Subaru Prime Focus Camera — Suprime-Cam

Miyazaki, Satoshi; Komiyama, Yutaka; Sekiguchi, M.; Okamura, S.; Doi, Mamoru; Furusawa, Hisanori; Hamabe, M.; Imi, Katsumi; Kimura, Masahiko; Nakata, Fumiaki; Okada, Norio; Ouchi, Masami; Shimasaku, Kazuhiro; Yagi, Masafumi; Yasuda, Naoki

doi:10.1093/pasj/54.6.833

Cited by 669 publications

(496 citation statements)

References 30 publications

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“…These SDF data were acquired with Suprime-Cam (Miyazaki et al 2002), the optical imager mounted at the prime focus of the Subaru telescope, between 2001 March and 2007 May. The acquisition and reduction of these data have been discussed extensively in Kashikawa et al (2004Kashikawa et al ( , 2006, Ly et al (2007;hereafter Ly07), as well as in Ly et al (2012b) for the narrowband data, and in Nagao et al (2008) for the intermediate-band data.…”

Section: The Subaru Deep Fieldmentioning

confidence: 99%

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

Ly¹,

Malhotra²,

Malkan³

et al. 2016

ApJS

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Deep rest-frame optical spectroscopy is critical for characterizing and understanding the physical conditions and properties of the ionized gas in galaxies. Here, we present a new spectroscopic survey called "Metal Abundances across Cosmic Time" or  , which will obtain rest-frame optical spectra for ∼3000 emission-line galaxies. This paper describes the optical spectroscopy that has been conducted with MMT/Hectospec and Keck/DEIMOS for ≈1900 z = 0.1-1 emission-line galaxies selected from our narrowband and intermediate-band imaging in the Subaru Deep Field. In addition, we present a sample of 164 galaxies for which we have measured the weak [O III] λ4363 line (66 with at least 3σ detections and 98 with significant upper limits). This nebular emission line determines the gas-phase metallicity by measuring the electron temperature of the ionized gas. This paper presents the optical spectra, emission-line measurements, interstellar properties (e.g., metallicity, gas density), and stellar properties (e.g., star formation rates, stellar mass). Paper II of the  survey (Ly et al.) presents the first results on the stellar mass-gas metallicity relation at z1 using the sample with [O III]λ4363 measurements.

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Section: The Subaru Deep Fieldmentioning

confidence: 99%

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

Ly¹,

Malhotra²,

Malkan³

et al. 2016

ApJS

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“…The Suprime-Cam camera is a mosaic of ten 2k ×4k CCDs with a pixel scale of 0.202 arcsec pix −1 , and it covers an area of 34 × 27 per field (Miyazaki et al 2002). The field-of-view corresponds to a physical scale of 624×458 kpc at the distance of NGC 6482, reaching the virial radius at the field edges.…”

Section: Observationsmentioning

confidence: 99%

A normal abundance of faint satellites in the fossil group NGC 6482

Lieder¹,

Mieske²,

Sánchéz-Janssen³

et al. 2013

A&A

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A fossil group is considered the end product in a galaxy group's evolution. It is a massive central galaxy that dominates the luminosity budget of the group, and is the outcome of efficient merging between intermediate-luminosity members. Little is known, however, about the faint satellite systems of fossil groups. Here we present a Subaru/Suprime-Cam wide-field, deep imaging study in the B− and R−bands of the nearest fossil group NGC 6482 (M tot ∼ 4 × 10 12 M ), covering the virial radius out to 310 kpc. We performed detailed completeness estimations and selected group member candidates by a combination of automated object detection and visual inspection. A fiducial sample of 48 member candidates down to M R ∼ −10.5 mag is detected, making this study the deepest of a fossil group to now. We investigate the photometric scaling relations, the color-magnitude relation, and the luminosity function of our galaxy sample. We find evidence of recent and ongoing merger events among bright group galaxies. The color-magnitude relation is comparable to that of nearby galaxy clusters, and it exhibits significant scatter at the faintest luminosities. The completeness-corrected luminosity function is dominated by early-type dwarfs and is characterized by a faint end slope α = −1.32 ± 0.05. We conclude that the NGC 6482 fossil group shows photometric properties consistent with those of regular galaxy clusters and groups, including a normal abundance of faint satellites.

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“…The ELAIS-N1 field will also be targeted with Subaru Hyper Suprime-Cam (Miyazaki et al 2002) to search for high-redshift Lyα emitters (LAEs). With a significant number of detected LAEs one could in principle study reionization using both the shape and normalization of the cross-power spectrum between the galaxies and EoR (e.g.…”

Section: Introductionmentioning

confidence: 99%

Initial LOFAR observations of epoch of reionization windows

Jelić

Bruyn

Mevius

et al. 2014

A&A

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Aims. This study aims to characterise the polarized foreground emission in the ELAIS-N1 field and to address its possible implications for extracting of the cosmological 21 cm signal from the LOw-Frequency ARray -Epoch of Reionization (LOFAR-EoR) data. Methods. We used the high band antennas of LOFAR to image this region and RM-synthesis to unravel structures of polarized emission at high Galactic latitudes. Results. The brightness temperature of the detected Galactic emission is on average ∼4 K in polarized intensity and covers the range from -10 to +13 rad m −2 in Faraday depth. The total polarized intensity and polarization angle show a wide range of morphological features. We have also used the Westerbork Synthesis Radio Telescope (WSRT) at 350 MHz to image the same region. The LOFAR and WSRT images show a similar complex morphology at comparable brightness levels, but their spatial correlation is very low. The fractional polarization at 150 MHz, expressed as a percentage of the total intensity, amounts to ≈1.5%. There is no indication of diffuse emission in total intensity in the interferometric data, in line with results at higher frequencies Conclusions. The wide frequency range, high angular resolution, and high sensitivity make LOFAR an exquisite instrument for studying Galactic polarized emission at a resolution of ∼1-2 rad m −2 in Faraday depth. The different polarized patterns observed at 150 MHz and 350 MHz are consistent with different source distributions along the line of sight wring in a variety of Faraday thin regions of emission. The presence of polarized foregrounds is a serious complication for epoch of reionization experiments. To avoid the leakage of polarized emission into total intensity, which can depend on frequency, we need to calibrate the instrumental polarization across the field of view to a small fraction of 1%.

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Subaru Prime Focus Camera — Suprime-Cam

Cited by 669 publications

References 30 publications

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

A normal abundance of faint satellites in the fossil group NGC 6482

Initial LOFAR observations of epoch of reionization windows

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