MegaMapper is a 6.5m Magellan-like telescope fitted with a wide-field-corrector (WFC) and atmospheric-dispersion-corrector (ADC) that delivers a 3° diameter corrected field-of-view. The telescope’s focal surface is populated by ∼25,000 robotic fiber-positioners feeding a cluster of 36 DESI-like medium resolution spectrographs. We present the facility concept for MegaMapper including: conceptual optical and opto-mechanical designs for the telescope and WFC/ADC that deliver ≲ 0.4” image quality over the full FOV for zenith distances ≤ 50°; the development of a new and modular robotic fiber-positioner focal plane design that can populate the focal surface at high densities (6.2 mm pitch or ∼1 per arcmin2); and concepts for hosting the MegaMapper spectrograph cluster under environmentally controlled conditions inside the telescope enclosure. Building on existing and proven designs and technologies, MegaMapper aims to minimize the project’s technical risk and cost while delivering a competitive next-generation massively multiplexed spectroscopic facility. MegaMapper will lead the study of inflation, dark energy, dark matter, and time-domain astronomy over the next decades by carrying out wide-field cosmological galaxy-redshift surveys, massive spectroscopic surveys of stars in the Milky Way halo and satellites, and by providing a spectroscopic follow-up counterpart to wide field imaging facilities like the Vera C. Rubin Observatory and the Nancy Grace Roman space telescope.
The Dark Energy Spectroscopic Instrument (DESI) is undertaking an ambitious spectroscopic survey of 35 million galaxies and quasars in its 5 year program. With this data, DESI will explore cosmic history through Baryon Acoustic Oscillations and will measure the growth of large scale structure with Redshift Space Distortions. To do this, DESI was constructed with a robotic focal plane system containing 5,020 fiber positioner robots, each equipped with a single fiber, enabling the collection of 5,000 simultaneous spectra. These positioner robots nominally have a 6mm patrol radius and a minimum pitch of 10.4mm such that neighboring robots have overlapping patrol regions. This presentation will give an overview of the focal plane system and its operation. We will begin by introducing its structure and key components. We will also discuss how the focal plane and its robots operate, detailing how the robots are positioned to targets. This will include an introduction to the software model for DESI fiber positioner robots, an overview of the anti-collision algorithm used to prevent collisions between neighboring robots and safety measures employed during operation.
The Dark Energy Spectroscopic Instrument (DESI) on the Mayall 4-m telescope has begun an ambitious survey of spectroscopic measurements of 40 million galaxies and quasars over an area of 14,000 deg2 . DESI is a wide field, multi-object, fiber-fed spectrograph, operating in the wavelength range of 360 - 980 nm. In this paper we present an overview of the DESI instrument focusing on key components including the prime-focus corrector, the focal plane with 5,020 remotely controlled fiber positioners, the procedures to position the fibers on selected targets and the spectrograph system. We then discuss the performance of the instrument during the first year of the DESI survey.
In preparation for the Dark Energy Spectroscopic Instrument (DESI), a new top end was installed on the Mayall 4-meter telescope at Kitt Peak National Observatory. The refurbished telescope and the DESI instrument were successfully commissioned on sky between 2019 October and 2020 March. Here we describe the pointing, tracking and imaging performance of the Mayall telescope equipped with its new DESI prime focus corrector, as measured by six guider cameras sampling the outer edge of DESI’s focal plane. Analyzing ~500,000 guider images acquired during commissioning, we find a median delivered image FWHM of 1.1 arcseconds (in the r-band at 650 nm), with the distribution extending to a best-case value of ~0.6 arcseconds. The point spread function is well characterized by a Moffat profile with a power-law index of β ≈ 3.5 and little dependence of β on FWHM. The shape and size of the PSF delivered by the new corrector at a field angle of 1.57 degrees are very similar to those measured with the old Mayall corrector on axis. We also find that the Mayall achieves excellent pointing accuracy (several arcseconds RMS) and minimal open-loop tracking drift (< 1 milliarcsecond per second), improvements on the telecope’s pre-DESI performance. In the future, employing DESI’s active focus adjustment capabilities will likely further improve the Mayall/DESI delivered image quality.
The recently commissioned Dark Energy Spectroscopic Instrument (DESI) will measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope delivers light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. We describe the use of a Faro Laser Tracker with custom hardware and software tools for alignment during integration of DESI’s focal plane. The focal plane is approximately one meter in diameter and consists primarily of ten radially symmetrical focal plane segments (“petals”) which were individually installed into the telescope. The nominal clearance between petals is 600 microns, and an alignment accuracy of 100 microns and 0.01 degrees was targeted. Alignment of the petals to their targeted locations on the telescope was accomplished by adjusting a purpose-built alignment structure with 14 degrees of freedom using feedback from the laser tracker, which measured the locations of retroreflectors attached to both the petal and the telescope and whose positions relative to key features were precisely known. These measurements were used to infer the locations of aligning features in both structures, which were in turn used to calculate the adjustments necessary to bring the system into alignment. Once alignment was achieved to within acceptable tolerances, each petal was installed while monitoring building movement due to wind and thermal variations.
