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Sketch of the OLIMPO experiment, with a labelling of the main components. The rear view and the side view are shown in the left and in the right panels, respectively.
Source publication
OLIMPO is a balloon-borne experiment aiming at spectroscopic measurements of the Sunyaev-Zel’dovich effect in clusters of galaxies. The instrument operates from the stratosphere, so that it can cover a wide frequency range (from ∼ 130 to ∼ 520 GHz in 4 bands), including frequencies which are not observable with ground-based instruments. OLIMPO is c...
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Context 1
... the telescope and the cryostat, which allows us to switch between photometric and spectroscopic configurations. The attitude control system is composed of an azimuth pivot, an elevation motor, three gyroscopes, a star camera, and two sun sensors, all controlled by two computers. Furthermore, it features a boresight precision of the order of Fig. 1. It was designed for a polar summer, longduration stratospheric flight. It is powered by four arrays of solar panels (∼ 8 m 2 ) that charge two sets of pressurized gel lead-acid batteries. OLIMPO has been launched from Longyearbyen airport on July 14 th , 2018. The flight duration was 5 days, at a float altitude of 37.8 km. ...
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Dit is het beste dat me ooit overkomen is tijdens mijn ganse onderwijscarrière. Voor het eerst heb ik me ten volle gewaardeerd gevoeld als leerkracht." Margaret, lid van een visitatieteam Uit: Wilson, 2001.
Zusammenfassung
Gesamtüberblick: Zu der zusammenfassenden Darstellung der unterschiedlichen Ergebnisse und zur Interpretation der Analyse zur Konzeptualisierung des Instruments zur sprachlichen Variation finden nachfolgend eine vergleichende Darstellung der Ergebnisse und eine Erörterung der inhaltlichen Erkenntnisse statt (Abschnitt 10.1). Aufgrun...
Citations
... Sensors 2024, 24, 359 2 of 20 characterizes their sensitivity-has decreased by about two orders of magnitude since the late 1960s and has come close to the so-called quantum limit. Many new groundbased [11][12][13][14] balloon [15][16][17] and space [18,19] radio telescopes of this range have been built, including several antenna arrays. ...
This article presents the results of evaluating the possibility of conducting radio astronomy studies in the windows of atmospheric transparency ~100, ~230, and ~350 GHz using the optical Big Telescope Alt-Azimuthal (BTA) of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS). A list of some promising astronomical tasks is proposed. The astroclimat conditions at the BTA site and possible optical, cryogenic, and mechanical interfaces for mounting a superconducting radio receiver at the focus of the optical telescope are considered. As a receiving system, arrays of detectors cooled to ~0.3 K based on the superconductor–insulator–normal metal–insulator–superconductor (SINIS) structure are proposed. The implementation of the project will make it possible to use the BTA site of the SAO RAS not only to solve some astronomical problems (it is possible to consider the implementation of a single observatory, the VLBI (very-long-baseline interferometry) mode in the Suffa, EHT (Event Horizon Telescope), and Millimetron projects), but it will also be used to test various cryogenic detectors in a real observatory.
... For such measurements, the combination of high angular resolution and mapping speed over the whole relevant microwave bandwidth is a key requirement to detect the SZ signatures from arcminute-scale clusters by exploiting the typical spectral signature of the ytype distortion through broad-band microwave spectrometry. Examples of such an instrument design are the OLIMPO balloon-borne experiment [40][41][42][43] and the MILLIMETRON Space Observatory 1 [44,45] proposed to Roscosmos, both equipped with large aperture optics and a differential FTS. ...
We have developed two arrays of lumped element kinetic inductance detectors working in the D-band, and optimised for the low radiative background conditions of a satellite mission aiming at precision measurements of the Cosmic Microwave Background (CMB) radiation. The first detector array is sensitive to the total power of the incoming radiation to which is coupled via single-mode waveguides and corrugated feed-horns, while the second is sensitive to the polarisation of the radiation thanks to orthomode transducers. Here, we focus on the total power detector array, which is suitable, for instance, for precision measurements of unpolarised spectral distortions of the CMB, where detecting both polarisations provides a sensitivity advantage. We describe the optimisation of the array design, fabrication and packaging, the dark and optical characterisation, and the performance of the black-body calibrator used for the optical tests. We show that almost all the detectors of the array are photon-noise limited under the radiative background of a 3.6 K black-body. This result, combined with the weak sensitivity to cosmic ray hits demonstrated with the OLIMPO flight, validates the idea of using lumped elements kinetic inductance detectors for precision, space-based CMB missions.
