Hyper Suprime-Cam: System design and verification of image quality

Miyazaki, Satoshi; Komiyama, Yutaka; Kawanomoto, Satoshi; Doi, Yoshihiro; Furusawa, Hisanori; Hamana, Takashi; Hayashi, Yusuke; Ikeda, Hiroyuki; Kamata, Yukiko; Karoji, Hiroshi; Koike, M.; Kurakami, Tomio; Miyama, Shoken M.; Morokuma, Tomoki; Nakata, Fumiaki; Namikawa, Kazuhito; Nakaya, Hidehiko; Nariai, Kyoji; Obuchi, Yasunari; Oishi, Yukie; Okada, Norio; Okura, Yuki; Tait, Philip J.; Takata, Tadafumi; Tanaka, Yôko; Tanaka, Masayuki; Terai, Tsuyoshi; Tomono, Daigo; Uraguchi, Fumihiro; Usuda, Tomonori; Utsumi, Yousuke; Yamada, Yoshiyuki; Yamanoi, Hitomi; Aihara, H.; Fujimori, Hiroki; Mineo, Sogo; Miyatake, Hironao; Oguri, Masamune; Uchida, Tomohisa; Tanaka, M.; Yasuda, Naoki; Takada, Masahiro; Murayama, Hitoshi; Nishizawa, Atsushi J.; Sugiyama, Naoshi; Chiba, Masashi; Futamase, Toshifumi; Wang, Shiang‐Yu; Chen, Hsin Yo; Ho, P. T. P.; Liaw, Eric J.-Y.; Chiu, Chi Fang; Ho, Cheng Lin; Lai, Tsang Chih; Lee, Yao Cheng; Jeng, D. Z.; Iwamura, Satoru; Armstrong, R.; Bickerton, Steve; Bosch, James; Gunn, James E.; Lupton, Robert H.; Loomis, Craig; Price, P. A.; Smith, S.G.; Strauss, Michael A.; Turner, Edwin L.; Suzuki, H.; Miyazaki, Yasuhito; Muramatsu, Masaaki; Yamamoto, K.; Endo, Mamoru; Ezaki, Yutaka; Itô, Noboru; Kawaguchi, Noboru; Sofuku, Satoshi; Taniike, Tomoaki; Akutsu, Kotaro; Dojo, Naoto; Kasumi, Kazuyuki; Matsuda, Toru; Imoto, Kohei; Miwa, Yoshinori; Suzuki, Masayuki; Takeshi, Kunio; Yokota, Hideo

doi:10.1093/pasj/psx063

Cited by 458 publications

(209 citation statements)

References 38 publications

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“…The results presented in the previous section are predictions for the established Subaru HSC Deep field, which has a field of view of ∼ 27 deg 2 and a depth of r ∼ 27 (Miyazaki et al 2018;Ouchi et al 2018). In Figure 9 we demonstrate the effect of expanding the LAE survey in either area or depth, in combination with an SKA 21-cm survey at z = 6.6.…”

Section: Future Survey Sensitivitiesmentioning

confidence: 79%

“…(2015); Chang et al (2015). e We assume a narrowband (∆z = 0.1) survey geometry, based on Miyazaki et al (2018); Takada et al (2014). † Observing at 150 MHz.…”

Section: Reionization Historiesmentioning

confidence: 99%

“…),LOFAR (van Haarlem et al 2013),HERA (DeBoer et al 2017), and SKA1low(Waterson et al 2016) interferometers. For the LAE galaxy survey we estimate the sensitivities of a Subaru survey, using a combination of narrowband selection with the Hyper Suprime-Cam (HSC)(Miyazaki et al 2018;Ouchi et al 2018) and spectroscopy from the Prime Focus Spectrograph (PFS)(Tamura et al 2018;Takada et al 2014). We assume an LAE survey with the field of view of the HSC Subaru Strategic Program's (SSP) Deep field (which has an area of 27 deg 2 ,Miyazaki et al 2018) when calculating LAE sensitivities.…”

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confidence: 99%

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Probing delayed-end reionization histories with the 21-cm LAE cross-power spectrum

Weinberger

Kulkarni

Haehnelt

2020

Monthly Notices of the Royal Astronomical Society

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We model the 21-cm signal and LAE population evolution during the epoch of reionization in order to predict the 21cm-LAE cross-power spectrum. We employ highdynamic-range simulations of the IGM to create models that are consistent with constraints from the CMB, Lyman-α forest and LAE population statistics. Using these models we consider the evolution of the cross-power spectrum for a selection of realistic reionization histories and predict the sensitivity of current and upcoming surveys to measuring this signal. We find that the imprint of a delayed-end to reionization can be observed by future surveys, and that strong constraints can be placed on the progression of reionization as late as z = 5.7 using a Subaru-SKA survey. We make predictions for the signal-to-noise ratios achievable by combinations of Subaru/PFS with the MWA, LOFAR, HERA and SKA interferometers. We find that a Subaru-SKA survey could measure the cross-power spectrum for a late reionization at z = 6.6 with a total signal-to-noise greater than 5, making it possible to constrain both the timing and bubble size at the end of reionization. Furthermore, we find that expanding the current Subaru/PFS survey area and depth by a factor of three would double the total signal-to-noise.

