The NASA/ESA Hubble Space Telescope provides us with many lessons regarding the interplay between science and technology that will be applicable to future telescopes. In this talk, we will consider several “case studies” where technological choices and advances had profound impacts on the science from HST and, conversely, where science needs drove technical and operational plans. HST is unique amongst astronomy space missions by virtue of its multiple upgrades during servicing missions. Furthermore, HST has been fortunate to have operated during a period of dramatic improvements in computational and communications capabilities which have changed how the scientific community interacts with both the observatory and its data. We will discuss how this has influenced both the evolution of astronomical research, the continuing development HST’s systems, and implications for future missions.
The Cosmic Origins Spectrograph (COS) has been collecting data since soon after its installation on the Hubble Space Telescope in May 2009. The two-segment microchannel plate-based detector for the FUV channel is subject to gain sag, and eventually a permanent loss of efficiency at the locations where the largest number of counts have fallen. The initial strategy for the use of the detector was to maximize the scientific productivity of the instrument over the five-year design lifetime. This has been accomplished by periodically adjusting the high voltage and moving the spectra to a different location on the detector in order to spread the damage on the detector and thus minimize gain sag. The instrument is now well past this point and performing well, so in late 2016 we began to investigate ways to extend the life of the detector for as long as possible without seriously affecting the scientific performance. As a result of these studies, we adopted a new lifetime extension strategy when the spectra were moved to Lifetime Position 4 (LP4) in October 2017, and placed restrictions on the G130M observing modes that put Lyman-α airglow lines on the detector. Central wavelengths 1300, 1309, 1318, and 1327 are no longer permitted to illuminate Segment B of the detector, and G130M/1291 is permitted on that segment only for FP-POS values 3 and 4 in order to concentrate the damage to the detector. These changes limit the damage from gain sag “holes” due to airglow to only two locations on the detector, rather than the twenty at the previous LPs. In addition, we modified our previous approach of increasing the high voltage or changing LPs before any hole experienced a sensitivity loss of 5%, and will permit the two G130M/1291 holes to become permanently sagged, thus creating a new detector gap. Science programs that require wavelength coverage near the rest-frame Lyman-α region (1216 Å) can be executed at LP3. Observations with other gratings remain unaffected, but the wavelength coverage on Segment B for a single exposure will now include gaps due to the gain sag holes from the G130M/1291 observations. Models of gain loss as a function of exposure suggest that by adopting this strategy and giving up these small regions of the detector, we will be able to use LP4 productively for six or more years, as opposed to the ~2.5 years that was available at previous positions.
Synergy is an Explorer class mission concept to obtain a large-area, multi-tier near-ultraviolet sky survey with lowresolution, spatially resolved slitless spectroscopy (R = 200-600) and simultaneous arc-second imaging between 210-320 nm. It’s Wide and Deep surveys will examine the co-evolution of more than 200 million galaxies, 500,000 AGN, and 30,000 gas halos between 0.8 < z < 2 to constrain the multi-parameter physical relationships between gas, star formation history, mergers, AGN, and environment at the epoch when star formation peaked, half of galaxies transitioned from star-forming to passive, and the Hubble sequence first emerged. Many facilities in the 2020s will probe galaxies at this epoch, but the key tracers of diffuse gas over the 10 Gyr of cosmic time since z = 2 require ultraviolet observations.
We present the key scientific questions that can be addressed by GMOX, a Multi-Object Spectrograph selected for feasibility study as a 4th generation instrument for the Gemini telescopes. Using commercial digital micro-mirror devices (DMDs) as slit selection mechanisms, GMOX can observe hundreds of sources at R~5000 between the U and K band simultaneously. Exploiting the narrow PSF delivered by the Gemini South GeMS MCAO module, GMOX can synthesize slits as small as 40mas reaching extremely faint magnitude limits, and thus enabling a plethora of applications and innovative science. Our main scientific driver in developing GMOX has been Resolving galaxies through cosmic time: GMOX 40mas slit (at GeMS) corresponds to 300 pc at z ~ 1:5, where the angular diameter distance reaches its maximum, and therefore to even smaller linear scales at any other redshift. This means that GMOX can take spectra of regions smaller than 300 pc in the whole observable Universe, allowing to probe the growth and evolution of galaxies with unprecedented detail. GMOXs multi-object capability and high angular resolution enable efficient studies of crowded fields, such as globular clusters, the Milky Way bulge, the Magellanic Clouds, Local Group galaxies and galaxy clusters. The wide-band simultaneous coverage and the very fast slit configuration mechanisms also make GMOX ideal for follow-up of LSST transients.
The geometric distortion of the CCD detectors used in the Hubble Space TelescopeWide Field Camera 3 (WFC3)
and Advanced Camera for Surveys (ACS) instruments is characterized by both large and fine-scale distortions.
The large-scale distortion, due to the complexity of the HST optical assembly, can be modeled by a high-order
polynomial. The majority of fine-distortion is inherent to the CCD detectors themselves, which manifests itself
as fine-scale, correlated systematic offsets in the residuals from the best-fit polynomial solution. Such systematic
offsets across the CCD chip introduce astrometric errors at the level of about 0.1 pix (up to 1.5 μm within the 15
μm pixels). These fine-scale and low-amplitude distortions apparently arise from the spatial irregularities in the
pixel grid. For the WFC3/UVIS CCD chips, there is a clear pattern of periodic skew in the lithographic-mask
stencil imprinted onto the detector. Similar irregularities in the pixel grid of ACS/WFC CCD chips are even
more pronounced by the narrow (68×2048 pixel) lithographic-mask stencil. To remove these distortions, a 2-D
correction in the form of a look-up table has been developed using HST images of very dense stellar fields. The
post-correction of fine-scale astrometric errors can be removed down to the level of 0.01 pix (0.15 μm) or better.
KEYWORDS: Space telescopes, Telescopes, Data centers, Calibration, Electroluminescent displays, Solar processes, Algorithm development, Solar telescopes, Data processing, Observatories
Although the imagers on the Hubble Space Telescope only provide fields of view of a few square arc minutes, the telescope has been extensively used to conduct large surveys. These range from relatively shallow mappings in a single filter, multi-filter and multi-epoch surveys, and a series of increasingly deep exposures in several carefully selected fields. HST has also conducted extensive “parallel” surveys either coordinated with a prime instrument (typically using two cameras together) or as “pure” parallel observations to capture images of areas on the sky selected by another science programs (typically spectroscopic observations). Recently, we have tested an approach permitting much faster mapping with the WFC3/IR detector under GYRO pointing control and avoiding the overhead associated with multiple target observations. This results in a four to eight fold increase in mapping speed (at the expense of shallower exposures). This approach enables 250-300 second exposures (reaching H~25th magnitude) covering one square degree in 100 orbits.
