The APEX-SZ Instrument
Daniel SchwanP. A. R. AdeKaustuv BasuA. N. BenderFrank BertoldiHsaio-Mei ChoG. ChonJohn ClarkeM. DobbsD. FerruscaR. GüstenN. W. HalversonW. L. HolzapfelC. HorellouDaniel JohanssonBradley R. JohnsonJames E. KennedyZ. KermishR. KneißlT. LantingAdrian T. LeeM. LuekerJ. MehlK. M. MentenD. MudersF. PacaudT. PlaggeC. L. ReichardtPaul L. RichardsRienhold SchaafP. SchilkeMartin W. SommerH. G. SpielerC. TuckerA. WeißBenjamin WestbrookO. Zahn
3
Citation
31
Reference
19
Related Paper
Citation Trend
Abstract:
The Atacama pathfinder experiment Sunyaev-Zel'dovich (APEX-SZ) instrument is a millimeter-wave cryogenic receiver designed to observe galaxy clusters via the Sunyaev-Zel'dovich effect from the 12 m APEX telescope on the Atacama plateau in Chile. The receiver contains a focal plane of 280 superconducting transition-edge sensor (TES) bolometers instrumented with a frequency-domain multiplexed readout system. The bolometers are cooled to 280 mK via a three-stage helium sorption refrigerator and a mechanical pulse-tube cooler. Three warm mirrors, two 4 K lenses, and a horn array couple the TES bolometers to the telescope. APEX-SZ observes in a single frequency band at 150 GHz with 1' angular resolution and a 22' field-of-view, all well suited for cluster mapping. The APEX-SZ receiver has played a key role in the introduction of several new technologies including TES bolometers, the frequency-domain multiplexed readout, and the use of a pulse-tube cooler with bolometers. As a result of these new technologies, the instrument has a higher instantaneous sensitivity and covers a larger field-of-view than earlier generations of Sunyaev-Zel'dovich instruments. The TES bolometers have a median sensitivity of 890 uKcmb-sqrt(s) (NEy of 3.5e-4 sqrt(s)). We have also demonstrated upgraded detectors with improved sensitivity of 530 uKcmb-sqrt(s) (NEy of 2.2e-4 sqrt(s)). Since its commissioning in April 2007, APEX-SZ has been used to map 48 clusters. We describe the design of the receiver and its performance when installed on the APEX telescope.Keywords:
South Pole Telescope
Transition edge sensor
Cite
The Advanced Atacama Cosmology Telescope Polarimeter (AdvACT) is an upgraded instrument for the Atacama Cosmology Telescope, which uses transition-edge sensor (TES) detector arrays to measure cosmic microwave background (CMB) polarization anisotropies in multiple frequency bands. We review the integration and characterization of the final polarimeter array, which is the low frequency (LF) array, consisting of 292 TES bolometers observing in two bands centered at 27 GHz and 39 GHz. This array is sensitive to synchrotron radiation from our galaxy as well as to the CMB, and complements the AdvACT arrays operating at 90, 150 and 230 GHz to provide robust detection and removal of foreground contamination. We present detector parameters for the LF array measured in the lab, including saturation powers, critical temperatures, thermal conductivities, time constants and optical efficiencies, and their uniformity across the entire wafer.
Polarimeter
Transition edge sensor
South Pole Telescope
Cosmic background radiation
Cite
Citations (11)
The Atacama Cosmology Telescope (ACT) aims to measure the Cosmic Microwave Background (CMB) temperature anisotropies on arcminute scales. The primary receiver for ACT is the Millimeter Bolometer Array Camera (MBAC). The MBAC is comprised of three 32×32 transition edge sensor (TES) bolometer arrays, each observing the sky with an independent set of band-defining filters. The MBAC arrays will be the largest pop-up detector arrays fielded, and among the largest TES arrays built. Prior to its assembly into an array and installation into the MBAC, a column of 32 bolometers is tested at ~ 0.4 K in a quick-turn-around dip probe. In this paper we describe the properties of the ACT bolometers as revealed by data from those tests, emphasizing a characterization that accounts for both the complex impedance and the noise as a function of frequency.
