39 research outputs found
The Simons Observatory: Beam characterization for the Small Aperture Telescopes
We use time-domain simulations of Jupiter observations to test and develop a
beam reconstruction pipeline for the Simons Observatory Small Aperture
Telescopes. The method relies on a map maker that estimates and subtracts
correlated atmospheric noise and a beam fitting code designed to compensate for
the bias caused by the map maker. We test our reconstruction performance for
four different frequency bands against various algorithmic parameters,
atmospheric conditions and input beams. We additionally show the reconstruction
quality as function of the number of available observations and investigate how
different calibration strategies affect the beam uncertainty. For all of the
cases considered, we find good agreement between the fitted results and the
input beam model within a ~1.5% error for a multipole range l = 30 - 700.Comment: 22 pages, 21 figures, to be submitted to Ap
Conceptual Design of the Modular Detector and Readout System for the CMB-S4 survey experiment
We present the conceptual design of the modular detector and readout system
for the Cosmic Microwave Background Stage 4 (CMB-S4) ground-based survey
experiment. CMB-S4 will map the cosmic microwave background (CMB) and the
millimeter-wave sky to unprecedented sensitivity, using 500,000 superconducting
detectors observing from Chile and Antarctica to map over 60 percent of the
sky. The fundamental building block of the detector and readout system is a
detector module package operated at 100 mK, which is connected to a readout and
amplification chain that carries signals out to room temperature. It uses
arrays of feedhorn-coupled orthomode transducers (OMT) that collect optical
power from the sky onto dc-voltage-biased transition-edge sensor (TES)
bolometers. The resulting current signal in the TESs is then amplified by a
two-stage cryogenic Superconducting Quantum Interference Device (SQUID) system
with a time-division multiplexer to reduce wire count, and matching
room-temperature electronics to condition and transmit signals to the data
acquisition system. Sensitivity and systematics requirements are being
developed for the detector and readout system over a wide range of observing
bands (20 to 300 GHz) and optical powers to accomplish CMB-S4's science goals.
While the design incorporates the successes of previous generations of CMB
instruments, CMB-S4 requires an order of magnitude more detectors than any
prior experiment. This requires fabrication of complex superconducting circuits
on over 10 square meters of silicon, as well as significant amounts of
precision wiring, assembly and cryogenic testing.Comment: 25 pages, 15 figures, presented at and published in the proceedings
of SPIE Astronomical Telescopes and Instrumentation 202
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The Simons Observatory: Science goals and forecasts
The Simons Observatory (SO) is a new cosmic microwave background experiment
being built on Cerro Toco in Chile, due to begin observations in the early
2020s. We describe the scientific goals of the experiment, motivate the design,
and forecast its performance. SO will measure the temperature and polarization
anisotropy of the cosmic microwave background in six frequency bands: 27, 39,
93, 145, 225 and 280 GHz. The initial configuration of SO will have three
small-aperture 0.5-m telescopes (SATs) and one large-aperture 6-m telescope
(LAT), with a total of 60,000 cryogenic bolometers. Our key science goals are
to characterize the primordial perturbations, measure the number of
relativistic species and the mass of neutrinos, test for deviations from a
cosmological constant, improve our understanding of galaxy evolution, and
constrain the duration of reionization. The SATs will target the largest
angular scales observable from Chile, mapping ~10% of the sky to a white noise
level of 2 K-arcmin in combined 93 and 145 GHz bands, to measure the
primordial tensor-to-scalar ratio, , at a target level of .
The LAT will map ~40% of the sky at arcminute angular resolution to an expected
white noise level of 6 K-arcmin in combined 93 and 145 GHz bands,
overlapping with the majority of the LSST sky region and partially with DESI.
With up to an order of magnitude lower polarization noise than maps from the
Planck satellite, the high-resolution sky maps will constrain cosmological
parameters derived from the damping tail, gravitational lensing of the
microwave background, the primordial bispectrum, and the thermal and kinematic
Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle
polarization signal to measure the tensor-to-scalar ratio. The survey will also
provide a legacy catalog of 16,000 galaxy clusters and more than 20,000
extragalactic sources
The Simons Observatory: Beam characterization for the small aperture telescopes
We use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a mapmaker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the mapmaker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions, and input beams. We additionally show the reconstruction quality as a function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within an âŒ1.5% error for a multipole range â = 30â700 and an âŒ0.5% error for a multipole range â = 50â200. We conclude by using a harmonic-domain component separation algorithm to verify that the beam reconstruction errors and biases observed in our analysis do not significantly bias the Simons Observatory r-measuremen
Broadband, millimeter-wave antireflection coatings for large-format, cryogenic aluminum oxide optics
We present two prescriptions for broadband (âŒ77â252GHz), millimeter-wave antireflection coatings for cryogenic, sintered polycrystalline aluminum oxide optics: one for large-format (700 mm diameter) planar and planoâconvex elements, the other for densely packed arrays of quasi-optical elementsâin our case, 5 mm diameter half-spheres (called âlensletsâ). The coatings comprise three layers of commercially available, polytetrafluoroethylene-based, dielectric sheet material. The lenslet coating is molded to fit the 150 mm diameter arrays directly, while the large-diameter lenses are coated using a tiled approach. We review the fabrication processes for both prescriptions, then discuss laboratory measurements of their transmittance and reflectance. In addition, we present the inferred refractive indices and loss tangents for the coating materials and the aluminum oxide substrate. We find that at 150 GHz and 300 K the large-format coating sample achieves (97±2)% transmittance, and the lenslet coating sample achieves (94±3)% transmittance
Simons Observatory HoloSim-ML: machine learning applied to the efficient analysis of radio holography measurements of complex optical systems
Near-field radio holography is a common method for measuring and aligning mirror surfaces for millimeter and sub-millimeter telescopes. In instruments with more than a single mirror, degeneracies arise in the holography measurement, requiring multiple measurements and new fitting methods. We present HoloSim-ML, a Python code for beam simulation and analysis of radio holography data from complex optical systems. This code uses machine learning to efficiently determine the position of hundreds of mirror adjusters on multiple mirrors with few micrometer accuracy. We apply this approach to the example of the Simons Observatory 6 m telescope. (C) 2021 Optical Society of Americ
The Simons Observatory: Beam characterization for the Small Aperture Telescopes
International audienceWe use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a map maker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the map maker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions and input beams. We additionally show the reconstruction quality as function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within a ~1.5% error for a multipole range l = 30 - 700
The Simons Observatory: Beam characterization for the Small Aperture Telescopes
International audienceWe use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a map maker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the map maker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions and input beams. We additionally show the reconstruction quality as function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within a ~1.5% error for a multipole range l = 30 - 700
The Simons Observatory: Beam characterization for the Small Aperture Telescopes
International audienceWe use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a map maker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the map maker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions and input beams. We additionally show the reconstruction quality as function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within a ~1.5% error for a multipole range l = 30 - 700