On-site performance of GroundBIRD, a CMB polarization telescope for large angular scale observations

Honda, S.; Choi, Jihoon; Génova-Santos, R. T.; Hattori, Makoto; Hazumi, M.; Ikemitsu, T.; Ishida, Hideyuki; Ishitsuka, H.; Jo, Yonggil; Karatsu, K.; Kiuchi, K.; Komine, Junta; Koyano, Ryo; Kutsuma, Hiroki; Lee, Kyung-Min; Mima, Silvana; Minowa, M.; Moon, J.; Nagai, Makoto; Nagasaki, T.; Naruse, Mitsuhide; Oguri, S.; Otani, Chiko; Peel, M.; Rebolo, R.; Rubiño-Martín, J. A.; Sekímoto, Yutaro; Sueno, Y.; Suzuki, Junya; Taino, Tohru; Tajima, O.; Tomita, Naohide; Tsuji, Yuta; Uchida, Tomohisa; Won, E.; Yoshida, Mitsuhiro

doi:10.1117/12.2560918

Cited by 5 publications

(3 citation statements)

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“…The telescope will be located at Teide Observatory, which is a word-class astronomical observatory that benefits from a highly stable atmosphere with a median precipitable water vapour of 3.5 mm [20]. Its suitability for these kinds of observations has been demonstrated by many other CMB experiments that have previously observed from this site, such as the Very Small Array [6], and that are currently operating, such as QUĲOTE [23] and GroundBIRD [24]. The basic parameters of the Strip instrument are listed in table 1.…”

Section: The Strip Instrumentmentioning

confidence: 99%

LSPE-Strip on-sky calibration strategy using bright celestial sources

Génova-Santos,

Bersanelli,

Franceschet

et al. 2024

J. Inst.

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In this paper we describe the global on-sky calibration strategy of the LSPE-Strip instrument. Strip is a microwave telescope operating in the Q- and W-bands (central frequencies of 43 and 95 GHz respectively) from the Observatorio del Teide in Tenerife, with the goal to observe and characterise the polarised Galactic foreground emission, and complement the observations of the polarisation of the cosmic microwave background to be performed by the LSPE-SWIPE instrument and other similar experiments operating at higher frequencies to target the detection of the B-mode signal from the inflationary epoch of the Universe. Starting from basic assumptions on some of the instrument parameters (NET, 1/f noise knee frequency, beam properties, observing efficiency) we perform realistic simulations to study the level of accuracy that can be achieved through observations of bright celestial calibrators in the Strip footprint (sky fraction of 30%) on the determination and characterisation of the main instrument parameters: global and relative gain factors (in intensity and in polarisation), polarisation direction, polarisation efficiency, leakage from intensity to polarisation, beams, window functions and pointing model.

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Section: The Strip Instrumentmentioning

confidence: 99%

LSPE-Strip on-sky calibration strategy using bright celestial sources

Génova-Santos,

Bersanelli,

Franceschet

et al. 2024

J. Inst.

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“…The QUIJOTE telescopes are based on an offset crossed-Dragone design with projected apertures of 2.25 and 1.89 m for the primary and secondary mirrors respectively, which provides optimal polarisation properties. QT-1 is focused on observations at low frequencies (10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20), and was operating between 2012 and 2018 with the Multi-Frequency Instrument (MFI, 2; 7).From 2018-2020 the KISS spectrometer was mounted(KISS, 8). QT-2 is dedicated to observations in the 30-40 GHz range, using two instruments, the Thirty-GHz Instrument (TGI) and the Forty-GHz Instrument (FGI) (7).…”

Section: Introductionmentioning

confidence: 99%

“…QUIJOTE is located at the Teide Observatory (2,400 m above sea level) in Tenerife (Canary Islands), a site with excellent observing conditions for microwave observations (median pwv of 3.5 mm, see 9), and with a long tradition of more than 35 years in CMB research. In addition to QUIJOTE, there are three CMB experiments that are either running at the moment, or to be installed in the next year: GroundBIRD (10), LSPE-STRIP (11), and the Tenerife Microwave Spectrometer (TMS, 12). QUIJOTE has a primary science goal: to provide essential information of the polarisation properties of the synchrotron and anomalous microwave emissions from our Galaxy (3).…”

Section: Introductionmentioning

confidence: 99%

The new multi-frequency instrument (MFI2) for the QUIJOTE facility in Tenerife

Hoyland¹,

Rubiño-Martín²,

Alonso-Arias³

et al. 2022

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI

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The QUIJOTE (Q-U-I JOint TEnerife) Experiment combines the operation of two radio-telescopes and three instruments working in the microwave bands 10-20 GHz, 26-36 GHz and 35-47 GHz at the Teide observatory, Tenerife, and has already been presented in previous SPIE meetings (1; 2). The Cosmology group at the IAC have designed a new upgrade to the MFI instrument in the band 10-20 GHz. The aim of the QUIJOTE telescopes is to characterise the polarised emission of the Cosmic Microwave Background (CMB), as well as Further author information: (Send correspondence to R.J.H.

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Commissioning the CMB polarization telescope GroundBIRD with the full set of detectors

Tsujii,

Baselmans,

Choi

et al. 2024

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XII

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GroundBIRD is a ground-based cosmic microwave background (CMB) experiment for observing the polarization pattern imprinted on large angular scales (ℓ > 6 ) from the Teide Observatory in Tenerife, Spain. Our primary scientific objective is a precise measurement of the optical depth τ (σ(τ ) ∼ 0.01) to the reionization epoch of the Universe to cross-check systematic effects in the measurements made by previous experiments. GroundBIRD observes a wide sky area in the Northern Hemisphere (∼ 40% of the full sky) while continuously rotating the telescope at a high speed of up to 20 rotations per minute (rpm) to overcome the fluctuations of atmospheric radiation. We have adopted the NbTiN/Al hybrid microwave kinetic inductance detectors (MKIDs) as focal plane detectors. We observe two frequency bands centered at 145 GHz and 220 GHz. The 145 GHz band picks up the peak frequency of the CMB spectrum. The 220 GHz band helps accurate removal of the contamination of thermal emission from the Galactic interstellar dust. The MKID arrays (138 MKIDs for 145GHz and 23 MKIDs for 220GHz) were designed and optimized so as to minimize the contamination of the two-level-system noise and maximize the sensitivity. The MKID arrays were successfully installed in May 2023 after the performance verification tests were performed at a laboratory. GroundBIRD has been upgraded to use the full MKID arrays, and scientific observations are now underway. The telescope is automated, so that all observations are performed remotely. Initial validations, including polarization response tests and observations of Jupiter and the moon, have been completed successfully. We are now running scientific observations.

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On-site performance of GroundBIRD, a CMB polarization telescope for large angular scale observations

Cited by 5 publications

References 0 publications

LSPE-Strip on-sky calibration strategy using bright celestial sources

LSPE-Strip on-sky calibration strategy using bright celestial sources

The new multi-frequency instrument (MFI2) for the QUIJOTE facility in Tenerife

Commissioning the CMB polarization telescope GroundBIRD with the full set of detectors

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