GroundBIRD

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GroundBIRD
GroundBIRD 2019 001.jpg
GroundBIRD in 2019
Part of Teide Observatory   OOjs UI icon edit-ltr-progressive.svg
Location(s) Tenerife, Atlantic Ocean
Coordinates 28°18′02″N16°30′37″W / 28.30042°N 16.51028°W / 28.30042; -16.51028 Coordinates: 28°18′02″N16°30′37″W / 28.30042°N 16.51028°W / 28.30042; -16.51028 OOjs UI icon edit-ltr-progressive.svg
Altitude2,400 m (7,900 ft) OOjs UI icon edit-ltr-progressive.svg
Wavelength 145, 220 GHz (2.07, 1.36 mm)
Telescope style cosmic microwave background experiment
radio telescope   OOjs UI icon edit-ltr-progressive.svg
Diameter30 cm (1 ft 0 in) OOjs UI icon edit-ltr-progressive.svg
Angular resolution 0.5 degree, 0.3 degree  OOjs UI icon edit-ltr-progressive.svg
Location map Spain Tenerife.png
Red pog.svg
Location of GroundBIRD
  Commons-logo.svg Related media on Commons
[ edit on Wikidata]

GroundBIRD is an experiment to observe the cosmic microwave background at 145 and 220GHz. It aims to observe the B-mode polarisation signal from inflation in the early universe. It is located at Teide Observatory, on the island of Tenerife in the Canary Islands.

Contents

Scientific goals

The telescope was constructed to measure the B-mode signal in the polarisation of the Cosmic Microwave Background (CMB), [1] in order to look for evidence of cosmic inflation in the early universe. It aims to observe the reionization bump at and the recombination peak around . [2] The name 'GroundBIRD' indicates that the telescope is ground-based, while BIRD stands for B-mode Imaging Radiation Detector. [2] It is related to the future, similarly-named, LiteBIRD CMB satellite.

Telescope

The detector focal plane (left) along with the primary (bottom) and secondary (right) mirrors, which are all located in the cryostat. At Teide Observatory 2019 090.jpg
The detector focal plane (left) along with the primary (bottom) and secondary (right) mirrors, which are all located in the cryostat.

The telescope consists of two mirrors in a Mizuguchi-Dragone configuration, with a diameter of 30 cm (12 in). The telescope is inside the cryostat, which is mounted on a rotation table, with a rotary joint that provides helium gas and electricity to the cryostat. [2] [3] The mirrors are cooled to 4 K (−269.15 °C) using a Pulse tube refrigerator to reduce the thermal noise from the mirror surfaces. [2]

The experiment uses microwave kinetic inductance detectors (MKIDs), [4] which are cooled to 250mK by a sorption cooler within the cryostat, which uses helium-3, and was manufactured by Chase Research Cryogenics Ltd. [2] The signals from the detector are multiplexed, and around 100 detectors can be measured in both phase and amplitude with a single digital read-out system with a bandwidth of 200MHz, recording 1,000 samples per second. The digital system uses 12-bit ADCs and a Kintex-7 FPGA from Xilinx initially, [4] and now uses Kintex ultrascale FPGAs.[ citation needed ] Raspberry Pis are used to monitor and control the telescope. [5]

The cryostat rotates at 20 rpm (120° per second, 1 rotation every 3 seconds) to minimize 1/f noise. [2] [6] [7] It observes at zenith angles up to 20°, mapping around 40% of the sky. The field of view is 10°, with an angular resolution of 0.5° FWHM at 145GHz, and 0.3° at 220GHz. [2] It will measure the CMB at [6]

The telescope was constructed at KEK in Japan. [2] Test observations started in Japan in 2014. While it was originally intended that it would observe from the Atacama Desert in Chile, [6] an agreement to install it at Teide Observatory was reached in 2016, [8] [1] [9] at an altitude of 2,400 metres (7,900 ft). [2] [10] It was shipped to Tenerife in January 2019. [7] In February 2020, the experiment was visited by Kenji Hiramatsu, the Japanese Ambassador to Spain. [11]

Collaboration

The inside of the cryostat being lifted into the telescope dome. GroundBIRD 2019 004.jpg
The inside of the cryostat being lifted into the telescope dome.

The collaboration includes scientists from:

Funding

GroundBIRD observing the night sky GroundBIRD 2019 006.jpg
GroundBIRD observing the night sky

The project is funded by:

with additional support from:

Related Research Articles

Observational cosmology is the study of the structure, the evolution and the origin of the universe through observation, using instruments such as telescopes and cosmic ray detectors.