We propose a novel approach to constructing a solar-blind near ultraviolet telescope using specialized mirror coatings. Each mirror in a three or four element optical system would have a coating reflective in the 200-300nm bandpass and transmissive at wavelengths longer than 300nm. This telescope can thus use CCD detectors providing high quantum efficiency, low noise, and a large pixel count. We have procured, from Materion Corporation, sample coatings with greater than 90% reflectance in the 200-300nm bandpass and less than 10% at wavelengths longer than 300nm. With three surfaces, these coatings provide <75% in band transmission for a telescope with better than 10,000 rejection at visible wavelengths. The use of ultraviolet optimized CCD detectors, combined with a three or four element telescope, would enable an Explorer class mission with near ultraviolet survey efficiency more than 100 times that of the recent GALEX mission. We will present measured reflectance and transmission curves from 200 - 1100nm for multiple samples. We will also show simulations of the expected performance of both 3 and 4 mirror systems for a conceptual space mission.
Vega is one of only a few stars calibrated against an SI-traceable blackbody, and is the historical flux standard. Photometric zeropoints of the Hubble Space Telescope’s instruments rely on Vega, through the transfer of its calibration via stellar atmosphere models to the suite of standard stars. HST’s recently implemented scan mode has enabled us to develop a path to an absolute SI traceable calibration for HST IR observations. To fill in the crucial gap between 0.9 and 1.7 micron in the absolute calibration, we acquired -1st order spectra of Vega with the two WFC3 infrared grisms. At the same time, we have improved the calibration of the -1st orders of both WFC3 IR grisms, as well as extended the dynamic range of WFC3 science observations by a factor of 10000. We describe our progress to date on the WFC3 ‘flux calibration ladder’ project to provide currently needed accurate zeropoint measurements in the IR
Wide Field Camera 3 (WFC3) is the most used instrument on board the Hubble Space Telescope. Providing a broad range of high quality imaging capabilities from 200 to 1700mn using Silicon CCD and HgCdTe IR detectors, WFC3 is fulfilling both our expectations and its formal requirements. With the re-establishment of the observatory level "spatial scan" capability, we have extended the scientific potential ofWFC3 in multiple directions. These controlled scans, often in combination with low resolution slit-less spectroscopy, enable extremely high precision differential photometric measurements of transiting exo-planets and direct measurement of sources considerably brighter than originally anticipated. In addition, long scans permit the measurement of the separation of star images to accuracies approaching 25 micro-arc seconds (a factor of 10 better than prior FGS or imaging measurements) enables direct parallax observations out to 4 kilo-parsecs. In addition, we have employed this spatial scan capability to both assess and improve the mid spatial frequency flat field calibrations.
WFC3 uses a Teledyne HgCdTe 1014xl014 pixel Hawaii-lR infrared detector array developed for this mission. One aspect of this detector with implications for many types of science observations is the localized trapping of charge. This manifests itself as both image persistence lasting several hours and as an apparent response variation with photon arrival rate over a large dynamic range. Beyond a generally adopted observing strategy of obtaining multiple observations with small spatial offsets, we have developed a multi-parameter model that accounts for source flux, accumulated signal level, and decay time to predict image persistence at the pixel level. Using a running window through the entirety of the acquired data, we now provide observers with predictions for each individual exposure within several days of its acquisition.
Ongoing characterization of the sources on infrared background and the causes of its temporal and spatial variation has led to the appreciation of the impact of He I 1.083 micron emission from the earth's atmosphere. This adds a significant and variable background to the two filters and two grisms which include this spectral feature when the HST spacecraft is outside of the earth's shadow.
After nearly five years in orbit, long term trending of the scientific and engineering behavior of WFC3 demonstrates excellent stability other than the expected decline in CCD charge transfer efficiency. Addition of post-flash signal to images is shown to markedly improve the transfer efficiency for low level signals. Combined with a pixel based correction algorithm developed at STScl, CCD performance is stabilized at levels only slightly degraded from its initial values.
Devices in low Earth orbit are particularly susceptible to the cumulative effects of radiation damage and the Hubble
Space Telescope Wide Field Camera 3 (HST/WFC3) UVIS detectors, installed on HST in May 2009, are no exception.
Such damage not only generates new hot pixels but also generates charge traps which degrade the charge transfer
efficiency (CTE), causing a loss in source flux as well as a systematic shift in the object centroid as the trapped charge is
slowly released during readout. Based on an analysis of internal and external monitoring data, we provide an overview
of the consequences of the ~3 years of radiation damage to the WFC3 CCD cameras. The advantages and disadvantages
of available mitigation options are discussed, including use of the WFC3 post-flash and charge injection modes now
available to observers, and the status of an empirical pixel-based correction similar to the one adopted for the HST
Advanced Camera for Surveys (ACS).
Like essentially all IR arrays, the IR detector in the Wide Field Camera 3 (WFC3) instrument on-board Hubble Space
Telescope (HST) exhibits afterimages, known as persistence, following exposures to light levels that approach or
exceed saturation of individual pixels of the detector. The nature of the persistence in the HgCdTe WFC3/IR detector is
distinctly non-linear in that the amount of persistence is not simply proportional to the exposure level. Instead, the
amount of persistence is small until the exposure reaches about half saturation at which point it rises fairly rapidly until
the exposure reaches about twice saturation and then it increases gradually with increasing saturation. The persistence
shows typical power law decay with time over the periods of time that are relevant to HST observations. Given the
frequent usage of the WFC3/IR detector on HST, it is not possible to completely avoid the effects of persistence in
observations obtained with HST by introducing time gaps between IR observations. Therefore, we have developed a
parameterized persistence model that we are using to estimate the amount of persistence in all WRC3/IR images. These
estimates are available for all existing WFC3/IR images through the Mikulski Archive at STScI (MAST) to help HST
users remove persistence from their images. Here we discuss the characterization of persistence in the WFC3 detector in
orbit, the fraction of observations that are affected by persistence, and the effectiveness of the tools we have developed
to reduce the effects of persistence in WFC3 images.
The WFC3 is the primary science instrument on HST. It accounts for over half of all observations since its installation
during SM4 in May 2009. We discuss the evolution of our understanding of the performance of WFC3 and our
calibration strategies. A key aspect of WFC3 is its high degree of stability which permits steadily improving calibrations.