The Dark Energy Spectroscopic Instrument (DESI) is a Stage IV ground-based dark energy experiment that will measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 square degrees will be measured during the life of the experiment. We describe the installation of the major elements of the instrument at the Mayall 4m telescope, completed in late 2019. The previous prime focus corrector, spider vanes, and upper rings were removed from the Mayall’s Serrurier truss and replaced with the newlyconstructed DESI ring, vanes, cage, hexapod, and optical corrector. The new corrector was optically aligned with the primary mirror using a laser tracker system. The DESI focal plane system was integrated to the corrector, with each of its ten 500-fiber-positioner petal segments installed using custom installation hardware and the laser tracker. Ten DESI spectrographs with 30 cryostats were installed in a newly assembled clean room in the Large Coude Room. The ten cables carrying 5000 optical fibers from the positioners in the focal plane were routed down the telescope through cable wraps at the declination and hour angle axes, and their integral slitheads were integrated with the ten spectrographs. The fiber view camera assembly was installed to the Mayall’s primary mirror cell. Servers for the instrument control system replaced existing computer equipment. The fully integrated instrument has been commissioned and is ready to start its operations phase.
The recently commissioned Dark Energy Spectroscopic Instrument (DESI) will measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14,000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope delivers light to 5,000 fiber optic positioners which in turn feed ten broad-band spectro- graphs. The DESI focal plane subsystem contains the fiber optic positioners and guide and focus cameras, which enable the alignment of fibers with astronomical targets. This paper describes the performance of the installed instrument.
We describe the design of the Commissioning Instrument for the Dark Energy Spectroscopic Instrument (DESI). DESI will obtain spectra over a 3 degree field of view using the 4-meter Mayall Telescope at Kitt Peak, AZ. In order to achieve the required image quality over this field of view, a new optical corrector is being installed at the Mayall Telescope. The Commissioning Instrument is designed to characterize the image quality of the new optical system. The Commissioning Instrument has five commercial cameras; one at the center of the focal surface and four near the periphery of the field and at the cardinal directions. There are also 22 illuminated fiducials, distributed throughout the focal surface, that will be used to test the system that will map between the DESI fiber positioners and celestial coordinates. We describe how the commissioning instrument will perform commissioning tasks for the DESI project and thereby eliminate risks.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. To achieve this goal, it is crucial to guarantee that fiber positioners work properly under the extremes of potential operating conditions, including the full range of temperatures, high speed wind disturbance etc. Thermal testing provides valuable insight into the functionality of the fiber positioners that can be used to help mitigate poor performance at extreme temperatures and wind disturbance test provide guidance to design of ventilation system. Here, we describe the thermal and wind disturbance tests for DESI fiber positioners and how the test results helped improve the robustness of the positioners.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to determine the expansion history of the Universe using the Baryon Acoustic Oscillation technique. Over the life of the experiment DESI will measure the spectra of 35 million galaxies and quasars over 14,000 square degrees out to a redshift of 3.5. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5,000 robotic fiber positioners located at the prime focus. The fibers in turn will feed ten broad-band spectrographs covering the wavelength range from 360nm to 980 nm. Rapid and accurate targeting of the fibers is provided by precision theta-phi robotic fiber positioners. The fiber positioners are manufactured at the University of Michigan. Following assembly each positioner passes through a burn-in and verification sequence. We describe the testing of the positioners and discuss the performance achieved.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. We will describe the production and manufacturing processes developed for the 5000 fiber positioner robots mounted on the focal plane of the Mayall telescope.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 square degrees will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. We present an overview of the instrumentation, the main technical requirements and challenges, and the current status of the project.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the baryon acoustic oscillation technique. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5,000 fiber optic positioners feeding ten broad-band spectrographs. The positioners have eccentric axis kinematics. Actuation is provided by two 4mm diameter DC brushless gear-motors. An attached electronics board accepts a DC voltage for power and CAN messages for communications and drives the two motors. The positioner accepts the ferrulized and polished fiber and provides a mechanically safe path through its internal mechanism. Positioning is rapid and accurate with typical RMS errors of less than 5 μm.
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryon Acoustic Oscillation technique. The spectra of 40 million galaxies over 14,000 sq. deg. will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fiber optic positioners. The fibers in turn feed ten broad-band spectrographs. We describe the ProtoDESI experiment, planned for installation and commissioning at the Mayall telescope in the fall of 2016, which will test the fiber positioning system for DESI. The ProtoDESI focal plate, consisting of 10 fiber positioners, illuminated fiducials, and a guide, focus and alignment (GFA) sensor module, will be installed behind the existing Mosaic prime focus corrector. A Fiber View Camera (FVC) will be mounted to the lower surface of the primary mirror cell and a subset of the Instrument Control System (ICS) will control the ProtoDESI subsystems, communicate with the Telescope Control System (TCS), and collect instrument monitoring data. Short optical fibers from the positioners will be routed to the back of the focal plane where they will be imaged by the Fiber Photometry Camera (FPC) or back-illuminated by a LED system. Target objects will be identified relative to guide stars, and using the GFA in a control loop with the ICS/TCS system, the guide stars will remain stable on pre-identified GFA pixels. The fiber positioners will then be commanded to the target locations and placed on the targets iteratively, using the FVC to centroid on back-illuminated fibers and fiducials to make corrective delta motions. When the positioners are aligned with the targets on-sky, the FPC will measure the intensities from the positioners’ fibers which can then be dithered to look for intensity changes, indicating how well the fibers were initially positioned on target centers. The final goal is to operate ProtoDESI on the Mayall telescope for a 6-hour period during one night, successfully placing targets on the intended fibers for the duration of a typical DESI science exposure.
