40 results on '"Murata, Ryoma"'
Search Results
2. The Richness-to-Mass Relation of CAMIRA Galaxy Clusters from Weak-lensing Magnification in the Subaru Hyper Suprime-Cam Survey
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Chiu, I-Non, Umetsu, Keiichi, Murata, Ryoma, Medezinski, Elinor, and Oguri, Masamune
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present a statistical weak-lensing magnification analysis on an optically selected sample of 3029 \texttt{CAMIRA} galaxy clusters with richness $N>15$ at redshift $0.2\leq z <1.1$ in the Subaru Hyper Suprime-Cam (HSC) survey. We use two distinct populations of color-selected, flux-limited background galaxies, namely the low-$z$ and high-$z$ samples at mean redshifts of $\approx1.1$ and $\approx1.4$, respectively, from which to measure the weak-lensing magnification signal by accounting for cluster contamination as well as masking effects. Our magnification bias measurements are found to be uncontaminated according to validation tests against the "null-test" samples for which the net magnification bias is expected to vanish. The magnification bias for the full \texttt{CAMIRA} sample is detected at a significance level of $9.51\sigma$, which is dominated by the high-$z$ background. We forward-model the observed magnification data to constrain the normalization of the richness-to-mass ($N$--$M$) relation for the \texttt{CAMIRA} sample with informative priors on other parameters. The resulting scaling relation is $N\propto {M_{500}}^{0.92\pm0.13} (1 + z)^{-0.48\pm0.69}$, with a characteristic richness of $N=\left(17.72\pm2.60\right)$ and intrinsic log-normal scatter of $0.15\pm0.07$ at $M_{500} = 10^{14}h^{-1}M_{\odot}$. With the derived $N$--$M$ relation, we provide magnification-calibrated mass estimates of individual \texttt{CAMIRA} clusters, with the typical uncertainty of $\approx39\%$ and $\approx32\%$ at richness$\approx20$ and $\approx40$, respectively. We further compare our magnification-inferred $N$--$M$ relation with those from the shear-based results in the literature, finding good agreement., Comment: 24 pages, 16 figures. Accepted for publication in the MNRAS
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- 2019
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3. Second Data Release of the Hyper Suprime-Cam Subaru Strategic Program
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Aihara, Hiroaki, AlSayyad, Yusra, Ando, Makoto, Armstrong, Robert, Bosch, James, Egami, Eiichi, Furusawa, Hisanori, Furusawa, Junko, Goulding, Andy, Harikane, Yuichi, Hikage, Chiaki, Ho, Paul T. P., Hsieh, Bau-Ching, Huang, Song, Ikeda, Hiroyuki, Imanishi, Masatoshi, Ito, Kei, Iwata, Ikuru, Jaelani, Anton T., Kakuma, Ryota, Kawana, Kojiro, Kikuta, Satoshi, Kobayashi, Umi, Koike, Michitaro, Komiyama, Yutaka, Li, Xiangchong, Liang, Yongming, Lin, Yen-Ting, Luo, Wentao, Lupton, Robert, Lust, Nate B., MacArthur, Lauren A., Matsuoka, Yoshiki, Mineo, Sogo, Miyatake, Hironao, Miyazaki, Satoshi, More, Surhud, Murata, Ryoma, Namiki, Shigeru V., Nishizawa, Atsushi J., Oguri, Masamune, Okabe, Nobuhiro, Okamoto, Sakurako, Okura, Yuki, Ono, Yoshiaki, Onodera, Masato, Onoue, Masafusa, Osato, Ken, Ouchi, Masami, Shibuya, Takatoshi, Strauss, Michael A., Sugiyama, Naoshi, Suto, Yasushi, Takada, Masahiro, Takagi, Yuhei, Takata, Tadafumi, Takita, Satoshi, Tanaka, Masayuki, Terai, Tsuyoshi, Toba, Yoshiki, Uchiyama, Hisakazu, Utsumi, Yousuke, Wang, Shiang-Yu, Wang, Wenting, and Yamada, Yoshihiko
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Solar and Stellar Astrophysics - Abstract
This paper presents the second data release of the Hyper Suprime-Cam Subaru Strategic Program, a wide-field optical imaging survey on the 8.2 meter Subaru Telescope. The release includes data from 174 nights of observation through January 2018. The Wide layer data cover about 300 deg^2 in all five broadband filters (grizy) to the nominal survey exposure (10min in gr and 20min in izy). Partially observed areas are also included in the release; about 1100 deg^2 is observed in at least one filter and one exposure. The median seeing in the i-band is 0.6 arcsec, demonstrating the superb image quality of the survey. The Deep (26 deg^2) and UltraDeep (4 deg^2) data are jointly processed and the UltraDeep-COSMOS field reaches an unprecedented depth of i~28 at 5 sigma for point sources. In addition to the broad-bands, narrow-band data are also available in the Deep and UltraDeep fields. This release includes a major update to the processing pipeline, including improved sky subtraction, PSF modeling, object detection, and artifact rejection. The overall data quality has been improved, but this release is not without problems; there is a persistent deblender problem as well as new issues with masks around bright stars. The user is encouraged to review the issue list before utilizing the data for scientific explorations. All the image products as well as catalog products are available for download. The catalogs are also loaded to a database, which provides an easy interface for users to retrieve data for objects of interest. In addition to these main data products, detailed galaxy shape measurements withheld from the Public Data Release 1 (PDR1) are now available to the community. The shape catalog is drawn from the S16A internal release, which has a larger area than PDR1 (160 deg^2). All products are available at the data release site, https://hsc-release.mtk.nao.ac.jp/., Comment: 26 pages, 23 figures, accepted for publication in PASJ. Data available at https://hsc-release.mtk.nao.ac.jp/
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- 2019
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4. The mass-richness relation of optically-selected clusters from weak gravitational lensing and abundance with Subaru HSC first-year data
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Murata, Ryoma, Oguri, Masamune, Nishimichi, Takahiro, Takada, Masahiro, Mandelbaum, Rachel, More, Surhud, Shirasaki, Masato, Nishizawa, Atsushi J., and Osato, Ken