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Section: Future Survey Sensitivitiesmentioning

confidence: 79%

“…(2015); Chang et al (2015). e We assume a narrowband (∆z = 0.1) survey geometry, based on Miyazaki et al (2018); Takada et al (2014). † Observing at 150 MHz.…”

Section: Reionization Historiesmentioning

confidence: 99%

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confidence: 99%

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Probing delayed-end reionization histories with the 21-cm LAE cross-power spectrum

Weinberger

Kulkarni

Haehnelt

2020

Monthly Notices of the Royal Astronomical Society

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“…To study AGN variability on decade timescales, we identified AGN from the SDSS (York et al 2000) DR7 Quasar catalog (Schneider et al 2010) that were also observed later by the Hyper Suprime-Cam (HSC; Miyazaki et al 2018) Subaru Strategic imaging survey. The SDSS survey used a dedicated 2.5 m (Gunn et al 2006) telescope at Apache Point Observatory to obtain images in five optical bands (ugriz) over a large patch (∼10000 deg 2 ) of the northern sky.…”

Section: Datamentioning

confidence: 99%

Observational Nonstationarity of AGN Variability: The Only Way to Go Is Down!

Čaplar

Peña

Johnson

et al. 2020

ApJL

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To gain insights into long-term variability of Active Galactic Nuclei (AGN), we analyze an AGN sample from the Sloan Digital Sky Survey (SDSS) and compare their photometry with observations from the Hyper Suprime-Cam survey (HSC) observed 14.85 years after SDSS. On average, the AGN are fainter in HSC than SDSS. We demonstrate that the difference is not due to subtle differences in the SDSS versus HSC filters or photometry. The decrease in mean brightness is redshift dependent, consistent with expectations for a change that is a function of the rest-frame time separation between observations. At a given redshift, the mean decrease in brightness is stronger for more luminous AGN and for objects with longer time separation between measurements. We demonstrate that the dependence on redshift and luminosity of measured mean brightness decrease is consistent with simple models of Eddington ratio variability in AGN on long (Myr, Gyr) timescales. We show how our results can be used to constrain the variability and demographic properties of AGN populations.

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“…In our companion papers (Chiu et al 2018;Sereno et al 2018), we explicitly account for the effects of triaxiality in forwardmodeling our multiprobe data sets, simultaneously constraining the cluster mass, concentration, triaxial shape, and orientation from Bayesian inference. Extending this analysis with large, well-controlled samples of clusters from ongoing and planned surveys, such as the XXL survey Pierre et al 2016), the Subaru Hyper Suprime-Cam survey (Mandelbaum et al 2018;Miyazaki et al 2018aMiyazaki et al , 2018bOguri et al 2018), the Dark Energy Survey, and the WFIRST and Euclid missions, will be a significant step forward in understanding the tidal and evolutionary effects of surrounding LSS on the intracluster mass distribution.…”

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confidence: 99%

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

Umetsu

Sereno

Tam

et al. 2018

ApJ

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We reconstruct the two-dimensional (2D) matter distributions in 20 high-mass galaxy clusters selected from the CLASH survey by using the new approach of performing a joint weak gravitational lensing analysis of 2D shear and azimuthally averaged magnification measurements. This combination allows for a complete analysis of the field, effectively breaking the mass-sheet degeneracy. In a Bayesian framework, we simultaneously constrain the mass profile and morphology of each individual cluster, assuming an elliptical Navarro-Frenk-White halo characterized by the mass, concentration, projected axis ratio, and position angle (PA) of the projected major axis. We find that spherical mass estimates of the clusters from azimuthally averaged weak-lensing measurements in previous work are in excellent agreement with our results from a full 2D analysis. Combining all 20 clusters in our sample, we detect the elliptical shape of weak-lensing halos at the 5σ significance level within a scale of 2 h Mpc 1 -. The median projected axis ratio is 0.67±0.07 at a virial mass of M M 15.2 2.8 10 vir 14 = ´ ( ) , which is in agreement with theoretical predictions from recent numerical simulations of the standard collisionless cold dark matter model. We also study misalignment statistics of the brightest cluster galaxy, X-ray, thermal Sunyaev-Zel'dovich effect, and strong-lensing morphologies with respect to the weak-lensing signal. Among the three baryonic tracers studied here, we find that the X-ray morphology is best aligned with the weak-lensing mass distribution, with a median misalignment angle of PA 21We also conduct a stacked quadrupole shear analysis of the 20 clusters assuming that the X-ray major axis is aligned with that of the projected mass distribution. This yields a consistent axis ratio of 0.67±0.10, suggesting again a tight alignment between the intracluster gas and dark matter.

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Hyper Suprime-Cam: System design and verification of image quality

Cited by 458 publications

References 38 publications

Probing delayed-end reionization histories with the 21-cm LAE cross-power spectrum

Probing delayed-end reionization histories with the 21-cm LAE cross-power spectrum

Observational Nonstationarity of AGN Variability: The Only Way to Go Is Down!

The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters*

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