H. T. Diehl, E. Neilsen, R. Gruendl, B. Yanny, T. M. Abbott, J. Aleksić, S. Allam, J. Annis, E. Balbinot, M. Baumer, L. Beaufore, K. Bechtol, G. Bernstein, S. Birrer, C. Bonnett, D. Brout, C. Bruderer, E. Buckley-Geer, D. Capozzi, A. Carnero Rosell, F. Castander, R. Cawthon, C. Chang, L. Clerkin, R. Covarrubias, C. Cuhna, C. D'Andrea, L. da Costa, R. Das, C. Davis, J. Dietrich, A. Drlica-Wagner, A. Elliott, T. Eifler, J. Etherington, B. Flaugher, J. Frieman, A. Fausti Neto, M. Fernández, C. Furlanetto, D. Gangkofner, D. Gerdes, D. Goldstein, K. Grabowski, R. Gupta, S. Hamilton, H. Head, J. Helsby, D. Hollowood, K. Honscheid, D. James, M. Johnson, S. Jouvel, T. Kacprzac, S. Kent, R. Kessler, A. Kim, E. Krause, C. Krawiec, A. Kremin, R. Kron, S. Kuhlmann, N. Kuropatkin, O. Lahav, J. Lasker, T. Li, E. Luque, N. Maccrann, M. March, J. Marshall, N. Mondrik, E. Morganson, D. Mudd, A. Nadolski, P. Nugent, P. Melchior, F. Menanteau, D. Nagasawa, B. Nord, R. Ogando, L. Old, A. Palmese, D. Petravick, A. Plazas, A. Pujol, A. Queiroz, K. Reil, A. Romer, R. Rosenfeld, A. Roodman, P. Rooney, M. Sako, A. Salvador, C. Sánchez, E. Sánchez Álvaro, B. Santiago, A. Schooneveld, M. Schubnell, E. Sheldon, A. Smith, R. Smith, M. Soares-Santos, F. Sobreira, M. Soumagnac, H. Spinka, S. Tie, D. Tucker, V. Vikram, K. Vivas, A. Walker, W. Wester, M. Wiesner, H. Wilcox, P. Williams, A. Zenteno, Y. Zhang, Z. Zhang
The Dark Energy Survey (DES) is an operating optical survey aimed at understanding the accelerating expansion of the universe using four complementary methods: weak gravitational lensing, galaxy cluster counts, baryon acoustic oscillations, and Type Ia supernovae. To perform the 5000 sq-degree wide field and 30 sq-degree supernova surveys, the DES Collaboration built the Dark Energy Camera (DECam), a 3 square-degree, 570-Megapixel CCD camera that was installed at the prime focus of the Blanco 4-meter telescope at the Cerro Tololo Inter-American Observatory (CTIO). DES has completed its third observing season out of a nominal five. This paper describes DES “Year 1” (Y1) to “Year 3” (Y3), the strategy, an outline of the survey operations procedures, the efficiency of operations and the causes of lost observing time. It provides details about the quality of the first three season's data, and describes how we are adjusting the survey strategy in the face of the El Niño Southern Oscillation.
The Dark Energy Survey Collaboration has completed construction of the Dark Energy Camera (DECam), a 3 square
degree, 570 Megapixel CCD camera which will be mounted on the Blanco 4-meter telescope at CTIO. DECam will be
used to perform the 5000 sq. deg. Dark Energy Survey with 30% of the telescope time over a 5 year period. During the
remainder of the time, and after the survey, DECam will be available as a community instrument. All components of
DECam have been shipped to Chile and post-shipping checkout finished in Jan. 2012. Installation is in progress. A
summary of lessons learned and an update of the performance of DECam and the status of the DECam installation and
commissioning will be presented.
The Dark Energy Survey is a Stage III Dark Energy Experiment that will obtain cosmological parameters by combining
four observational techniques; Galaxy Clusters, Weak Lensing, Type Ia Supernovae and Baryon Acoustic Oscillations.
The observations will be performed with a new wide field camera (DECam) that will be placed on the Blanco 4 m
telescope at CTIO. Here we describe the large format (600 mm clear aperture) Filter Changer Mechanism (FCM) for the
Dark Energy Survey Camera (DECam). The FCM, based on the Pan-STARRS design, is the largest ever constructed.
Fabrication of the filter changer has been completed and it has been tested under realistic conditions.
Many future space telescope missions are designed as wide-field surveys. The increased area of the survey is often
achieved by increasing the plate scale of the detectors. This can result in under-sampled instruments. Under these
conditions response variations within an individual pixel degrade photometric and shape information of observed
astronomical sources. These effects can be corrected for by mapping the sub-pixel response of all pixels on a detector.
Measuring sub-pixel sensitivity by projecting a single, micron-size spot is effective in understanding intrapixel response
variations, but the time required to create a detector-wide map is prohibitive. The existing Spot-O-Matic single spot
projector concept, has been extended to the design of a multi-spot projector, the Spots-O-Matic, enabling the mapping of
an entire detector. This new projector is under development to achieve the small spot size required for pixel
characterization over the field of view of an entire detector.
Flux dependent non-linearity (reciprocity failure) in HgCdTe NIR detectors with 1.7 μm cut-off was investigated.
A dedicated test station was designed and built to measure reciprocity failure over the full dynamic range of near
infrared detectors. For flux levels between 1 and 100,000 photons/sec a limiting sensitivity to reciprocity failure
of 0.3 %/decade was achieved. First measurements on several engineering grade 1.7 μm cut-off HgCdTe detectors
show a wide range of reciprocity failure, from less than 0.5 %/decade to about 10%/decade. For at least two
of the tested detectors, significant spatial variation in the effect was observed. No indication for wavelength
dependency was found. The origin of reciprocity failure is currently not well understood. In this paper we
present details of our experimental set-up and show the results of measurements for several detectors.
The Dark Energy Survey Collaboration is building the Dark Energy Camera (DECam), a 3 square degree, 520
Megapixel CCD camera which will be mounted on the Blanco 4-meter telescope at CTIO. DECam will be used to
perform the 5000 sq. deg. Dark Energy Survey with 30% of the telescope time over a 5 year period. During the
remainder of the time, and after the survey, DECam will be available as a community instrument. Construction of
DECam is well underway. Integration and testing of the major system components has already begun at Fermilab and
the collaborating institutions.
