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Anthony Horton ; Lee Spitler ; Naomi Mathers ; Michael Petkovic ; Douglas Griffin ; Simon Barraclough ; Craig Benson ; Igor Dimitrijevic ; Andrew Lambert; Anthony Previte ; John Bowen ; Solomon Westerman ; Jordi Puig-Suari ; Sam Reisenfeld ; Jon Lawrence ; Ross Zhelem ; Matthew Colless and Russell Boyce " The Australian Space Eye: studying the history of galaxy formation with a CubeSat ", Proc. SPIE 9904, Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, 99041Q (July 29, 2016)

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Copyright 2016 Society of Photo-Optical Instrumentation Engineers (SPIE). One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited.

The Australian Space Eye: studying the history of galaxy formation with a CubeSat

Anthony Hortona, Lee Spitlera,b, Naomi Mathersc, Michael Petkovicc, Douglas Griffind, Simon Barracloughd, Craig Bensond, Igor Dimitrijevicd, Andrew Lambertd, Anthony Previtee, John Bowene, Solomon Westermane, Jordi Puig-Suarie,f, Sam Reisenfeldb, Jon Lawrencea, Ross Zhelema, Matthew Collessc, and Russell Boyced aAustralian Astronomical Observatory, Sydney, Australia bMacquarie University, Sydney, Australia cAustralian National University, Canberra, Australia dUNSW Canberra, Canberra, Australia eTyvak Inc., Irvine CA, USA fCal Poly, San Luis Obispo CA, USA

ABSTRACT The Australian Space Eye is a proposed astronomical telescope based on a 6 U CubeSat platform. The Space Eye will exploit the low level of systematic errors achievable with a small space based telescope to enable high accuracy measurements of the optical extragalactic background light and low surface brightness emission around nearby galaxies. This project is also a demonstrator for several technologies with general applicability to astronomical observations from nanosatellites. Space Eye is based around a 90 mm aperture clear aperture all refractive telescope for broadband wide field imaging in the i0 and z0 bands. Keywords: Space telescope, nanosatellite, CubeSat, extragalactic background, low surface brightness

1. INTRODUCTION In December 2014 the Advanced Instrumentation Technology Centre at the Australian National University hosted the AstroSats 2014 workshop. The workshop was held to explore concepts for astronomical nanosatellite missions, with the goal of identifying viable missions that could be funded within existing Australian grant schemes. Concepts were required to be justifiable by the expected scientific results alone, i.e. without reference to the development of technology or accumulation of expertise, valuable as those outcomes would be. Additionally proposed spacecraft were to be no larger than a 6 U CubeSat. The Australian Space Eye was conceived in response to this call for proposals. Meeting the combination of scientific value, cost and size constraints is very challenging, essentially it means identifying a compelling science programme that is within the capabilities of a very small instrument in low earth orbit but which could not be done with (much larger) ground based instruments for comparable cost. The two most well known benefits of situating an astronomical telescope above the Earth’s atmosphere are accessing wavelengths that are absorbed by the Earth’s atmosphere and avoiding the degradation of spatial resolution caused by atmospheric turbulence. Neither of these are of great relevance to an astronomical CubeSat however, at least one conceived within the AstroSats constraints. The gamma ray, X-ray, far ultraviolet and infrared wavelength regions all require exotic optics and/or image sensors which are not compatible with the cost, volume, thermal and power limitations of the platform. For this reason we limited our consideration to the near ultravoilet to very near infrared wavelength region (∼ 200–1000 nm) that is accessible with silicon based image sensors and conventional optics. Within this wavelength range there is no spatial resolution advantage to being above the Earth’s atmosphere either, the fundamental diffraction limit of a CubeSat sized telescope aperture (. 90 mm diameter) is greater than atmospheric seeing at the same wavelengths. Send correspondence to A.J.H: E-mail: [email protected], Telephone: +61 2 9372 4847

Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, edited by Howard A. MacEwen, Giovanni G. Fazio, Makenzie Lystrup, Proc. of SPIE Vol. 9904, 99041Q · © 2016 SPIE · CCC code: 0277-786X/16/$18 · doi: 10.1117/12.2232467

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx There are however two other effects of the atmosphere which are relevant to a CubeSat based optical tele- scope: atmospheric scattering and emission. Atmospheric scattering spreads the light from astronomical objects in a similar way to scattering from the instrument’s optics however the impact is compounded by the fact that the distribution of aerosols in the atmosphere is spatially and temporally variable, the amount of scattered light surrounding a given source can vary by several percent of the source brightness even in good ‘photometric’ conditions, on timescales of minutes to months. The variability in the scattering makes it difficult to accu- rately characterise and subtract,1 thereby introducing problematic systematic errors. Similar issues arise from atmospheric emission, particularly at longer wavelengths (> 700 nm). Here the atmosphere glows increasingly brightly, primarily due to line emission from OH∗ molecules in the mesosphere, reducing the sensitivity of ground based telescopes. This emission is sensitive to dynamic processes in the upper atmosphere (e.g. gravity waves) and consequenty it is also spatially and temporally variable on timescales of minutes and longer2 which makes accurate subtraction difficult. As a result of these effects locating a telescope in space not only helpfully reduces both scattered light and sky background levels but crucially makes both far more stable. Above the atmosphere the only sources of scattered light are associated with the instrument itself and the dominant source of sky background is the zodiacal light3 which, while it does exhibit large scale spatial and seasonal variations, is much less variable, more uniform and more predictable than atmospheric emission. The scientific competitiveness of small telescope for certain types of observations is well proven. For exam- ple while large astronomical telescopes are able to detect extremely faint compact or point-like objects their sensitivity to diffuse emission is limited by systematic errors from a number of sources. A significant contribu- tion to these systematic errors is contamination with light from brighter objects within/near the instrument’s field of view, caused by a combination of diffraction, scattered light and internal reflections. The difficulties caused by these effects have been discussed by, for example, Sandin4,5 and by Duc et al,6 who noted that the simpler optics of small telescopes suffer less from internal reflections. In addition small telescopes can more readily be constructed with unobscured apertures to minimise diffraction, and simpler optics also make them less prone to internal scattering of light. The resulting competitiveness of optimised small telescopes in the context of ‘low surface brightness’ (LSB) imaging has been demonstrated by the Dragonfly Telephoto Array, an astronomical imaging system based on an array of telephoto camera lenses.7 This instrument exhibits less diffraction/scattering/internal reflections than other telescopes for which comparable data are available4,7 and the system has produced impressive results, including the discovery of a new class of ‘ultra-diffuse galaxies’.8 Two of this paper’s authors (AJH & LS) are currently assembling a ground based instrument based on the same principles, the Huntsman Telephoto Array.9 We conclude that a CubeSat based astronomical telescope may be scientifically competitive, especially an optimised telescope performing measurements that are typically limited by systematic errors. We identify the 700–1000 nm wavelength region as particularly promising as it is accessible to instrumentation compatible with the constraints of a CubeSat mission while ground based instruments would be hampered by bright atmospheric emission, in terms of both reduced sensitivity and increased systematic errors. We have based the Australian Space Eye proposal on two science goals which would be well served by a telescope operating in this regime, the measurement of extragalactic background light and imaging of low surface brightness structures around nearby galaxies. These are discussed in more detail in the next section.

2. SCIENCE CASE 2.1 Extragalactic Background Light A fundamental measurement of the universe is its total luminosity, which contains the entire history of all sources of light, from signatures of the Big Bang in the cosmic microwave background and, at optical wavelengths, all past radiative processes including light from stars and even black hole accretion disks. Although the microwave background has been securely measured the cosmic optical background (the total luminosity at optical wave- lengths) has not due to our non-ideal vantage point - we are embedded in the dust cloud of the solar system. This dust scatters sunlight into the observer’s telescope and so we must separate the background light we want to measure from the light scattered by this foreground dust, the so-called Zodiacal light. This has proved very challenging (see Cooray 201610), though there have been a few attempts (e.g. Bernstein 2007,11 Aharonian et al.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 200612 and Tsumura et al. 201013). What is needed is an instrument that can measure and separate the Zodiacal and extragalatic background light. One approach for disentangling the Zodiacal and extragalactic light exploits spectral features of the former. As Zodiacal light is scattered sunlight its spectrum is similar to that of the Sun, subject to reddening due to the wavelength dependence of the scattering strength.3, 14, 15 This includes the strong Calcium triplet absorption lines near 860 nm, which will be present in the Zodiacal light spectrum with the same equivalent width as in the solar spectrum but will be absent from the spectrum of the extragalactic background due to the effects of cosmological redshifts. Consequently the observed equivalent width of absorption lines in the total background light (Zodiacal plus extragalactic) provided a measure of the relative contributions of the two components. This was the goal of one of the instruments of the CIBER sounding rocket experiment,16 a narrowband imaging spectrometer based on a tilted objective filter,17 however the measurement proved extremely difficult to make with the limited total exposure time of a sounding rocket campaign. An orbital space telescope, able to accumulate a year or more of observing time, promises secure measurements of both the absolute total sky brightness and the relative contributions of the Zodiacal light and extragalactic background.

2.2 Low Surface Brightness Galaxies A new ground-based imaging system called the Dragonfly Telephoto Array7 uses commercial-off-the-shelf camera lenses to reach 16× (3 magnitudes) fainter surface brightness levels than existing telescopes at optical wavelengths (0.4–0.7 µm, g0 and r0 bands). The key innovation is the use of unobscured refracting optics, which significantly reduce scattered and diffracted light compared to conventional large reflecting telescopes and bring the limiting systematic uncertainties down to 8 × 10−21 W m−2 µm−1 arcsecond−2 (32 AB mag./arcsecond2 in g0).4 The Dragonfly observing system has led to a number of important results, including finding an entirely new class of galaxy (e.g. van Dokkum, Abraham, Merritt 2014,18 van Dokkum et al. 20158). By adapting the Dragonfly concept to observing galaxies at longer wavelengths of light from space we can constrain the stellar population properties of these galaxies. The Australian Space Eye will target several nearby galaxies in order to obtain images at the lowest possible surface brightness levels and detect extremely faint structures in their outskirts. When the Space Eye i0 and z0 band imaging is combined with optical g0 and r0 band imaging from the Dragonfly and Huntsman9 ground-based observing facilities we will have valuable information about the stellar age and chemical content of these faint structures.

3. SPACE EYE CONCEPT The Australian Space Eye is a nano-satellite based on the 6 U CubeSat form factor standard19 housing an optical imaging telescope. The specifications of the system are driven by the aims discussed in Sec.2, subject to the constraints discussed in Sec.1. An artist’s impression of Space Eye is shown in Fig.1.

3.1 Optical Payload 3.1.1 Requirements The scientific goals described in Sec.2 call for a wide field imaging instrument with moderate spatial resolution, an exceptionally ‘clean’ and stable point spread function (PSF), and the highest low light sensitivity achievable within the other constraints of the platform. The imager must be capable of both broadband imaging in the i0 and z0 bands (approximately 700–850 nm and 850–1000 nm respectively) as well as measurement of the strength of the Calcium absorption lines in the sky background spectrum. The optical system is expected to occupy approximately 50% of the spacecraft internal volume. The optical axis will be aligned with the long axis of the spacecraft body and positioned on the centreline to assist with centre of mass positioning. The bulk of the optical payload is therefore confined to an approximately 300×100×100 mm 3 U volume, however 1–2 U of the remaining 3 U of internal volume will be available for payload electronics. The largest practical optical aperture within these constraints is ∼ 90 mm in diameter. Considerations of cosmic variance, sky background gradients and the angular extents of galaxy groups/clusters result in a desire for a field of view at least 1◦ across, preferably close to 2◦.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Figure 1. Artist’s impression of the Australian Space Eye in orbit over the Tasman Sea.

We have selected a image scale of 3 00 pixel−1, this is close to Nyquist sampling of the diffraction limited PSF at the Space Eye aperture size and operating wavelengths (1.22λ/D = 2.000–2.800). Coarser spatial sampling could increase the signal to noise ratio for diffuse sources however we are wary of significantly undersampling the PSF due to the potential impact on the accuracy of PSF fitting and subsequent point source subtraction. We will show that Space Eye can still be sky background noise limited at this pixel scale. 3 00 pixel−1 is also a good match to the pixel scale of ground based low surface brightness imaging facilities such as the Dragonfly Telephoto Array7 and Huntsman Telephoto Array.9 To accomplish the required measurements of both broadband i0 and z0 surface brightness and Calcium ab- sorption we proposed to use a set of 6 slightly modified i0 and z0 band filters with band edges positioned around the strong absoprtion line at 854.2 nm. More details are discussed in Sec. 3.1.4. For Space Eye the requirement for a clean and stable PSF translates to minimising all sources of stray light, including surface and bulk scattering, internal reflections, stray sunlight/Earthshine/moonlight and diffraction. The highest possible sensitivity will be achieved when the optical aperture is as large as it can be within the space constraints of the CubeSat, the optical throughput and quantum efficiency (QE) of the image sensor are

Table 1. Summary of main optical payload requirements

Field of view > 1◦ (goal ∼ 2◦) Pixel scale 3 00 pixel−1 Wavelength range 700–1000 nm Aperture diameter 90 mm Optical system dimensions 300 × 100 × 100 mm max Payload electronics volume < 2 U

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx The CIS115 is a 20 (saturation) 1 C ◦ − C per channel pixel ◦ at 21 1 − 1 e − − 1504 s 4 % 1 × C–+60 40 mW m square 90 % − ± ◦ µ ∼ 0 . m pitch. The main specifications, taken from 55 2000 7 µ pixel 2 Mpixel s − . − e (linear), 33 k at 6 1 20 − − e 5 pixel − e 1504 pixels on a 7 27 k × II IIIIIIIIIIIIIIIIIIIIIIII 9904 99041Q-5 Proc. of SPIE Vol. Figure 2. CIS-115 CMOS image sensor, photo credit e2v. Non-linearity Operating temperature Power consumption Pixel size Quantum efficiency at 650 nm Dark current Read noise Well depth Number of pixels

The CIS115 is a new image sensor developed with space based scientific imaging in mind, in particular the Astronomical instruments operating at these wavelengths typically use charge-coupled device (CCD) image Table 2. Summary of CIS115‘typical’. specifications taken from draft datasheet dated December 2015. All performance values are the draft e2v datasheet, are given in2. Tab. ESA JUICE mission. In general its performance is close to that of back side illuminated CCD image sensors back-side illuminated image sensor with 2000 sensors however for Space Eye we have selected the CIS115 CMOS image sensor from e2v. 3.1.2 Image sensor The choice ofthe image system sensor but is thethermal key, control, specifications not power, for only etc.) many is depend of it on the the the other specifications biggest subsystems of variable (optics, the in sensor. data determining handling, the downlink overall capacity, sensitivity of close to 100%, and the total instrumental noise is below the Poisson noise from the sky background light. Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx e2v CIS115 predicted QE (Soman et al) 1.0