<span class="mw-page-title-main">Cosmic Background Imager</span> Interferometer at Llano de Chajnantor Observatory in Chile

The Cosmic Background Imager was a 13-element interferometer perched at an elevation of 5,080 metres at Llano de Chajnantor Observatory in the Chilean Andes. It started operations in 1999 to study the cosmic microwave background radiation and ran until 2008.

<span class="mw-page-title-main">BOOMERanG experiment</span>

In astronomy and observational cosmology, the BOOMERanG experiment was an experiment which measured the cosmic microwave background radiation of a part of the sky during three sub-orbital (high-altitude) balloon flights. It was the first experiment to make large, high-fidelity images of the CMB temperature anisotropies, and is best known for the discovery in 2000 that the geometry of the universe is close to flat, with similar results from the competing MAXIMA experiment.

<span class="mw-page-title-main">Very Small Array</span> Radio telescope in the Canary Islands

The Very Small Array (VSA) was a 14-element interferometric radio telescope operating between 26 and 36 GHz that is used to study the cosmic microwave background radiation. It was a collaboration between the University of Cambridge, University of Manchester and the Instituto de Astrofisica de Canarias (Tenerife), and was located at the Observatorio del Teide on Tenerife. The array was built at the Mullard Radio Astronomy Observatory by the Cavendish Astrophysics Group and Jodrell Bank Observatory, and was funded by PPARC. The design was strongly based on the Cosmic Anisotropy Telescope.

<span class="mw-page-title-main">Teide Observatory</span> Observatory

Teide Observatory, IAU code 954, is an astronomical observatory on Mount Teide at 2,390 metres (7,840 ft), located on Tenerife, Spain. It has been operated by the Instituto de Astrofísica de Canarias since its inauguration in 1964. It became one of the first major international observatories, attracting telescopes from different countries around the world because of the good astronomical seeing conditions. Later the emphasis for optical telescopes shifted more towards Roque de los Muchachos Observatory on La Palma.

<span class="mw-page-title-main">South Pole Telescope</span> Telescope at the South Pole

The South Pole Telescope (SPT) is a 10-metre (390 in) diameter telescope located at the Amundsen–Scott South Pole Station, Antarctica. The telescope is designed for observations in the microwave, millimeter-wave, and submillimeter-wave regions of the electromagnetic spectrum, with the particular design goal of measuring the faint, diffuse emission from the cosmic microwave background (CMB). The first major survey with the SPT—designed to find distant, massive, clusters of galaxies through their interaction with the CMB, with the goal of constraining the dark energy equation of state—was completed in October 2011. In early 2012, a new camera (SPTpol) was installed on the SPT with even greater sensitivity and the capability to measure the polarization of incoming light. This camera operated from 2012–2016 and was used to make unprecedentedly deep high-resolution maps of hundreds of square degrees of the Southern sky. In 2017, the third-generation camera SPT-3G was installed on the telescope, providing nearly an order-of-magnitude increase in mapping speed over SPTpol.

<span class="mw-page-title-main">Atacama Cosmology Telescope</span> Telescope in the Atacama Desert, northern Chile

The Atacama Cosmology Telescope (ACT) is a cosmological millimeter-wave telescope located on Cerro Toco in the Atacama Desert in the north of Chile. ACT makes high-sensitivity, arcminute resolution, microwave-wavelength surveys of the sky in order to study the cosmic microwave background radiation (CMB), the relic radiation left by the Big Bang process. Located 40 km from San Pedro de Atacama, at an altitude of 5,190 metres (17,030 ft), it is one of the highest ground-based telescopes in the world.

<span class="mw-page-title-main">Atacama Submillimeter Telescope Experiment</span>

The Atacama Submillimeter Telescope Experiment (ASTE) is a 10-meter-diameter antenna built by Mitsubishi Electric as a preprototype for ALMA.

The Degree Angular Scale Interferometer (DASI) was a telescope installed at the U.S. National Science Foundation's Amundsen–Scott South Pole Station in Antarctica. It was a 13-element interferometer operating between 26 and 36 GHz in ten bands. The instrument is similar in design to the Cosmic Background Imager (CBI) and the Very Small Array (VSA). In 2001 The DASI team announced the most detailed measurements of the temperature, or power spectrum of the Cosmic microwave background (CMB). These results contained the first detection of the 2nd and 3rd acoustic peaks in the CMB, which were important evidence for inflation theory. This announcement was done in conjunction with the BOOMERanG and MAXIMA experiment. In 2002 the team reported the first detection of polarization anisotropies in the CMB.