High detector quantum efficiency (QE) can greatly improve speed and performance of wide field instruments
that strive for fast precision photometry. SNAP, a proposed satellite mission dedicated to exploring the nature
of the dark energy will employ a very large focal plane instrumented with about equal number of CCD and
NIR sensors totaling more than 600 million pixels covering roughly 0.7 square degrees on the sky. To precisely
characterize the NIR detector QE, the SNAP project has put in place a test set-up capable of measuring absolute
QE at the 5% level with the goal of ultimately reaching a precision better than 2%. Illumination of the NIR
detectors is provided by either a quartz tungsten halogen lamp combined with a set of narrow band filters or
a manually tunable monochromator. The two light sources feed an integrating sphere at a distance of roughly
60 cm from the detector to be tested and a calibrated InGaAs photodiode, mounted adjacent to the NIR
detector provides absolute photon flux measurements. This paper describes instrumentation, performance and
measurement procedures and summarizes results of detailed characterization of the QE on several SNAP devices
as a function of wavelength.
Over the past decade scientists have collected convincing evidence that the content of our universe is dominated
by a mysterious dark energy. Understanding the nature of dark energy is a very difficult task, and requires a
variety of independent experimental approaches. Most of these approaches rely on photometric calibrations over
a wide range of intensities using standardized stars and internal reference sources, and hence on a complete
understanding of the linearity of the detectors. The SNAP near infrared (NIR) instrument team has performed
a comprehensive study of precision photometry on 1.7 micron cut-off HgCdTe detectors. Among those studies
are the count rate dependent detector non-linearity that was recently discovered with the NICMOS array on
the Hubble Space Telescope, and possible pixel size variations seen in quantum efficiency (QE) data. The nonlinearity
on NICMOS exhibits an unexpected behavior, where pixels with high (low) count rates detect slightly
more (less) flux than expected for a linear system. To test this count rate dependent non-linearity a dedicated
setup was built that produces a known amount of light on a detector, and measures its response as a function of
light intensity and wavelength. If the pixel response variations seen in QE data are due to pixel area variations,
standard flat-fielding will degrade photometry precision for point sources in an undersampled telescope. Studies
have been performed to estimate the magnitude of pixel area variations.
We describe the Dark Energy Camera (DECam), which will be the primary instrument used in the Dark Energy Survey.
DECam will be a 3 sq. deg. mosaic camera mounted at the prime focus of the Blanco 4m telescope at the Cerro-Tololo
International Observatory (CTIO). DECam includes a large mosaic CCD focal plane, a five element optical corrector,
five filters (g,r,i,z,Y), and the associated infrastructure for operation in the prime focus cage. The focal plane consists of
62 2K x 4K CCD modules (0.27"/pixel) arranged in a hexagon inscribed within the roughly 2.2 degree diameter field of
view. The CCDs will be 250 micron thick fully-depleted CCDs that have been developed at the Lawrence Berkeley
National Laboratory (LBNL). Production of the CCDs and fabrication of the optics, mechanical structure, mechanisms,
and control system for DECam are underway; delivery of the instrument to CTIO is scheduled for 2010.
We compare a more complete characterization of the low temperature performance of a nominal 1.7um cut-off
wavelength 1kx1k InGaAs (lattice-matched to an InP substrate) photodiode array against similar, 2kx2k HgCdTe
imagers to assess the suitability of InGaAs FPA technology for scientific imaging applications. The data we present
indicate that the low temperature performance of existing InGaAs detector technology is well behaved and comparable
to those obtained for state-of-the-art HgCdTe imagers for many space astronomical applications. We also discuss key
differences observed between imagers in the two material systems.
Precision near infrared (NIR) measurements are essential for the next generation of ground and space based instruments. The SuperNova Acceleration Probe (SNAP) will measure thousands of type Ia supernovae up to a redshift of 1.7. The highest redshift supernovae provide the most leverage for determining cosmological parameters, in particular the dark energy equation of state and its possible time evolution. Accurate NIR observations are needed to utilize the full potential of the highest redshift supernovae. Technological improvements in NIR detector fabrication have lead to high quantum efficiency, low noise detectors using a HgCdTe diode with a band-gap that is tuned to cutoff at 1.7 μm. The effects of detector quantum efficiency, read noise, and dark current on lightcurve signal to noise, lightcurve parameter errors, and distance modulus fits are simulated in the SNAPsim framework. Results show that improving quantum efficiency leads to the largest gains in photometric accuracy for type Ia supernovae. High quantum efficiency in the NIR reduces statistical errors and helps control systematic uncertainties at the levels necessary to achieve the primary SNAP science goals.
We present the results of a study of the performance of InGaAs detectors conducted for the SuperNova Acceleration
Probe (SNAP) dark energy mission concept. Low temperature data from a nominal 1.7um cut-off wavelength 1kx1k
InGaAs photodiode array, hybridized to a Rockwell H1RG multiplexer suggest that InGaAs detector performance is
comparable to those of existing 1.7um cut-off HgCdTe arrays. Advances in 1.7um HgCdTe dark current and noise
initiated by the SNAP detector research and development program makes it the baseline detector technology for SNAP.
However, the results presented herein suggest that existing InGaAs technology is a suitable alternative for other future
astronomy applications.
