primarily for ground-based astronomy applications. The focal plane arrays are currently undergoing initial system testing at ESO.

While the Aquarius-1k is mainly for use in ground-based observatories, the next generation instrument—Aquarius-2k—will also be appropriate for space-based astronomy. According to Chris Packham, an astronomer from the University of Florida (personal communication, May 11, 2011), “The 2k Aquarius array has been baselined for several instruments in their planning phase for use on the 30m-class of telescopes and NASA's SOFIA [Stratospheric Observatory for Infrared Astronomy] airborne telescope. The large format of the Aquarius makes it ideal where either a wide spectral range or a wide field of view is required by the science drivers of the instrument. Coupled with the sensitivity, readout noise and other key parameters of the Aquarius array, it is becoming the default option for instruments operating at 7–25μ. The science drivers are typically diverse, spanning the search of planets in discs around nearby stars to investigations of the effects of supermassive black holes in distant galaxies.”


Figure 3. Complex dust structures in the mid-infrared range. (Image used by permission of the National Astronomical Observatory of Japan, NAOJ, and is Copyright © Subaru Telescope, NAOJ. All rights reserved.)

Figure 4. Evolution of our IBC focal plane arrays. From left to right: SIRTF (Space Infrared Telescope Facility model used on Spitzer) 256×256, CRC-774 model 320×240, Aquarius 1024×1024, and Phoenix 2048×2048 devices.

In conclusion, we see that the evolution of IBC focal plane arrays is far from over as end-user demand consistently pushes for larger and larger formats with improved performance (e.g., lower noise and detector dark current, smaller unit cells, and greater ROIC functionality). In the future, we plan to collaborate with Japan's Aerospace Exploration Agency to reconfigure an existing 2048×2048, 25μm high performance array (named Phoenix) that will feature high quantum efficiency and state-of-the-art IBC detectors. This version will also incorporate flight qualified packaging to support space-based astronomy applications: see Figure 4 (far right).


Robert E. Mills, Eric Beuville, Elizabeth Corrales
Raytheon Vision Systems
Goleta, CA

Robert Mills is a senior focal plane design engineer. He has been involved in the design, test, and study of radiation effects on impurity band conductor sensors for 29 years.

Dr. Beuville is the primary readout electronics designer for astronomy arrays at RVS.

Mrs. Corrales is the program manager for astronomy programs at RVS.


References:
1. P. Love, E. Beuville, E. Corrales, J. J. Drab, A. W. Hoffman, R. S. Holcombe, 1024×1024 Si:As IBC detector arrays for mid-IR astronomy, Proc. SPIE 6276, pp. 62761Y, 2006. doi:10.1117/12.684504
2. M. E. Ressler, H. Cho, R. A. M. Lee, K. G. Sukhatme, J. J. Drab, G. Domingo, M. E. McKelvey, R. E. McMurray, Jr., J. L. Dotson, Performance of the JWST/MIRI Si:As detectors, Proc. SPIE 7021, pp. 70210O, 2008. doi:10.1117/12.789606