<span class="mw-page-title-main">Spider (polarimeter)</span>

Spider is a balloon-borne experiment designed to search for primordial gravitational waves imprinted on the cosmic microwave background (CMB). Measuring the strength of this signal puts limits on inflationary theory.

<span class="mw-page-title-main">Archeops</span>

Archeops was a balloon-borne instrument dedicated to measuring the Cosmic microwave background (CMB) temperature anisotropies. The study of this radiation is essential to obtain precise information on the evolution of the Universe: density, Hubble constant, age of the Universe, etc. To achieve this goal, measurements were done with devices cooled down at 100mK temperature placed at the focus of a warm telescope. To avoid atmospheric disturbance the whole apparatus is placed on a gondola below a helium balloon that reaches 40 km altitude.

<span class="mw-page-title-main">QUIET</span>

QUIET was an astronomy experiment to study the polarization of the cosmic microwave background radiation. QUIET stands for Q/U Imaging ExperimenT. The Q/U in the name refers to the ability of the telescope to measure the Q and U Stokes parameters simultaneously. QUIET was located at an elevation of 5,080 metres at Llano de Chajnantor Observatory in the Chilean Andes. It began observing in late 2008 and finished observing in December 2010.

QUBIC is a cosmology project to study cosmic inflation by measuring the B-modes of the polarization of the Cosmic Microwave Background (CMB), by observing the sky with a millimeter wave radio telescope interferometer. It uses bolometric interferometry, which combines the advantages of interferometry and those of the bolometer detectors. QUBIC observes the sky at two frequencies, 150 and 220 GHz, so that it can separate the cosmological signal from foreground emission, in particular thermal dust emission.

<span class="mw-page-title-main">BICEP and Keck Array</span> Series of cosmic microwave background (CMB) experiments at the South Pole

BICEP and the Keck Array are a series of cosmic microwave background (CMB) experiments. They aim to measure the polarization of the CMB; in particular, measuring the B-mode of the CMB. The experiments have had five generations of instrumentation, consisting of BICEP1, BICEP2, the Keck Array, BICEP3, and the BICEP Array. The Keck Array started observations in 2012 and BICEP3 has been fully operational since May 2016, with the BICEP Array beginning installation in 2017/18.

<span class="mw-page-title-main">POLARBEAR</span>

POLARBEAR is a cosmic microwave background polarization experiment located in the Atacama Desert of northern Chile in the Antofagasta Region. The POLARBEAR experiment is mounted on the Huan Tran Telescope (HTT) at the James Ax Observatory in the Chajnantor Science Reserve. The HTT is located near the Atacama Cosmology Telescope on the slopes of Cerro Toco at an altitude of nearly 5,200 m (17,100 ft).

<span class="mw-page-title-main">C-Band All Sky Survey</span>

The C-Band All Sky Survey (C-BASS) is a radio astronomy project that aims to map the entire sky in the C Band (5 GHz). It has been conducted on two radio telescopes, one operating in the Karoo in South Africa, the other at Owens Valley Radio Observatory in California.

<span class="mw-page-title-main">Cosmology Large Angular Scale Surveyor</span>

The Cosmology Large Angular Scale Surveyor (CLASS) is an array of microwave telescopes at a high-altitude site in the Atacama Desert of Chile as part of the Parque Astronómico de Atacama. The CLASS experiment aims to improve our understanding of cosmic dawn when the first stars turned on, test the theory of cosmic inflation, and distinguish between inflationary models of the very early universe by making precise measurements of the polarization of the Cosmic Microwave Background (CMB) over 65% of the sky at multiple frequencies in the microwave region of the electromagnetic spectrum.

<span class="mw-page-title-main">Simons Observatory</span>

The Simons Observatory is located in the high Atacama Desert in Northern Chile inside the Chajnator Science Preserve, at an altitude of 5,200 meters (17,000 ft). The Atacama Cosmology Telescope (ACT) and the Simons Array are located nearby and these experiments are currently making observations of the Cosmic Microwave Background (CMB). Their goals are to study how the universe began, what it is made of, and how it evolved to its current state. The Simons Observatory shares many of the same goals but aims to take advantage of advances in technology to make far more precise and diverse measurements. In addition, it is envisaged that many aspects of the Simons Observatory will be pathfinders for the future CMB-S4 array.