We discuss four main topics: the calibration and trending of photometric and astrometric observations, the techniques we
are using to achieve markedly improved flat field calibrations (and their associated challenges), the evolution of the
WFC3 CCD and HgCdTe detectors in the space environment, and the recent implementation of a spatial scanning
observing technique which enables very high signal to noise ratio observations of bright sources including exo-planets
and also high precision astrometry.
Installed in the Hubble Space Telescope (HST) in May 2009, the Wide Field Camera 3 (WFC3) is performing extremely
well on-orbit. Designed to complement the other instruments on-board the Hubble Space Telescope (HST) and enhance
the overall science performance of the observatory, WFC3 is effectively two instruments in one. The UVIS channel,
with its pair of e2v 4Kx2K CCD chips provides coverage from 200 to 1000 nm while the IR channel, with a Teledyne
HgCdTe focal plane array (FPA) on a Hawaii-1R multiplexer, covers the 800-1700 nm range. This report summarizes
the performance of the WFC3 detectors, including primary characteristics such as quantum efficiency, read noise, dark
current levels, and cosmetics, as well as hysteresis prevention and the impact of radiation damage in the CCDs. In
addition, we discuss effects in the IR detector such as persistence, count rate non-linearity, 'snowballs', and 'negative'
cosmic rays.
The Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) is fitted with three grisms for slitless spectroscopy.
In the UVIS channel there is one grism, G280, for the near-UV to visible range (200 - 400nm;
1.4nm/pix). The IR channel has two grisms: G102 for the shorter (800-1150nm; 2.45nm/pix) and G141 for the
longer (1100-1700nm; 4.65nm/pix) NIR wavelengths. Using Servicing Mission Observatory Verification (SMOV)
and Cycle 17 calibration data we have assessed the performance of the grisms. We have measured the fielddependent
trace locations and dispersion solutions and determined the throughputs. The trace and wavelength
solutions for the IR grisms were found to be linear functions, varying smoothly across the field of view. The UVIS
grism exhibits a highly bent trace and significantly non-linear dispersion solutions. The maximum throughputs
for the G102 and G141 grisms, including the telescope optics, are 41% at 1100 nm and 48% at 1450 nm, respectively.
Limiting magnitudes at S/N=5 and a 1h exposure are JAB=22.6 and HAB=22.9 for the G102 and G141
grisms, respectively. The calibration results are published in the form of sensitivity and configuration files that
can be used with our dedicated extraction software aXe to reduce WFC3 slitless data.
We now know that the flux of a source measured with HgCdTe arrays is not a simple, linear function, but depends on the
count-rate as well as the total number of counts. In addition to the count-rate non-linearity (and probably related to the
same physical mechanism), HgCdTe detectors are also susceptible to image persistence. Most of the persistence image
fades in a few minutes, but there is a longer-term component that can result in faint afterimages in the next orbit,
approximately 45 minutes later. For sources saturated at ~100 times full-well, the afterimages can persist for hours
afterwards. This report describes results from ground and on-orbit tests to characterize the persistence and the count-rate
non-linearity in the WFC3 IR detector during its first year of operation.
The Wide Field Camera 3 (WFC3) was installed into the Hubble Space Telescope during Servicing Mission 4 in May
2009. This panchromatic camera considerably improves the ultraviolet, visible, and infrared imaging capabilities of
HST. Commissioned over the summer of 2009, WFC3 is now fully functional and responsible for approximately half of
the Cycle 17 HST Science Program. This paper will review the scientific performance of WFC3 including its sensitivity
in absolute terms and relative to other HST instruments. The paper will also discuss the calibration programs for WFC3
and the achieved photometric and astrometric calibration accuracies. Lessons learned from the ground calibration and in-flight
commissioning will also be considered.
In ground testing of the Hubble Space Telescope Wide Field Camera 3 (HST/WFC3), the CCDs of its UV/visible channel exhibited an unanticipated quantum efficiency hysteresis (QEH) behavior. The QEH first manifested itself as an occasionally observed contrast in response across the format of the CCDs, with an amplitude of typically 0.1-0.2% or less at the nominal -83°C operating temperature, but with contrasts of up to 3-5% observed at warmer temperatures. The behavior has been replicated in the laboratory using flight spare detectors and has been found to be related to an initial response deficiency of ~5% amplitude when the CCDs
are cooled with no illumination. A visible light flat-field (540nm) with a several times full-well signal level is found to pin the detector response at both optical (600nm) and near-UV (230nm) wavelengths, suppressing the QEH behavior. We have characterized the timescale for the detectors to become unpinned (days for significant
response loss at -83°C and have developed a protocol to stabilize the response in flight by flashing the WFC3 CCDs with the instrument's internal calibration system.
The IRMOS (Infrared Multiobject Spectrometer) is a multi-object imaging dispersive spectrometer for
astronomy, with a micromirror array to select desired objects. In standard operation, the mirrors are used to
select multiple compact sources such that their resulting spectra do not overlap on the detector. The IRMOS
can also be operated in a Hadamard mode, in which the spectra are allowed to overlap, but are modulated by
opening the mirrors in many combinations to enable deconvolution of the individual spectra. This mode
enables integral field spectroscopy with no penalty in sensitivity relative to the standard mode. There are
minor penalties in overhead and systematics if there are sky or instrumental drifts. We explain the concept and
discuss the benefits with an example observation of the Orion Trapezium using the 2.1 m telescope at Kitt
Peak National Observatory.
The Wide-field Camera 3 (WFC3) is a fourth-generation instrument planned for installation in Hubble Space Telescope
(HST). Designed as a panchromatic camera, WFC3's UVIS and IR channels will complement the other instruments onboard
HST and enhance the observatory's scientific performance. UVIS images are obtained via two 4096×2051 pixel
e2v CCDs while the IR images are taken with a 1024×1024 pixel HgCdTe focal plane array from Teledyne Imaging
Sensors. Based upon characterization tests performed at NASA/GSFC, the final flight detectors have been chosen and
installed in the instrument. This paper summarizes the performance characteristics of the WFC3 flight detectors based
upon component and instrument-level testing in ambient and thermal vacuum environments.
Wide Field Camera 3 is the next generation of Hubble Space Telescope imaging instruments. Designed to complement
and extend the existing capabilities of the HST, WFC3 will provide large increases in scientific performance in the near
ultraviolet and near infrared wavelength regions. This paper describes the scientific capabilities of WFC3, provides a
projection of its anticipated scientific performance, and discusses the plans for on-orbit testing and calibration during the
Servicing Mission Orbital Verification period.