+20 ◦ C

40 ◦ C −

0.8 1

− 0.6 n o t o h p

e

/

E 0.4 Q

0.2

0.0 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 Wavelength/µm

Figure 3. Predicted CIS115 quantum efficiency as a function of wavelength at both 20 ◦C and −40 ◦C, data from Soman et al.21

operated in inverted mode, the main difference being a 2–3× higher read noise when compared to the best CCDs. CMOS image sensors offer a number of advantages for a CubeSat space telescope however, including lower power consumption and greater resistance to radiation induced damage than CCDs. Of particular importance to Space Eye is the relatively small pixel size, 7 µm versus the 12–15 µm of available scientific CCDs. This factor of 2 reduction in pixel size enables a corresponding reduction in the focal length of the optics required for a given on-sky pixel scale which has a significant impact on the design of the optics as discussed in the next section. An additional advantage is the ability to operate regions of the sensor independently of others, opening up the possibility of using small regions for high frame rate autoguiding/star tracking while simultaneously taking a long exposure with the rest of the sensor (‘on-chip guiding’). Predicted quantum efficiency data for the CIS115 are plotted in Fig.3. These data are reproduced from Soman et al.21 and we regard them as conservative estimates, Wang et al.22 report slightly higher peak QE from both their own and e2v’s measurements of a prototype device (CIS107). The decline in QE for wavelengths greater than 700 nm is due to the increasing transparency of silicon at these wavelengths and is common to all silicon based image sensors. In this wavelength range only deep depletion or high rho CCDs offer significantly higher QE, due to the greater effective thickness of their photosensitive layer. We consider these devices unsuitable for Space Eye however as those currently available have large pixels and, more importantly, require deep cooling (< −100 ◦C) to control dark current due to their non-inverted operation. Deep depletion/high rho CMOS image sensors show promise however at the time of writing no devices suitable for Space Eye were known to the authors. The dark current of the CIS107 prototype was measured by Wang et al. between +27 ◦C and −23 ◦C and they found the expected exponential temperature dependence with a halving of dark current for every 6.2 ◦C drop. Their best fit model is shown in Fig.4. The dark current of cooled production CIS115 image sensors may be somewhat lower, e2v’s draft datasheet suggests a typical dark current that is ∼ 50 % lower at 20 ◦C that also falls more rapidly with cooling, halving with each 5.5–6.0 ◦C temperature drop. Based on these data we − −1 −1 ◦ confidently expect a dark current of . 0.04 e pixel s at −40 C. Wang et al. also note a helpful reduction

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx e2v CIS-115 Dark Current Model

101 1 − l e x i p

1 −

s 0 10 − e

/

t n e r r u c

k r a D 10-1

10-2 50 40 30 20 10 0 10 20

Temperature / ◦ C

Figure 4. CIS115 dark current as a function of temperature, based on the model from Wang et al.22

in read noise on cooling, to approximately 4 e−.

3.1.3 Telescope optics The combination of the requirements from Tab.1 and the image sensor specifications from Tab.2 enable us to determine the remaining requirements for the telescope optics. The resulting specifications are summarised in Tab.3. The biggest consideration for the design of the Space Eye optics is minimising the wings of the PSF due to internal scattering, reflections and diffraction. For this reason we have decided to use an all refractive design. Abraham and van Dokkum7 have argued that refractive designs have a fundamental advantage over reflecting or catadioptric telescopes in this respect, and comparisons of telescope PSF measurements by Sandin4 appear to support this view. Note that the relatively small pixels of the CIS115 image sensor are essential to allow a refractive design to be used. With 3 00 pixel−1 and 7 µm pixels the required effective focal length is about twice the length of the space available for the optics, necessitating a moderately telephoto design but not presenting any insuperable problems. With the larger pixels typical of back side illuminated CCDs the focal length would have to be approximately four times the length of the available space, in which case folded light path reflective or catadioptric designs would be the only practical options. We have produced a baseline optical design for Space Eye which is illustrated in figure5. The design consists of 6 elements in 4 groups with two CaF2 elements (L2 and L3) and two aspheric surfaces (L3-S1 and L4-S1). Six elements were required to achieve the desired image quality within the overall length constraints however we are able to limit the number of vacuum-glass interfaces to 7 which will assist with minimising surface scattering and internal reflections/ghosting. The image quality is essentially diffraction limited across the full field of view, as confirmed by the ensquared energy plots in Fig.6. The calculation was performed using the Huygens-Fresnel method with the Zemax OpticStudio software. The ensquared energies are polychromatic (700–1000 nm) and have been calculated for 5 field points at a range of positions from the centre to the corner of the field of view. Bulk scattering will be minimised through the use of high purity, high homogeneity lens blanks. Super polishing and high performance anti-reflection coatings will be used to minimise surface scattering and internal

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Table 3. Summary of telescope optics specifications

Field of view 1.67◦ × 1.25◦ Effective focal length 481 mm Aperture diameter 90 mm Focal ratio f/5.34 Wavelength range 700–1000 nm Overall length 250 mm

Figure 5. Cross section optical layout diagram of the baseline design for the Australian Space Eye.

1.0

0.8

0.6

0.4

0.2

2.0 4.0 6.0 8.0 10.0 12.0 4.0 8.0 20.0 Half Width From Centroid in um

10-Diff. Limit 0- 0.0000, 0.0000 (deg) 0- 0.4170, 0.3133 (deg) 0- 0.0000, 0.6270 (deg) 0- 0.8330, 0.0000 (deg) 0-0.8330, 0.6270 (deg)

Huygens Diffraction Ensquared Energy Figure 6. Ensquared energy as a function of half-width for the baseline optical design.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx i1i2 i3 i1 i2 i3

z1z2 z3 z1 z2 z3

i1 i2 i3 i1 i2 i3

z1z2 z3 z1 z2 z3

Figure 7. Example mosaic filter layout. Each filter covers an area of 333 × 376 pixel, 16.70 × 18.80 on sky.

reflections. We are pursuing the possibility of using nano-structured anti-reflection coatings (as employed in some high end DSLR lenses) for this purpose, these are capable of very low reflectivities for a wide range of wavelengths and angles of incidence. Internal knife-edge baffles will be used, along with an external deployable baffle designed to prevent illumination of the optics by sunlight, Earthshine or moonlight during observations. A 700–1000 nm bandpass filter will be applied to the 1st lens surface. A full stray light analysis will be performed as part of a general review of the optical design when the project is confirmed however we are confident that we will be able to acheive the required clean and stable PSF. The telescope will include a bistable optical shutter between the L5 and L6 elements to enable on orbit image sensor dark current measurements. 3.1.4 Mosaic filter In order to provide the necessary data to allow both broadband i0 and z0 band imagery and seperate measurements of the Zodiacal light and extragalactic components of the sky background we propose the use of 6 broadband filters, 3 variants on the i0 filter and 3 variants on the z0 filter. Nominal transmission profiles for these filters are shown in Fig.8, together with a model of the Zodiacal light photon spectral flux density. The filters differ in their red cutoff wavelength in the case of the i0 filters and their blue cutoff wavelength in the case of the z0 filters. The cutoffs are chosen to bracket the strongest of the Calcium triplet absorption lines (854.2 nm) as well as an adjacent region of continuum. The pairwise surface brightness differences between filters provide information on the relative strength of the Calcium absorption that can used together with sky background models to separate the Zodiacal light and extragalactic components. Meanwhile the sum of the 3 i0 or z0 band filters gives deep broadband data with effective filter response close to the standard i0 or z0 filter bands. Multiband astronomical imaging is typically accomplished by taking full frame images through each individual filter sequentially, i.e. temporal multiplexing. This approach requires a set of full frame filters and some sort of filter exchange mechanism, e.g. a filter wheel. For space based instruments, and especially those intended for nanosatellites, there are strong incentives to avoid introducing mechanisms if at all possible due to complexity, cost and potential for failure. Consequently we favour a spatial multiplexing based approach in which the field of view is divided up amongst the 6 different filters by a fixed mosaic filter at the focal plane, an example layout of which can be seen in Fig.7. By taking sequences of 6 images with pointing offsets equal to the dimensions of the filter regions contiguous images can be built up for each filter. 3.1.5 Performance modelling In order to determine appropriate operational parameters and predict the approximate sensitivity of Space Eye we have developed performance models for the optical payload. These are not full end-to-end simulations but are instead parametric models, suitable for efficiently exploring parameter space ahead of the more detailed analysis to follow. As noted in Sec. 3.1.1 obtaining the maximum sensitivty for a fixed telescope aperture size requires both maximising the end-to-end efficiency (optical throughput and image sensor QE) and ensuring the instrumental

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Australian Space Eye filter profiles 1.0

0.8

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Transmission 0.4

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0.0 0.65 0.70 0.75 0.80 0.85 0.90 0.95 1.00 1.05 Wavelength/µm

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i1

0.6 i2 i3 z1 z2

Transmission 0.4 z3 Zodiacal light

0.2

0.0 0.84 0.85 0.86 0.87 0.88 Wavelength/µm

Figure 8. Nominal filter transmission profiles shown together with a model of the Zodiacal light photon spectral flux density.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx SNR relative to SNR without instrumental noise 1.0

i2, 45 ◦ C − i2, 40 ◦ C − i2, 35 ◦ C − 0.9 i2, 30 ◦ C − z2, 45 ◦ C − z2, 40 ◦ C − z2, 35 ◦ C 0.8 − z2, 30 ◦ C −

0.7 Relative signal to noise ratio

0.6

0.5 0 100 200 300 400 500 600 700 800 900 Sub-exposure time / second

Figure 9. Predicted SNR relative to the SNR without instrumental noise for the i2 and z2 filters as a function sub-exposure time for a range of image sensor temperatures. The calculation uses the ecliptic pole Zodical light surface brightness values.

noise sources do not add significantly to the fundamental Poisson noise of the light received from the sky, which at these wavelengths is predominantly Zodiacal light. For the purpose of these calculations we use a model for the Zodiacal light based on that used by the Hubble Space Telescope Exposure Time Calculator.14 The starting point is a solar spectrum from Colina, Bohlin and Castelli,23 to which we apply a normalisation, reddening and spatial dependency following the prescription of Leinert et al.3 with the revised parameters from Aldering.15 Using the aperture size, estimated optical throughput, filter transmission profiles, pixel scale and image sensor quantum efficiency we can predict the observed Zodiacal light signal (in photo-electrons per second per pixel) and then, with the estimated image sensor dark current and read noise values, we can predict the signal to noise ratio (SNR). By comparing the predicted SNR with the value it would have in the absence of dark current and read noise we can quantify the degree to which instrumental noise is effecting sensitivity. The key results are summarised in Fig.9, which shows the SNR relative to the SNR without instrumental noise for the i2 and z2 filters for a range of image sensor temperatures and sub-exposure time. The calculation uses the Zodiacal light model surface brightness values for the eclipitc poles, which are close to the minimum possible value and therefore place the most stringent demands on instrumental noise. Due primarily to the falling image sensor QE the z0 band is more sensitive to instrumental noise and drives the selection of operating parameters. Based on these results we have selected a nominal exposure time for individual science exposures of 600 s and an image sensor operating temperature of −40 ◦C. Using these parameters we then calculate the predicted sensitivity limit for Space Eye, specifically the source surface brightness spectral flux density that would correspond to a signal to noise of 1 per pixel, for each filter. This is plotted as a function of total exposure time in Fig. 10, with a horizontal scale that runs from 600 s (i.e. a single exposure) to 2 × 106 s. The latter value corresponds to the approximate total exposure time per filter per celestial hemisphere for a 2 year duration mission, assuming the duty cycle discussed in Sec. 4.3. Of more relevance to the broadband imaging science goals, we have also calculated the predicted sensitivity limit from summing the 3 i0 and z0 filters. At the end of the 2 year mission we predict ultimate 1σ per pixel

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Sensitivity limit, ecliptic pole, no extinction, SNR = 1 per pixel, tsub = 600 s

i1 i2 i3 -18 1 10 − i 0 sum m µ

z1 2 −

c z2 e s c

r z3 a

2 z sum

− 0 m

W

/

s s

e -19 n 10 t h g i r b

e c a f r u S

10-20 103 104 105 106 Total exposure time per filter / second

Figure 10. Predicted surface brightness spectral flux density corresponding to a signal to noise ratio of 1 per pixel as a function of total exposure time per filter. The calculcation is for the ecliptic pole Zodiacal light surface brightness, an image sensor temperature of −40 ◦C and sub-exposures of 600 s.

sensitivity limits of 1.1 × 10−20 W m−2 arcsecond−2 µm−1 and 1.9 × 10−20 W m−2 arcsecond−2 µm−1 for i0 and z0 bands respectively, equivalent to 30.5 and 29.6 in AB magnitude surface brightness units. The Zodiacal light model includes spatial (and seasonal) variations, allowing us to calculate how the predicted sensitivity varies with position on the sky. For extragalactic sources, such as other galaxies and the extragalactic background light, we must also take into account extinction by Galactic dust. For this we use the all sky dust reddening (E(B-V)) maps from the Planck Legacy Archive24 and convert to extinctions at our filter wavlengths using the prescription of Fitzpatrick,25 with R = 3.1. Fig 11 shows the resulting i0 band relative sensitivity maps for regions near the ecliptic poles at the times of the equinoxes and solstices. Due to the seasonal variation in Zodiacal light regions close to the north ecliptic pole are preferred from February to July, and close to the south ecliptic pole from August to January. The tightest constraints come the Galactic dust, in order to minimise its effects target should be chosen from within regions between 15.5 and 16.5 hours Right Ascension and +55 and +60 degrees declination in the north, and between 4 and 5 hours Right Ascension and -50 and -60 degrees declination in the south.