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Constraining the relation between the richness $N$ and the halo mass $M$ over a wide redshift range for optically-selected clusters is a key ingredient for cluster-related science in optical surveys, including the Subaru Hyper Suprime-Cam (HSC) survey. We measure stacked weak lensing profiles around 1747 HSC CAMIRA clusters over a redshift range of $0.1\leq z_{\rm cl}\leq 1.0$ with $N\geq 15$ using the HSC first-year shear catalog covering $\sim$$140$ ${\rm deg^2}$. The exquisite depth and image quality of the HSC survey allow us to measure lensing signals around the high-redshift clusters at $0.7\leq z_{\rm cl}\leq 1.0$ with a signal-to-noise ratio of 19 in the comoving radius range $0.5\lesssim R\lesssim 15 h^{-1}{\rm Mpc}$. We constrain richness-mass relations $P(\ln N|M,z)$ of the HSC CAMIRA clusters assuming a log-normal distribution without informative priors on model parameters, by jointly fitting to the lensing profiles and abundance measurements under both Planck and WMAP cosmological models. We show that our model gives acceptable $p$-values when we add redshift dependent terms which are proportional to $\ln (1+z)$ and $[\ln (1+z)]^{2}$ into the mean and scatter relations of $P(\ln N|M,z)$. Such terms presumably originate from the variation of photometric redshift errors as a function of the redshift. We show that the constraints on the mean relation $\langle M|N \rangle$ are consistent between the Planck and WMAP models, whereas the scatter values $\sigma_{\ln M|N}$ for the Planck model are systematically larger than those for the WMAP model. We also show that the scatter values for the Planck model increase toward lower richness values, whereas those for the WMAP model are consistent with constant values as a function of richness. This result highlights the importance of the scatter in the mass-richness relation for cluster cosmology., Comment: 31 pages, 14 figures, 3 tables. v2 matches accepted version that will be published in PASJ (minor changes from v1)
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- 2019
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5. Dark Quest. I. Fast and Accurate Emulation of Halo Clustering Statistics and Its Application to Galaxy Clustering
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Nishimichi, Takahiro, Takada, Masahiro, Takahashi, Ryuichi, Osato, Ken, Shirasaki, Masato, Oogi, Taira, Miyatake, Hironao, Oguri, Masamune, Murata, Ryoma, Kobayashi, Yosuke, and Yoshida, Naoki
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We perform an ensemble of $N$-body simulations with $2048^3$ particles for 101 flat $w$CDM cosmological models sampled based on a maximin-distance Sliced Latin Hypercube Design. By using the halo catalogs extracted at multiple redshifts in the range of $z=[0,1.48]$, we develop Dark Emulator, which enables fast and accurate computations of the halo mass function, halo-matter cross-correlation, and halo auto-correlation as a function of halo masses, redshift, separations and cosmological models, based on the Principal Component Analysis and the Gaussian Process Regression for the large-dimensional input and output data vector. We assess the performance of the emulator using a validation set of $N$-body simulations that are not used in training the emulator. We show that, for typical halos hosting CMASS galaxies in the Sloan Digital Sky Survey, the emulator predicts the halo-matter cross correlation, relevant for galaxy-galaxy weak lensing, with an accuracy better than $2\%$ and the halo auto-correlation, relevant for galaxy clustering correlation, with an accuracy better than $4\%$. We give several demonstrations of the emulator. It can be used to study properties of halo mass density profiles such as the mass-concentration relation and splashback radius for different cosmologies. The emulator outputs can be combined with an analytical prescription of halo-galaxy connection such as the halo occupation distribution at the equation level, instead of using the mock catalogs, to make accurate predictions of galaxy clustering statistics such as the galaxy-galaxy weak lensing and the projected correlation function for any model within the $w$CDM cosmologies, in a few CPU seconds., Comment: 46 pages, 47 figures; version accepted for publication in ApJ
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- 2018
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6. Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data
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Hikage, Chiaki, Oguri, Masamune, Hamana, Takashi, More, Surhud, Mandelbaum, Rachel, Takada, Masahiro, Köhlinger, Fabian, Miyatake, Hironao, Nishizawa, Atsushi J., Aihara, Hiroaki, Armstrong, Robert, Bosch, James, Coupon, Jean, Ducout, Anne, Ho, Paul, Hsieh, Bau-Ching, Komiyama, Yutaka, Lanusse, François, Leauthaud, Alexie, Lupton, Robert H., Medezinski, Elinor, Mineo, Sogo, Miyama, Shoken, Miyazaki, Satoshi, Murata, Ryoma, Murayama, Hitoshi, Shirasaki, Masato, Sifón, Cristóbal, Simet, Melanie, Speagle, Joshua, Spergel, David N., Strauss, Michael A., Sugiyama, Naoshi, Tanaka, Masayuki, Utsumi, Yousuke, Wang, Shiang-Yu, and Yamada, Yoshihiko
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We measure cosmic weak lensing shear power spectra with the Subaru Hyper Suprime-Cam (HSC) survey first-year shear catalog covering 137deg$^2$ of the sky. Thanks to the high effective galaxy number density of $\sim$17 arcmin$^{-2}$ even after conservative cuts such as magnitude cut of $i<24.5$ and photometric redshift cut of $0.3\leq z \leq 1.5$, we obtain a high significance measurement of the cosmic shear power spectra in 4 tomographic redshift bins, achieving a total signal-to-noise ratio of 16 in the multipole range $300 \leq \ell \leq 1900$. We carefully account for various uncertainties in our analysis including the intrinsic alignment of galaxies, scatters and biases in photometric redshifts, residual uncertainties in the shear measurement, and modeling of the matter power spectrum. The accuracy of our power spectrum measurement method as well as our analytic model of the covariance matrix are tested against realistic mock shear catalogs. For a flat $\Lambda$ cold dark matter ($\Lambda$CDM) model, we find $S_8\equiv \sigma_8(\Omega_{\rm m}/0.3)^\alpha=0.800^{+0.029}_{-0.028}$ for $\alpha=0.45$ ($S_8=0.780^{+0.030}_{-0.033}$ for $\alpha=0.5$) from our HSC tomographic cosmic shear analysis alone. In comparison with Planck cosmic microwave background constraints, our results prefer slightly lower values of $S_8$, although metrics such as the Bayesian evidence ratio test do not show significant evidence for discordance between these results. We study the effect of possible additional systematic errors that are unaccounted in our fiducial cosmic shear analysis, and find that they can shift the best-fit values of $S_8$ by up to $\sim 0.6\sigma$ in both directions. The full HSC survey data will contain several times more area, and will lead to significantly improved cosmological constraints., Comment: 43 pages, 21 figures, accepted for publication in PASJ
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- 2018
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7. Weak-Lensing Mass Calibration of ACTPol Sunyaev-Zel'dovich Clusters with the Hyper Suprime-Cam Survey