Wide Field Camera 3 (WFC3) is a powerful UV/visible/near-infrared camera that has just completed development for
installation into the Hubble Space Telescope during upcoming Servicing Mission 4. WFC3 provides two imaging
channels. The UVIS channel incorporates a 4102 × 4096 pixel CCD focal plane with sensitivity from 200 to 1000 nm
and a 162 × 162 arcsec field of view. The UVIS channel features unprecedented sensitivity and field of view in the near
ultraviolet for HST, as well as a rich filter set that complements the visible capabilities of the HST/Advanced Camera for
Surveys, whose repair will be attempted in the Servicing Mission. The IR channel features a 1024 × 1024 pixel HgCdTe
focal plane covering 850 to 1700 nm with a 136 × 123 arcsec field of view, providing a major advance in IR survey
efficiency for HST. We report here on the design of the instrument, on recent activities that have completed the
integration of the instrument for flight, and on results of the ground test and calibration program.
Wide Field Camera 3 (WFC3), a panchromatic imager developed for the Hubble Space Telescope (HST), is fully
integrated with its flight detectors and has undergone several rounds of ground testing and calibration at Goddard Space
Flight Center (GSFC). The testing processes are highly automated, with WFC3 and the optical stimulus, which is used to
provide external targets and illumination, being commanded by coordinated computer scripts. All test data are captured
and stored in the long-term Hubble Data Archive. A full suite of instrument characterization and calibration tests has
been performed, including the measurement of key detector properties such as dark current, read noise, flat field
response, gain, linearity, and persistence, as well as instrument-level properties like total system throughput, imaging
quality and encircled energy, grism dispersions, IR thermal background, and image stability. Nearly all instrument
characteristics have been shown to meet or exceed expectations and requirements.
The Universe appears to be expanding at an accelerating rate, driven by a mechanism called Dark Energy. The nature of Dark Energy is largely unknown and needs to be derived from observation of its effects. JEDI (Joint Efficient Dark-energy Investigation) is a candidate implementation of the NASA-DOE Joint Dark Energy Mission (JDEM). It will probe the effects of Dark Energy in three independent ways: (1) using Type Ia supernovae as cosmological standard candles over a range of distances, (2) using baryon acoustic oscillations as a cosmological standard ruler over a range of cosmic epochs, and (3) mapping the weak gravitational lensing distortion by foreground galaxies of the images of background galaxies at different distances. JEDI provides crucial systematic error checks by simultaneously applying these three independent observational methods to derive the Dark Energy parameters. The concordance of the results from these methods will not only provide an unprecedented understanding of Dark Energy, but also indicate the reliability of such an understanding. JEDI will unravel the nature of Dark Energy by obtaining observations only possible from a vantage point in space, coupled with a unique instrument design and observational strategy. Using a 2 meter-class space telescope with simultaneous wide-field imaging (~ 1 deg2, 0.8 to 4.2 μm in five bands) and multi-slit spectroscopy (minimum wavelength coverage 1 to 2 μm), JEDI will efficiently execute the surveys needed to solve the mystery of Dark Energy.
Wide Field Camera 3 (WFC3) is a powerful UV/visible/near-infrared camera currently in development for installation
into the Hubble Space Telescope. WFC3 provides two imaging channels. The UVIS channel features a 4096 x 4096
pixel CCD focal plane covering 200 to 1000 nm wavelengths with a 160 x 160 arcsec field of view. The UVIS channel
provides unprecedented sensitivity and field of view in the near ultraviolet for HST. It is particularly well suited for
studies of the star formation history of local galaxies and clusters, searches for Lyman alpha dropouts at moderate
redshift, and searches for low surface brightness structures against the dark UV sky background. The IR channel features
a 1024 x 1024 pixel HgCdTe focal plane covering 800 to 1700 nm with a 139 x 123 arcsec field of view, providing a
major advance in IR survey efficiency for HST. IR channel science goals include studies of dark energy, galaxy
formation at high redshift, and star formation. The instrument is being prepared for launch as part of HST Servicing
Mission 4, tentatively scheduled for late 2007, contingent upon formal approval of shuttle-based servicing after
successful shuttle return-to-flight. We report here on the status and performance of WFC3.
The Infrared Multi-Object Spectrometer employs a novel approach to slit definition by using a rapidly configured array
of 848 x 600 MEMS mirrors. Developed by a collaboration between STScI, NASA/GSFC, and KPNO, IRMOS provides
low to medium resolution spectroscopy of several tens of simultaneous targets in the Z, J, H, and K bands. IRMOS is
presently undergoing commissioning to become a facility instrument at Kitt Peak National Observatory in 2006. We
report on the success of this concept, the performance of the Texas Instruments DMD array of MEMS mirrors in this
application, and our ongoing software development. Examples of observations using both a "Point and Click" approach
to slit positioning and the synthesis of full aperture integral field spectroscopy using Hadamard slit mask patterns are
presented.
Wide-Field Camera 3 (WFC3) has been built for installation on the Hubble Space Telescope (HST) during the next servicing mission. The WFC3 instrument consists of both a UVIS and an IR channel, each with its own complement of filters. On the UVIS side, a selectable optical filter assembly (SOFA) contains a set of 12 wheels that house 48 elements (42 full-frame filters, 5 quadrant filters, and 1 UV grism). The IR channel has one filter wheel which houses 17 elements (15 filters and 2 grisms). While the majority of UVIS filters exhibited excellent performance during ground testing, a subset of filters showed filter ghosting; improved replacements for these filters have been procured and installed. No filter ghosting was found in any of the IR filters; however, the new IR detector for WFC3 will have significantly more response blueward of 800 nm than the original detector, requiring that two filters originally constructed on a fused silica substrate be remade to block any visible light transmission. This paper summarizes the characterization of the final complement of the WFC3 UVIS and IR filters, highlighting improvements in the replacement filters and the projected benefit to science observations.
Wide Field Camera 3 (WFC3), a panchromatic imager being developed for the Hubble Space Telescope (HST), is now
fully integrated and has undergone extensive ground testing at Goddard Space Flight Center, in both ambient and
thermal-vacuum test environments. The thermal-vacuum testing marks the first time that both of the WFC3 UV/Visible
and IR channels have been operated and characterized in flight-like conditions. The testing processes are completely
automated, with WFC3 and the optical stimulus that is used to provide external targets and sources being commanded
by coordinated computer scripts. All test data are captured and stored in the long-term Hubble Data Archive. A full suite
of instrument calibration tests have been performed, including measurements of detector properties such as dark current,
read noise, flat field response, gain, linearity, and persistence, as well as total system throughput, encircled energy,
grism dispersions, IR thermal background, and image stability tests. Nearly all instrument characteristics have been
shown to meet or exceed expectations and requirements. Solutions to all issues discovered during testing are in the
process of being implemented and will be verified during future ground tests.
