vic haynes - Academia.edu (original) (raw)
Papers by vic haynes
Journal of Cosmology and Astroparticle Physics
The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro ... more 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 centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, 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 small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 µK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r) = 0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 µK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. 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 tensorto-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources a .
Universe
In this paper, we describe QUBIC, an experiment that will observe the polarized microwave sky wit... more In this paper, we describe QUBIC, an experiment that will observe the polarized microwave sky with a novel approach, which combines the sensitivity of state-of-the-art bolometric detectors with the systematic effects control typical of interferometers. QUBIC’s unique features are the so-called “self-calibration”, a technique that allows us to clean the measured data from instrumental effects, and its spectral imaging power, i.e., the ability to separate the signal into various sub-bands within each frequency band. QUBIC will observe the sky in two main frequency bands: 150 GHz and 220 GHz. A technological demonstrator is currently under testing and will be deployed in Argentina during 2019, while the final instrument is expected to be installed during 2020.
Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation II, 2016
Millimeter and Submillimeter Detectors and Instrumentation for Astronomy IV, 2008
Astrophysical experiments dedicated to the study of the Cosmic Microwave Background are in needs ... more Astrophysical experiments dedicated to the study of the Cosmic Microwave Background are in needs of very well defined beam shape in order to get an accurate reconstruction of the anisotropies power spectrum. These beams have to be carefully designed, but also properly characterised. Some of these instruments will be located in a cryostat for which filters and windows are necessary, and the effects of these additional optical components on the beam shape need to be taken into account. We present here, measurements of such effects on the co-and cross-polarisation radiation patterns of corrugated horns using a Vector Network Analyser.
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 2014
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 2012
ABSTRACT
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 2012
ABSTRACT Telescopes for the next generation of CMB (Cosmic Microwave Background) experiments coul... more ABSTRACT Telescopes for the next generation of CMB (Cosmic Microwave Background) experiments could be based on either reflective (such as Planck, Clover) or refractive optics (BICEP, LSPE, SPIDER). Both techniques have advantages and disadvantages. On-axis lens based telescopes can be compact while off-axis reflective configurations can be large. The RF performances of mirror based telescopes are very well understood, whereas lens based systems have a lower technology readiness level: specifically, the systematic effects (aberrations such as chromaticity, birefringence, losses, standing waves and cross-polarisation) that they can introduce need to be accurately quantified at millimetre-wave. This paper reports on both RF modelling and preliminary experimental studies of a lens coupled to a feed-horn antenna for which the co- and cross-polarisation beam patterns are characterised.
SPICA joint European/Japanese Workshop, 2009
Progress In Electromagnetics Research M, 2012
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 2014
ABSTRACT
The 8th European Conference on Antennas and Propagation (EuCAP 2014), 2014
Proceedings of SPIE - The International Society for Optical Engineering, 2012
ABSTRACT By use of a metamaterial based on the ‘cut wire pair’ geometry, highly birefringent wave... more ABSTRACT By use of a metamaterial based on the ‘cut wire pair’ geometry, highly birefringent wave plates may be constructed by virtue of the geometry’s ability of having a negative and positive refractive index along its perpendicular axes. Past implementations have been narrow band in nature due to the reliance on producing a resonance to achieve a negative refractive index band and the steep gradient in the phase difference that results. In this paper we attempt to design and manufacture a W-band quarter wave plate embedded in polypropylene that applies the Pancharatnam method to increase the useable bandwidth. Our modelling demonstrates that a broadening of the phase difference’s bandwidth defined as the region 90° +/- 2° is possible from 0.6% (101.7 GHz - 102.3 GHz) to 7.8% (86.2 GHz - 93.1 GHz). Our experimental results show some agreement with our modelling but differ at higher frequencies.