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Miyatake, Hironao, Battaglia, Nicholas, Hilton, Matt, Medezinski, Elinor, Nishizawa, Atsushi J., More, Surhud, Aiola, Simone, Bahcall, Neta, Bond, J. Richard, Calabrese, Erminia, Choi, Steve K., Devlin, Mark J., Dunkley, Joanna, Dunner, Rolando, Fuzia, Brittany, Gallardo, Patricio, Gralla, Megan, Hasselfield, Matthew, Halpern, Mark, Hikage, Chiaki, Hill, J. Colin, Hincks, Adam D., Hložek, Renée, Huffenberger, Kevin, Hughes, John P., Koopman, Brian, Kosowsky, Arthur, Louis, Thibaut, Madhavacheril, Mathew S., McMahon, Jeff, Mandelbaum, Rachel, Marriage, Tobias A., Maurin, Loïc, Miyazaki, Satoshi, Moodley, Kavilan, Murata, Ryoma, Naess, Sigurd, Newburgh, Laura, Niemack, Michael D., Nishimichi, Takahiro, Okabe, Nobuhiro, Oguri, Masamune, Osato, Ken, Page, Lyman, Partridge, Bruce, Robertson, Naomi, Sehgal, Neelima, Shirasaki, Masato, Sievers, Jonathan, Sifón, Cristóbal, Simon, Sara, Sherwin, Blake, Spergel, David N., Staggs, Suzanne T., Stein, George, Takada, Masahiro, Trac, Hy, Umetsu, Keiichi, van Engelen, Alex, and Wollack, Edward J.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present weak-lensing measurements using the first-year data from the Hyper Suprime-Cam Strategic Survey Program on the Subaru telescope for eight galaxy clusters selected through their thermal Sunyaev-Zel'dovich (SZ) signal measured at 148 GHz with the Atacama Cosmology Telescope Polarimeter experiment. The overlap between the two surveys in this work is 33.8 square degrees, before masking bright stars. The signal-to-noise ratio of individual cluster lensing measurements ranges from 2.2 to 8.7, with a total of 11.1 for the stacked cluster weak-lensing signal. We fit for an average weak-lensing mass distribution using three different profiles, a Navarro-Frenk-White profile, a dark-matter-only emulated profile, and a full cosmological hydrodynamic emulated profile. We interpret the differences among the masses inferred by these models as a systematic error of 10\%, which is currently smaller than the statistical error. We obtain the ratio of the SZ-estimated mass to the lensing-estimated mass (the so-called hydrostatic mass bias $1-b$) of $0.74^{+0.13}_{-0.12}$, which is comparable to previous SZ-selected clusters from the Atacama Cosmology Telescope and from the {\sl Planck} Satellite. We conclude with a discussion of the implications for cosmological parameters inferred from cluster abundances compared to cosmic microwave background primary anisotropy measurements., Comment: 19 pages, 11 figures, 2 tables, comments are welcome
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- 2018
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8. Weak lensing shear calibration with simulations of the HSC survey
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Mandelbaum, Rachel, Lanusse, François, Leauthaud, Alexie, Armstrong, Robert, Simet, Melanie, Miyatake, Hironao, Meyers, Joshua E., Bosch, James, Murata, Ryoma, Miyazaki, Satoshi, and Tanaka, Masayuki
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Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We present results from a set of simulations designed to constrain the weak lensing shear calibration for the Hyper Suprime-Cam (HSC) survey. These simulations include HSC observing conditions and galaxy images from the Hubble Space Telescope (HST), with fully realistic galaxy morphologies and the impact of nearby galaxies included. We find that the inclusion of nearby galaxies in the images is critical to reproducing the observed distributions of galaxy sizes and magnitudes, due to the non-negligible fraction of unrecognized blends in ground-based data, even with the excellent typical seeing of the HSC survey (0.58" in the $i$-band). Using these simulations, we detect and remove the impact of selection biases due to the correlation of weights and the quantities used to define the sample (S/N and apparent size) with the lensing shear. We quantify and remove galaxy property-dependent multiplicative and additive shear biases that are intrinsic to our shear estimation method, including a $\sim 10$ per cent-level multiplicative bias due to the impact of nearby galaxies and unrecognized blends. Finally, we check the sensitivity of our shear calibration estimates to other cuts made on the simulated samples, and find that the changes in shear calibration are well within the requirements for HSC weak lensing analysis. Overall, the simulations suggest that the weak lensing multiplicative biases in the first-year HSC shear catalog are controlled at the 1 per cent level., Comment: 29 pages, 18 figures, 3 tables. Matches MNRAS accepted version. The Hubble Space Telescope postage stamp images used as the inputs to the simulations were publicly released at https://hsc-release.mtk.nao.ac.jp/doc/index.php/weak-lensing-simulation-catalog-pdr1/
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- 2017
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9. Constraints on the mass-richness relation from the abundance and weak lensing of SDSS clusters
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Murata, Ryoma, Nishimichi, Takahiro, Takada, Masahiro, Miyatake, Hironao, Shirasaki, Masato, More, Surhud, Takahashi, Ryuichi, and Osato, Ken
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We constrain the scaling relation between optical richness ($\lambda$) and halo mass ($M$) for a sample of SDSS redMaPPer galaxy clusters within the context of the {\it Planck} cosmological model. We use a forward modeling approach where we model the probability distribution of optical richness for a given mass, $P(\ln \lambda| M)$. To model the abundance and the stacked lensing profiles, we use an emulator specifically built to interpolate the halo mass function and the stacked lensing profile for an arbitrary set of halo mass and redshift, which is calibrated based on a suite of high-resolution $N$-body simulations. We apply our method to 8,312 SDSS redMaPPer clusters with $20\le \lambda \le 100$ and $0.10\le z_{\lambda}\le0.33$, and show that the log-normal distribution model for $P(\lambda|M)$, with four free parameters, well reproduces the measured abundances and lensing profiles simultaneously. The constraints are characterized by the mean relation, $\left\langle \ln{\lambda}\right\rangle(M)=A+B\ln(M/M_{\rm pivot})$, with $A=3.207^{+0.044}_{-0.046}$ and $B=0.993^{+0.041}_{-0.055}$ (68\%~CL), where the pivot mass scale $M_{\rm pivot}=3\times 10^{14} h^{-1}M_\odot$, and the scatter $\sigma_{\mathrm{\ln\lambda}|M}=\sigma_0+q\ln(M/M_{\rm pivot})$ with $\sigma_0=0.456^{+0.047}_{-0.039}$ and $q=-0.169^{+0.035}_{-0.026}$. We find that a large scatter in halo masses is required at the lowest richness bins ($20\le \lambda \lesssim 30$) in order to reproduce the measurements. Without such a large scatter, the model prediction for the lensing profiles tends to overestimate the measured amplitudes. This might imply a possible contamination of intrinsically low-richness clusters due to the projection effects. Such a low-mass halo contribution is significantly reduced when applying our method to the sample of $30\le \lambda \le 100$., Comment: 20 figures, 5 tables, v3 matches accepted version that will be published in ApJ (minor changes from v2)
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- 2017
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10. Source Selection for Cluster Weak Lensing Measurements in the Hyper Suprime-Cam Survey