Wide Field Camera 3 (WFC3) is a panchromatic UV/visible/near-infrared camera whose development is currently nearing completion, for a planned installation into the Hubble Space Telescope. WFC3 provides two imaging channels. The UVIS channel features a 4096 × 4096 pixel CCD focal plane with sensitivity from 200 to 1000 nm and a 160 × 160 arcsec field of view. The UVIS channel provides unprecedented sensitivity and field of view in the near ultraviolet for HST. The IR channel features a 1014 × 1014 pixel HgCdTe focal plane covering 800 to 1700 nm with a 139 × 123 arcsec field of view, providing a substantial advance in IR survey efficiency for HST. The construction of WFC3 is nearly complete, and the instrument is well into its integration and test program. At the time of this writing (July 2004) the manned HST Servicing Mission 4 that was intended to install WFC3 and other hardware has been cancelled, but a robotic servicing possibility is under intensive investigation. We present the current status and performance of the instrument and also describe some aspects of WFC3 that are relevant to a robotic installation.
KEYWORDS: Digital micromirror devices, Mirrors, Sensors, Telescopes, Infrared spectroscopy, Spectroscopy, Space telescopes, Astronomical imaging, Micromirrors, James Webb Space Telescope
The Infrared Multi-Object Spectrometer (IRMOS) is an innovative near-IR instrument employing an array of MEMS micro mirrors for focal plane target selection. IRMOS is a joint project of the Space Telescope Science Institute, the NASA James Webb Space Telescope, and the Kitt Peak National Observatory and will shortly become available to the community at Kitt Peak. IRMOS uses a Texas Instruments 848x600 element DMD as a micro mirror array to synthesize slits to obtain up to 100 simultaneous spectra. It provides R~300, 1000, and 3000 spectroscopy in the J, H, and K bands plus R~1000 in Z together with imaging in all bands. Designed for the KPNO 4 and 2.1-meter telescopes, IRMOS will provide 3x2 and 6x4 arc minute fields of view on these telescopes. We describe the design and status of IRMOS, summarize its expected performance, and present early test data from system level lab tests.
We present the science case, design overview and sensitivity estimate for the design study for the WIYN High Resolution Infrared Camera (WHIRC). The WIYN telescope is an active 3.5 m telescope located at an excellent seeing site on Kitt Peak and operated by University of Wisconsin, Indiana University, Yale University and National Optical Astronomical Observatory (NOAO). As a dedicated near-infrared (0.8-2.5 micron) camera on the WIYN Tip-Tilt Module (WTTM), WHIRC will provide near diffraction limited imaging, i.e. FWHM~0.25" typically and 0.12" on exceptional nights. The optical design goal is to use a 2048x2048 HgCdTe array with a plate scale of 0.09" per pixel, resulting in a field of view (FOV), 3'x3', which is a compromise between the highest angular resolution achievable and the largest FOV correctable by WTTM. WHIRC will be used for high definition near-infrared imaging studies such as star formation, proto-planetary disks, galactic dust enshrouded B clusters, dust enshrouded stellar populations in nearby galaxies, and supernova and gamma-ray burst searches.
KEYWORDS: Mirrors, Telescopes, Digital micromirror devices, Optical alignment, Infrared spectroscopy, Optical design, Point spread functions, Spectroscopy, Space telescopes, James Webb Space Telescope
The Infrared Multi-Object Spectrometer (IRMOS) is a principle investigator-class instrument for the Kitt Peak National Observatory 2.1 m and Mayall 3.8 m telescopes. IRMOS is a near-IR (0.8-2.5 micron) spectrometer with low- to mid-resolving power (R = λ/Δλ = 300-3000). On the 3.8 m telescope, IRMOS produces simultaneous spectra of ~100 objects in its 2.8 x 2.0 arcmin field of view using a commercial micro electro-mechanical systems (MEMS) digital micro-mirror device (DMD) from Texas Instruments. The multi-mirror array DMD operates as a real-time programmable slit mask. The all-reflective optical design consists of two imaging subsystems. The focal reducer images the focal plane of the telescope onto the DMD field stop, and the spectrograph images the DMD onto a large-format detector. The instrument operates at ~90 K, cooled by a single electro-mechanical cryocooler. The bench and all components are made from aluminum 6061. There are three cryogenic mechanisms. We describe laboratory integration and test of IRMOS before shipment to Kitt Peak National Observatory. We give an overview of the optical alignment technique and integration of optical, mechanical, electrical and cryogenic subsystems. We compare optical test results to model predictions of point spread function size. We discuss some lessons learned and conclude with a prediction for performance on the telescope.
We present the performance of the IR detectors developed for the WFC3 project. These are HgCdTe 1Kx1K devices with cutoff wavelength at 1.7 μm and 150K operating temperature. The two selected flight parts, FPA#64 (prime) and FPA#59 (spare) show quantum efficiency higher than 80% at λ=1.6 μm and greater than 40% at λ>1.1μm, readout noise of ~25 e- rms with double correlated sampling, and mean dark current of ~0.04 e/s/pix at 150K. We also report the results obtained at NASA GSFC/DCL on these and other similar devices in what concerns the QE long-term stability, intra-pixel response, and dark current variation following illumination or reset.
Wide Field Camera 3 is a fourth generation instrument for the
Hubble Space Telescope (HST), to be installed during the next HST Servicing Mission 4. For its infrared channel Rockwell Scientific Company has developed a new type of HgCdTe 1Kx1K detector, called WFC3-1R, with cutoff wavelength at 1.7μm and 150K operating temperature. The WFC3-IR detectors are based on HgCdTe MBE grown on a CdZnTe substrate and use a new type of multiplexer, the Hawaii-1R
MUX. Two flight detectors, a prime and a spare, have been recently selected on the basis of the measures performed at NASA Goddard Research Center - Detector Characterization Laboratory. These parts show quantum efficiency higher than 80% at λ=1.6μm and greater than 40% at λ>1.1μm, readout noise of ~25 e- rms with double correlated sampling, and mean dark current of ~0.04 e/s/pix at 150K. We show that the IR channel of WFC3, equipped with one of these flight detectors, beats the instrument requirements in all configurations and promises to have a discovery efficiency
significantly higher than NICMOS. In particular, a two-band
wide-area, deep survey made with WFC3 exceeds the discovery
efficiency of NICMOS before and after the installation of NCS
by a factor of 15 and 10, respectively.
We describe the population, optomechanical alignment, and alignment verification of near-infrared gratings on the grating wheel mechanism (GWM) for the Infrared Multi-Object Spectrometer (IRMOS). IRMOS is a cryogenic (80 K), principle investigator-class instrument for the 2.1 m and Mayall 3.8 m telescopes at Kitt Peak National Observatory, and a MEMS spectrometer concept demonstrator for the James Webb Space Telescope.