3.2 Spacecraft Bus The Space Eye spacecraft bus will be based on the Tyvak Endeavour platform. This highly integrated, high performance platform incorporates almost all the systems required for a functional 3–12 U Cubesat, including Command and Data Handling (C & DH), Electrical Power System (EPS) and thermal management, Attitude Determination, Control and Navigation System (ADCNS), and structural and mechanical parts. In a typical configuration the avionics package, including battery modules, occupies approximately 1 U of volume. As noted in Sec. 3.1.1 the Space Eye telescope will occupy a 3 U volume leaving a final ∼ 2 U of volume for other mission specific hardware, e.g. the image sensor control electronics, image sensor thermal control system (Sec. 3.2.2), image stabilisation system/ADCS 2nd stage (Sec. 3.2.1) and communication equipment.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx i 0 band relative sensitivity, NEP, March i 0 band relative sensitivity, SEP, March

i 0 band relative sensitivity, NEP, June i 0 band relative sensitivity, SEP, June

i 0 band relative sensitivity, NEP, September i 0 band relative sensitivity, SEP, September

i 0 band relative sensitivity, NEP, December i 0 band relative sensitivity, SEP, December

Figure 11. Predicted i0 band sensitivity relative to the ecliptic pole, zero extinction case. The maps show 45◦ × 45◦ gnomonic projections centred on the north and south ecliptic poles in March, June, September and December, with a colourmap running from halved sensitivity (black) to full sensitivity (white). Equatorial coordinate grids are also shown, with 1 hour spacing in RA and 10◦ in dec, as well as the outlines of the designated target regions.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx OC &DH and ADCS Processor Inertial Measurement Unit Reaction Wheels 8Star Trackers ®Torque Coils

Figure 12. Main components of the standard Tyvak Endeavour attitude determination and control system (ADCS). Space Eye’s ADCS will be based on an updated Endeavour system.

An initial power budget analysis has indicated that Space Eye will require body mounted solar panels on the largest face of the spacecraft body plus 1 U wide deployable panels along both long edges, as shown schematically in figure1. Based on a preliminary analysis we believe that standard UHF telemetry/command and S-band downlink systems will be sufficient given the expected data rates (see section4). 26

3.2.1 Attitude Determination & Control The main technical challenge for astronomical imaging from CubeSats is instrument pointing stability. Long exposures are required to prevent image sensor noise overwhelming the faint signals from the sky (see Sec. 3.1.5) and the instrument must be kept stable to within less than 1 pixel for the duration of the exposures to avoid blurring. For Space Eye the required exposure times are 600 s and 1 pixel corresponds to 300, these requirements are well beyond the capabilities of any current commercially available CubeSat ADCS system. Improvements are required in both the attitude determination and attitude control aspects. The standard Tyvak Endeavour main attitude determination system is based on a set of two orthogonal Tyvak-developed star trackers and a three-axis MEMS gyro. These sensors are paired with a set of three Tyvak reaction wheels as primary attitude control actuators. The system also incorporates three magnetic torque coils for wheel desaturation and a set of sun sensors and magnetometers to provide coarse attitude determination. Attitude determination and control computations are performed on a dedicated processor on the Endeavor main board. Pointing stability of the Endeavour platform is primarily driven by rate noise from the gyroscope in the attitude control loop. Disturbances from the reaction wheels also contribute jitter to a lesser extent; however, reaction wheel induced jitter can be mitigated with placement and isolation. Modest software and firmware updates to the current Endeavour platform achieve 3000 (3 σ) stability in simulation. Tyvak has investigated several paths to achieve arcsecond level pointing stability with the Endeavour platform. The highest technology readiness level path for arcsecond level pointing of an imaging payload is a two-stage control system with piezoelectric actuators driving lateral translation of the focal plane assembly (FPA) in a high bandwidth second stage. The two-stage approach is well suited to CubeSats since it is orbit agnostic and CubeSat rideshares generally cannot select their orbit. The piezoelectric second stage consists of the FPA (image sensor, interface board, mosaic filter and field flatenner lens), piezoelectric actuators driving lateral translation of the FPA, a dedicated processor for calculating

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Deployed stray -light baffle

Deployed solar array

Main spacecraft chassis

-- Radiator

Thermal IR baffle

Figure 13. Configuration of the spacecraft showing the deployed thermal IR radiator baffle (left), and spacecraft attitude and solar illumination during (northern) summer solstice in a 14:00 LTAN orbit without Earth IR avoidance manoeuvres outside of the observation windows (right).

guide star centroids and performing control calculations, and the electrical and power system for the piezoelectric actuators. Space Eye will use fine star tracking (autoguiding) in the main telescope focal plane to provide the precision pointing information required. Dedicated sensors adjacent to the main image sensor could be used however the CIS115 image sensor and its control electronics are capable of continuously reading out sub-regions of the image sensor for fine star tracking while the remainder of the sensor is simultaneously doing a long science exposure. A fraction of the science image is lost in this way however avoiding a dedicated set of fine star tracking sensors and associated control electronics reduces complexity considerably. Preliminary design for the dual-stage controller indicates the control bandwidth of the piezoelectric second stage needs to be greater than 3.5 Hz with centroiding noise of less than 100. Control inputs (centroids from guide stars) need to be computed at roughly 20 Hz and with delay of no more than roughly 1 ms. Specific piezoelectric actuators have not been analyzed however the required actuator throw is within COTS hardware capability. Significant work remains to refine guide star sensor selection, actuator selection, packaging, and the algorithms to drive the second stage control system.

3.2.2 Thermal control Cooling the image sensor below the temperature where the dark current is a negligible contributor to the system radiometric noise budget (see Sec. 3.1.5) is both critical to the scientific performance of the mission as well as a very difficult engineering challenge within the resource constraints of a 6 U CubeSat spacecraft. In order to address the feasibility of achieving this requirement, a number of configurations of the spacecraft, attitude control strategies and Concept of Operations need to be assessed. In order to cool the detector over an extended period of time a radiator needs to be integrated onto an external face of the spacecraft to reject heat to deep space. Through the orbit the radiator will in general be in radiative exchange with deep space, the Earth, the solar heat load from the direct view of the radiator to the Sun as well as the solar energy reflected from the Earth to the radiator (i.e. the Albedo heat load). The overall efficacy of a particular radiator design will then depend on the area, thermal conductivity and thermo-optical properties of the radiator as well as the relative geometry of the radiator surface to the Earth, Sun and any other appendages of the spacecraft. Ultimately, these geometric factors depend on the accommodation of the subsystems within the spacecraft, the attitude of the spacecraft, the season and the orbital parameters of the spacecraft and the location of the spacecraft in its orbit.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Australian Space Eye thermal mathematical model 15

20

25 C ◦

/ Sensor, no S/C rotation

e r

u Radiator, no S/C rotation t 30 a r Sensor, S/C rotation e p Radiator, S/C rotation m e T 35

40

45 0 30 60 90 120 150 180 Elapsed time/minute

Figure 14. Predicted image sensor and thermal radiator temperature variations during several orbits with a thermal IR baffle, both with and without Earth IR avoidance manoeuvres outside of the observation window. When Earth IR avoidance manoeuvres are used the image sensor temperature remains below the nominal −40 ◦C operating temperature throughout the observation windows.

The most favorable orbit, from the point of view of thermal control of the detector radiator, is dawn-dusk Sun synchronous. In this orbit the detector radiator can be placed on the opposite side of the spacecraft to the main solar array. has a very good view factor towards deep space and is protected from direct solar illumination. There are several drawbacks of baselining this orbit which makes it unattractive from the mission level perspective. Firstly, only a relatively small minority of CubeSat launches are dawn-dusk and therefore adopting it involves a risk of incurring a significant programmatic delay to wait for a suitable launch opportunity. Secondly, due to the fact that the sequencing of the deployments of the primary and secondary payloads is planned to optimize the orbital parameters of the primary payload, there is generally an injection error of the CubeSat with respect to a fully sun synchronous orbit. Finally, without a propulsion system, as the orbit decays it will drift further and further away from the ideal orbit and compromise the thermal performance. In the light of these considerations it was decided to abandon the dawn-dusk sun-synchronous orbit approach and consider Sun-synchronous orbits with a Local time of the Ascending Node (LTAN) closer to local noon. A Thermal Mathematical Model (TMM) of the spacecraft and orbit was built using ESATAN TMS. For the purpose of the analysis we assumed a 600 km Sun-synchronous circular orbit with a 96.7 minute period and LTAN of 14:00. The initial analysis showed that a 100 mm × 100 mm radiator on the anti-Sun facing surface of the spacecraft would not provide sufficient cooling to the image sensor due to the thermal IR load from the Earth (and to a lesser extent the solar albedo load). In order to improve the efficiency of the radiator a deployable Thermal IR baffle was modelled (see Fig. 13). The inside faces of this baffle are to be coated with a low-emissivity coating (for example, vacuum deposited aluminum) to improve the effective view factor of the radiator to deep space while blocking views to Earth. In order to avoid interference with the spacecraft Attitude Determination and Control System (ADCS) the stiffness and first eigenmode of the deployed baffle needs to be outside of the control bandwidth of the fine pointing system.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx The TMM indicated that although the thermal IR baffle improves the performance of the radiator, there are periods of the orbit where the radiator is exposed to the Earth and does not provide enough cooling to the image sensor. Fortunately, these periods occur outside the observation windows and therefore the spacecraft is able to slew the radiator away from the Earth without significantly compromising the power generating capacity of the solar arrays. This can be seen in Fig. 14, where the image sensor temperatures are plotted during several orbits with and without the Earth IR avoidance manoeuvres. The design and analysis carried out on the image sensor cooling system shows the fundamental feasibility for this aspect of the mission.

4. CONCEPT OF OPERATIONS The concept of operations for Space Eye is very much a work in progress at the time of writing, however some aspects have been worked out. The science aims of the project require the telescope to obtain repeated long exposure images of a small number of target fields for as long as possible.

4.1 Target fields The exact positions of the target fields will be chosen based on a number of factors, including the positions of suitable guide stars, avoidance of very bright stars and the locations of galaxies and galaxy groups. It is possible to constrain the general location of the target fields based on sensitivity and systematic error considerations, however. Sensitivity models for the baseline design which include the effects of Zodiacal light and Galactic dust show that the preferred regions of sky are those close to the North ecliptic pole from February to July and close to the South ecliptic pole from August to January, and that the tightest constraints come from Galactic dust (see Sec. 3.1.5. We can use relative sensitivity maps (Fig. 11) to narrow down the optimum target field positions to between 15.5 and 16.5 hours Right Ascension and +55 and +60 degrees declination in the north and between 4 and 5 hours Right Ascension and -50 and -60 degrees declination in the south. Within each of these regions we expect to select 1 or 2 target fields, and each region will be observed for approximately 6 months before switching to the other region.

4.2 Operational requirements In order to observe both northern and southern target fields under favourable Zodiacal light conditions we require an operational lifetime of at least 1 year, with a goal of 2 years or more. Based on this lifetime requirement and the results our initial power, thermal and communications budget analyses we have selected a nominal circular Sun-synchronous orbit at 600 km altitude, 96.7 min period and LTAN of 14:00.

4.3 Observing constraints Useful scientific data can only be acquired when certain constraints are met. These include image sensor tem- perature (−40 ◦C) and minimum angular separations of the target field from the Earth’s disc, the Sun and the Moon (25◦, 60◦ and 60◦ respectively). Preliminary analyses indicate that for the nominal orbit and approximate target field positions approximately 3–4 600 s science exposures will be possible during each 96.7 min orbit.

4.4 Observing sequence The nominal sequence of operations for science observations is as follows:

1. Slew spacecraft to target field, arcminute level pointing accuracy is sufficient. Roll angle is chosen to orientate the main solar array towards the Sun 2. Take a short exposure with the main image sensor to locate positions of pre-selected guide stars (2-3) on the image sensor, define regions-of-interest (RoIs) around them. 3. Begin continuous imaging of the guide star RoIs and start closed loop image stabilisation using guide star centroids (ADCS 2nd stage). 4. Take a long exposure using the remainder of the main image sensor. Usually this would be a 600s exposure but some shorter exposures will be taken to obtain unsaturated images of the brightest stars.

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 5. Repeat 4 until orbital motion causes observing constraints to be no longer satisfied, likely after 3–4 expo- sures 6. Perform Earth IR avoidance manoeuvres until observering constraints met again. 7. Repeat from 1 with pointing offset to the next dither position

Over the course of 6 orbits Space Eye will obtain images at each of 6 dither positions in order to construct contiguous images for each of the 6 filters in the focal plane mosaic. Over the course of a 6 month period spent observing either the northern or southern targets the spacecraft will observe at roll angles spanning a range of 180◦ as the spacecraft tracks the Sun with its main solar array. This ensures that each position on the sky is observed at a range of field positions, which helps in suppressing residual calibration errors and internal reflections.

4.5 Calibration sequences Space Eye will be extensively characterised before launch however these data will be supplemented with on orbit calibrations, including dark current measurements and flat fielding using a combination of Earth streak images, stellar photometry and median sky frames. The on-orbit measurements will account for changes caused by radiation damage, etc. In addition science observations will be interspersed with exposures of bright stars (‘PSF standards’) to regularly characterise the faint, outer parts of the PSF wings in a strategy similar to that reported by Tujillo and Fliri.27

4.6 Data handling Each main image sensor image will be captured at 2000 x 1504 pixel resolution and 16 bits/pixel depth, i.e. each comprises 6.016 MB of raw data. Image data will be stored as losslessly compressed Flexible Image Transport System (FITS) files, which typically have compression factors of around 2 for astronomical data. On board data processing will be limited to insertion of relevant spacecraft and instrument status information into FITS file headers, all raw images will be downlinked for processing and analysis on the ground. Based on the assumption of 3–4 science images per 96.7 min orbit the average (compressed) data rate would be ∼ 135–180 MB per day. Downlinking this volume of data from a CubeSat using standard S-band communications and 1–2 ground stations would be a challenge, but is achievable.26

5. STATUS AND PLANS At the time of writing funding to complete the design, construction, testing, launch, and commissioning of the Australian Space Eye is being sought via the Australian Research Council’s Linkage Infrastructure, Equipment & Facilities (LIEF) national competitive grant scheme. The LIEF grant scheme allows consortia lead by an Australian higher education institution to seek part funding (typically ∼ 50%) for a research infrastructure project from the government, with the remainder to come from the institutions of the consortium. The Space Eye LIEF consortium is lead by PI Lee Spitler of Macquarie University and includes astronomers, instrument scientists and engineers from 7 Australian universities (Macquarie University, Australian National University, UNSW, University of Sydney, University of Queensland, Western Sydney University and Swinburne), the Australian Astronomical Observatory, and both Tyvak and California Polytechnic State University, San Luis Obispo from the USA. The outcome of our grant application is expected in October/November 2016 and, if successful, will be followed by a 3 year construction phase with launch and commissioning planned for H2 2019.