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Medezinski, Elinor, Oguri, Masamune, Nishizawa, Atsushi J., Speagle, Joshua S., Miyatake, Hironao, Umetsu, Keiichi, Leauthaud, Alexie, Murata, Ryoma, Mandelbaum, Rachel, Sifón, Cristóbal, Strauss, Michael A., Huang, Song, Simet, Melanie, Okabe, Nobuhiro, Tanaka, Masayuki, and Komiyama, Yutaka
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present optimized source galaxy selection schemes for measuring cluster weak lensing (WL) mass profiles unaffected by cluster member dilution from the Subaru Hyper Suprime-Cam Strategic Survey Program (HSC-SSP). The ongoing HSC-SSP survey will uncover thousands of galaxy clusters to $z\lesssim1.5$. In deriving cluster masses via WL, a critical source of systematics is contamination and dilution of the lensing signal by cluster {members, and by foreground galaxies whose photometric redshifts are biased}. Using the first-year CAMIRA catalog of $\sim$900 clusters with richness larger than 20 found in $\sim$140 deg$^2$ of HSC-SSP data, we devise and compare several source selection methods, including selection in color-color space (CC-cut), and selection of robust photometric redshifts by applying constraints on their cumulative probability distribution function (PDF; P-cut). We examine the dependence of the contamination on the chosen limits adopted for each method. Using the proper limits, these methods give mass profiles with minimal dilution in agreement with one another. We find that not adopting either the CC-cut or P-cut methods results in an underestimation of the total cluster mass ($13\pm4\%$) and the concentration of the profile ($24\pm11\%$). The level of cluster contamination can reach as high as $\sim10\%$ at $R\approx 0.24$ Mpc/$h$ for low-z clusters without cuts, while employing either the P-cut or CC-cut results in cluster contamination consistent with zero to within the 0.5% uncertainties. Our robust methods yield a $\sim60\sigma$ detection of the stacked CAMIRA surface mass density profile, with a mean mass of $M_\mathrm{200c} = (1.67\pm0.05({\rm {stat}}))\times 10^{14}\,M_\odot/h$., Comment: 19 pages, 4 tables, 12 figures, accepted to PASJ special issue
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- 2017
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11. The Hyper Suprime-Cam Software Pipeline
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Bosch, James, Armstrong, Robert, Bickerton, Steven, Furusawa, Hisanori, Ikeda, Hiroyuki, Koike, Michitaro, Lupton, Robert, Mineo, Sogo, Price, Paul, Takata, Tadafumi, Tanaka, Masayuki, Yasuda, Naoki, AlSayyad, Yusra, Becker, Andrew C., Coulton, William, Coupon, Jean, Garmilla, Jose, Huang, Song, Krughoff, K. Simon, Lang, Dustin, Leauthaud, Alexie, Lim, Kian-Tat, Lust, Nate B., MacArthur, Lauren A., Mandelbaum, Rachel, Miyatake, Hironao, Miyazaki, Satoshi, Murata, Ryoma, More, Surhud, Okura, Yuki, Owen, Russell, Swinbank, John D., Strauss, Michael A., Yamada, Yoshihiko, and Yamanoi, Hitomi
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
In this paper, we describe the optical imaging data processing pipeline developed for the Subaru Telescope's Hyper Suprime-Cam (HSC) instrument. The HSC Pipeline builds on the prototype pipeline being developed by the Large Synoptic Survey Telescope's Data Management system, adding customizations for HSC, large-scale processing capabilities, and novel algorithms that have since been reincorporated into the LSST codebase. While designed primarily to reduce HSC Subaru Strategic Program (SSP) data, it is also the recommended pipeline for reducing general-observer HSC data. The HSC pipeline includes high level processing steps that generate coadded images and science-ready catalogs as well as low-level detrending and image characterizations., Comment: 39 pages, 21 figures, 2 tables. Submitted to Publications of the Astronomical Society of Japan
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- 2017
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12. The first-year shear catalog of the Subaru Hyper Suprime-Cam SSP Survey
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Mandelbaum, Rachel, Miyatake, Hironao, Hamana, Takashi, Oguri, Masamune, Simet, Melanie, Armstrong, Robert, Bosch, James, Murata, Ryoma, Lanusse, François, Leauthaud, Alexie, Coupon, Jean, More, Surhud, Takada, Masahiro, Miyazaki, Satoshi, Speagle, Joshua S., Shirasaki, Masato, Sifón, Cristóbal, Huang, Song, Nishizawa, Atsushi J., Medezinski, Elinor, Okura, Yuki, Okabe, Nobuhiro, Czakon, Nicole, Takahashi, Ryuichi, Coulton, Will, Hikage, Chiaki, Komiyama, Yutaka, Lupton, Robert H., Strauss, Michael A., Tanaka, Masayuki, and Utsumi, Yousuke
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Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We present and characterize the catalog of galaxy shape measurements that will be used for cosmological weak lensing measurements in the Wide layer of the first year of the Hyper Suprime-Cam (HSC) survey. The catalog covers an area of 136.9 deg$^2$ split into six fields, with a mean $i$-band seeing of $0.58$ arcsec and $5\sigma$ point-source depth of $i\sim 26$. Given conservative galaxy selection criteria for first year science, the depth and excellent image quality results in unweighted and weighted source number densities of 24.6 and 21.8 arcmin$^{-2}$, respectively. We define the requirements for cosmological weak lensing science with this catalog, then focus on characterizing potential systematics in the catalog using a series of internal null tests for problems with point-spread function (PSF) modeling, shear estimation, and other aspects of the image processing. We find that the PSF models narrowly meet requirements for weak lensing science with this catalog, with fractional PSF model size residuals of approximately $0.003$ (requirement: 0.004) and the PSF model shape correlation function $\rho_1<3\times 10^{-7}$ (requirement: $4\times 10^{-7}$) at 0.5$^\circ$ scales. A variety of galaxy shape-related null tests are statistically consistent with zero, but star-galaxy shape correlations reveal additive systematics on $>1^\circ$ scales that are sufficiently large as to require mitigation in cosmic shear measurements. Finally, we discuss the dominant systematics and the planned algorithmic changes to reduce them in future data reductions., Comment: 42 figures, 4 tables, v3 matches accepted version that will be published in PASJ (minor changes from v2). For high-resolution figures and cross-references with other HSC articles that will be in the same PASJ issue, please see the published version of the article
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- 2017
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13. Characterization and Photometric Performance of the Hyper Suprime-Cam Software Pipeline
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Huang, Song, Leauthaud, Alexie, Murata, Ryoma, Bosch, James, Price, Paul, Lupton, Robert, Mandelbaum, Rachel, Lackner, Claire, Bickerton, Steve, Miyazaki, Satoshi, Coupon, Jean, and Tanaka, Masayuki