The GWM consists of 13 planar diffraction gratings and one flat imaging mirror (58x57 mm), each mounted at a unique compound angle on a 32 cm diameter gear. The mechanism is predominantly made of Al 6061. The grating substrates are stress relieved for enhanced cryogenic performance. The optical surfaces are replicated from off-the-shelf masters. The imaging mirror is diamond turned. The GWM spans a projected diameter of ~48 cm when assembled, utilizes several flexure designs to accommodate potential thermal gradients, and is controlled using custom software with an off-the-shelf controller.
Under ambient conditions, each grating is aligned in six degrees of freedom relative to a coordinate system that is referenced to an optical alignment cube mounted at the center of the gear. The local tip/tilt (Rx/Ry) orientation of a given grating is measured using the zero-order return from an autocollimating theodolite. The other degrees of freedom are measured using a two-axis cathetometer and rotary table. Each grating's mount includes a one-piece shim located between the optic and the gear. The shim is machined to fine align each grating. We verify ambient alignment by comparing grating diffractive properties to model predictions.
The Infrared Multi-Object Spectrometer (IRMOS) is a principle investigator class instrument for the Kitt Peak National Observatory 4 and 2.1 m telescopes. IRMOS is a near-IR (0.8 - 2.5 μm) spectrometer with low- to mid-resolving power (R = 300 - 3000). IRMOS produces simultaneous spectra of ~100 objects in its 2.8 - 2.0 arc-min field of view (4 m telescope) using a commercial Micro Electro-Mechanical Systems (MEMS) micro-mirror array (MMA) from Texas Instruments. The IRMOS optical design consists of two imaging subsystems. The focal reducer images the focal plane of the telescope onto the MMA field stop, and the spectrograph images the MMA onto the detector. We describe ambient breadboard subsystem alignment and imaging performance of each stage independently, and ambient imaging performance of the fully assembled instrument. Interferometric measurements of subsystem wavefront error serve as a qualitative alignment guide, and are accomplished using a commercial, modified Twyman-Green laser unequal path interferometer. Image testing provides verification of the optomechanical alignment method and a measurement of near-angle scattered light due to mirror small-scale surface error. Image testing is performed at multiple field points. A mercury-argon pencil lamp provides a spectral line at 546.1 nm, a blackbody source provides a line at 1550 nm, and a CCD camera and IR camera are used as detectors. We use commercial optical modeling software to predict the point-spread function and its effect on instrument slit transmission and resolution. Our breadboard and instrument level test results validate this prediction. We conclude with an instrument performance prediction for cryogenic operation and first light in late 2003.
We present the results of an on-going test program designed to empirically determine the effects of different stress relief procedures for aluminum mirrors. Earlier test results identified a preferred heat treatment for flat and spherical mirrors diamond turned from blanks cut out of Al 6061-T651 plate stock. Further tests were performed on mirrors from forged stock to measure the effect of this variable on cryogenic performance. The mirrors are tested for figure error and radius of curvature at room temperature and at 80 K for at least three thermal cycles. We correlate the results of our optical testing with heat treatment and metallographic data.
The Infrared Multi-Object Spectrograph (IRMOS) is a facility instrument for the Kitt Peak National Observatory Mayall Telescope (3.8 meter). IRMOS is a low- to mid-resolving power (R = λ/Δλ = 300-3800), near-IR (0.8-2.5 µm) spectrograph that produces simultaneous spectra of ~100 objects in its 2.8 × 2.0 arcmin field of view using a real-time programmable, multi-aperture field stop.
The instrument operating temperature is ~80 K to allow for IR detector operation and for improved K-band performance. The optical bench and mirrors are machined from aluminum 6061-T651, allowing easier ambient temperature optical alignment. IRMOS utilizes four powered mirrors, three flat mirrors, two rotary mechanisms, one linear mechanism, a commercial MEMS multi-mirror array device and a large format, HgCdTe detector. The final design of the instrument and all of its components evolved through several iterations and a series of requirement/feasibility trades. During the design process, we found the heritage of past instruments with similar operating conditions to be invaluable in understanding our challenge, maximizing performance, and minimizing cost. The decision-making process of our design, as well as some of the major technical achievements, are described from a systems point of view in order to provide a list of "lessons learned" for future cryogenic instrument design and construction.
The Infrared Multi-Object Spectrometer (IRMOS) is an innovative near-IR instrument approaching completion. IRMOS will provide R~300, 1000, and 3000 spectroscopy in the J, H, and K bands plus R~1000 in Z together with imaging in all bands. Using a Texas Instruments 848x600 element DMD as a micro mirror array to synthesize slits in an imaging spectrometer obtaining up to 100 simultaneous spectra will be possible. Designed for the KPNO 4 and 2.2 meter telescopes, IRMOS will provide 3x2 and 6x4 arc minute fields of view on these telescopes. IRMOS is constructed mainly of 6061 Aluminum using diamond machined optics which has permitted a complex, compact, all reflective optical design. We describe the design and status of IRMOS, summarize its expected performance, and discuss several interesting aspects of its development and the use of TI DMD devices. IRMOS is a joint project of the Space Telescope Science Institute, the NASA Next Generation Space Telescope Project, and the Kitt Peak National Observatory.
The Infrared Multi-Object Spectrometer (IRMOS) is a facility-class instrument for the Kitt Peak National Observatory 4 and 2.l meter telescopes. IRMOS is a near-IR (0.8-2.5 μm) spectrometer and operates at ~80 K. The 6061-T651 aluminum bench and mirrors constitute an athermal design. The instrument produces simultaneous spectra at low- to mid-resolving power (R = λ/Δλ = 300-3000) of ~100 objects in its 2.8×2.0 arcmin field.
We describe ambient and cryogenic optical testing of the IRMOS mirrors across a broad range in spatial frequency (figure error, mid-frequency error, and microroughness). The mirrors include three rotationally symmetric, off-axis conic sections, one off-axis biconic, and several flat fold mirrors. The symmetric mirrors include convex and concave prolate and oblate ellipsoids. They range in aperture from 94×86 mm to 286×269 mm and in f-number from 0.9 to 2.4. The biconic mirror is concave and has a 94×76 mm aperture, Rx=377 mm, kx=0.0778, Ry=407 mm, and ky=0.1265 and is decentered by -2 mm in X and 227 mm in Y. All of the mirrors have an aspect ratio of approximately 6:1. The surface error fabrication tolerances are < 10 nm RMS microroughness, best effort for mid-frequency error, and < 63.3 nm RMS figure error.