ACKNOWLEDGMENTS This research made use of Astropy, a community-developed core Python package for astronomy,28 and the affiliated package ccdproc.29 Some of the results in this paper have been derived using the HEALPix∗30 package. This work also used the NumPy,31 Scipy,32 Matplotlib33 and IPython34 Python packages. ∗http://healpix.sf.net/

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx REFERENCES [1] McGraw, J. T. et al., “Ground-based observatory operations optimized and enhanced by direct atmospheric measurements,” Proc. SPIE 7739, 7739-29 (2010). [2] Moreels, G. et al., “Near-infrared sky background fluctuations at mid- and low latitudes,” Exp. Astron. 22, 87–107 (2008). [3] Leinert, C. et al., “The 1997 reference of diffuse night sky brightness,” Astron. Astrophys. Suppl. Ser. 127, 1–99 (1998). [4] Sandin, C., “The influence of diffuse scattered light. I. The PSF and its role in observations of the edge-on galaxy NGC 5907,” Astron. Astrophys. 567, A97 (2014). [5] Sandin, C., “The influence of diffuse scattered light. II. Observations of galaxy haloes and thick discs and hosts of blue compact galaxies,” Astron. Astrophys. 577, A106 (2015). [6] Duc, P.-A. et al., “The ATLAS 3D project XXIX. The new look of early-type galaxies and surrounding fields disclosed by extremely deep optical images,” MNRAS 446, 120–143 (2015). [7] Abraham, R. G. and van Dokkum, P. G., “Ultralow surface brightness imaging with the Dragonfly Telephoto Array,” Publ. Astron. Soc. Pacific 126, 55–69 (2014). [8] van Dokkum, P. G. et al., “Forty-seven Milky Way-sized, extremely diffuse galaxies in the Coma cluster,” Astrophys. J. 798, L45 (2015). [9] Horton, A. et al., “The Huntsman Telephoto Array: low surface brightness imaging with COTS optics,” Proc. SPIE 9906, 9906-163 (2016). [10] Cooray, A., “Extragalactic background light: measurements and applications,” R. Soc. Open Sci. 3 (2016). [11] Bernstein, R. A., “The optical extragalactic background Light: revisions and further comments,” Astrophys. J. 666, 663–673 (2007). [12] Aharonian, F. et al., “A low level of extragalactic background light as revealed by gamma-rays from blazars.,” Nature 440, 1018–1021 (2006). [13] Tsumura, K. et al., “Observations of the near-infrared spectrum of the Zodiacal light with CIBER,” Astro- phys. J. 719, 394–402 (2010). [14] Giavalisco, M., Sahu, K., and Bohlin, R., “New estimates of the sky background for the HST exposure time calculator,” STScI Instrument Science Tech. Tep. (2002). [15] Aldering, G., “SNAP Sky Background at the North Ecliptic Pole,” LBNL Tech. Rep., LBNL-51157 (2001). [16] Zemcov, M. et al., “The Cosmic Infrared Background Experiment (CIBER): a sounding tocket payload to study the near infrared extragalactic background light,” Astrophys. J. Suppl. Ser. 207, 31 (2013). [17] Korngut, P. M. et al., “The Cosmic Infrared Background Experiment (CIBER): the narrow-band spectrom- eter,” Astrophys. J. Suppl. Ser. 207, 34 (2013). [18] van Dokkum, P. G., Abraham, R., and Merritt, A., “First results from the Dragonfly Telephoto Array: the apparent lack of a stellar halo in the massive spiral galaxy M101,” Astrophys. J. 782, L24 (2014). [19] Hevner, R. et al., “An advanced standard for CubeSats,” Proc. 25th AIAA/USU Small Satellite Conf., SC11-II-3 (2011). [20] Jorden, P. R. et al., “e2v new CCD and CMOS technology developments for astronomical sensors,” Proc. SPIE 9154, 9154-0M (2014). [21] Soman, M. et al., “Design and characterisation of the new CIS115 sensor for JANUS, the high resolution camera on JUICE,” Proc. SPIE 9154, 9154-07 (2014). [22] Wang, S.-Y. et al., “Characteristic of e2v CMOS sensors for astronomical applications,” Proc. SPIE 9154, 9154-2I (2014). [23] Colina, L., Bohlin, R. C., and Castelli, F., “The 0.12-2.5 micron absolute flux distribution of the Sun for comparison with solar analog stars,” Astron. J. 112, 307 (jul 1996). [24] Abergel, A. et al., “Planck 2013 results. XI. All-sky model of thermal dust emission,” Astron. Astrophys. 571, A11 (2014). [25] Fitzpatrick, E. L., “Correcting for the effects of interstellar extinction,” Publ. Astron. Soc. Pacific 111, 63–75 (1999).

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx [26] Reisenfeld, S., Spitler, L., and Horton, A., “The Australian Space Eye: ultra-faint astronomy imaging from space,” in 33rd AIAA Int. Commun. Satell. Syst. Conf. Exhib., AIAA 20115-4337 (2015). [27] Trujillo, I. and Fliri, J., “Beyond 31 mag arcsec−2 : the frontier of low surface brightness imaging with the largest optical telescopes,” Astrophys. J. 823, 123 (2016). [28] Robitaille, T. P. et al., “Astropy: A community Python package for astronomy,” Astron. Astrophys. 558, A33 (2013). [29] Craig, M. W. et al., “ccdproc: CCD data reduction software,” (2015). [30] Gorski, K. M. et al., “HEALPix – a Framework for High Resolution Discretization, and Fast Analysis of Data Distributed on the Sphere,” Astrophys. J. 622, 759–771 (2004). [31] Van Der Walt, S., Colbert, S. C., and Varoquaux, G., “The NumPy array: A structure for efficient numerical computation,” Comput. Sci. Eng. 13, 22–30 (2011). [32] Jones, E. et al., “SciPy: Open source scientific tools for Python,” (2001). [33] Hunter, J. D., “Matplotlib: A 2D graphics environment,” Comput. Sci. Eng. 9(3), 99–104 (2007). [34] P´erez,F. and Granger, B. E., “IPython: A system for interactive scientific computing,” Comput. Sci. Eng. 9(3), 21–29 (2007).

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx PROCEEDINGS OF SPIE

Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave

Howard A. MacEwen Giovanni G. Fazio Makenzie Lystrup Editors

26 June – 1 July 2016 Edinburgh, United Kingdom

Sponsored by SPIE

Cooperating Organizations American Astronomical Society (United States) • Australian Astronomical Observatory (Australia) • Association of Universities for Research in Astronomy (AURA) Canadian Astronomical Society (CASCA) (Canada) • Canadian Space Agency (Canada) European Astronomical Society (Switzerland) • European Southern Observatory (Germany) National Radio Astronomy Observatory • Royal Astronomical Society (United Kingdom) Science & Technology Facilities Council (United Kingdom)

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Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, edited by Howard A. MacEwen, Giovanni G. Fazio, Makenzie Lystrup, Proc. of SPIE Vol. 9904, 990401 · © 2016 SPIE · CCC code: 0277-786X/16/$18 · doi: 10.1117/12.2249638

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xv Authors

xxvii Conference Committee

xxxi Introduction

Part One

SESSION 1 JWST I

9904 03 Status of the JWST optical telescope element [9904-2]

9904 04 JWST telescope integration and test progress [9904-3]

SESSION 2 JWST II

9904 06 The JWST science instrument payload: mission context and status [9904-5]

9904 07 James Webb Space Telescope optical telescope element/integrated science instrument module (OTIS) status [9904-6]

9904 08 Cryo-vacuum testing of the JWST Integrated Science Instrument Module [9904-7]

9904 09 Wavefront-error performance characterization for the James Webb Space Telescope (JWST) Integrated Science Instrument Module (ISIM) science instruments [9904-164]

SESSION 3 JWST III

9904 0A Stray light field dependence for the James Webb Space Telescope [9904-9]

9904 0B The JWST/NIRSpec instrument: update on status and performances [9904-14]

9904 0C Hartmann test for the James Webb Space Telescope [9904-11]

9904 0D Getting JWST’s NIRSpec back in shape [9904-12]

9904 0E Slitless spectroscopy with the James Webb Space Telescope Near-Infrared Camera (JWST NIRCam) [9904-13]

9904 0F Preparing for JWST wavefront sensing and control operations [9904-10]

iii

Proc. of SPIE Vol. 9904 990401-3

Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx SESSION 4 NASA LARGE MISSION CONCEPTS

9904 0G Potential large missions enabled by NASA’s space launch system [9904-15]

9904 0H End-to-end assessment of a large aperture segmented ultraviolet optical infrared (UVOIR) telescope architecture [9904-16]

9904 0J Initial technology assessment for the Large-Aperture UV-Optical-Infrared (LUVOIR) mission concept study [9904-18]

SESSION 5 NASA MISSION STUDIES: JOINT SESSION WITH CONFERENCES 9904 AND 9905

9904 0K The Far-Infrared Surveyor Mission study: paper I, the genesis (Invited Paper) [9904-301]

9904 0M The LUVOIR science and technology definition team (STDT): overview and status (Invited Paper) [9904-303]

9904 0N The X-Ray Surveyor mission concept study: forging the path to NASA astrophysics 2020 decadal survey prioritization (Invited Paper) [9904-304]

SESSION 6 EUCLID

9904 0O The Euclid mission design [9904-19]

9904 0P Euclid end-to-end straylight performance assessment [9904-21]

9904 0Q VIS: the visible imager for Euclid [9904-20]

9904 0R Optical verification tests of the NISP/Euclid Grism qualification model [9904-24]

9904 0T Euclid Near Infrared Spectrometer and Photometer instrument concept and first test results obtained for different breadboards models at the end of phase C [9904-22]

9904 0U The read-out shutter unit of the Euclid VIS instrument [9904-89]

9904 0V Coating induced phase shift and impact on Euclid imaging performance [9904-87]

SESSION 7 DEEP SURVEYS

9904 0W The Primordial Inflation Explorer (PIXIE) [9904-26]

9904 0X LiteBIRD: lite satellite for the study of B-mode polarization and inflation from cosmic microwave background radiation detection [9904-27]

SESSION 8 SOLAR SYSTEM STUDIES

9904 0Z Main results of the PICARD mission [9904-29]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 9904 10 Geometrical distortion calibration of the stereo camera for the BepiColombo mission to Mercury [9904-30]

9904 11 Development of compact metal-mirror image slicer unit for optical telescope of the SOLAR-C mission [9904-31]

SESSION 9 WFIRST I

9904 13 Canadian contributions studies for the WFIRST instruments [9904-33]

SESSION 10 WFIRST II

9904 18 Low order wavefront sensing and control for WFIRST coronagraph [9904-38]

9904 19 Closing the contrast gap between testbed and model prediction with WFIRST-CGI shaped pupil coronagraph [9904-39]

9904 1A PISCES: an integral field spectrograph technology demonstration for the WFIRST coronagraph [9904-119]

SESSION 11 TECHNOLOGIES

9904 1B The LATT way towards large active primaries for space telescopes [9904-41]

9904 1C Telescope polarization and image quality: Lyot coronagraph performance [9904-42]

9904 1D Innovative focal plane design for large space telescopes [9904-43]

9904 1E The CaSSIS imaging system: optical performance overview [9904-44]

SESSION 12 SYSTEMS I

9904 1H The Configurable Aperture Space Telescope (CAST) [9904-47]

9904 1I APERTURE: a precise extremely large reflective telescope using re-configurable elements [9904-48]

9904 1J ASTRO-1: a 1.8m unobscured space observatory for next generation UV/visible astrophysics and exoplanet exploration [9904-49]

SESSION 13 SYSTEMS II

9904 1K Optical telescope system-level design considerations for a space-based gravitational wave mission [9904-50]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 9904 1L A development roadmap for critical technologies needed for TALC: a deployable 20m annular space telescope [9904-51]

SESSION 14 IN-SPACE SERVICING

9904 1N SEL2 servicing: increased science return via on-orbit propellant replenishment [9904-53]

9904 1O In-space assembly and servicing infrastructures for the Evolvable Space Telescope (EST) [9904-54]

SESSION 15 NANOSATS AND CUBESATS

9904 1P FalconSAT-7: a membrane space solar telescope [9904-55]

9904 1Q The Australian Space Eye: studying the history of galaxy formation with a CubeSat [9904-56]

9904 1R Image processing in the BRITE nano-satellite mission [9904-57]

SESSION 16 EXOPLANETS I

9904 1S The maturing of high contrast imaging and starlight suppression techniques for future NASA exoplanet characterization missions [9904-58]

9904 1T A comparison of analytical depth of search metrics with mission simulations for exoplanet imagers [9904-59]

9904 1U A direct comparison of exoEarth yields for starshades and coronagraphs [9904-60]

9904 1W ARIEL: an ESA M4 mission candidate [9904-62]

9904 1X The science of ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey) [9904-63]

SESSION 17 EXOPLANETS II

9904 1Y Lyot coronagraph design study for large, segmented space telescope apertures [9904-64]

Part Two

9904 20 The Segmented Aperture Interferometric Nulling Testbed (SAINT) I: overview and air-side system description [9904-66]

9904 21 A new deformable mirror architecture for coronagraphic instrumentation [9904-67]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx SESSION 18 EXOPLANETS III

9904 22 High contrast imaging in multi-star systems: technology development and first lab results [9904-68]

9904 25 Starshade starlight-suppression performance with a deployable structure [9904-71]

SESSION 19 EXOPLANETS IV

9904 28 PLATO: a multiple telescope spacecraft for exo-planets hunting [9904-73]

9904 29 ESA CHEOPS mission: development status [9904-74]

9904 2A CHEOPS: status summary of the instrument development [9904-75]

9904 2C The TESS camera: modeling and measurements with deep depletion devices [9904-77]

SESSION 20 ASTROMETRY

9904 2D Gaia: focus, straylight and basic angle [9904-78]

9904 2E Enabling science with Gaia observations of naked-eye stars [9904-79]

9904 2F Microarcsecond astrometric observatory Theia: from dark matter to compact objects and nearby earths [9904-80]

SESSION 21 IR SYSTEMS

9904 2H New cryogenic system of the next-generation infrared astronomy mission SPICA [9904-82]

9904 2I SPICA Mid-infrared Instrument (SMI): technical concepts and scientific capabilities [9904-83]

9904 2K The Far Infrared Spectroscopic Explorer (FIRSPEX): probing the lifecycle of the ISM in the universe [9904-85]

9904 2L The Space High Angular Resolution Probe for the Infrared (SHARP-IR) [9904-86]

9904 2M Final tolerancing approach and the value of short-cutting tolerances by measurement [9904-23]

9904 2N The FLARE mission: deep and wide-field 1-5um imaging and spectroscopy for the early universe: a proposal for M5 cosmic vision call [9904-179]

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9904 2Q Detailed design and first tests of the application software for the instrument control unit of Euclid-NISP [9904-92]