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 2014
ABSTRACT ArTeMiS is a submillimeter camera planned to work simultaneously at 450 μm, 350 μm and 2... more ABSTRACT ArTeMiS is a submillimeter camera planned to work simultaneously at 450 μm, 350 μm and 200 μm by use of 3 focal planes of, respectively, 8, 8 and 4 bolometric arrays, each one made of 16 x18 pixels. In July 2013, with a preliminary setting reduced to 4 modules and to the 350 μm band, ArTeMiS was installed successfully at the Cassegrain focus of APEX, a 12 m antenna located on the Chajnantor plateau, Chile. After the summary of the scientific requirements, we describe the main lines of the ArTeMiS nominal optical design with its rationale and performances. This optical design is highly constrained by the room allocation available in the Cassegrain cabin. It is an all-reflective design including a retractable pick off mirror, a warm Fore Optics to image the focal plane of the telescope inside the cryostat, and the cold optics. The large size of the field of view at the focal plane of the telescope, 72 mm x 134 mm for the 350 μm and 450 μm beams, leads to the use of biconical toroidal mirrors. In this way, the nominal image quality obtained on the bolometric arrays is only just diffraction limited at some corners of the field of view. To keep a final PSF as much uniform as possible across the field of view, we have used the technic of manufacturing by diamond turning to machine the mirrors. This approach, while providing high accuracy on the shape of the mirrors, made easier the control of the two sub units, the Fore Optics and the cold optics, in the visible domain and at room temperature. Moreover, the use of the similar material (Aluminium alloy 6061) for the optical bench and the mirrors with their mount ensures a homothetic shrinking during the cooling down. The alignment protocol, drew up at the early step of the study, is also presented. It required the implementation of two additional mechanisms inside the cryostat to check the optical axis of the cold optics, in the real conditions of operation of ArTeMiS. In this way, it was possible to pre-align the Fore Optics sub unit with respect to the cold optics. Finally, despite the high constraints of the operating conditions of APEX, this protocol allowed to align ArTeMiS with respect to the telescope in a single adjustment. The first images obtained on the sky, Saturn with its rings, are given.
The Astrophysical Journal, 2009
Journal of Cosmology and Astroparticle Physics
The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro ... more 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 centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, 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 small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 µK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r) = 0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 µK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. 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 tensorto-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources a .
Universe
In this paper, we describe QUBIC, an experiment that will observe the polarized microwave sky wit... more In this paper, we describe QUBIC, an experiment that will observe the polarized microwave sky with a novel approach, which combines the sensitivity of state-of-the-art bolometric detectors with the systematic effects control typical of interferometers. QUBIC’s unique features are the so-called “self-calibration”, a technique that allows us to clean the measured data from instrumental effects, and its spectral imaging power, i.e., the ability to separate the signal into various sub-bands within each frequency band. QUBIC will observe the sky in two main frequency bands: 150 GHz and 220 GHz. A technological demonstrator is currently under testing and will be deployed in Argentina during 2019, while the final instrument is expected to be installed during 2020.
Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation II, 2016
Millimeter and Submillimeter Detectors and Instrumentation for Astronomy IV, 2008
Astrophysical experiments dedicated to the study of the Cosmic Microwave Background are in needs ... more Astrophysical experiments dedicated to the study of the Cosmic Microwave Background are in needs of very well defined beam shape in order to get an accurate reconstruction of the anisotropies power spectrum. These beams have to be carefully designed, but also properly characterised. Some of these instruments will be located in a cryostat for which filters and windows are necessary, and the effects of these additional optical components on the beam shape need to be taken into account. We present here, measurements of such effects on the co-and cross-polarisation radiation patterns of corrugated horns using a Vector Network Analyser.