We present the results of a detailed study of the noise performance of candidate NIR detectors for the proposed Super-Nova Acceleration Probe. Effects of Fowler sampling depth and frequency, temperature, exposure time, detector material, detector reverse-bias and multiplexer type are quantified. We discuss several tools for determining which sources of low frequency noise are primarily responsible for the sub-optimal noise improvement when multiple sampling, and the selection of optimum fowler sampling depth. The effectiveness of reference pixel subtraction to mitigate zero point drifts is demonstrated, and the circumstances under which reference pixel subtraction should or should not be applied are examined. Spatial and temporal noise measurements are compared, and a simple method for quantifying the effect of hot pixels and RTS noise on spatial noise is described.
Large format (1k × 1k and 2k × 2k) near infrared detectors manufactured by Rockwell Scientific Center and Raytheon Vision Systems are characterized as part of the near infrared R&D effort for SNAP (the Super-Nova/Acceleration Probe). These are hybridized HgCdTe focal plane arrays with a sharp high wavelength cut-off at 1.7 μm. This cut-off provides a sufficiently deep reach in redshift while it allows at the same time low dark current operation of the passively cooled detectors at 140 K. Here the baseline SNAP near infrared system is briefly described and the science driven requirements for the near infrared detectors are summarized. A few results obtained during the testing of engineering grade near infrared devices procured for the SNAP project are highlighted. In particular some recent measurements that target correlated noise between adjacent detector pixels due to capacitive coupling and the response uniformity within individual detector pixels are discussed.
Anne Ealet, Eric Prieto, Alain Bonissent, Roger Malina, Gérard Smadja, A. Tilquin, Gary Bernstein, Stephane Basa, D. Fouchez, Olivier Le Fevre, Alain Mazure, Greg Aldering, R. Amanullah, Pierre Astier, E. Barrelet, Christopher Bebek, Lars Bergstrom, Manfred Bester, Roger Blandford, Ralph Bohlin, Charles Bower, Mark Brown, Myron Campbell, William Carithers, Eugene Commins, W. Craig, C. Day, F. DeJongh, Susana Deustua, H. Diehl, S. Dodelson, Richard Ellis, M. Emmet, Josh Frieman, Andrew Fruchter, D. Gerdes, L. Gladney, Gerson Goldhaber, Ariel Goobar, Donald Groom, Henry Heetderks, M. Hoff, Stephen Holland, M. Huffer, L. Hui, Dragan Huterer, B. Jain, Patrick Jelinsky, Armin Karcher, Steven Kent, Steven Kahn, Alex Kim, William Kolbe, B. Krieger, G. Kushner, N. Kuznetsova, Robin Lafever, J. Lamoureux, Michael Lampton, Michael Levi, P. Limon, Huan Lin, Eric Linder, Stewart Loken, W. Lorenzon, J. Marriner, P. Marshall, R. Massey, Timothy McKay, Shawn McKee, Ramon Miquel, Nicholas Morgan, E. Mörtsell, Nick Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nick Palaio, David Pankow, John Peoples, Saul Perlmutter, David Rabinowitz, Alexandre Refregier, Jason Rhodes, Natalie Roe, D. Rusin, V. Scarpine, Michael Schubnell, Michael Sholl, Roger Smith, George Smoot, Jeffrey Snyder, Anthony Spadafora, A. Stebbins, Christopher Stoughton, Andrew Szymkowiak, Gregory Tarlé, Keith Taylor, Andrew Tomasch, Douglas Tucker, Henrik von der Lippe, D. Vincent, Jean-Pierre Walder, Guobin Wang, W. Wester
A well-adapted spectrograph concept has been developed for the SNAP (SuperNova/Acceleration Probe) experiment. The goal is to ensure proper identification of Type Iz supernovae and to standardize the magnitude of each candidate by determining explosion parameters. The spectrograph is also a key element for the calibration of the science mission. An instrument based on an integral field method with the powerful concept of imager slicing has been designed and is presented in this paper. The spectrograph concept is optimized to have high efficiency and low spectral resolution (R~100), constant through the wavelength range (0.35-1.7μm), adapted to the scientific goals of the mission.
Michael Sholl, Michael Lampton, Greg Aldering, W. Althouse, R. Amanullah, James Annis, Pierre Astier, Charles Baltay, E. Barrelet, Stephane Basa, Christopher Bebek, Lars Bergstrom, Gary Bernstein, Manfred Bester, Bruce Bigelow, Roger Blandford, Ralph Bohlin, Alain Bonissent, Charles Bower, Mark Brown, Myron Campbell, William Carithers, Eugene Commins, W. Craig, C. Day, F. DeJongh, Susana Deustua, T. Diehl, S. Dodelson, Anne Ealet, Richard Ellis, W. Emmet, D. Fouchez, Josh Frieman, Andrew Fruchter, D. Gerdes, L. Gladney, Gerson Goldhaber, Ariel Goobar, Donald Groom, Henry Heetderks, M. Hoff, Stephen Holland, M. Huffer, L. Hui, Dragan Huterer, B. Jain, Patrick Jelinsky, Armin Karcher, Steven Kahn, Steven Kent, Alex Kim, William Kolbe, B. Krieger, G. Kushner, N. Kuznetsova, Robin Lafever, J. Lamoureux, Olivier Le Fevre, Michael Levi, P. Limon, Huan Lin, Eric Linder, Stewart Loken, W. Lorenzon, Roger Malina, J. Marriner, P. Marshall, R. Massey, Alain Mazure, Timothy McKay, Shawn McKee, Ramon Miquel, Nicholas Morgan, E. Mörtsell, Nick Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nick Palaio, David Pankow, John Peoples, Saul Perlmutter, Eric Prieto, David Rabinowitz, Alexandre Refregier, Jason Rhodes, Natalie Roe, D. Rusin, V. Scarpine, Michael Schubnell, Gérard Smadja, Roger Smith, George Smoot, Jeffrey Snyder, Anthony Spadafora, A. Stebbins, Christopher Stoughton, Andrew Szymkowiak, Gregory Tarlé, Keith Taylor, A. Tilquin, Andrew Tomasch, Douglas Tucker, D. Vincent, Henrik von der Lippe, Jean-Pierre Walder, Guobin Wang, W. Wester
Mission requirements, the baseline design, and optical systems budgets for the SuperNova/Acceleration Probe (SNAP) telescope are presented. SNAP is a proposed space-based experiment designed to study dark energy and alternate explanations of the acceleration of the universe’s expansion by performing a series of complementary systematics-controlled astrophysical measurements. The goals of the mission are a Type Ia supernova Hubble diagram and a wide-field weak gravitational lensing survey. A 2m widefield three-mirror telescope feeds a focal plane consisting of 36 CCDs and 36 HgCdTe detectors and a high-efficiency, low resolution integral field spectrograph. Details of the maturing optical system, with emphasis on structural stability during terrestrial testing as well as expected environments during operations at L2 are discussed. The overall stray light mitigation system, including illuminated surfaces and visible objects are also presented.