9904 2R Modeling effects of common molecular contaminants on the Euclid infrared detectors [9904-93]

9904 2T EGSE customization for the Euclid NISP Instrument AIV/AIT activities [9904-97]

9904 2U How to test NISP instrument for EUCLID mission in laboratory [9904-95]

9904 2V Focal plane mechanical design of the NISP/Euclid instrument [9904-96]

POSTER SESSION: EXOPLANETS

9904 2X Testing and characterization of the TESS CCDs [9904-100]

9904 2Y The instrument control unit of the ESA-PLATO 2.0 mission [9904-101]

9904 2Z Manufacturing and alignment tolerance analysis through Montecarlo approach for PLATO [9904-102]

9904 30 Radiation, thermal gradient and weight: a threefold dilemma for PLATO [9904-103]

9904 31 Thermal effects on PLATO point spread function [9904-104]

9904 32 A display model for the TOU of PLATO: just a cool toy or a benchmark of opportunities? [9904-105]

9904 33 An integrated payload design for the Atmospheric Remote-sensing Infrared Exoplanet Large-survey (ARIEL) [9904-106]

9904 34 Design of an afocal telescope for the ARIEL mission [9904-107]

9904 36 The Atmospheric Remote-sensing Infrared Exoplanets Large-survey (ARIEL) payload electronic subsystems [9904-109]

9904 37 Dimensional stability testing in thermal vacuum of the CHEOPS optical telescope assembly [9904-111]

9904 38 The performance of the CHEOPS on-ground calibration system [9904-112]

9904 39 Aligning the demonstration model of CHEOPS [9904-113]

9904 3A Coronagraphic wavefront sensing with COFFEE: high spatial-frequency diversity and other news [9904-114]

9904 3C High-contrast imager for Complex Aperture Telescopes (HiCAT). 4. Status and wavefront control development [9904-118]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 9904 3D Recent achievements on ASPIICS, an externally occulted coronagraph for PROBA-3 [9904-121]

9904 3E Contrast improvement with imperfect pre-coronagraph and dark-hole [9904-122]

9904 3F Low-signal, coronagraphic wavefront estimation with Kalman filtering in the high contrast imaging testbed [9904-123]

9904 3G Experimental study of starshade at flight Fresnel numbers in the laboratory [9904-125]

9904 3H Results of edge scatter testing for a starshade mission [9904-126]

9904 3I Ground-based testing and demonstrations of starshades [9904-127]

9904 3J Diffraction-based analysis of tunnel size for a scaled external occulter testbed [9904-128]

9904 3K Measurements of high-contrast starshade performance in the field [9904-129]

9904 3L Engineering considerations applied to starshade repointing [9904-130]

9904 3O The JWST/NIRSpec exoplanet exposure time calculator [9904-135]

9904 3P Exoplanets with JWST: degeneracy, systematics and how to avoid them [9904-136]

9904 3R Exploring the potential of the ExoSim simulator for transit spectroscopy noise estimation [9904-138]

POSTER SESSION: INFRARED

9904 3U SAFARI optical system architecture and design concept [9904-141]

9904 3V Sensitivity estimates for the SPICA Mid-Infrared Instrument (SMI) [9904-142]

9904 3W Mechanical cooler system for the next-generation infrared space telescope SPICA [9904-143]

POSTER SESSION: JWST

9904 3Y Use of living technical budgets to manage risk on the James Webb Space Telescope optical element [9904-146]

9904 3Z Alignment of the James Webb Space Telescope optical telescope element [9904-147]

9904 40 Characterization of the JWST Pathfinder mirror dynamics using the center of curvature optical assembly (CoCOA) [9904-150]

9904 41 MIRI/JWST detector characterization [9904-151]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 9904 42 Calibration results using highly aberrated images for aligning the JWST instruments to the telescope [9904-152]

9904 44 In-orbit commissioning of the NIRSpec instrument on the James Webb Space Telescope [9904-154]

9904 45 The spectral calibration of JWST/NIRSpec: results from the recent cryo-vacuum campaign (ISIM-CV3) [9904-156]

9904 46 Flat-fielding strategy for the JWST/NIRSpec multi-object spectrograph [9904-157]

Part Three

9904 47 First light of the NIRISS Optical Simulator (NOS) [9904-158]

9904 48 In-focus phase retrieval using JWST-NIRISS's non-redundant mask [9904-159]

9904 49 Alignment test results of the JWST Pathfinder Telescope mirrors in the cryogenic environment [9904-161]

9904 4A James Webb Space Telescope optical simulation testbed III: first experimental results with linear-control alignment [9904-162]

9904 4B A new method of superbias construction for NIRCam [9904-163]

9904 4C Model predictions and observed performance of JWST's cryogenic position metrology system [9904-166]

9904 4D Updated cryogenic performance test results for the flight model JWST fine guidance sensor [9904-167]

9904 4E Performance of the primary mirror center-of-curvature optical metrology system during cryogenic testing of the JWST Pathfinder telescope [9904-251]

POSTER SESSION: SYSTEMS

9904 4F On the performance of the Gaia auto-collimating flat mirror assembly: could it be even better? [9904-168]

9904 4G How mission requirements affect observations: case of the PICARD mission [9904-169]

9904 4H Optical designing of LiteBIRD [9904-170]

9904 4J The cosmic infrared background experiment-2 (CIBER-2) for studying the near-infrared extragalactic background light [9904-172]

9904 4K Prime focus architectures for large space telescopes: reduce surfaces to save cost [9904-173]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 9904 4L Reaching sub-milimag photometric precision on Beta Pictoris with a nanosat: the PicSat mission [9904-174]

9904 4N The infrared spectrometer for Twinkle [9904-176]

9904 4R Status and path forward for the large ultraviolet/optical/infrared surveyor (LUVOIR) mission concept study [9904-181]

POSTER SESSION: INSTRUMENTS

9904 4T Correcting for the effects of pupil discontinuities with the ACAD method [9904-184]

9904 4U A four mirror anastigmat collimator design for optical payload calibration [9904-185]

9904 4V Xenon arc lamp spectral radiance modelling for satellite instrument calibration [9904-186]

9904 4W Application of Peterson’s stray light model to complex optical instruments [9904-187]

9904 4Z The shadow position sensors (SPS) formation flying metrology subsystem for the ESA PROBA- 3 mission: present status and future developments [9904-191]

9904 50 Preliminary evaluation of the diffraction behind the PROBA 3/ASPIICS optimized occulter [9904-192]

9904 51 Trade-off between TMA and RC configurations for JANUS camera [9904-193]

9904 52 Alignment procedure for detector integration and characterization of the CaSSIS instrument onboard the TGO mission [9904-194]

9904 54 Achromatic interfero-coronagraph with variable rotational shear in laboratory experiments [9904-196]

9904 56 The front-end electronics of the LSPE-SWIPE experiment [9904-198]

9904 58 PILOT optical alignment [9904-200]

9904 59 Near-infrared imaging spectrometer onboard NEXTSat-1 [9904-201]

9904 5A Testing and characterization of a prototype telescope for the evolved Laser Interferometer Space Antenna (eLISA) [9904-202]

9904 5B SINBAD electronic models of the interface and control system for the NOMAD spectrometer on board of ESA ExoMars Trace Gas Orbiter mission [9904-203]

9904 5C Concept study for a compact planetary homodyne interferometer (PHI) for temporal global observation of methane on Mars in IR [9904-204]

9904 5D HST/WFC3: understanding and mitigating radiation damage effects in the CCD detectors [9904-205]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx 9904 5E Performance of a cryogenic test facility for 4 K interferometer delay line investigations [9904-206]

9904 5G The latest results from DICE (Detector Interferometric Calibration Experiment) [9904-209]

9904 5H A cryogenic testbed for the characterisation of large detector arrays for astronomical and Earth-observing applications in the near to very-long-wavelength infrared [9904-210]

POSTER SESSION: PROCESSING

9904 5J Low noise flux estimate and data quality control monitoring in EUCLID-NISP cosmological survey [9904-91]

9904 5K Small-grid dithers for the JWST coronagraphs [9904-165]

9904 5M Data processing and algorithm development for the WFIRST coronagraph: comparison of RDI and ADI strategies and impact of spatial sampling on post-processing [9904-215]

9904 5N Accuracy analysis of a new method to estimate chromatic wavefront error [9904-216]

9904 5O Characterization of the ASPIICS/OPSE metrology sub-system and PSF centroiding procedure [9904-217]

9904 5Q Performance analysis of the GR712RC dual-core LEON3FT SPARC V8 processor in an asymmetric multi-processing environment [9904-219]

9904 5R On-board data processing for the near infrared spectrograph and photometer instrument (NISP) of the EUCLID mission [9904-220]

9904 5S Design-oriented analytic model of phase and frequency modulated optical links [9904-222]

9904 5U Gain determination of non-linear IR detectors with the differential photon transfer curve (dPTC) method [9904-224]

9904 5V Hi-fidelity multi-scale local processing for visually optimized far-infrared Herschel images [9904-225]

9904 5W The boot software of the control unit of the near infrared spectrograph of the Euclid space mission: technical specification [9904-226]

9904 5Z Spitzer Infrared Array Camera (IRAC) Pipeline: final modifications and lessons learned [9904-230]

9904 60 Instrument workstation for the EGSE of the Near Infrared Spectro-Photometer instrument (NISP) of the EUCLID mission [9904-231]

9904 62 The control unit of the near infrared spectrograph of the Euclid space mission: detailed design [9904-254]

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9904 63 Zernike wavefront sensor (ZWFS) development for Low Order Wavefront Sensing (LOWFS) [9904-243]

9904 64 Sparse aperture mask wavefront sensor testbed results [9904-244]

9904 66 Modeling of microelectromechanical systems deformable mirror diffraction grating [9904-246]

9904 68 Unimorph piezoelectric deformable mirrors for space telescopes [9904-248]

9904 69 HYPATIA and STOIC: an active optics system for a large space telescope [9904-249]

9904 6A Wavefront sensing in space from the PICTURE-B sounding rocket [9904-252]

POSTER SESSION: TECHNOLOGIES

9904 6B Use of updated material properties in parametric optimization of spaceborne mirrors [9904-233]

9904 6C Laboratory demonstration of a primary active mirror for space with the LATT: large aperture telescope technology [9904-234]

9904 6D Co-phasing primary mirror segments of an optical space telescope using a long stroke Zernike WFS [9904-235]

9904 6E The satellite formation flying in lab: PROBA-3/ASPIICS metrology subsystems test-bed [9904-236]

9904 6F CFRP mirror technology for cryogenic space interferometry: review and progress to date [9904-237]

9904 6H A novel design of dual-channel optical system of star-tracker based on non-blind area PAL system [9904-239]

9904 6I Distortion of the pixel grid in HST WFC3/UVIS and ACS/WFC CCD detectors and its astrometric correction [9904-240]

9904 6J Battery-powered thin film deposition process for coating telescope mirrors in space [9904-253]

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Authors

Numbers in the index correspond to the last two digits of the six-digit citation identifier (CID) article numbering system used in Proceedings of SPIE. The first four digits reflect the volume number. Base 36 numbering is employed for the last two digits and indicates the order of articles within the volume. Numbers start with 00, 01, 02, 03, 04, 05, 06, 07, 08, 09, 0A, 0B...0Z, followed by 10-1Z, 20-2Z, etc.

Abreu, A., 2E Bajaj, V., 5D Accatino, L., 4Z Balasubramanian, Kunjithapatham, 18 Acton, D. Scott, 0C, 0F, 42 Balestra, Andrea, 0T, 2Q, 2T, 5R, 60 Ade, Peter A. R., 58, 5H Ballard, Marlin, 20 Aigrain, Suzanne, 3P Bandy, Timothy, 28, 2Z, 30, 31 Akiba, Y., 0X Barbier, Rémi, 0T, 2R, 5J Alato, S., 0K Barker, Elizabeth, 0F Albert, Loïc, 47 Barraclough, Simon, 1Q Alberts, Stacey, 41 Barrière, Jean Christophe, 0T Allen, Marsha, 0F Barron, D., 0X Alves de Oliveira, Catarina, 0B, 3O, 44, 45, 46 Barstow, Joanna K., 1X, 3P Amiaux, Jérôme, 0O, 0P, 0Q, 0T, 0V, 1L Barto, Allison A., 3Y Andersen, Geoff, 1P Bartos, Randall, 18 Andersen, J. J., 2T Basso, Stefano, 28, 2Z, 30, 31 Andersen, Michael Ingemann, 0T, 2U Battersby, C., 0K Anderson, Jay, 5D, 6I Battle, John, 4J André, Y., 58 Baudoz, P., 3A Anglada Escudé, Guillem, 2F Baustista, L., 58 Anselmi, Alberto, 0O Beaton, Alexander, 4D Aparicio del Moral, Beatriz, 5B Beaulieu, Jean-Philippe, 1X, 33 Arai, Toshiaki, 4J Beaumont, Florent, 0T, 2U Aranyos, Thomas, 1N Beck, T., 2A, 39 Arcidiacono, Carmelo, 1B, 6C Behar, E., 5G Arenberg, Jon, 0H Belenguer, Tomás, 3U Armus, L., 0K Belikov, Ruslan, 22, 5N, 66 Arnold, K., 0X Bello, Mara, 1L Aroldi, Gianluca, 10 Bemporad, Alessandro, 4Z, 50, 5O, 6E Aronstein, David L., 09 Bendek, Eduardo A., 1H, 22 Arrazola, David, 3U Bender, Ralf, 2M Artigau, Étienne, 13, 47 Benson, Craig, 1Q Artigues, B., 36 Benz, Willy, 28, 29, 2A, 2Z, 30, 31, 39 Asano, Kentaroh, 2I Bergin, E., 0K Asmolova, Olha, 1P Bergomi, Maria, 28, 2A, 2Z, 30, 31, 32, 39

Asquier, J., 29 Berkenbosch, Sophie, 5B Atkinson, Charlie, 03 Bernard, J.-Ph., 58 Audley, Michael D., 3U Berthé, Michel, 0O, 0Q, 0T Auguères, Jean-Louis, 33 Bevilacqua, A., 56 Aumont, J., 58 Bianucci, Giovanni, 1L Auricchio, Natalia, 0T, 2Q, 2T, 5R, 60 Biasi, Roberto, 1B, 6C Austin, James, 1L Biasotti, M., 56 Autissier, N., 0U Biermann, M., 2D Awan, S., 0Q Biondi, Federico, 28, 2Z, 30, 31, 32, 39 Azzollini, Ruyman, 0O, 0Q Birkmann, Stephan M., 08, 0B, 0D, 3O, 44, 45, 46 Baccani, Cristian, 4Z, 50, 5O, 6E Bishop, Georgia, 33 Bacinski, J., 44 Bisson, Gary, 3Z Bacon, Charles, 1N Bock, James, 4J Baggett, S. M., 5D Bode, Andreas, 2M Baggett, Wayne, 0F Bodendorf, Christof, 2M Bai, Jian, 6H Bodin, Pierre, 28