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 2014
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 2012
ABSTRACT
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, 2012
ABSTRACT Telescopes for the next generation of CMB (Cosmic Microwave Background) experiments coul... more ABSTRACT Telescopes for the next generation of CMB (Cosmic Microwave Background) experiments could be based on either reflective (such as Planck, Clover) or refractive optics (BICEP, LSPE, SPIDER). Both techniques have advantages and disadvantages. On-axis lens based telescopes can be compact while off-axis reflective configurations can be large. The RF performances of mirror based telescopes are very well understood, whereas lens based systems have a lower technology readiness level: specifically, the systematic effects (aberrations such as chromaticity, birefringence, losses, standing waves and cross-polarisation) that they can introduce need to be accurately quantified at millimetre-wave. This paper reports on both RF modelling and preliminary experimental studies of a lens coupled to a feed-horn antenna for which the co- and cross-polarisation beam patterns are characterised.
SPICA joint European/Japanese Workshop, 2009
Progress In Electromagnetics Research M, 2012
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 2014
ABSTRACT
The 8th European Conference on Antennas and Propagation (EuCAP 2014), 2014
Proceedings of SPIE - The International Society for Optical Engineering, 2012
ABSTRACT By use of a metamaterial based on the ‘cut wire pair’ geometry, highly birefringent wave... more ABSTRACT By use of a metamaterial based on the ‘cut wire pair’ geometry, highly birefringent wave plates may be constructed by virtue of the geometry’s ability of having a negative and positive refractive index along its perpendicular axes. Past implementations have been narrow band in nature due to the reliance on producing a resonance to achieve a negative refractive index band and the steep gradient in the phase difference that results. In this paper we attempt to design and manufacture a W-band quarter wave plate embedded in polypropylene that applies the Pancharatnam method to increase the useable bandwidth. Our modelling demonstrates that a broadening of the phase difference’s bandwidth defined as the region 90° +/- 2° is possible from 0.6% (101.7 GHz - 102.3 GHz) to 7.8% (86.2 GHz - 93.1 GHz). Our experimental results show some agreement with our modelling but differ at higher frequencies.
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII, 2014
ABSTRACT ArTeMiS is a submillimeter camera planned to work simultaneously at 450 μm, 350 μm and 2... more ABSTRACT ArTeMiS is a submillimeter camera planned to work simultaneously at 450 μm, 350 μm and 200 μm by use of 3 focal planes of, respectively, 8, 8 and 4 bolometric arrays, each one made of 16 x18 pixels. In July 2013, with a preliminary setting reduced to 4 modules and to the 350 μm band, ArTeMiS was installed successfully at the Cassegrain focus of APEX, a 12 m antenna located on the Chajnantor plateau, Chile. After the summary of the scientific requirements, we describe the main lines of the ArTeMiS nominal optical design with its rationale and performances. This optical design is highly constrained by the room allocation available in the Cassegrain cabin. It is an all-reflective design including a retractable pick off mirror, a warm Fore Optics to image the focal plane of the telescope inside the cryostat, and the cold optics. The large size of the field of view at the focal plane of the telescope, 72 mm x 134 mm for the 350 μm and 450 μm beams, leads to the use of biconical toroidal mirrors. In this way, the nominal image quality obtained on the bolometric arrays is only just diffraction limited at some corners of the field of view. To keep a final PSF as much uniform as possible across the field of view, we have used the technic of manufacturing by diamond turning to machine the mirrors. This approach, while providing high accuracy on the shape of the mirrors, made easier the control of the two sub units, the Fore Optics and the cold optics, in the visible domain and at room temperature. Moreover, the use of the similar material (Aluminium alloy 6061) for the optical bench and the mirrors with their mount ensures a homothetic shrinking during the cooling down. The alignment protocol, drew up at the early step of the study, is also presented. It required the implementation of two additional mechanisms inside the cryostat to check the optical axis of the cold optics, in the real conditions of operation of ArTeMiS. In this way, it was possible to pre-align the Fore Optics sub unit with respect to the cold optics. Finally, despite the high constraints of the operating conditions of APEX, this protocol allowed to align ArTeMiS with respect to the telescope in a single adjustment. The first images obtained on the sky, Saturn with its rings, are given.
The Astrophysical Journal, 2009