Michael Lampton, Michael Sholl, Michael Krim, R. Besuner, Carl Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, Charles Baltay, E. Barrelet, Stephane Basa, Christopher Bebek, John Bercovitz, Lars Bergstrom, Gary Berstein, Manfred Bester, Ralph Bohlin, Alain Bonissent, Charles Bower, Myron Campbell, William Carithers, Eugene Commins, C. Day, Susana Deustua, Richard DiGennaro, Anne Ealet, Richard Ellis, William Emmett, Mikael Eriksson, D. Fouchez, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Henry Heetderks, Stephen Holland, Dragan Huterer, William Johnston, Richard Kadel, Armin Karcher, Alex Kim, William Kolbe, Robin Lafever, J. Lamoureux, Oliver LeFevre, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, Roger Malina, Alain Mazure, Timothy McKay, Shawn McKee, Ramon Miquel, Nicholas Morgan, E. Mortsell, Nick Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nick Palaio, David Pankow, Saul Perlmutter, Eric Prieto, David Rabinowitz, Alexandre Refregier, Jason Rhodes, Natalie Roe, Michael Schubnell, G. Smadja, R. Smith, George Smoot, Jeffrey Snyder, Anthony Spadafora, Andrew Szymkowiak, Gregory Tarle, Keith Taylor, A. Tilquin, Andrew Tomasch, D. Vincent, Henrik von der Lippe, Jean-Pierre Walder, Guobin Wang
We present the baseline telescope design for the telescope for the SuperNova/Acceleration Probe (SNAP) space mission. SNAP’s purpose is to determine expansion history of the Universe by measuring the redshifts, magnitudes, and spectral classifications of thousands of supernovae with unprecedented accuracy. Discovering and measuring these supernovae demand both a wide optical field and a high sensitivity throughout the visible and near IR wavebands. We have adopted the annular-field three-mirror anastigmat (TMA) telescope configuration, whose classical aberrations (including chromatic) are zero. We show a preliminary optmechanical design that includes important features for stray light control and on-orbit adjustment and alignment of the optics. We briefly discuss stray light and tolerance issues, and present a preliminary wavefront error budget for the SNAP Telescope. We conclude by describing some of the design tasks being carried out during the current SNAP research and development phase.
Christopher Bebek, Carl Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, Charles Baltay, E. Barrelet, Stephane Basa, John Bercovitz, Lars Bergstrom, Gary Berstein, Manfred Bester, Ralph Bohlin, Alain Bonissent, Charles Bower, Myron Campbell, William Carithers, Eugene Commins, C. Day, Susana Deustua, Richard DiGennaro, Anne Ealet, Richard Ellis, William Emmett, Mikael Eriksson, D. Fouchez, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Henry Heetderks, Stephen Holland, Dragan Huterer, William Johnston, Richard Kadel, Armin Karcher, Alex Kim, William Kolbe, Robin Lafever, J. Lamoureux, Michael Lampton, Oliver LeFevre, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, Roger Malina, Alain Mazure, Timothy McKay, Shawn McKee, Ramon Miquel, Nicholas Morgan, E. Mortsell, N. Mostek, Stuart Mufson, J. Musser, Natalie Roe, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nicholas Palaio, David Pankow, Saul Perlmutter, Eric Prieto, David Rabinowitz, Alexandre Refregier, Jason Rhodes, Michael Schubnell, Michael Sholl, G. Smadja, R. Smith, George Smoot, Jeffrey Snyder, Anthony Spadafora, Andrew Szymkowiak, Gregory Tarle, Keith Taylor, A. Tilquin, Andrew Tomasch, D. Vincent, Henrik von der Lippe, Jean-Pierre Walder, Guobin Wang
The proposed SuperNova/Acceleration Probe (SNAP) mission will have a two-meter class telescope delivering diffraction-limited images to an instrumented 0.7 square degree field in the visible and near-infrared wavelength regime. The requirements for the instrument suite and the present configuration of the focal plane concept are presented. A two year R&D phase, largely supported by the Department of Energy, is just beginning. We describe the development activities that are taking place to advance our preparedness for mission proposal in the areas of detectors and electronics.