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Boehm, Céline, 2F Candini, Gian Paolo, 5B Boenke, Tobias, 0O, 0P, 0T, 0V Cao, J., 1I Boerner, Anko, 28 Capobianco, Gerardo, 4Z, 50, 5O, 6E Böker, Torsten, 0B, 3O, 44, 45, 46 Capobianco, V., 2Q, 2T, 60 Boland, John, 4C Cara, C., 0Q, 5G

Bolcar, Matthew R., 0H, 0J, 20, 4R Carey, Sean J., 0K, 5Z Bolognese, Jeff, 20 Carle, Michael, 0T, 2U Bombrun, A., 2D Carlotti, Alexis, 1Y Bon, William, 0T, 2V Carminati, Lionel, 0P, 0V Bonino, D., 2Q, 2T, 60 Carter, R., 0K Bonino, Luciana, 0P, 0V Casas, Ricard, 0T Bonnefoi, Anne, 0T, 2V Case, A., 1I Bonnefois, Aurélie, 4A Casement, Suzanne, 25, 3H Bonnewijn, Sabrina, 5B Cash, Webster, 3I Bonoli, Carlotta, 0T, 2Q, 2T, 5R, 60 Castera, Alain, 5J Borncamp, David, 6I Casti, M., 4Z, 5O, 6E Borrelli, Donato, 10 Catala, Claude, 28 Borrill, J., 0X Catalán, Jordi, 62 Borsa, Francesco, 28, 2Z, 30, 31 Caux, E., 2K Borsato, Enrico, 0T, 5R Cazaubiel, Vincent, 0O Bortoletto, Favio, 0T, 2Q, 2T, 5R, 60 Cernica, Ileana, 3D, 5O, 6E Bos, A., 4F Cessa, V., 2A, 39 Bouchet, P., 41 Cessateur, G., 0Z Boulade, O., 58 Chabanat, Eric, 5J Boumier, P., 0Z Chae, Jangsoo, 59 Bourque, M., 5D Chaigneau, M., 58 Bousquet, F., 58 Chakrabarti, Supriya, 6A Bouzit, M., 58 Chambers, Victor J., 1A Bowen, John, 1Q Chaney, David, 40, 4E Bowles, N., 1X Charlieu, Florence, 5J Boyadjian, J., 2D Charra, M., 58 Boyce, Russell, 1Q Chassat, F., 2D Bozzo, E., 0Q, 0U Chayer, Pierre, 4D Bradford, C. M., 0K Chazelas, B., 38 Bramall, David G., 4U Chendra, R., 0X Brandeker, Alexis, 28, 2Z, 30, 31 Chesbrough, Christian, 2C Brändli, Mathias, 28, 2Z, 30, 31 Chesné, Simon, 1L Brandt, Timothy, 1A Chevalier, A., 0Z Bray, N., 58 Chiarusi, T., 0T, 2Q, 60 Breckinridge, J. B., 1C, 4K Chinellato, Simonetta, 28, 2Z, 30, 31 Brien, Thomas L. R., 5H Chinone, Y., 0X Bright, Stacey N., 41 Chipman, R. A., 1C Briguglio, Runa, 1B, 6C Chluba, Jens, 0W Broeg, Chris, 29, 2A Cho, H., 2R Brousseau, Denis, 13, 47 Cho, S., 0X Bruno, Giordano, 28, 2Z, 30, 31 Choquet, Élodie, 3C, 4A

Buckley, Steve, 3D, 4Z, 6E Chrisp, Michael, 2C Buder, M., 2A Chu, Laurie, 0E Budianu, E., 6E Chung, Y.-W., 1I Bulgarelli, A., 2T, 60 Cillis, A., 2R Burgarella, D., 2N Cimmino, Rosario F., 5S Burke, Barry, 2C Citterio, Oberto, 1L Buttice, V., 58 Clairquin, Roland, 5B Cabrera, Juan, 28 Clampin, Mark, 1U, 20, 5K Cady, Eric J., 19, 1A, 1U, 3F Clark, Kristin, 2C Caillat, Amandine, 0R, 0T, 58 Clark, Paul, 4V Calabria, Peter, 5J Claudi, Riccardo, 34 Calcines, Ariadna, 4U Clemens, Jean-Claude, 0T, 2R, 2U, 5J Caldwell, M., 2K Cole, R., 0Q Calvi, Adriano, 0O Colless, Matthew, 1Q

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Collette, Christophe, 1L Denniston, J., 0Q Colodro-Conde, Carlos, 0T, 2Q, 5W, 62 De Roche, Thierry, 28, 2Z, 30, 31 Colombo, Cyril, 0O De Rosa, Adriano, 0T, 2T, 60 Colomé, J., 36 De Sio, Antonio, 52 Comber, Brian J., 08 Desselle, Richard, 3D Comeau, Thomas, 0F Devaney, Nicholas, 69

Conforti, V., 2T, 60 de Vos, Lieve, 3D Connolly, Mark, 40, 4E DeWeese, Keith, 1N Conscience, C., 0Z Dewitte, S., 0Z Cook, Timothy A., 6A Dhabal, A., 2L Cooray, Asantha, 0K, 2K, 4J DiAntonio, Andrew, 4C Coppock, Eric, 0F Díaz-García, José Javier, 0T, 62 Corbard, T., 0Z Dichmann, Donald, 3L Corberand, P., 2D Dicken, D., 41 Corbineau, M.-C., 1I Di Ferdinando, D., 2T Corcione, Leonardo, 0T, 2Q, 2T, 5R, 60 Di Giorgio, Anna M., 0Q, 2Y, 36, 5Q, 5V Cordiner, M., 2L Di Lellis, Andrea M., 5Q Corral Van Damme, C., 29, 2A Dima, Marco, 28, 2Z, 30, 31, 32, 39 Correia, Sébastien, 1L Dimitrijevic, Igor, 1Q Cosentino, Joseph, 40, 4E DiPirro, M., 0K, 2L Cosentino, R., 2Y Djafer, D., 0Z, 4G Costille, Anne, 0R, 0T, 2M, 2U Dobbs, M., 0X Coudé du Foresto, V., 1X Dogoda, Peter, 20 Coulter, Daniel R., 1S Dohlen, K., 2N Coustenis, A., 1X Domagal-Goldman, Shawn D., 1U, 3L, 4R Coverstone, V. L., 1I Dominjon, A., 0X Crane, B., 58 Donati, M., 5G Cremonese, Gabriele, 10, 1E, 51, 52 Dormoy, Doriane, 0T Cretot-Richert, G., 13 Dorner, Bernhard, 0B, 45 Crook, M., 36 Dotani, T., 0X Crooke, Julie A., 4R Douchin, F., 58 Cropper, Mark, 0O, 0Q Douglas, Ewan S., 6A Crouzet, P.-E., 1W Doumayrou, Eric, 58, 5G Crouzier, Antoine, 2F, 4L, 5G Doyle, D., 2D Crowley, C. M., 2E Doyon, René, 47 Crussaire, J.-P., 58 Drossart, P., 1X Cukierman, A., 0X Drummond, Rachel, 5B Da Deppo, Vania, 10, 1E, 33, 34, 52 Dubois, J.-P., 58 Daigle, O., 13 Ducharme, M.-È., 13 Dal Corso, F., 0T, 2Q, 2T Ducret, Franck, 0T D'Alessandro, Maurizio, 0T, 5R Dufoing, C., 4L d'Amato, Francesco, 1B, 6C Duò, Fabrizio, 1B, 6C Damé, L., 0Z, 4G Dupont, J., 5G Dami, Michele, 10 Dupuis, J., 13 David, L., 4L Durand, Gilles A., 1L Davidson, M., 2D Dusini, Stefano, 0T, 2Q, 2T, 5R, 60 Dawson, O., 2R Dworzanski, Daniel, 20

Dean, Bruce H., 0F, 42 Ealet, Anne, 0O, 0T, 2R, 2U, 5J Debei, S., 2Q, 2T, 51, 60 Eccleston, Paul, 1X, 33, 36 de Bernardis, P., 58 Eder, Robert, 0D Decin, L., 1X Egami, Eiichi, 0E de Haan, T., 0X Egerman, Robert, 1J Delanoye, Sofie, 5B Eggens, Martin, 3U Delboulbe, A., 5G Egron, Sylvain, 3C, 4A Deline, A., 38 Ehrenreich, D., 2A Della Corte, V., 51 Ehrenwinkler, Ralf, 0D Delo, G., 2R Eldorado Riggs, A. J., 21, 3C, 3F, 64 de Marchi, G., 46 Elleflot, T., 0X Demers, Richard, 1A Ellis, Scott, 3H Denis, François, 3D Ellison, B., 2K

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Escudero Sanz, I., 1W García Muñoz, Antonio, 3O Etcheto, P., 58 Garcia, José, 0T, 2V Evers, Jaap, 3U García-Marín, Macarena, 41 Fabron, Christophe, 0T, 2U Garrett, Daniel, 1T Faiz, H., 4L Gaskin, Jessica, 0N Farina, Maria, 36, 5Q Gaspar Venancio, Luis M., 0O, 0P, 0V Farinato, Jacopo, 28, 2Z, 30, 31, 32, 39 Geis, Norbert, 2M Farinelli, Ruben, 0T, 2T, 5R Gélot, P., 58 Farisato, G., 32, 39 Genolet, L., 0Q, 0U Fatig, Curtis C., 08 Gerber, Michael, 1E, 52 Feautrier, P., 5G Gerin, M., 0K, 2K Febvre, Aurélien, 0T Gesa, L., 36 Feinberg, Lee D., 03, 04, 07, 0C, 0H, 0J Ghigo, Mauro, 28, 2Z, 30, 31 Feizi, A., 2R Giacomini, F., 0T, 2Q, 2T, 60 Fernández-Conde, Jesús, 5W Gianotti, F., 2T, 60 Fernández-Rodriguez, M., 3U Giardino, Giovanna, 0B, 3O, 45, 46 Ferrari, Marc, 1D, 4A Gielesen, W. L. M., 2D Ferraro, N., 2R Gigliotti, Trevis, 4C Ferriol, Sylvain, 0T, 5J Gillard, William, 0T, 2U, 5J Ferruit, Pierre, 0B, 3O, 44, 45, 46 Gillis, Jean-Marie, 3D Ficai Veltroni, Iacopo, 10, 1E Gimenez, Jean-Luc, 0T Fienup, James R., 09 Giusi, Giovanni, 2Y, 5Q Fineschi, Silvano, 3D, 4Z, 50, 5O, 6E Glaccum, William, 5Z Fioretti, V., 2T, 60 Glasse, Alistair C. H., 08, 41 Fixsen, Dale J., 0W, 2L Glassman, Tiffany M., 25, 3K, 3Z Fleury-Frenette, Karl, 3D Glazer, Stuart D., 08 Flores, A., 0K Goeckner-Wald, N., 0X Focardi, Mauro, 2Y, 33, 34, 36, 4Z, 50, 5O, 6E Goepel, M., 4W Foenard, G., 58 Goicoechea, J. R., 2K Foltz, R., 2R Goldsmith, P., 2K Fontanelli, F., 56 Golimovski, David, 6I Forget, F., 1X Gom, Brad G., 5E, 6F Fornari, F., 0T, 2Q, 2T, 60 Gómez López, Juan M., 5B Fortier, A., 2A Gomez, Jaime, 0T Foulon, Benjamin, 0R, 0T, 2V Gómez-Sáenz-de-Tejada, Jaime, 5W, 62 Fox, Ori, 41 Goncharov, Alexander, 69 France, Kevin C., 0J, 0M Gondoin, Philippe, 28 Franceschi, Enrico, 0T, 2Q, 2T, 5R, 60 Gong, Qian, 1A Fray, S., 4W Gonzales, Alexandria, 2C

Friso, E., 51 González Fernández, Luis M., 3U Friswell, M., 1X Goodsall, T., 2R Frolov, Pavel, 54 Gosmeyer, C., 5D Fujii, Takenori, 4H Goto, K., 2H Fujino, T., 0X Goullioud, Renaud, 2F, 5G Fujishiro, Naofumi, 3V Gow, J., 0Q Fuke, H., 0X Goy, Matthias, 69 Funaki, T., 0X Graas, Estelle, 3D Furesz, Gabor, 2C Grabarnik, S., 58 Fusco, Thierry, 3C, 4A Graczyk, Rafal, 3D Galano, Damien, 3D Grammer, Bryan, 1A

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Grandmont, F. J., 13 Hoffmann, H., 51 Grassi, Emmanuel, 0T Höhnemann, Holger, 5H Greeley, Bradford, 1A Holl, Berry, 2F Greenbaum, Alexandra Z., 48 Holland, A., 0Q Greene, Thomas P., 0E Holmes, Warren, 0T, 2R Greenhouse, Matthew A., 06 Holzapfel, W., 0X Greggio, Davide, 28, 2Z, 30, 31, 32, 39, 51 Hopkins, Randall C., 0G Griffin, Douglas, 1Q Hori, Y., 0X Griffin, M., 1X, 58 Hormuth, Felix, 0T Groff, Tyler D., 21, 3F Hornstrup, Allan, 0T Grogin, Norman, 6I Horodyska, Petra, 3D