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Subaru Strategic Program (SSP) is an ambitious multi-band survey using the Hyper Suprime-Cam (HSC) on the Subaru telescope. The Wide layer of the SSP is both wide and deep, reaching a detection limit of i~26.0 mag. At these depths, it is challenging to achieve accurate, unbiased, and consistent photometry across all five bands. The HSC data are reduced using a pipeline that builds on the prototype pipeline for the Large Synoptic Survey Telescope. We have developed a Python-based, flexible framework to inject synthetic galaxies into real HSC images called SynPipe. Here we explain the design and implementation of SynPipe and generate a sample of synthetic galaxies to examine the photometric performance of the HSC pipeline. For stars, we achieve 1% photometric precision at i~19.0 mag and 6% precision at i~25.0 in the i-band. For synthetic galaxies with single-Sersic profiles, forced CModel photometry achieves 13% photometric precision at i~20.0 mag and 18% precision at i~25.0 in the i-band. We show that both forced PSF and CModel photometry yield unbiased color estimates that are robust to seeing conditions. We identify several caveats that apply to the version of HSC pipeline used for the first public HSC data release (DR1) that need to be taking into consideration. First, the degree to which an object is blended with other objects impacts the overall photometric performance. This is especially true for point sources. Highly blended objects tend to have larger photometric uncertainties, systematically underestimated fluxes and slightly biased colors. Second, >20% of stars at 22.5< i < 25.0 mag can be misclassified as extended objects. Third, the current CModel algorithm tends to strongly underestimate the half-light radius and ellipticity of galaxy with i>21.5 mag., Comment: Submitted to the PASJ special issue for Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP); 26 pages, 17 figures, 4 tables. The SynPipe code can be found here: https://github.com/dr-guangtou/synpipe
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- 2017
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14. First Data Release of the Hyper Suprime-Cam Subaru Strategic Program
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Aihara, Hiroaki, Armstrong, Robert, Bickerton, Steven, Bosch, James, Coupon, Jean, Furusawa, Hisanori, Hayashi, Yusuke, Ikeda, Hiroyuki, Kamata, Yukiko, Karoji, Hiroshi, Kawanomoto, Satoshi, Koike, Michitaro, Komiyama, Yutaka, Lupton, Robert H., Mineo, Sogo, Miyatake, Hironao, Miyazaki, Satoshi, Morokuma, Tomoki, Obuchi, Yoshiyuki, Oishi, Yukie, Okura, Yuki, Price, Paul A., Takata, Tadafumi, Tanaka, Manobu M., Tanaka, Masayuki, Tanaka, Yoko, Uchida, Tomohisa, Uraguchi, Fumihiro, Utsumi, Yousuke, Wang, Shiang-Yu, Yamada, Yoshihiko, Yamanoi, Hitomi, Yasuda, Naoki, Arimoto, Nobuo, Chiba, Masashi, Finet, Francois, Fujimori, Hiroki, Fujimoto, Seiji, Furusawa, Junko, Goto, Tomotsugu, Goulding, Andy, Gunn, James E., Harikane, Yuichi, Hattori, Takashi, Hayashi, Masao, Helminiak, Krzysztof G., Higuchi, Ryo, Hikage, Chiaki, Ho, Paul T. P., Hsieh, Bau-Ching, Huang, Kuiyun, Huang, Song, Imanishi, Masatoshi, Iwata, Ikuru, Jaelani, Anton T., Jian, Hung-Yu, Kashikawa, Nobunari, Katayama, Nobuhiko, Kojima, Takashi, Konno, Akira, Koshida, Shintaro, Kusakabe, Haruka, Leauthaud, Alexie, Lee, C. -H., Lin, Lihwai, Lin, Yen-Ting, Mandelbaum, Rachel, Matsuoka, Yoshiki, Medezinski, Elinor, Miyama, Shoken, Momose, Rieko, More, Anupreeta, More, Surhud, Mukae, Shiro, Murata, Ryoma, Murayama, Hitoshi, Nagao, Tohru, Nakata, Fumiaki, Niikura, Hiroko, Nishizawa, Atsushi J., Oguri, Masamune, Okabe, Nobuhiro, Ono, Yoshiaki, Onodera, Masato, Onoue, Masafusa, Ouchi, Masami, Pyo, Tae-Soo, Shibuya, Takatoshi, Shimasaku, Kazuhiro, Simet, Melanie, Speagle, Joshua, Spergel, David N., Strauss, Michael A., Sugahara, Yuma, Sugiyama, Naoshi, Suto, Yasushi, Suzuki, Nao, Tait, Philip J., Takada, Masahiro, Terai, Tsuyoshi, Toba, Yoshiki, Turner, Edwin L., Uchiyama, Hisakazu, Umetsu, Keiichi, Urata, Yuji, Usuda, Tomonori, Yeh, Sherry, and Yuma, Suraphong
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) is a three-layered imaging survey aimed at addressing some of the most outstanding questions in astronomy today, including the nature of dark matter and dark energy. The survey has been awarded 300 nights of observing time at the Subaru Telescope and it started in March 2014. This paper presents the first public data release of HSC-SSP. This release includes data taken in the first 1.7 years of observations (61.5 nights) and each of the Wide, Deep, and UltraDeep layers covers about 108, 26, and 4 square degrees down to depths of i~26.4, ~26.5, and ~27.0 mag, respectively (5sigma for point sources). All the layers are observed in five broad bands (grizy), and the Deep and UltraDeep layers are observed in narrow bands as well. We achieve an impressive image quality of 0.6 arcsec in the i-band in the Wide layer. We show that we achieve 1-2 per cent PSF photometry (rms) both internally and externally (against Pan-STARRS1), and ~10 mas and 40 mas internal and external astrometric accuracy, respectively. Both the calibrated images and catalogs are made available to the community through dedicated user interfaces and database servers. In addition to the pipeline products, we also provide value-added products such as photometric redshifts and a collection of public spectroscopic redshifts. Detailed descriptions of all the data can be found online. The data release website is https://hsc-release.mtk.nao.ac.jp/., Comment: 34 pages, 20 figures, 7 tables, moderate revision, accepted for publication in PASJ
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- 2017
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15. Robust covariance estimation of galaxy-galaxy weak lensing: validation and limitation of jackknife covariance
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Shirasaki, Masato, Takada, Masahiro, Miyatake, Hironao, Takahashi, Ryuichi, Hamana, Takashi, Nishimichi, Takahiro, and Murata, Ryoma
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We develop a method to simulate galaxy-galaxy weak lensing by utilizing all-sky, light-cone simulations and their inherent halo catalogs. Using the mock catalog to study the error covariance matrix of galaxy-galaxy weak lensing, we compare the full covariance with the "jackknife" (JK) covariance, the method often used in the literature that estimates the covariance from the resamples of the data itself. We show that there exists the variation of JK covariance over realizations of mock lensing measurements, while the average JK covariance over mocks can give a reasonably accurate estimation of the true covariance up to separations comparable with the size of JK subregion. The scatter in JK covariances is found to be $\sim10\%$ after we subtract the lensing measurement around random points. However, the JK method tends to underestimate the covariance at the larger separations, more increasingly for a survey with a higher number density of source galaxies. We apply our method to the the Sloan Digital Sky Survey (SDSS) data, and show that the 48 mock SDSS catalogs nicely reproduce the signals and the JK covariance measured from the real data. We then argue that the use of the accurate covariance, compared to the JK covariance, allows us to use the lensing signals at large scales beyond a size of the JK subregion, which contains cleaner cosmological information in the linear regime., Comment: 25 pages, 12 figures, 2 tables, accepted for publication in MNRAS