<span class="mw-page-title-main">QUIJOTE Experiment</span>

The QUIJOTE CMB Experiment is an ongoing experiment started in November 2012, and led by Rafael Rebolo López, with the goal of characterizing the polarization of the cosmic microwave background (CMB) and other galactic and extragalactic emission in the frequency range 10 to 40 GHz, at angular scales of 1°. These measurements will complement at low frequency and correct from galactic contamination those obtained by the Planck satellite from 2009 to 2013.

LiteBIRD is a planned small space observatory that aims to detect the footprint of the primordial gravitational wave on the cosmic microwave background (CMB) in a form of polarization pattern called B-mode.

References

  1. 1 2 PROVINCIA, LA (16 December 2016). "Tenerife suma un telescopio para buscar la huella del 'Big Bang' en el Universo". La Provincia - Diario de Las Palmas (in Spanish). Retrieved 16 November 2020.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 Choi, J.; Génova-Santos, R.; Hattori, M.; Hazumi, M.; Ishitsuka, H.; Kanno, F.; Karatsu, K.; Kiuchi, K.; Koyano, R.; Kutsuma, H.; Lee, K.; Mima, S.; Minowa, M.; Nagai, M.; Nagasaki, T.; Naruse, M.; Oguri, S.; Okada, T.; Otani, C.; Rebolo, R.; Rubiño-Martín, J.; Sekimoto, Y.; Suzuki, J.; Taino, T.; Tajima, O.; Tomita, N.; Uchida, T.; Won, E.; Yoshida, M. (2018). "Status of the GroundBIRD Telescope". EPJ Web of Conferences. 168: 01014. Bibcode:2018EPJWC.16801014C. doi: 10.1051/epjconf/201816801014 . ISSN   2100-014X.
  3. ↑ "ロータリージョイント | ＴＫＤ（株）武田エンジニアリング". www.takeda-eng.jp.
  4. 1 2 3 4 5 Ishitsuka, H.; Ikeno, M.; Oguri, S.; Tajima, O.; Tomita, N.; Uchida, T. (13 January 2016). "Front–End Electronics for the Array Readout of a Microwave Kinetic Inductance Detector Towards Observation of Cosmic Microwave Background Polarization". Journal of Low Temperature Physics. 184 (1–2): 424–430. Bibcode:2016JLTP..184..424I. doi:10.1007/s10909-015-1467-7. S2CID   111807277.
  5. ↑ "GroundBIRD telescope". The MagPi magazine. Retrieved 9 August 2022.
  6. 1 2 3 4 5 6 7 Oguri, S.; Choi, J.; Hazumi, M.; Kawai, M.; Tajima, O.; Won, E.; Yoshida, M. (28 February 2014). "GroundBIRD Experiment: Detecting CMB Polarization Power in a Large Angular Scale from the Ground". Journal of Low Temperature Physics. 176 (5–6): 691–697. Bibcode:2014JLTP..176..691O. doi:10.1007/s10909-014-1138-0. S2CID   121462368.
  7. 1 2 "茨城）宇宙の膨張、証拠を探せ 原子重力波観測に新装置：朝日新聞デジタル". 朝日新聞デジタル (in Japanese). Retrieved 16 November 2020.
  8. ↑ "Japón buscará evidencias del Big Bang desde el Observatorio del Teide". The Diplomat in Spain. 9 January 2017. Retrieved 16 November 2020.
  9. ↑ S.L, Titania Cía Editorial. "Experimento japonés se suma en Canarias a buscar primeros pasos del Universo - Miércoles, 14 Diciembre 2016 20:16". El Confidencial (in Spanish). Retrieved 16 November 2020.
  10. ↑ INC, SANKEI DIGITAL (27 January 2019). "【クローズアップ科学】原始重力波の証拠を探せ 宇宙誕生の謎、日本も本格観測". 産経ニュース (in Japanese). Retrieved 16 November 2020.
  11. ↑ Time, El. "El embajador de Japón en España visita el Roque de Los Muchachos". El Time (in European Spanish). Retrieved 16 November 2020.
  12. ↑ "Department Information | KASI". www.kasi.re.kr. Retrieved 26 August 2020.
  13. ↑ "About OpenIt — Open-It". openit.kek.jp. Retrieved 20 December 2019.
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