Gregory Tarle, Carl Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, E. Barrelet, Christopher Bebek, Lars Bergstrom, John Bercovitz, Gary Bernstein, Manfred Bester, Alain Bonissent, C. Bower, Mark Brown, William Carithers, Eugene Commins, C. Day, Susana Deustua, Richard DiGennaro, Anne Ealet, Richard Ellis, Mikael Eriksson, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Stewart Harris, Peter Harvey, Henry Heetderks, Steven Holland, Dragan Huterer, Armin Karcher, Alex Kim, William Kolbe, B. Krieger, R. Lafever, J. Lamoureux, Michael Lampton, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, Roger Malina, R. Massey, Ramon Miquel, Timothy McKay, Shawn McKee, E. Moertsell, N. Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nicholas Palaio, David Pankow, Saul Perlmutter, R. Pratt, Eric Prieto, Alexandre Refregier, Jason Rhodes, Kem Robinson, N. Roe, Michael Schubnell, Michael Sholl, G. Smadja, George Smoot, Anthony Spadafora, Andrew Tomasch, D. Vincent, H. von der Lippe, J.-P. Walder, Guobin Wang
The SuperNova/Acceleration Probe (SNAP) will measure precisely the cosmological expansion history over both the acceleration and deceleration epochs and thereby constrain the nature of the dark energy that dominates our universe today. The SNAP focal plane contains equal areas of optical CCDs and NIR sensors and an integral field spectrograph. Having over 150 million pixels and a field-of-view of 0.34 square degrees, the SNAP NIR system will be the largest yet constructed. With sensitivity in the range 0.9-1.7 μm, it will detect Type Ia supernovae between z = 1 and 1.7 and will provide follow-up precision photometry for all supernovae. HgCdTe technology, with a cut-off tuned to 1.7 μm, will permit passive cooling at 140 K while maintaining noise below zodiacal levels. By dithering to remove the effects of intrapixel variations and by careful attention to other instrumental effects, we expect to control relative photometric accuracy below a few hundredths of a magnitude. Because SNAP continuously revisits the same fields we will be able to achieve outstanding statistical precision on the photometry of reference stars in these fields, allowing precise monitoring of our detectors. The capabilities of the NIR system for broadening the science reach of SNAP are discussed.
Anne Ealet, Eric Prieto, Alain Bonissent, Roger Malina, G. Bernstein, Stephane Basa, Oliver LeFevre, Alain Mazure, Christophe Bonneville, Carl Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, E. Barrelet, Christopher Bebek, Lars Bergstrom, John Bercovitz, Manfred Bester, C. Bower, William Carithers, Eugene Commins, C. Day, Susana Deustua, Richard DiGennaro, R. Ellis, Mikael Eriksson, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Stewart Harris, Peter Harvey, Henry Heetderks, Steven Holland, Dragan Huterer, Armin Karcher, Alex Kim, William Kolbe, B. Krieger, R. Lafever, J. Lamoureux, Michael Lampton, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, R. Massey, Timothy McKay, Shawn McKee, Ramon Miquel, E. Moertsell, N. Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nicholas Palaio, David Pankow, Saul Perlmutter, R. Pratt, Alexandre Refregier, J. Rhodes, Kem Robinson, N. Roe, Michael Sholl, Michael Schubnell, G. Smadja, George Smoot, Anthony Spadafora, Gregory Tarle, Andrew Tomasch, H. von der Lippe, D. Vincent, J.-P. Walder, Guobin Wang
A well-adapted spectrograph concept has been developed for the SNAP (SuperNova/Acceleration Probe) experiment. The goal is to ensure proper identification of Type Ia supernovae and to standardize the magnitude of each candidate by determining explosion parameters. An instrument based on an integral field method with the powerful concept of imager slicing has been designed and is presented in this paper. The spectrograph concept is optimized to have very high efficiency and low spectral resolution (R~100), constant through the wavelength range (0.35-1.7μm), adapted to the scientific goals of the mission.
Michael Lampton, Christopher Bebek, Carl Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, E. Barrelet, Lars Bergstrom, John Bercovitz, Gary Bernstein, Manfred Bester, Alain Bonissent, C. Bower, William Carithers, Eugene Commins, C. Day, Susana Deustua, Richard DiGennaro, Anne Ealet, Richard Ellis, Mikael Eriksson, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Stewart Harris, Peter Harvey, Henry Heetderks, Steven Holland, Dragan Huterer, Armin Karcher, Alex Kim, William Kolbe, B. Krieger, R. Lafever, J. Lamoureux, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, Roger Malina, R. Massey, Timothy McKay, Steven McKee, Ramon Miquel, E. Moertsell, N. Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nicholas Palaio, David Pankow, Saul Perlmutter, R. Pratt, Eric Prieto, Alexandre Refregier, J. Rhodes, Kem Robinson, N. Roe, Michael Sholl, Michael Schubnell, G. Smadja, George Smoot, Anthony Spadafora, Gregory Tarle, Andrew Tomasch, H. von der Lippe, D. Vincent, J.-P. Walder, Guobin Wang
The proposed SuperNova/Acceleration Probe (SNAP) mission will have a two-meter class telescope delivering diffraction-limited images to an instrumented 0.7 square-degree field sensitive in the visible and near-infrared wavelength regime. We describe the requirements for the instrument suite and the evolution of the focal plane design to the present concept in which all the instrumentation -- visible and near-infrared imagers, spectrograph, and star guiders -- share one common focal plane.