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- 2016
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16. Detection of the Splashback Radius and Halo Assembly bias of Massive Galaxy Clusters
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More, Surhud, Miyatake, Hironao, Takada, Masahiro, Diemer, Benedikt, Kravtsov, Andrey V., Dalal, Neal K., More, Anupreeta, Murata, Ryoma, Mandelbaum, Rachel, Rozo, Eduardo, Rykoff, Eli S., Oguri, Masamune, and Spergel, David N.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We show that the projected number density profiles of SDSS photometric galaxies around galaxy clusters displays strong evidence for the splashback radius, a sharp halo edge corresponding to the location of the first orbital apocenter of satellite galaxies after their infall. We split the clusters into two subsamples with different mean projected radial distances of their members, $\langle R_{\rm mem}\rangle$, at fixed richness and redshift, and show that the sample with smaller $\langle R_{\rm mem}\rangle$ has a smaller ratio of the splashback radius to the traditional halo boundary $R_{\rm 200m}$, than the subsample with larger $\langle R_{\rm mem}\rangle$, indicative of different mass accretion rates for the two subsamples. The same cluster samples were recently used by Miyatake et al. to show that their large-scale clustering differs despite their similar weak lensing masses, demonstrating strong evidence for halo assembly bias. We expand on this result by presenting a 6.6-$\sigma$ detection of halo assembly bias using the cluster-photometric galaxy cross-correlations. Our measured splashback radii are smaller, while the strength of the assembly bias signal is stronger, than expectations from N-body simulations based on the $\Lambda$-dominated, cold dark matter structure formation model. Dynamical friction or cluster-finding systematics such as miscentering or projection effects are not likely to be the sole source of these discrepancies., Comment: 18 pages, 13 figures. Have comments, criticisms, new ideas or new tests, please email me. For Savitzky-Golay filter for data with error covariance, see http://ascl.net/code/v/1299
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- 2016
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17. Erratum: The splashback radius of optically selected clusters with Subaru HSC Second Public Data Release
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Murata, Ryoma, primary, Sunayama, Tomomi, additional, Oguri, Masamune, additional, More, Surhud, additional, Nishizawa, Atsushi J, additional, Nishimichi, Takahiro, additional, and Osato, Ken, additional
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- 2021
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18. すばるハイパーシュプリームカムの可視光観測により検出された銀河団の統計的研究
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Murata, Ryoma
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学位の種別: 課程博士, 審査委員会委員 : (主査)東京大学教授 半場 藤弘, (副査)東京大学PROFESSOR CANNON KIPP, 東京大学教授 手嶋 政廣, 東京大学教授 大内 正己, 東京大学准教授 日下 暁人
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- 2020
19. The splashback radius of optically selected clusters with Subaru HSC Second Public Data Release
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Murata, Ryoma, primary, Sunayama, Tomomi, additional, Oguri, Masamune, additional, More, Surhud, additional, Nishizawa, Atsushi J, additional, Nishimichi, Takahiro, additional, and Osato, Ken, additional
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- 2020
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20. The richness-to-mass relation of CAMIRA galaxy clusters from weak-lensing magnification in the Subaru Hyper Suprime-Cam survey
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Chiu, I-Non, primary, Umetsu, Keiichi, additional, Murata, Ryoma, additional, Medezinski, Elinor, additional, and Oguri, Masamune, additional
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- 2020
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21. Second data release of the Hyper Suprime-Cam Subaru Strategic Program
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Aihara, Hiroaki, primary, AlSayyad, Yusra, additional, Ando, Makoto, additional, Armstrong, Robert, additional, Bosch, James, additional, Egami, Eiichi, additional, Furusawa, Hisanori, additional, Furusawa, Junko, additional, Goulding, Andy, additional, Harikane, Yuichi, additional, Hikage, Chiaki, additional, Ho, Paul T P, additional, Hsieh, Bau-Ching, additional, Huang, Song, additional, Ikeda, Hiroyuki, additional, Imanishi, Masatoshi, additional, Ito, Kei, additional, Iwata, Ikuru, additional, Jaelani, Anton T, additional, Kakuma, Ryota, additional, Kawana, Kojiro, additional, Kikuta, Satoshi, additional, Kobayashi, Umi, additional, Koike, Michitaro, additional, Komiyama, Yutaka, additional, Li, Xiangchong, additional, Liang, Yongming, additional, Lin, Yen-Ting, additional, Luo, Wentao, additional, Lupton, Robert, additional, Lust, Nate B, additional, MacArthur, Lauren A, additional, Matsuoka, Yoshiki, additional, Mineo, Sogo, additional, Miyatake, Hironao, additional, Miyazaki, Satoshi, additional, More, Surhud, additional, Murata, Ryoma, additional, Namiki, Shigeru V, additional, Nishizawa, Atsushi J, additional, Oguri, Masamune, additional, Okabe, Nobuhiro, additional, Okamoto, Sakurako, additional, Okura, Yuki, additional, Ono, Yoshiaki, additional, Onodera, Masato, additional, Onoue, Masafusa, additional, Osato, Ken, additional, Ouchi, Masami, additional, Shibuya, Takatoshi, additional, Strauss, Michael A, additional, Sugiyama, Naoshi, additional, Suto, Yasushi, additional, Takada, Masahiro, additional, Takagi, Yuhei, additional, Takata, Tadafumi, additional, Takita, Satoshi, additional, Tanaka, Masayuki, additional, Terai, Tsuyoshi, additional, Toba, Yoshiki, additional, Uchiyama, Hisakazu, additional, Utsumi, Yousuke, additional, Wang, Shiang-Yu, additional, Wang, Wenting, additional, and Yamada, Yoshihiko, additional
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- 2019
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22. Dark Quest. I. Fast and Accurate Emulation of Halo Clustering Statistics and Its Application to Galaxy Clustering