Grupp, Frank, 0T, 2M, 2U Horton, Anthony, 1Q Güdel, Manuel, 1X, 33 Hosseini, Sona, 5C Guilpain, T., 2D Howard, Joseph, 0C Guizzo, Gian Paolo, 0T, 2Q, 2T, 60 Hristov, Viktor, 4J Gullieuszik, Marco, 28, 2Z, 30, 31, 39 Hubmayr, J., 0X Gunuganti, Sudhakar, 5E Hughes, A., 58 Guyon, Olivier, 0H Hugot, Emmanuel, 1D, 4A Hadaway, James B., 40, 49, 4E Hull, Tony, 6B Hadjimichael, Theo, 3Z Hunt, Thomas, 0Q, 33 Hahn, Walter, 3Z Hwang, T., 2R Hailey, M., 0Q Ichiki, K., 0X Haiml, Markus, 5H Ikhlef, R., 0Z Haley, Craig, 4D Imada, Hiroaki, 0X, 4H Hall, D., 0Q Inatani, J., 0X Hallibert, Pascal, 69 Ingalls, James G., 5Z Halverson, N., 0X Inoue, Masanori, 0X, 4H Hargrave, Peter C., 58, 5H Inoue, Y., 0X Harness, Anthony, 3I, 3K Irbah, A., 0Z, 4G Hartig, George, 0F Irie, F., 0X Hartogh, Paul, 1X, 33 Irwin, K., 0X Harvey, P., 0X Irwin, Patrick G. J., 3P Hasebe, T., 0X Isaacs, John C., 5K Hasegawa, M., 0X Isaak, Kate, 29, 2A, 3O Hattori, K., 0X Ishihara, Daisuke, 2I, 3V Hattori, M., 0X Ishino, Hirokazu, 0X, 4H Hauchecorne, A., 0Z, 4G Ishitsuka, H., 0X Hayden, William L., 0F Isobe, Naoki, 2H, 2I Hazumi, M., 0X Israel, H., 0Q Hein, Randall, 18 Israelsson, Ulf, 0T, 2R Helmbrecht, Michael A., 20 Ito, Makoto, 4H Helmich, F., 0K Jackman, Angela, 0G Hénault, F., 5G Jackson, Kate, 6D Heras, Ana Maria, 28 Jahn, Wilfried, 1D Hernandez, J., 2D Jahnke, Knud, 0O, 0T Hernandez, Olivier, 47 Jakobsen, Peter, 0T, 2U Herscovici-Schiller, O., 3A Jaumann, R., 51 Heske, A., 1W, 1X Jellema, Willem, 3U Hickey, M., 2R Jensen, Peter, 0B, 0D Hicks, Brian A., 20 Jeong, O., 0X Hidehira, N., 0X Jeong, Woong-Seob, 59

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Jordan, Margaret, 0F Kotani, Takayuki, 3E Juanola-Parramon, R., 2L Koyama, M., 11 Jurling, Alden S., 0F, 42 Kozhurina-Platais, Vera, 6I Kahle, D., 2R Kramer, C., 2K Kan, Em., 2R Kranitis, Nektarios, 3D Kan, Er., 2R Krick, Jessica E., 5Z Kanai, H., 0X Krist, John E., 19, 5M Kanai, Yoshikazu, 4J Kroneberger, M., 4W Kaneda, Hidehiro, 2I, 3V Krone-Martins, Alberto, 2F Karatsu, K., 0X Kubik, Bogna, 0T, 5J Karl, Hermann, 0B, 44 Kulp, Trey, 0F Kasdin, N. Jeremy, 1Y, 3C, 3F, 3G, 3J, 64 Kumagai, Shiomi, 3E

Kashima, Shingo, 0X, 4H Kuo, C.-L., 0X Katayama, N., 0X Kurokawa, Takashi, 3E Katterloher, Reinhard, 2M Kuromiya, S., 0X Kawada, Mitsunobu, 2H, 2I, 3W Kurowski, Michal, 3D Kawano, I., 0X Kusaka, A., 0X Kawasaki, T., 0X Labadie, Lucas, 2F Keating, B., 0X Lacour, S., 4L Kelly, Douglas M., 08, 0E Ladno, Michal, 3D Kendrew, Sarah, 3P Lafrasse, S., 5G Kern, Brian D., 19, 3F Lafrenière, D., 13 Kern, P., 5G Lagage, P. O., 1X, 5G Kernasovskiy, S., 0X Laine, B., 2D Keski-Kuha, Ritva, 03, 04, 07 Lajoie, Charles-Philippe, 0F, 4A, 5K Keskitalo, R., 0X Lallo, Matthew D., 0F Ketchazo, C., 5G Lam, Raymond, 18 Khandrika, H., 5D LaMarr, B., 2X Kholikov, S., 0Z Lambert, Andrew, 1Q Kibayashi, A., 0X Lamensans, Mikel, 0T Kida, Y., 0X Lander, Juli A., 04, 07 Kienlen, Michael, 1N Landini, Federico, 4Z, 50, 5O, 6E Kim, Il-Joong, 59 Lange, Nicolas, 69 Kim, Min Gyu, 4J, 59 Lanz, Alicia, 4J Kim, Minjin, 59 Lapeyrère, V., 4L Kim, Yunjong, 3G Larcheveque, C., 0U Kimble, Randy A., 08 Laudisio, Fulvio, 0T, 2Q, 2T, 5R Kimura, Kimihiro, 0X, 4H Laureijs, René J., 0O, 0P, 0Q, 0T, 0V, 58 Kimura, N., 0X Laurent, Philippe, 0T Kirchhoff, Rule, 6B Laurin, D., 13 Kirschner, V., 2D Lavigne, J.-F., 13 Kiselev, Alexander, 54 Lawrence, Jon, 1Q Kisner, T., 0X Lazzarini, Paolo, 1B, 6C Kissel, S., 2X Leboulleux, Lucie, 3C, 4A Kitching, T., 0Q Leconte, J., 1X Klebor, Maximilian, 28, 2Z, 30, 31 Le Duigou, J.-M., 3A, 5G Klioner, S. A., 2D Lee, A., 0X Klop, W. A., 37 Lee, Dae-Hee, 4J, 59 Knight, J. Scott, 0C, 0F, 3Y, 40, 42, 49 Lee, Dukhang, 59 Ko, Jongwan, 59 Leese, Mark, 5B Ko, Kyeongyeon, 59 Léger, Alain, 2F, 5G

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Lessio, L., 32, 39 Marafatto, Luca, 28, 2Z, 30, 31, 32, 39 Levacher, Patrick, 28, 2N Maresi, Luca, 6C Levesque, L. E., 13 Margiotta, A., 0T, 2Q, 60 Levi, Joshua, 3Z Marinai, M., 39 Li Causi, G., 5V Marois, C., 13 Li, D., 0X Marston, Anthony, 0B, 44 Liebecq, Sylvie, 3D Martel, André R., 08 Liepmann, Till, 3Z Martellato, Elena, 10 Lightsey, Paul A., 0A, 3Y Martignac, J., 0Q, 58 Ligori, Sebastiano, 0T, 2Q, 2T, 5R, 60 Martin, G., 5G Lilje, Per B., 0T Martin, Laurent, 0T Lillie, Charles F., 1O, 4K Martín-Fleitas, J., 2E Lindegren, L., 2D Martlin, C., 5D Linder, E., 0X Marty, C., 58

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Parot, G., 58 Prigozhin, Gregory, 2C, 2X Pascal, Sandrine, 0R, 2N Prigozhin, I., 2X Pascale, Enzo, 1X, 33, 3R, 5H Primeau, Brian, 2C Paschalis, Antonis, 3D Pucci, Mauro, 1B, 6C Pasian, Fabio, 0O Pueyo, Laurent, 1Y, 3C, 4A, 4T, 5K, 5M Pasqualini, L., 0T, 2Q Puig, L., 1W, 1X Pastor Morales, M. Carmen, 5B Puig-Suari, Jordi, 1Q Pastor, Carmen, 3U Purica, M., 5O, 6E Patauner, Christian, 1B, 6C Pyo, Jeonghyun, 59 Patel, Manish R., 5B Quiller, Trey, 1P Patočka, Karel, 3D Qureshi, Atif, 1N Patrizii, Laura, 0T, 2Q, 2T, 5R, 60 Racca, Giuseppe D., 0O, 0Q, 0T Patterson, Keith D., 18, 3K Radzik, Bartlomiej, 3D Pearson, C., 2K Ragazzoni, Roberto, 28, 2A, 2Z, 30, 31, 32, 39, 51 Pekosh, J., 1I Raichs, Cayetano, 62 Pellegrino, Joseph, 1N Rando, N., 29, 2A Pellegrino, Sergio, 6D Rapp, Robert, 0B Pelo, E., 1E Rataj, Miroslaw, 1X, 33, 36, 3D Penanen, Konstantin I., 08 Ratti, F., 29, 2A Penfornis, Yann, 1L Rauer, Heike, 28, 2Z, 30, 31

Penka, Daniela, 2M Rausch, P., 68 Pereboom, H. P., 4F Rauscher, Bernard J., 0J Peresty, Radek, 3D Rawle, Timothy, 0B, 3O, 44, 45, 46 Perez, Mario R., 4R Ray, Tom, 1X, 33 Pérez-Lizán, David, 5W, 62 Re, Cristina, 10 Pérot, E., 58 Rebeiz, G., 0X Perrin, Marshall D., 0F, 1A, 1Y, 3C, 4A, 5K, 5M Rebolo-López, Rafael, 62 Peter, Gisbert, 28, 2A, 2Y Redding, David, 0J Petkovic, Michael, 1Q Reed, Benjamin B., 1N Petrone, Peter, III, 20 Reinlein, Claudia, 69 Pezzuto, S., 2Y, 36 Reisenfeld, Sam, 1Q Philippon, A., 0Q Renaud, C., 0Z Piazza, Daniele, 1E, 28, 2A, 2Z, 30, 31, 32, 39 Renotte, Etienne, 3D, 4Z, 50, 5O, 6E Piersanti, Osvaldo, 0O Ressler, M. E., 41 Pilbratt, G. L., 1W, 1X Rest, Armin, 4B, 5U Pimentao, J., 58 Rhodes, David, 4C Pinel, Jacques, 0O Ribas, Ignasi, 1X, 33, 36 Piotto, Giampaolo, 28 Riccardi, Armando, 1B, 6C Pisano, G., 0X, 58 Richards, Michael C., 3K Plasson, P., 2Y Richards, P., 0X Plesseria, J. Y., 2A Ricker, George, 2C, 2X Pluzhnik, Eugene, 22, 5N, 66 Rieder, Martin, 28, 2Z, 30, 31 Poberezhskiy, Ilya, 18, 19 Rieke, G. H., 41 Pommerol, A., 1E Rieke, Marcia, 0E, 5U Pompei, C., 39 Rigopoulou, D., 2K Ponthieu, N., 58 Rinehart, S. A., 2L Pontoppidan, K., 0K Rioux, Norman M., 0H, 3L, 4R Pope, A., 0K Ristic, Bojan, 5B Popowicz, Adam, 1R Ristorcelli, I., 58 Porpora, Daniel A., 3Y, 3Z Rizzo, M. J., 2L Portaluri, E., 39 Robberto, Massimo, 0E, 4B, 5U Potin, S., 5G Roberge, Aki, 1U, 2L, 3L, 4R Pottinger, Sabrina, 0O, 0Q Robinson, Tyler D., 1U Powers, T., 2R Robles Muñoz, Nicolás, 5B Prada, Camilo Mejia, 19, 3F Rocchetto, M., 1X Pravdo, S., 2R Rochat, S., 5G Preis, O., 5G Roedel, Andreas, 0D Previte, Anthony, 1Q Rodríguez Gómez, Julio F., 5B Prezelus, Sylvain, 0O Rodriguez, L., 58

Prieto, Eric, 0P, 0T, 2M, 2R, 2U, 5J Roelfsema, Peter, 3U

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Roellig, T., 0K Secroun, Aurélia, 0T, 5J Rohrbach, Scott O., 08 Segawa, Y., 0X Roloff, V., 1E Seidel, Gregor, 0T Rolt, Stephen, 4U, 4V Seiffert, Michael, 0T, 2R Romoli, Marco, 4Z, 50, 5O, 6E Sekiguchi, S., 0X Rosato, Pierluigi, 0O Sekimoto, Yutaro, 0X, 4H Rosset, Cyrille, 0T Sekine, M., 0X Rossin, Christelle, 0R, 0T Seljak, U., 0X Roudil, G., 58 Selsis, F., 1X Rouzé, M., 0Z Sepulveda, J., 1I Rowlands, Neil, 13, 4D Serpell, E., 2D Rozemeijer, Hans, 0O Serra, Benoit, 0T, 5J Rudolph, Andreas, 0O Servaye, Jean-Sébastien, 3D, 4Z, 50, 5O, 6E Rumler, Peter, 0B, 0D Shaklan, Stuart B., 1S, 1U, 1Y Saavedra Criado, Gonzalo, 0O Shao, Mike, 2F, 5G Saccoccio, M., 58 Shaw, Benjamin J. R., 4V Safa, F., 29 Sheikh, David A., 6J Sahlmann, J., 2E Sherwin, B., 0X

Saint-Pe, M., 5G Shi, Fang, 18, 63 Saito, K., 11 Shibai, Hiroshi, 2H, 2I, 3W Saitto, Antonio, 5S Shields, Joel, 18 Sakai, S., 0X Shimizu, T., 0X Sakon, Itsuki, 0K, 2I, 3V Shin, Goo-Hwan, 59 Sakurai, Yuki, 0X, 4H Shinozaki, Keisuke, 0X, 2H, 3W Salabert, D., 0Z Shipley, Ann, 3I Salatino, M., 58 Shirahata, Mai, 4J Salvador, Lucas, 3D Shiri, Ron, 20 Salvignol, Jean-Christophe, 0O, 0P, 0Q, 0T, 0V Short, Alex, 0O, 0P, 0Q, 0V Sanchez, Patrice, 0R, 0T Shu, S., 0X Sánchez-Prieto, Sebastián, 5W Sias, Marco, 0O Sandstrom, K., 0K Siccardi, F., 56 Sankar, Shannon R., 1K, 5A Sicilia, Daniela, 28, 2Z, 30, 31 Sano, Kei, 4J Sidick, Erkin, 18 Sanz Mesa, Rosario, 5B Siegler, Nicholas, 1S Sarajlic, M., 38 Sierra-Roig, C., 36 Sarkar, Subhajit, 1X, 3R Simioni, Emanuele, 10 Sato, N., 0X Simonella, O., 58 Sato, Yoichi, 0X, 2H, 3W Sirbu, Dan, 22, 3G, 3J, 5N, 66 Sauerwein, Timothy, 2C, 2X Sirianni, Marco, 0B, 3O, 44, 45, 46, 6I Sauvage, Jean-François, 3A, 3C Sirignano, Chiara, 0T, 2Q, 2T, 5R, 60 Sauvage, Marc, 0O, 1L Sironi, Giorgia, 1L Savini, Giorgio, 2K, 58 Sirri, Gabriele, 0T, 2Q, 2T, 5R, 60 Savransky, Dmitry, 1T, 1U Sivaramakrishnan, Anand, 1Y, 48 Scaramella, Roberto, 0O Skottfelt, J., 0Q Schade, D., 13 Smadja, Gerard, 5J Schiminovich, David, 0J Smith, Daniel, 3H, 3K Schirra, Florent, 5J Smith, David Alan, 0G Schisano, E., 5V Smith, Erin C., 4R Schistad, Robert, 2V Smith, J. Scott, 09 Schlawin, Everett, 0E Smith, Koby Z., 0C, 42 Schmidt, Micha, 0O Snodgrass, Stephen , 0D Schmitz, N., 51 Solheim, Bjarte G. B., 2V Schmoll, Jürgen, 4V Sordet, M., 38 Schmutz, W., 0Z Sørensen, Anton Norup, 0T, 2U Schneider, A., 1I Sortino, Francesca, 0T, 2T, 60 Schnell, Andrew, 0G Sosey, M., 5D Schweitzer, Hagen, 50 Soummer, Rémi, 0F, 1Y, 3C, 4A, 4T, 5K, 5M

