Subaru Prime Focus Camera — Suprime-Cam

By S. Miyazaki, Y. Komiyama, M. Sekiguchi, S. Okamura, M. Doi, H. Furusawa, M. Hamabe, K. Imi, Masahiki Kimura, F. Nakata and 5 more. 2002

641 citations recorded by the source corpus.

We have built an 80-mega pixels (10240 ×8192) mosaic CCD camera, called Suprime-Cam, for the wide-field prime focus of the 8.2m Subaru telescope. Suprime-Cam covers a field of view 34 � ×27 � , a unique facility among the 8-10m class telescopes, with a resolution of 0. �� 202 per pixel. The focal plane consists of ten high-resistivity 2k ×4k CCDs developed by MIT Lincoln Laboratory, which are cooled by a large Stirling-cycle cooler. The CCD readout electronics was designed to be scalable, which allows the multiple read-out of tens of CCDs. It takes 50 seconds to readout entire arrays. We designed a filter-exchange mechanism of the jukebox type that can hold up to ten large filters (205 ×170 ×15mm 3 ). The wide-field corrector is basically a three-lens Wynne-type, but has a new type of atmospheric dispersion corrector. The corrector provides a flat focal plane and an un-vignetted field of view of 30 � in diameter. The achieved co-planarity of the focal array mosaic is smaller than 30 µm peak-to-peak, which realizes mostly the seeing limited image over the entire field. The median seeing in the Ic-band, measured over one year and ah alf, is 0. 61. The PSF anisotropy in Suprime-Cam images, estimated by stellar ellipticities, is about 2% under this median seeing condition. At the time of commissioning, Suprime-Cam had the largest survey speed, which is defined as the field of view multiplied by the primary mirror area of the telescope, among those cameras built for

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

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Citations in the corpus

Large-Scale Structure of Emission-Line Galaxies at z = 3.1 (2004, methodology): “5 sample, are distributed in the Suprime-Cam field as shown in Figure 2 ( filled black circles).”
Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “In this paper, we present a systematic study of strong and weak lensing analysis for a sample of 28 clusters from the SGAS, based on our extensive follow-up imaging observations with Subaru/Suprime-cam (Miyazaki et al. 2002).”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, methodology): “We verify and calibrate the shear pipeline using simulated images from the STEP2 project (Massey et al. 2007), which were designed to mimic the depth, sampling, and PSF typical of SuprimeCam data (Figure 3).”
A DOZEN NEW GALAXIES CAUGHT IN THE ACT: GAS STRIPPING AND EXTENDED EMISSION LINE REGIONS IN THE COMA CLUSTER (2010, positive): “We thank Dr. Russel J. Smith for information on their gaseous stripping event galaxies and the suggestive comments, Dr. H. Yamanoi for discussion on the photometric calibration of the Suprime-Cam data, and Dr. M. Sun for informing us about their latest results.”
Identification of the brightest Lyα emitters at z = 6.6 : Implications for the evolution of the luminosity function in the reionization era (2015, methodology): “Optical imaging data was obtained with Subaru’s Suprime-Cam (Miyazaki et al. 2002) using the NB921 narrow-band filter (Fig.”
The Hyper Suprime-Cam SSP Survey: Overview and Survey Design (2017, background): “SuprimeCam (Miyazaki et al. 2002), with its ∼ 0.25deg2 field of view and superb delivered image quality (routinely 0.6′′ FWHM), has been a world leader in wide-field studies of the distant narrow-band filters lie in relatively dark regions of the sky spectrum. and faint Universe (e.g., Iye et al.…”
The Environmental Dependence of Galaxy Properties in the Local Universe: Dependences on Luminosity, Local Density, and System Richness (2004, background): “With the wide-field camera Suprime-Cam on the Subaru Telescope (Miyazaki et al. 2002), Kodama et al. (2001) identified galaxy groups surrounding the A851 cluster (z = 0.41).”
FOCAS: faint object camera and spectrograph for the Subaru Telescope (2000, methodology): “The quantum efficiency of the CCD is presented in Miyazaki et al. (2002).”
CATALOG OF ULTRA-DIFFUSE GALAXIES IN THE COMA CLUSTERS FROM SUBARU IMAGING DATA (2016, methodology): “Stimulated by this work, Koda et al. (2015) revisited the Coma cluster data (Okabe et al. 2014) obtained with the Subaru Prime Focus Camera (Suprime-Cam; Miyazaki et al. 2002) on the Subaru telescope (Iye et al. 2004).”
The SUBARU Deep Field Project: Lymanα Emitters at a Redshift of 6.6 (2004, neutral): “′′202 pixel−1 (Miyazaki et al. 2002) on the 8.2 m Subaru Telescope (Kaifu et al. 2000; Iye et al. 2004).”
A Subaru Search for Lyα Blobs in and around the Protocluster Region At Redshift z = 3.1 (2004, methodology): “The raw data are the same as presented in H04 and were reduced with IRAF and a custom software developed for Suprime-Cam data reduction (Yagi et al. 2002; Ouchi et al. 2003) in a manner similar to that presented in H04.”
APPROXIMATELY A THOUSAND ULTRA-DIFFUSE GALAXIES IN THE COMA CLUSTER (2015, methodology): “Yamanoi et al. (2012) used the Subaru Prime Focus Camera (SuprimeCam; Miyazaki et al. 2002) on the Subaru telescope and derived a galaxy luminosity function down to MR ∼ −10 in Coma.”
Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies (2017, methodology): “Galaxy sizes and ellipticities are drawn from distributions fit to SuprimeCam i ′ -band data (Miyazaki et al. 2002).”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, methodology): “The SuprimeCam filter set resembles the SDSSr+ and i+ filters more so than tradition Johnson-Cousin filters5.”
PRIMUS: THE DEPENDENCE OF AGN ACCRETION ON HOST STELLAR MASS AND COLOR (2011, methodology): “…we use BJVJg +r+i+z+ imaging obtained with the 10 http://www.cfht.hawaii.edu/Science/CFHLS Suprime-Cam instrument on the Subaru 8.2m telescope (Miyazaki et al. 2002), u∗ and i∗ imaging from Megacam on the CFHT, and Ks imaging from the Widefield Infrared Camera at the CFHT (McCracken et al.…”