Alex Kim, Carl Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, E. Barrelet, Christopher Bebek, Lars Bergstrom, J. Bercovitz, Gary Bernstein, M. Bester, A. Bonissent, C. Bower, William Carithers, Eugene Commins, C. Day, Susana Deustua, R. DiGennaro, A. Ealet, Richard Ellis, M. Eriksson, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Stewart Harris, Peter Harvey, Henry Heetderks, Steven Holland, Dragan Huterer, Armin Karcher, William Kolbe, B. Krieger, Robin Lafever, J. Lamoureux, Michael Lampton, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, Roger Malina, R. Massey, Timothy McKay, Shawn McKee, Ramon Miquel, E. Mortsell, N. Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nicholas Palaio, David Pankow, Saul Perlmutter, R. Pratt, Eric Prieto, Alexandre Refregier, Jason Rhodes, Kem Robinson, N. Roe, Michael Sholl, Michael Schubnell, G. Smadja, George Smoot, Anthony Spadafora, Gregory Tarle, Andrew Tomasch, H. von der Lippe, D. Vincent, J.-P. Walder, Guobin Wang
The Supernova / Acceleration Probe (SNAP) is a proposed space-borne observatory that will survey the sky with a wide-field optical/near-infrared (NIR) imager. The images produced by SNAP will have an unprecedented combination of depth, solid-angle, angular resolution, and temporal sampling. For 16 months each, two 7.5 square-degree fields will be observed every four days to a magnitude depth of AB=27.7 in each of the SNAP filters, spanning 3500-17000Å. Co-adding images over all epochs will give AB=30.3 per filter. In addition, a 300 square-degree field will be surveyed to AB=28 per filter, with no repeated temporal sampling. Although the survey strategy is tailored for supernova and weak gravitational lensing observations, the resulting data will support a broad range of auxiliary science programs.
Michael Lampton, Carl Akerlof, Greg Aldering, R. Amanullah, Pierre Astier, E. Barrelet, Christopher Bebek, Lars Bergstrom, John Bercovitz, G. Bernstein, Manfred Bester, Alain Bonissent, C. Bower, William Carithers, Eugene Commins, C. Day, Susana Deustua, Richard DiGennaro, Anne Ealet, Richard Ellis, Mikael Eriksson, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Stewart Harris, Peter Harvey, Henry Heetderks, Steven Holland, Dragan Huterer, Armin Karcher, Alex Kim, William Kolbe, B. Krieger, R. Lafever, J. Lamoureux, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, Roger Malina, R. Massey, Timothy McKay, Shawn McKee, Ramon Miquel, E. Mortsell, N. Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nicholas Palaio, David Pankow, Saul Perlmutter, R. Pratt, Eric Prieto, Alexandre Refregier, J. Rhodes, Kem Robinson, N. Roe, Michael Sholl, Michael Schubnell, G. Smadja, George Smoot, A. Spadafora, Gregory Tarle, Andrew Tomasch, H. von der Lippe, R. Vincent, J.-P. Walder, Guobin Wang
The SuperNova/Acceleration Probe (SNAP) mission will require a two-meter class telescope delivering diffraction limited images spanning a one degree field in the visible and near infrared wavelength regime. This requirement, equivalent to nearly one billion pixel resolution, places stringent demands on its optical system in terms of field flatness, image quality, and freedom from chromatic aberration. We discuss the advantages of annular-field three-mirror anastigmat (TMA) telescopes for applications such as SNAP, and describe the features of the specific optical configuration that we have baselined for the SNAP mission. We discuss the mechanical design and choice of materials for the telescope. Then we present detailed ray traces and diffraction calculations for our baseline optical design. We briefly discuss stray light and tolerance issues, and present a preliminary wavefront error budget for the SNAP Telescope. We conclude by describing some of tasks to be carried out during the upcoming SNAP research and development phase.
Greg Aldering, Carl Akerlof, R. Amanullah, Pierre Astier, E. Barrelet, Christopher Bebek, Lars Bergstrom, John Bercovitz, Gary Bernstein, Manfred Bester, Alain Bonissent, Charles Bower, William Carithers, Eugene Commins, C. Day, Susana Deustua, Richard DiGennaro, Anne Ealet, Richard Ellis, Mikael Eriksson, Andrew Fruchter, Jean-Francois Genat, Gerson Goldhaber, Ariel Goobar, Donald Groom, Stewart Harris, Peter Harvey, Henry Heetderks, Steven Holland, Dragan Huterer, Armin Karcher, Alex Kim, William Kolbe, B. Krieger, R. Lafever, James Lamoreux, Michael Lampton, Michael Levi, Daniel Levin, Eric Linder, Stewart Loken, Roger Malina, R. Massey, Timothy McKay, Shawn McKee, Ramon Miquel, E. Moertsell, N. Mostek, Stuart Mufson, J. Musser, Peter Nugent, Hakeem Oluseyi, Reynald Pain, Nicholas Palaio, David Pankow, Saul Perlmutter, R. Pratt, Eric Prieto, Alexandre Refregier, J. Rhodes, Kem Robinson, N. Roe, Michael Sholl, Michael Schubnell, G. Smadja, George Smoot, Anthony Spadafora, Gregory Tarle, Andrew Tomasch, H. von der Lippe, D. Vincent, J.-P. Walder, Guobin Wang
The SuperNova / Acceleration Probe (SNAP) is a space-based experiment to measure the expansion history of the Universe and study both its dark energy and the dark matter. The experiment is motivated by the startling discovery that the expansion of the Universe is accelerating. A 0.7~square-degree imager comprised of 36 large format fully-depleted n-type CCD's sharing a focal plane with 36 HgCdTe detectors forms the heart of SNAP, allowing discovery and lightcurve measurements simultaneously for many supernovae. The imager and a high-efficiency low-resolution integral field spectrograph are coupled to a 2-m three mirror anastigmat wide-field telescope, which will be placed in a high-earth orbit. The SNAP mission can obtain high-signal-to-noise calibrated light-curves and spectra for over 2000 Type Ia supernovae at redshifts between z = 0.1 and 1.7. The resulting data set can not only determine the amount of dark energy with high precision, but test the nature of the dark energy by examining its equation of state. In particular, dark energy due to a cosmological constant can be differentiated from alternatives such as "quintessence", by measuring the dark energy's equation of state to an accuracy of ± 0.05, and by studying its time dependence.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.