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Nishimichi, Takahiro, primary, Takada, Masahiro, additional, Takahashi, Ryuichi, additional, Osato, Ken, additional, Shirasaki, Masato, additional, Oogi, Taira, additional, Miyatake, Hironao, additional, Oguri, Masamune, additional, Murata, Ryoma, additional, Kobayashi, Yosuke, additional, and Yoshida, Naoki, additional
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- 2019
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23. The mass–richness relation of optically selected clusters from weak gravitational lensing and abundance with Subaru HSC first-year data
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Murata, Ryoma, primary, Oguri, Masamune, additional, Nishimichi, Takahiro, additional, Takada, Masahiro, additional, Mandelbaum, Rachel, additional, More, Surhud, additional, Shirasaki, Masato, additional, Nishizawa, Atsushi J, additional, and Osato, Ken, additional
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- 2019
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24. Weak-lensing Mass Calibration of ACTPol Sunyaev–Zel’dovich Clusters with the Hyper Suprime-Cam Survey
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Miyatake, Hironao, primary, Battaglia, Nicholas, additional, Hilton, Matt, additional, Medezinski, Elinor, additional, Nishizawa, Atsushi J., additional, More, Surhud, additional, Aiola, Simone, additional, Bahcall, Neta, additional, Bond, J. Richard, additional, Calabrese, Erminia, additional, Choi, Steve K., additional, Devlin, Mark J., additional, Dunkley, Joanna, additional, Dunner, Rolando, additional, Fuzia, Brittany, additional, Gallardo, Patricio, additional, Gralla, Megan, additional, Hasselfield, Matthew, additional, Halpern, Mark, additional, Hikage, Chiaki, additional, Hill, J. Colin, additional, Hincks, Adam D., additional, Hložek, Renée, additional, Huffenberger, Kevin, additional, Hughes, John P., additional, Koopman, Brian, additional, Kosowsky, Arthur, additional, Louis, Thibaut, additional, Madhavacheril, Mathew S., additional, McMahon, Jeff, additional, Mandelbaum, Rachel, additional, Marriage, Tobias A., additional, Maurin, Loïc, additional, Miyazaki, Satoshi, additional, Moodley, Kavilan, additional, Murata, Ryoma, additional, Naess, Sigurd, additional, Newburgh, Laura, additional, Niemack, Michael D., additional, Nishimichi, Takahiro, additional, Okabe, Nobuhiro, additional, Oguri, Masamune, additional, Osato, Ken, additional, Page, Lyman, additional, Partridge, Bruce, additional, Robertson, Naomi, additional, Sehgal, Neelima, additional, Sherwin, Blake, additional, Shirasaki, Masato, additional, Sievers, Jonathan, additional, Sifón, Cristóbal, additional, Simon, Sara, additional, Spergel, David N., additional, Staggs, Suzanne T., additional, Stein, George, additional, Takada, Masahiro, additional, Trac, Hy, additional, Umetsu, Keiichi, additional, Engelen, Alex van, additional, and Wollack, Edward J., additional
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- 2019
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25. Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data
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Hikage, Chiaki, primary, Oguri, Masamune, primary, Hamana, Takashi, primary, More, Surhud, primary, Mandelbaum, Rachel, primary, Takada, Masahiro, primary, Köhlinger, Fabian, primary, Miyatake, Hironao, primary, Nishizawa, Atsushi J, primary, Aihara, Hiroaki, primary, Armstrong, Robert, primary, Bosch, James, primary, Coupon, Jean, primary, Ducout, Anne, primary, Ho, Paul, primary, Hsieh, Bau-Ching, primary, Komiyama, Yutaka, primary, Lanusse, François, primary, Leauthaud, Alexie, primary, Lupton, Robert H, primary, Medezinski, Elinor, primary, Mineo, Sogo, primary, Miyama, Shoken, primary, Miyazaki, Satoshi, primary, Murata, Ryoma, primary, Murayama, Hitoshi, primary, Shirasaki, Masato, primary, Sifón, Cristóbal, primary, Simet, Melanie, primary, Speagle, Joshua, primary, Spergel, David N, primary, Strauss, Michael A, primary, Sugiyama, Naoshi, primary, Tanaka, Masayuki, primary, Utsumi, Yousuke, primary, Wang, Shiang-Yu, primary, and Yamada, Yoshihiko, primary
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- 2019
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26. Weak lensing shear calibration with simulations of the HSC survey
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Mandelbaum, Rachel, primary, Lanusse, François, additional, Leauthaud, Alexie, additional, Armstrong, Robert, additional, Simet, Melanie, additional, Miyatake, Hironao, additional, Meyers, Joshua E, additional, Bosch, James, additional, Murata, Ryoma, additional, Miyazaki, Satoshi, additional, and Tanaka, Masayuki, additional
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- 2018
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27. Source selection for cluster weak lensing measurements in the Hyper Suprime-Cam survey
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Medezinski, Elinor, primary, Oguri, Masamune, additional, Nishizawa, Atsushi J, additional, Speagle, Joshua S, additional, Miyatake, Hironao, additional, Umetsu, Keiichi, additional, Leauthaud, Alexie, additional, Murata, Ryoma, additional, Mandelbaum, Rachel, additional, Sifón, Cristóbal, additional, Strauss, Michael A, additional, Huang, Song, additional, Simet, Melanie, additional, Okabe, Nobuhiro, additional, Tanaka, Masayuki, additional, and Komiyama, Yutaka, additional
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- 2018
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28. Constraints on the Mass–Richness Relation from the Abundance and Weak Lensing of SDSS Clusters
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Murata, Ryoma, primary, Nishimichi, Takahiro, additional, Takada, Masahiro, additional, Miyatake, Hironao, additional, Shirasaki, Masato, additional, More, Surhud, additional, Takahashi, Ryuichi, additional, and Osato, Ken, additional
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- 2018
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29. The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey
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Mandelbaum, Rachel, primary, Miyatake, Hironao, additional, Hamana, Takashi, additional, Oguri, Masamune, additional, Simet, Melanie, additional, Armstrong, Robert, additional, Bosch, James, additional, Murata, Ryoma, additional, Lanusse, François, additional, Leauthaud, Alexie, additional, Coupon, Jean, additional, More, Surhud, additional, Takada, Masahiro, additional, Miyazaki, Satoshi, additional, Speagle, Joshua S, additional, Shirasaki, Masato, additional, Sifón, Cristóbal, additional, Huang, Song, additional, Nishizawa, Atsushi J, additional, Medezinski, Elinor, additional, Okura, Yuki, additional, Okabe, Nobuhiro, additional, Czakon, Nicole, additional, Takahashi, Ryuichi, additional, Coulton, William R, additional, Hikage, Chiaki, additional, Komiyama, Yutaka, additional, Lupton, Robert H, additional, Strauss, Michael A, additional, Tanaka, Masayuki, additional, and Utsumi, Yousuke, additional