Ambient temperature (~293 K) testing is performed for each of the three surface error regimes, and figure testing is also performed at ~80 K. Operation of the ADE PhaseShift MicroXAM white light interferometer (micro-roughness) and the Bauer Model 200 profilometer (mid-frequency error) is described. Both the sag and conic values of the aspheric mirrors make these tests challenging. Figure testing is performed using a Zygo GPI interferometer, custom computer generated holograms (CGH), and optomechanical alignment fiducials.
Cryogenic CGH null testing is discussed in detail. We discuss complications such as the change in prescription with temperature and thermal gradients. Correction for the effect of the dewar window is also covered. We discuss the error budget for the optical test and alignment procedure. Data reduction is accomplished using commercial optical design and data analysis software packages. Results from CGH testing at cryogenic temperatures are encouraging thus far.
KEYWORDS: Mirrors, Aluminum, Optical alignment, Spindles, Off axis mirrors, Tolerancing, Diamond, Space telescopes, Optical fabrication, Single point diamond turning
Challenges in fabrication and testing have historically limited the choice of surfaces available for the design of reflective optical instruments. Spherical and conic mirrors are common, but, for future science instruments, more degrees of freedom will be necessary to meet performance and packaging requirements. These instruments will be composed of surfaces of revolution located far off-axis with large spherical departure, and some designs will even require asymmetric surface profiles. We describe the design and diamond machining of seven aluminum mirrors: three rotationally symmetric, off-axis conic sections, one off-axis biconic, and three flat mirror designs. These mirrors are for the Infrared Multi-Object Spectrometer instrument, a facility instrument for the Kitt Peak National Observatory’s Mayall Telescope (3.8 m) and a pathfinder for the future Next Generation Space Telescope multi-object spectrograph. The symmetric mirrors include convex and concave prolate and oblate ellipsoids, and range in aperture from 92 x 77 mm to 284 x 264 mm and in f-number from 0.9 to 2.4. The biconic mirror is concave and has a 94 x 76 mm aperture, (formula available in paper) and is decentered by -2 mm in x and 227 mm in y. The mirrors have an aspect ratio of approximately 6:1. The fabrication tolerances for surface error are < 63.3 nm RMS figure error and < 10 nm RMS microroughness. The mirrors are attached to the instrument bench using semi-kinematic, integral flexure mounts and optomechanically aligned to the instrument coordinate system using fiducial marks and datum surfaces. We also describe in-process profilometry and optical testing.
The Infrared Multi-Object Spectrometer (IRMOS) is a facility instrument for the Kitt Peak National Observatory 4 and 2.1 meter telescopes. IRMOS is a near-IR (0.8 - 2.5 μm) spectrometer with low- to mid-resolving power (R = 300 - 3000). The IRMOS spectrometer produces simultaneous spectra of ~100 objects in its 2.8 x 2.0 arcmin field of view using a commercial MEMS multi-mirror array device (MMA) from Texas Instruments. The IRMOS optical design consists of two imaging subsystems. The focal reducer images the focal plane of the telescope onto the MMA field stop, and the spectrograph images the MMA onto the detector. We describe the breadboard subsystem alignment method and imaging performance of the focal reducer. This testing provides verification of the optomechanical alignment method and a measurement of near-angle scattered light due to mirror small-scale surface error. Interferometric measurements of subsystem wavefront error serve to verify alignment and are accomplished using a commercial, modified Twyman-Green laser unequal path interferometer. Image testing is then performed for the central field point. A mercury-argon pencil lamp provides the spectral line at 546.1 nm, and a CCD camera is the detector. We use the Optical Surface Analysis Code to predict the point-spread function and its effect on instrument slit transmission, and our breadboard test results validate this prediction. Our results show that scattered light from the subsystem and encircled energy is slightly worse than expected. Finally, we perform component level image testing of the MMA, and our results show that scattered light from the MMA is of the same magnitude as that of the focal reducer.
Rockwell Scientific Company is developing a new type of HgCdTe 1K 1K detector, called WFC3-1R, with cutoff
wavelength at 1.7 m and 150K operating temperature. The detector will be installed on the Wide Field Camera 3, the
fourth generation panchromatic instrument for the Hubble Space Telescope (HST) to be installed during HST Servicing
Mission 4, currently scheduled for 2004. The detector uses HgCdTe MBE grown on a CdZnTe substrate and a new type
of multiplexer, the Hawaii-1R MUX. Six lots of detectors have been produced so far, and have demonstrated the
capability to meet or exceed the project requirements. In particular, detectors show quantum efficiency as high as ~90%
at =1.4-1.6 m and greater than 50% at >1.0 m, readout noise of 30 e- rms with double correlated sampling, and dark
current <0.2 e/s/pix at 150K. We illustrate the behavior of the reference pixels, showing that they allow the
compensation of drifts in the dc output level. A number of detectors show a peculiar instability related to the variations
of diode polarization, still under investigation. We also report on the environmental testing needed to qualify the WFC3-
1R detectors as suitable for flight on the HST. We finally provide an update of the project status.
KEYWORDS: Mirrors, Aluminum, Heat treatments, Spherical lenses, Cryogenics, Temperature metrology, Single point diamond turning, Camera shutters, Error analysis, Space telescopes
The Infrared Multi-Object Spectrograph is a facility instrument for the KPNO Mayall Telescope. IRMOS is a low- to mid-resolution, near-IR (0.8-2.5 um) spectrograph that produces simultaneous spectra of ~100 objects in its 2.8 × 2.0 arcmin field of view. The instrument operating temperature is ~80 K and the design is athermal. The bench and mirrors are machined from Al 6061-T651.
In spite of its baseline mechanical stress relief, Al 6061-T651 harbors residual stress, which, unless relieved during fabrication, may distort mirror figure to unacceptable levels at the operating temperature (~80 K). Other cryogenic, astronomy instruments using Al mirrors have employed a variety of heat treatment formulae, with mixed results.
We present the results of a test program designed to empirically determine the best stress relief procedure for the IRMOS mirrors. Identical test mirrors are processed with six different stress relief formulae from the literature and institutional heritage. After figuring via diamond turning, the mirrors are tested for figure error at room temperature and at ~80 K for three thermal cycles. The heat treatment procedure for the mirrors that yielded the least and most repeatable change in figure error is applied to the IRMOS mirror blanks. We correlate the results of our optical testing with heat treatment and metallographic data.