... Balloon-borne experiments have the potential to make significant contributions. For instance, PIPER has frequency coverage up to 600 GHz (Essinger-Hileman et al. 2020), OLIMPO observes up to 460 GHz (Presta et al. 2020), and PILOT extends to 1.2 THz (Bernard et al. 2016). Submillimeter experiments such as the proposed Balloon-Borne Large Aperture Submillimeter Telescope (BLAST) Observatory (Lowe et al. 2020) would have the capability to survey hundreds of square degrees at frequencies between 850 GHz and 1.7 THz, providing a strong lever arm to distinguish between proposed dust models. ...
Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised to address many questions in Galactic astrophysics in addition to its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for a range of Galactic science cases. We find that SO can: constrain the frequency spectrum of polarized dust emission at a level of Δ β d ≲ 0.01 and thus test models of dust composition that predict that β d in polarization differs from that measured in total intensity; measure the correlation coefficient between polarized dust and synchrotron emission with a factor of two greater precision than current constraints; exclude the nonexistence of exo-Oort clouds at roughly 2.9 σ if the true fraction is similar to the detection rate of giant planets; map more than 850 molecular clouds with at least 50 independent polarization measurements at 1 pc resolution; detect or place upper limits on the polarization fractions of CO(2–1) emission and anomalous microwave emission at the 0.1% level in select regions; and measure the correlation coefficient between optical starlight polarization and microwave polarized dust emission in 1° patches for all lines of sight with N H ≳ 2 × 10 ²⁰ cm ⁻² . The goals and forecasts outlined here provide a roadmap for other microwave polarization experiments to expand their scientific scope via Milky Way astrophysics. ³⁷ ³⁷ A supplement describing author contributions to this paper can be found at https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf .
... For such measurements, the combination of high angular resolution and mapping speed over the whole relevant microwave bandwidth is a key requirement to detect the SZ signatures from arcminute-scale clusters by exploiting the typical spectral signature of the y-type distortion through broad-band microwave spectrometry. Examples of such an instrument design are the OLIMPO balloon-borne experiment [40][41][42][43] and the MILLIMETRON Space Observatory 1 [44,45] proposed to Roscosmos, both equipped with large aperture optics and a differential FTS. ...
We have developed two arrays of lumped element kinetic inductance detectors working in the D-band, and optimised for the low radiative background conditions of a satellite mission aiming at precision measurements of the Cosmic Microwave Background (CMB). The first detector array is sensitive to the total power of the incoming radiation to which is coupled via single-mode waveguides and corrugated feed-horns, while the second is sensitive to the polarisation of the radiation thanks to orthomode transducers. Here, we focus on the total power detector array, which is suitable, for instance, for precision measurements of unpolarised spectral distortions of the CMB, where detecting both polarisations provides a sensitivity advantage. We describe the optimisation of the array design, fabrication and packaging, the dark and optical characterisation, and the performance of the black-body calibrator used for the optical tests. We show that almost all the detectors of the array are photon-noise limited under the radiative background of a 3.6 K black-body. This result, combined with the weak sensitivity to cosmic rays hits demonstrated with the OLIMPO flight, validates the idea of using lumped elements kinetic inductance detectors for precision, space-based CMB missions.
... Balloon-borne experiments have the potential to make significant contributions. For instance, PIPER has frequency coverage up to 600 GHz (Essinger-Hileman et al. 2020), OLIMPO observes up to 460 GHz (Presta et al. 2020), and PILOT extends to 1.2 THz (Bernard et al. 2016). Submillimeter experiments such as the proposed Balloon-Borne Large Aperture Submillimeter Telescope (BLAST) Observatory (Lowe et al. 2020) would have the capability to survey hundreds of square degrees at frequencies between 850 GHz and 1.7 THz, providing a strong lever arm to distinguish between proposed dust models. ...
Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised to address many questions in Galactic astrophysics in addition to its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for a range of Galactic science cases. We find that SO can: constrain the frequency spectrum of polarized dust emission at a level of $\Delta\beta_d \lesssim 0.01$ and thus test models of dust composition that predict that $\beta_d$ in polarization differs from that measured in total intensity; measure the correlation coefficient between polarized dust and synchrotron emission with a factor of two greater precision than current constraints; exclude the non-existence of exo-Oort clouds at roughly 2.9$\sigma$ if the true fraction is similar to the detection rate of giant planets; map more than 850 molecular clouds with at least 50 independent polarization measurements at 1 pc resolution; detect or place upper limits on the polarization fractions of CO(2-1) emission and anomalous microwave emission at the 0.1% level in select regions; and measure the correlation coefficient between optical starlight polarization and microwave polarized dust emission in $1^\circ$ patches for all lines of sight with $N_{\rm H} \gtrsim 2\times10^{20}$ cm$^{-2}$. The goals and forecasts outlined here provide a roadmap for other microwave polarization experiments to expand their scientific scope via Milky Way astrophysics.
... Many ground-based observatories already exist, as well as balloon and space missions for space exploration in this frequency range have been launched and being developed. As an example, such projects are ALMA [2], [3], South Pole Telescope [4], [5], OLIMPO [6], [7], Planсk [8], [9], MILLIMETRON [10], [11], etc. The requirements set by those projects to modern receiving systems include a wide dynamic range and noise equivalent power (NEP) below 10 −16 W/Hz 0.5 for ground-based observatories and 10 −19 W/Hz 0.5 for space missions. ...
A superconductor-insulator-normal metal-insulator-superconductor (SINIS) detector integrated in a planar 90 GHz band twin-slot antenna with a 2 GHz superconducting resonator readout was fabricated and experimentally studied. In order to achieve high pixel count, the traditional dc readout of the SINIS detector is replaced by NbN coplanar 13.850 mm long superconducting resonator. SINIS detectors have traditionally dc Junction Field Effect Transistor (JFET) room-temperature readout. Such readout requires individual wiring for each pixel, while the microwave readout is far less cluttered as only one coaxial line is needed for hundreds of devices. Such readout operates similar to frequency domain multiplexing (FDM) for microwave kinetic inductance detectors (MKID). The planar twin slot antenna has two parallel slots in a metal ground plane which are excited coherently by short sections of a coplanar waveguide (CPW) line with a SINIS detector at the center. One section of the CPW is extended past the slot in a long superconducting section which functions as a quarter wavelength resonator. This resonator is short circuited to the ground plane at the far end, with the expected open circuited end terminated by the SINIS detector in the antenna. We measured the response of sample to black body radiation temperatures 6 K and 9 K. The corresponding dynamic resistance maximum drops from 50 k down to 30 k. An RF readout channel comprising a coplanar coupler and a coplanar resonator has a resonant frequency of 1.8 GHz. Unloaded Q factor (without incoming irradiation) is 200. The signal spectral characteristics and the response to the black body radiation have shown design values as expected.
... The MKID arrays for the six spectrometers use a microwave multiplexing readout scheme with heritage from The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) 16 and the Far Infrared Observatory Mounted on a Pointed Balloon (OLIMPO). 17 The EXCLAIM gondola design, attitude determination and control system, and flight electronics are based on those of PIPER with modest modifications and improvements. EXCLAIM will observe at constant elevation with scans in azimuth between 5 • and 10 • wide to map strips on the sky. ...
This work describes the optical design of the EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM). EXCLAIM is a balloon-borne telescope that will measure integrated line emission from carbon monoxide (CO) at redshifts z < 1 and ionized carbon ([CII]) at redshifts z = 2.5-3.5 to probe star formation over cosmic time in cross-correlation with galaxy redshift surveys. The EXCLAIM instrument will observe at frequencies of 420--540 GHz using six microfabricated silicon integrated spectrometers with spectral resolving power R = 512 coupled to kinetic inductance detectors (KIDs). A completely cryogenic telescope cooled to a temperature below 5 K provides low-background observations between narrow atmospheric lines in the stratosphere. Off-axis reflective optics use a $90$-cm primary mirror to provide 4.2' full-width at half-maximum (FWHM) resolution at the center of the EXCLAIM band over a field of view of 22.5'. Illumination of the 1.7 K cold stop combined with blackened baffling at multiple places in the optical system ensures low (< -40 dB) edge illumination of the primary to minimize spill onto warmer elements at the top of the dewar.