Transition edge sensor
South Pole Telescope
Cite
Citations (21)
We describe the recent reoptimization of the detector array in the APEX‐SZ receiver, which is currently operating at the APEX telescope in Chile. APEX‐SZ is designed to image the Sunyaev Zel'dovich effect (SZE). Observations are made in a single spectral band centered on 150 GHz, which is where the decrement of the SZE peaks. The APEX‐SZ transition‐edge sensor bolometers are micro‐fabricated in six 55‐element sub arrays, which combine to form the full 330‐element focal plane operating at 280 mK. We report on the newest generation of sub‐arrays that use a λ/4 silicon‐filled backshort. Compared to the first generation array which used a 3λ/4 backshort, the new arrays have a broader bandwidth and an increased optical efficiency. We present spectral bandpass and efficiency measurements and compare these to electromagnetic simulations of the bolometer absorption. The overall improvement in optical coupling reduces the noise equivalent temperature (NET) of each bolometer by a factor of approximately 1.5. Several galaxy clusters have been observed using the new detectors and analysis of the data is currently underway. We also present plans for future upgrades to the receiver.
Transition edge sensor
Cite
Citations (3)
The Atacama Cosmology Telescope was designed to measure small-scale anisotropies in the Cosmic Microwave Background and detect galaxy clusters through the Sunyaev-Zel'dovich effect. The instrument is located on Cerro Toco in the Atacama Desert, at an altitude of 5190 meters. A six-meter off-axis Gregorian telescope feeds a new type of cryogenic receiver, the Millimeter Bolometer Array Camera. The receiver features three 1000-element arrays of transition-edge sensor bolometers for observations at 148 GHz, 218 GHz, and 277 GHz. Each detector array is fed by free space mm-wave optics. Each frequency band has a field of view of approximately 22' x 26'. The telescope was commissioned in 2007 and has completed its third year of operations. We discuss the major components of the telescope, camera, and related systems, and summarize the instrument performance.
South Pole Telescope
Transition edge sensor
Instrumentation
Cite
Citations (215)
We summarize the fabrication, flight qualification, and dark performance of bolometers completed at the Jet Propulsion Laboratory for the High Frequency Instrument (HFI) of the joint ESA/NASA Herschel/Planck mission to be launched in 2009. The HFI is a multicolor focal plane which consists of 52 bolometers operated at 100 mK. Each bolometer is mounted to a feedhorn-filter assembly which defines one of six frequency bands centered between 100-857 GHz. Four detectors in each of five bands from 143-857 GHz are coupled to both linear polarizations and thus measure the total intensity. In addition, eight detectors in each of four bands (100, 143, 217, and 353 GHz) couple only to a single linear polarization and thus provide measurements of the Stokes parameters, Q and U, as well as the total intensity. The measured noise equivalent power (NEP) of all detectors is at or below the background limit for the telescope and time constants are a few ms, short enough to resolve point sources as the 5 to 9 arc min beams move across the sky at 1 rpm.
Jet propulsion
Cite
Citations (38)
The Advanced Atacama Cosmology Telescope Polarimeter (AdvACT) \cite{thornton} is an upgrade for the Atacama Cosmology Telescope using Transition Edge Sensor (TES) detector arrays to measure cosmic microwave background (CMB) temperature and polarization anisotropies in multiple frequencies. The low frequency (LF) array was deployed early 2020. It consists of 292 TES bolometers observing in two bands centered at 27 GHz and 39 GHz. At these frequencies, it is sensitive to synchrotron radiation from our galaxy as well as to the CMB, and complements the AdvACT arrays operating at 90, 150 and 230 GHz. We present the initial LF array on-site characterization, including the time constant, optical efficiency and array sensitivity.