The optical design for an Infrared Multiple Object Spectrometer (IRMOS) intended for Astronomical research is presented. To accomplish spectroscopy of multiple objects simultaneous, IRMOS utilizes a Micro- Mirror array (MMA) as an electronically controlled slit device. This approach makes object selection simple and offers great versatility for performing spectral analysis on many objects within a field location. Furthermore, it allows a field location to be imaged without spectra prior to object selection. The optical design of IRMOS has two distinct stages. The first stage reduces an f/15 incoming beam to f/4.5, with a tilted focal plane located at the MMA (the MMA removes some of the tilt of the focal plane, since the micro-mirrors tilt individually). The second stage consists of the spectrometer, capable of resolutions of 300, 1000, and 3000 in the astronomical J, H and K bands. This stage transforms the tilted focal plane into a collimated pupil on a grating, and then re-images onto a HAWAII detector. When used with the Kitt Peak National Observatory 4 meter telescope, a plate scale of approximately equals 0.2 arcseconds per pixel is realized at both the MMA and the detector. A total of 6 mirrors are used, two flat fold mirrors, two off-axis concave aspheres, one off-axis convex asphere, and one off-axis concave biconic mirror. The selection of a biconic surface in this design helped reduce the overall size of the instrument by reducing the size and number of necessary mirrors, simplifying alignment.
In June 1997, NASA made the decision to extend the end of the Hubble Space Telescope (HST) mission from 2005 until 2010. As a result, the age of the instruments on board the HST became a consideration. After careful study, NASA decided to ensure the imaging capabilities of the HST by replacing the Wide Field Planetary Camera 2 with a low-cost facility instrument, the Wide Field Camera 3. This paper provides an overview of the scientific goals and capabilities of the instrument.
This paper summarizes the findings of the Next Generation Space Telescope (NGST) Detector Requirements Review Panel. This panel was comprised of NGST Integrated Science Instrument Module study representatives, detector specialists, and members of the NGST project science team. It has produced a report that recommends detector performance levels, and has provided rationale for deriving these levels from basic, anticipated NGST science goals and programs. Key parameters such as detector array format, quantum efficiency, and noise are discussed and prioritized.
On the basis of the measured NICMOS performance in HST-Cycle 7 and Cycle 7N programs, we analyze the behavior of the HST optical assembly at IR wavelengths. An accurate analysis of the telescope thermal status allows us to estimate the background flux observed by NICMOS, and compare it with the flux actually measured in different filters. The very close match between expected and measured fluxes confirms the validity of our model. A good understanding of the HST emissivity, which turns out to be lower than previous estimates, allows to predict with higher accuracy the performance of the future IR instruments on HST like NICMOS+cooling system and to specify critical design parameters for WFC3. Also, issues related to the long term stability of the system can be addressed more properly, providing useful quantitative insight on future missions such as the Next Generation Space Telescope.
We report on first observation run with the Achromatic Interfero Coronagraph (AIC) developed at Observatoire de la Cote d'Azure, France. Observations took place last Fall at Observatoire de Haute Provence with the 1.52 m telescope equipped at that time with adaptive optics. The AIC is an imaging device providing the nulling of a star without nulling the close environment of this star. Nulling results from a destructive interference process. Morphological features located as close to the star as the first angular Airy ring can be detected, thus breaking a limitation of the classical Lyot coronagraphs. The objectives of the observation run is to demonstrate that the AIC can image faint companions very close to the diffraction limit with ground-based telescope. After a short reminding of the principle of the AIC, conditions of observations are reported and first coronagraphed-images are shown. Finally limitations are discussed and improvements to carry on are described.
We describe the instrument package concept that we have investigated as part of the Goddard Space Flight Center study for NGST. It is composed of highly integrated, high performance cameras and spectrometers covering the spectral region from 0.6 to 30 microns and with a large field of view.the suite has been configured to reduce cost and complexity with no sacrifice in scientific merit. A common optical bench minimizes interfaces, a guiding system integrated in the science module makes use of the science cameras with minimal penalty to science, and all near IR instruments are built around the same detector module.
We describe the on-orbit characterization of the HgCdTe detectors aboard NICMOS. The flat-field response is strongly wavelength dependent, and we show the effect of this on the photometric uncertainties in data, as well as the complications it introduces into calibration of slitless grism observations. We present the first rigorous treatment of the dark current as a function of exposure time for HgCdTe array detectors, and show that they consist of three independent components which we have fully characterized - a constant component which is the true dark current, an 'amplifier glow' component which results from operation of the four readout amplifiers situated near the detector corners and injects a spatially dependent signal each time the detector is non-destructively read out, and finally the 'shading', a component well known in HgCdTe detectors which we show is simply a pixel dependent bias change whose amplitude is a function of the time since the detector was last non-destructively read out. We show that with these three components fully characterized, we are able to generate 'synthetic' dark current images for calibration purposes which accurately predict the actual performance of the three flight detectors. In addition, we present linearity curves produced in ground testing before launch. Finally, we report a number of detector related anomalies which we have observed with NICMOS some of which have limited the observed sensitivity of the instrument, and which at the time of writing are still not fully understood.
The wide field planetary camera was launched onboard the Hubble Space Telescope in April 1990 and returned to earth during the HST first servicing mission in December 1993. We report on the ongoing examination of the returned hardware. In particular, a significant decline in performance at UV wavelengths in the exterior optics has been found and studied. This appears to be the result of polymerization of molecular contamination on the external optics by UV light reflected off the Earth's atmosphere. Some conlusions from a partial disassembly of the instrument and an examination of its filter elements are presented. We also discuss the effects of radiation on the CCD detectors during their stay in orbit. Radiation damage increased the numbers of hot pixels over time but had no other discernible effects on the performance of the CCDs.
The Wide Field Planetary Camera (WF/PC) onboard the Hubble Space Telescope contains contaminants which condense on the windows in front of each CCD detector. These contaminants are UV opaque and increase with time to the extent that after several months they block 50% of the flux at 300 nm. Also, when the contaminants are warmed above -40 degree(s)C and then returned to the normal CCD operating temperature of -87 degree(s)C, particles form and severely degrade the image quality. The windows may be temporarily cleaned by raising their temperature to 0 degree(s)C. However, this results in a change in the structure of the flat field due to the partial removal of the UV flood which was applied after launch to suppress Quantum Efficiency Hysteresis in the CCDs. Repeated decontaminations will reintroduce the QEH and necessitate another time consuming UV flood and recalibration of the instrument. After 22 months of on-orbit operation, the contaminants could no longer be fully removed by the decontamination procedure. This paper describes the current state of the contaminants, what has been deduced concerning their properties and sources, the results of our efforts to remove them, and some lessons for future space-based instruments using cryogenic UV sensitive detectors.
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