Schweitzer, Mario, 28, 2Z, 30, 31 Southworth, R., 29 Sciortino, A., 0Q Sozzetti, Alessandro, 2F Scott, D., 0K Speckmaier, Max, 0D

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Spergel, David, 0W Tennyson, J., 1X Spiga, Daniele, 28, 2Z, 30, 31 Tenti, M., 0T, 2Q, 2T, 60 Spitler, Lee, 1Q te Plate, Maurice B. J., 0B, 0D Spolyar, Douglas, 2F Texter, Scott, 03 Spurio, M., 0T, 2Q Thayer, Carolyn, 2C, 2X Stadler, E., 5G Thibault, Simon, 13, 47 Stagnaro, Luca, 0O Thizy, Cédric, 0T, 3D, 4Z, 50, 5O, 6E Staguhn, J. G., 2L Thomas, C., 0U Stahl, H. Philip, 0G Thomas, Nicolas, 1E, 2A, 52 Stanco, L., 0T, 2Q, 2T, 60 Thomas, Sandrine J., 22 Stansberry, John, 0E, 0F Thoral, P., 2D St-Antoine, Jonathan, 47 Tielens, X., 2K Stapelfeldt, Karl R., 1A, 1S, 1U, 2L Tilquin, Andre, 5J Stark, Christopher C., 0F, 0H, 1U, 1Y, 3L Tinetti, Giovanna, 1X, 33 Stauffer, John, 5Z Tintori, Matteo, 1B, 6C Steinbuch, M., 4F Toledo-Moreo, Rafael, 0T, 5W, 62 Steller, M., 2A, 2Y Tomaru, T., 0X

Stephen, John, 2Q, 2T, 5R, 60 Tomita, N., 0X St. Laurent, Kathryn E., 1Y Tommasino, Pasquale, 5S Stockman, Yvan, 3D Toon, Geoffrey, 5C Stompor, R., 0X Torre, J.-P., 58 Stoneking, Eric, 3L Torres Redondo, Josefina, 3U Stover, John, 3H Torvanger, Oyvind, 2V Strada, Paolo, 0O, 0P, 0T, 0V, 2R Toulouse-Aastrup, Corinne, 0T Stuhlinger, Martin, 0B Tournois, Severine C., 09 Su, K. Y. L., 0K Traub, Wesley A., 1S, 5C Subedi, Hari, 64 Trauger, John, 5C Sudiwala, Rashmi V., 5H Travaglini, R., 0T, 2Q Suematsu, Y., 11 Trébuchet, P., 4L Sugai, Hajime, 0X, 4H Trifiletti, Alessandro, 5S Sugita, Hiroyuki, 0X, 2H, 3W Trifoglio, Massimo, 0T, 2Q, 2T, 5R, 60 Sukegawa, T., 11 Truong, Tuan, 18 Sullivan, Joseph F., 08 Tsumura, Kohji, 2I, 4J Suntharalingam, Vyshnavi, 2C, 2X Tsunematsu, Shoji, 3W Surace, Jason A., 5Z Tubío-Araujo, Óscar, 62 Suzuki, A., 0X Tucker, C., 2R, 58 Suzuki, J., 0X Turck, K., 2R Suzuki, Toyoaki, 0X, 2I Turck-Chièze, S., 0Z Swindells, I., 0Q Turella, A., 51 Szafraniec, M., 0Q Turin, P., 0X Taccola, Matteo, 50 Turrini, D., 1X Tajima, O., 0X Ulmer, M. P., 1I Takada, S., 0X Uozumi, S., 0X Takakura, S., 0X Utsunomiya, S., 0X Takano, K., 0X Uzawa, Y., 0X Takatori, S., 0X Vaillon, Ludovic, 0O Takei, Y., 0X Valenti, Jeff, 3O Takeuchi, S., 2H Valenziano, Luca, 0T, 2Q, 2T, 5R, 60 Takeyama, Norihide, 4J Valieri, C., 2T Tamura, Motohide, 3E Vallée, Philippe, 47 Tan, B. K., 2K Valsecchi, Giuseppe, 1L Tanabe, D., 0X Van Aken, Dirk, 5H Tanaka, Yosuke, 3E Van Campen, Julie M., 08 Tang, Hong, 18, 1A Vandaele, Ann Carine, 5B Tapie, P., 58 Vandenbussche, Bart, 1X, 33 Tatry, P., 2D Vanderbei, Robert J., 1Y, 3G, 3J

Tauber, J., 58 Vanderspek, Roland, 2C, 2X Tavrov, Alexander, 54 Vannucci, Antonello, 5S Taylor, William, 1X, 33 van Ruymbeke, M., 0Z Telfer, Randal, 09, 0F, 40, 4E Vasisht, Gautam, 5M

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Vives, Sébastien, 0R, 0T, 2N, 2V Yotsumoto, K., 0X Volk, Kevin, 4D Young, Zion, 1H Voyton, Mark F., 04, 07 Zacchei, Andrea, 0O Wachter, Stefanie, 0T Zak, Dean, 08 Waczynski, Augustyn, 0T, 2R Zapatero-Osorio, M. R., 1X Wada, Takehiko, 0X, 2I, 3V, 4J Zarzycka, Alicja, 3D Walczak, Tomasz, 3D Zemcov, Michael, 4J Waldman, Mark, 4E Zhai, C., 5G Waldmann, I. P., 1X Zhelem, Ross, 1Q Walker, David, 5E, 6F Zhou, Hanying, 19, 3F Wallace, James Kent, 18, 63, 6D Zhou, Julia, 08, 4D Wang, F., 2R Zhu, P., 0Z Wang, Shiang-Yu, 4J Zhukov, Andrei, 3D Wang, Xu, 18, 63 Zielinski, Thomas P., 09, 0F, 42 Warfield, Keith R., 0G Ziethe, Ruth, 1E, 52 Warner, Gerry, 4D Zimmerman, Neil T., 0F, 1Y, 5M, 64 Warwick, Steven, 25, 3H, 3I, 3K Zingales, T., 1X Watanabe, H., 0X Zmuidzinas, J., 0K Wawer, P., 36 Zoli, A., 2T, 60 Weber, C., 2R Zoubian, Julien, 5J Webster, Chris, 5C Zuccaro Marchi, Alessandro, 1B, 6C Weidmann, Guenter, 6B Zuluaga-Ramírez, Pablo, 3U Weigel, T., 1E Zusi, M., 51 Wells, Conrad, 40, 49, 4C, 4E Wells, Martyn, 4N Welsh, Andria L., 0F Westbrook, B., 0X Westerhoff, Thomas, 6B Westerman, Solomon, 1Q Whitehorn, N., 0X Whitman, Tony L., 04, 0C, 40, 49, 4E Wiedner, M., 2K Wieser, Matthias, 28, 2Z, 30, 31 Wildi, F. P., 38 Wilkes, Belinda, 1J Williams, J., 2R Willis, Dewey, 3L Wilson, Daniel W., 18 Wimmer, Carolin, 0T Winter, Calvin, 5E Wittrock, Ulrich, 1L, 68 Witvoet, G., 4F Wolkenberg, P., 1X

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Conference Committee

Symposium Chairs Colin Cunningham, UK Astronomy Technology Centre (United Kingdom) Masanori Iye, National Astronomical Observatory of Japan (Japan)

Symposium Co-chairs Allison A. Barto, Ball Aerospace & Technologies Corporation (United States) Suzanne K. Ramsay, European Southern Observatory (Germany)

Conference Chairs Howard A. MacEwen, Reviresco LLC (United States) Giovanni G. Fazio, Harvard-Smithsonian Center for Astrophysics (United States) Makenzie Lystrup, Ball Aerospace & Technologies Corporation (United States)

Conference Program Committee Natalie Batalha, NASA Ames Research Center (United States) Beth A. Biller, The Royal Observatory, Edinburgh (United Kingdom) James B. Breckinridge, Breckinridge Associates (United States) Richard W. Capps, Jet Propulsion Laboratory (United States) Mark Clampin, NASA Goddard Space Flight Center (United States) Mattheus W. M. de Graauw, P.N. Lebedev Physical Institute (Russian Federation) Lee D. Feinberg, NASA Goddard Space Flight Center (United States) Andreas Glindemann, European Southern Observatory (Germany) Qian Gong, NASA Goddard Space Flight Center (United States) James C. Green, University of Colorado at Boulder (United States) Matthew J. Griffin, Cardiff University (United Kingdom) Astrid Heske, European Space Research and Technology Center (Netherlands) Robert A. Laskin, Jet Propulsion Laboratory (United States) David T. Leisawitz, NASA Goddard Space Flight Center (United States) Charles F. Lillie, Lillie Consulting (United States) Jean-Pierre Maillard, Institut d'Astrophysique de Paris (France) Gary W. Matthews, Harris Corporation (United States) Takao Nakagawa, Japan Aerospace Exploration Agency (Japan)

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Jim M. Oschmann Jr., Ball Aerospace & Technologies Corporation (United States) Ronald S. Polidan, Northrop Grumman Aerospace Systems (United States) David C. Redding, Jet Propulsion Laboratory (United States) Aki Roberge, NASA Goddard Space Flight Center (United States) Giorgio Savini, University College London (United Kingdom) Bernard D. Seery, NASA Goddard Space Flight Center (United States) Nicholas Siegler, Jet Propulsion Laboratory (United States) H. Philip Stahl, NASA Marshall Space Flight Center (United States) Giovanna Tinetti, University College London (United Kingdom) Edward C. Tong, Harvard-Smithsonian Center for Astrophysics (United States) Gillian S. Wright, UK Astronomy Technology Centre (United Kingdom) Toru Yamada, Japan Aerospace Exploration Agency (Japan)

Session Chairs 1 JWST I Gillian S. Wright, UK Astronomy Technology Centre (United Kingdom)

2 JWST II Jim M. Oschmann Jr., Ball Aerospace & Technologies Corporation (United States)

3 JWST III James B. Breckinridge, Breckinridge Associates (United States)

4 NASA Large Mission Concepts Matthew J. Griffin, Cardiff University (United Kingdom)

5 NASA Mission Studies: Joint Session with Conferences 9904 and 9905 Mario R. Perez, NASA Headquarters (United States) Howard A. MacEwen, Reviresco LLC (United States)

6 Euclid Beth A. Biller, The Royal Observatory, Edinburgh (United Kingdom)

7 Deep Surveys Mattheus W. M. de Graauw, P.N. Lebedev Physical Institute (Russian Federation)

8 Solar System Studies Mark Clampin, NASA Goddard Space Flight Center (United States)

9 WFIRST I Nicholas Siegler, Jet Propulsion Laboratory (United States)

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11 Technologies H. Philip Stahl, NASA Marshall Space Flight Center (United States)

12 Systems I Howard A. MacEwen, Reviresco LLC (United States)

13 Systems II Lee D. Feinberg, NASA Goddard Space Flight Center (United States)

14 In-Space Servicing Jean-Pierre Maillard, Institut d'Astrophysique de Paris (France)

15 Nanosats and CubeSats Charles F. Lillie, Lillie Consulting (United States)

16 Exoplanets I David B. Gallagher, Jet Propulsion Laboratory (United States)

17 Exoplanets II David C. Redding, Jet Propulsion Laboratory (United States)

18 Exoplanets III Howard A. MacEwen, Reviresco LLC (United States)

19 Exoplanets IV Makenzie Lystrup, Ball Aerospace (United States)

20 Astrometry Makenzie Lystrup, Ball Aerospace (United States)

21 IR Systems Giovanni G. Fazio, Harvard-Smithsonian Center for Astrophysics (United States)

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx Introduction

This conference met throughout the duration of the SPIE Astronomical Telescopes and Instrumentation Conference 2016 in Edinburgh, Scotland, United Kingdom. It was part of a series of annual conferences addressing systems and technologies in the optical, infrared, and millimeter wavelength region that are held alternately in the Eastern and Western hemispheres, the preceding conference having been held in 2014 in Montreal, Quebec, Canada.

Many of the presentations addressed major milestones in the space telescope development that have recently passed or are rapidly approaching. In particular:

• NASA is currently preparing foundational material for the 2020 Astrophysics Decadal Survey that the National Academies of Science will be starting in about two years. One of the major efforts underway in this project is a set of four community mission concept studies to be presented to the Survey team. The objectives, technologies, approach, teaming, and current status and progress of each of the four Science Technology Definition Teams (STDTs) were presented in a joint session with Conference 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray. • The James Webb Space Telescope (JWST) is well along in construction and testing, and is scheduled for launch in October 2018. The current status and development plans for this program were discussed in detail during three oral presentation sessions and in a number of Poster Papers. • The Euclid dark universe mission of the European Space Agency (ESA) passed its Preliminary Design Review in December 2015, and is ramping up into development, construction, and testing phases. The status of this program was summarized during an oral presentation session and a number of Poster Papers. • Finally, major technology development efforts for NASA’s Wide Field InfraRed Space Telescope (WFIRST) are well underway in preparation for an expected program initiation once funding pressures from the JWST program have eased in the 2017–2018 time frame. Several of these projects were presented during the conference, again both orally and in poster formats.

In addition to the presentations related directly to specific, identifiable programs, there were a number of projects and studies of concepts and technologies in earlier stages of development that were addressed during the conference. This included brief discussion of aspects of systems, some currently operational, some

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Downloaded From: http://proceedings.spiedigitallibrary.org/ on 01/30/2017 Terms of Use: http://spiedigitallibrary.org/ss/termsofuse.aspx in various stages of development (including those with technology development well underway), and some still very much in the early concept development stages. A major topic under this heading was the development and testing of coronagraphic technology (both internal and external) for exoplanet detection and characterization (indeed, four oral presentation sessions were devoted to this topic). Other topics addressed under this general heading included infrared technologies and systems (notably for the far infrared); astrometry; deep surveys; new system concepts; advanced telescope technologies; very small satellites; and in-space assembly and servicing for space telescopes.

Howard A. MacEwen Giovanni G. Fazio Makenzie Lystrup

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