Polarimeter
Transition edge sensor
South Pole Telescope
Cosmic background radiation
Cite
Citations (4)
Views Icon Views Article contents Figures & tables Video Audio Supplementary Data Peer Review Share Icon Share Twitter Facebook Reddit LinkedIn Tools Icon Tools Reprints and Permissions Cite Icon Cite Search Site Citation Dominic J. Benford, Johannes G. Staguhn, Christine A. Jhabvala, Catherine T. Marx, Elmer H. Sharp, Stephen F. Maher; Design of the Millimeter‐Wavelength Superconducting Bolometer Camera GISMO. AIP Conf. Proc. 16 December 2009; 1185 (1): 546–550. https://doi.org/10.1063/1.3292401 Download citation file: Ris (Zotero) Reference Manager EasyBib Bookends Mendeley Papers EndNote RefWorks BibTex toolbar search Search Dropdown Menu toolbar search search input Search input auto suggest filter your search All ContentAIP Publishing PortfolioAIP Conference Proceedings Search Advanced Search |Citation Search
Icon
Download
Cite
Citations (0)
We have made a submillimeter-wave telescope for a Japanese sounding rocket, -520-17, which is dedicated for an observation of cold dust in Orion molecular cloud region. The submillimeter-wave telescope was launched on January 23, 1995. The telescope include an off-axis Gregorian telescope with aperture of 30cm, focal plane bolometer array, cryogenic cooling system down to 0.3K, and a star sensor using charge modulation device. A very low emissivity optical arrangement of less than 1% is achieved using pure aluminum mirror, off axis reflector and cold optics. Single moded conical feed horn is effectively coupled with bolometers with efficiency of more than 90%. The focal plane array consists of 12-element bolometers, six for 250 micrometers observation and six for 500 micrometers observation. NEPs of the bolometers are 5 X 10-17 W/(root)Hz which is read out by AC bridge read-out circuit. Total system gives sensitivities of about 10-12 W/cm2 (DOT) sr for diffuse objects or 2Jy for compact objects at 500 micrometers over 100deg2 region with a beam size of 10arcmin. This observation should give unique data on cold dust distribution, which is believed to dominate the dust mass distributional, over Orion Molecular Cloud region. Also discussed in the last section is a development of array detectors for future space mission in far-infrared and submillimeter-wave region.
South Pole Telescope
Reflecting telescope
Aperture (computer memory)
Cite
Citations (0)
The Simons Array is a set of three millimeter-wavelength telescopes in the Atacama Desert in northern Chile. It is designed to measure the polarization of the cosmic microwave background caused by density perturbations, gravitational lensing, and primordial gravitational waves. Polarbear-2b (PB-2b) is the receiver that will be mounted onto the Paul Simons Telescope, the second Simons Array telescope. Each pixel in the PB-2b focal plane has a broadband sinuous antenna coupled to transition-edge sensor (TES) bolometers. In all, there are more than 7,500 antenna-coupled TES bolometers which are biased and read out using a digital frequency-domain multiplexing framework. We implement a multiplexing factor of 40 with resonator frequencies ranging from 1.6 MHz to 4.6 MHz. These resonators are connected to superconducting quantum interference device arrays that provide a signal amplification stage. We present Polarbear-2b detector and readout characterization results from in-lab testing that enabled the deployment of PB-2b to Chile in March 2020.
Transition edge sensor
South Pole Telescope
Cite
Citations (2)
We describe a close-packed, two-dimensional imaging detector system for operation at 90GHz (3.3mm) for the 100 m Green Bank Telescope (GBT) This system will provide high sensitivity (<1mjy in 1s rapid imaging (15'x15' to 250 microJy in 1 hr) at the world's largest steerable aperture. The heart of this camera is an 8x8 close packed, Nyquist-sampled array of superconducting transition edge sensor bolometers. We have designed and are producing a functional superconducting bolometer array system using a monolithic planar architecture and high-speed multiplexed readout electronics. With an NEP of approx. 2.10(exp 17) W/square root Hz, the TES bolometers will provide fast linear sensitive response for high performance imaging. The detectors are read out by and 8x8 time domain SQUID multiplexer. A digital/analog electronics system has been designed to enable read out by SQUID multiplexers. First light for this instrument on the GBT is expected within a year.
Transition edge sensor
Cite
Citations (0)