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- 2017
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30. Characterization and photometric performance of the Hyper Suprime-Cam Software Pipeline
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Huang, Song, primary, Leauthaud, Alexie, additional, Murata, Ryoma, additional, Bosch, James, additional, Price, Paul, additional, Lupton, Robert, additional, Mandelbaum, Rachel, additional, Lackner, Claire, additional, Bickerton, Steven, additional, Miyazaki, Satoshi, additional, Coupon, Jean, additional, and Tanaka, Masayuki, additional
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- 2017
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31. The Hyper Suprime-Cam software pipeline
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Bosch, James, primary, Armstrong, Robert, additional, Bickerton, Steven, additional, Furusawa, Hisanori, additional, Ikeda, Hiroyuki, additional, Koike, Michitaro, additional, Lupton, Robert, additional, Mineo, Sogo, additional, Price, Paul, additional, Takata, Tadafumi, additional, Tanaka, Masayuki, additional, Yasuda, Naoki, additional, AlSayyad, Yusra, additional, Becker, Andrew C, additional, Coulton, William, additional, Coupon, Jean, additional, Garmilla, Jose, additional, Huang, Song, additional, Krughoff, K Simon, additional, Lang, Dustin, additional, Leauthaud, Alexie, additional, Lim, Kian-Tat, additional, Lust, Nate B, additional, MacArthur, Lauren A, additional, Mandelbaum, Rachel, additional, Miyatake, Hironao, additional, Miyazaki, Satoshi, additional, Murata, Ryoma, additional, More, Surhud, additional, Okura, Yuki, additional, Owen, Russell, additional, Swinbank, John D, additional, Strauss, Michael A, additional, Yamada, Yoshihiko, additional, and Yamanoi, Hitomi, additional
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- 2017
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32. First data release of the Hyper Suprime-Cam Subaru Strategic Program
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Aihara, Hiroaki, primary, Armstrong, Robert, additional, Bickerton, Steven, additional, Bosch, James, additional, Coupon, Jean, additional, Furusawa, Hisanori, additional, Hayashi, Yusuke, additional, Ikeda, Hiroyuki, additional, Kamata, Yukiko, additional, Karoji, Hiroshi, additional, Kawanomoto, Satoshi, additional, Koike, Michitaro, additional, Komiyama, Yutaka, additional, Lang, Dustin, additional, Lupton, Robert H, additional, Mineo, Sogo, additional, Miyatake, Hironao, additional, Miyazaki, Satoshi, additional, Morokuma, Tomoki, additional, Obuchi, Yoshiyuki, additional, Oishi, Yukie, additional, Okura, Yuki, additional, Price, Paul A, additional, Takata, Tadafumi, additional, Tanaka, Manobu M, additional, Tanaka, Masayuki, additional, Tanaka, Yoko, additional, Uchida, Tomohisa, additional, Uraguchi, Fumihiro, additional, Utsumi, Yousuke, additional, Wang, Shiang-Yu, additional, Yamada, Yoshihiko, additional, Yamanoi, Hitomi, additional, Yasuda, Naoki, additional, Arimoto, Nobuo, additional, Chiba, Masashi, additional, Finet, Francois, additional, Fujimori, Hiroki, additional, Fujimoto, Seiji, additional, Furusawa, Junko, additional, Goto, Tomotsugu, additional, Goulding, Andy, additional, Gunn, James E, additional, Harikane, Yuichi, additional, Hattori, Takashi, additional, Hayashi, Masao, additional, Hełminiak, Krzysztof G, additional, Higuchi, Ryo, additional, Hikage, Chiaki, additional, Ho, Paul T P, additional, Hsieh, Bau-Ching, additional, Huang, Kuiyun, additional, Huang, Song, additional, Imanishi, Masatoshi, additional, Iwata, Ikuru, additional, Jaelani, Anton T, additional, Jian, Hung-Yu, additional, Kashikawa, Nobunari, additional, Katayama, Nobuhiko, additional, Kojima, Takashi, additional, Konno, Akira, additional, Koshida, Shintaro, additional, Kusakabe, Haruka, additional, Leauthaud, Alexie, additional, Lee, Chien-Hsiu, additional, Lin, Lihwai, additional, Lin, Yen-Ting, additional, Mandelbaum, Rachel, additional, Matsuoka, Yoshiki, additional, Medezinski, Elinor, additional, Miyama, Shoken, additional, Momose, Rieko, additional, More, Anupreeta, additional, More, Surhud, additional, Mukae, Shiro, additional, Murata, Ryoma, additional, Murayama, Hitoshi, additional, Nagao, Tohru, additional, Nakata, Fumiaki, additional, Niida, Mana, additional, Niikura, Hiroko, additional, Nishizawa, Atsushi J, additional, Oguri, Masamune, additional, Okabe, Nobuhiro, additional, Ono, Yoshiaki, additional, Onodera, Masato, additional, Onoue, Masafusa, additional, Ouchi, Masami, additional, Pyo, Tae-Soo, additional, Shibuya, Takatoshi, additional, Shimasaku, Kazuhiro, additional, Simet, Melanie, additional, Speagle, Joshua, additional, Spergel, David N, additional, Strauss, Michael A, additional, Sugahara, Yuma, additional, Sugiyama, Naoshi, additional, Suto, Yasushi, additional, Suzuki, Nao, additional, Tait, Philip J, additional, Takada, Masahiro, additional, Terai, Tsuyoshi, additional, Toba, Yoshiki, additional, Turner, Edwin L, additional, Uchiyama, Hisakazu, additional, Umetsu, Keiichi, additional, Urata, Yuji, additional, Usuda, Tomonori, additional, Yeh, Sherry, additional, and Yuma, Suraphong, additional
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- 2017
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33. The Hyper Suprime-Cam SSP Survey: Overview and survey design
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Aihara, Hiroaki, primary, Arimoto, Nobuo, additional, Armstrong, Robert, additional, Arnouts, Stéphane, additional, Bahcall, Neta A, additional, Bickerton, Steven, additional, Bosch, James, additional, Bundy, Kevin, additional, Capak, Peter L, additional, Chan, James H H, additional, Chiba, Masashi, additional, Coupon, Jean, additional, Egami, Eiichi, additional, Enoki, Motohiro, additional, Finet, Francois, additional, Fujimori, Hiroki, additional, Fujimoto, Seiji, additional, Furusawa, Hisanori, additional, Furusawa, Junko, additional, Goto, Tomotsugu, additional, Goulding, Andy, additional, Greco, Johnny P, additional, Greene, Jenny E, additional, Gunn, James E, additional, Hamana, Takashi, additional, Harikane, Yuichi, additional, Hashimoto, Yasuhiro, additional, Hattori, Takashi, additional, Hayashi, Masao, additional, Hayashi, Yusuke, additional, Hełminiak, Krzysztof G, additional, Higuchi, Ryo, additional, Hikage, Chiaki, additional, Ho, Paul T P, additional, Hsieh, Bau-Ching, additional, Huang, Kuiyun, additional, Huang, Song, additional, Ikeda, Hiroyuki, additional, Imanishi, Masatoshi, additional, Inoue, Akio K, additional, Iwasawa, Kazushi, additional, Iwata, Ikuru, additional, Jaelani, Anton T, additional, Jian, Hung-Yu, additional, Kamata, Yukiko, additional, Karoji, Hiroshi, additional, Kashikawa, Nobunari, additional, Katayama, Nobuhiko, additional, Kawanomoto, Satoshi, additional, Kayo, Issha, additional, Koda, Jin, additional, Koike, Michitaro, additional, Kojima, Takashi, additional, Komiyama, Yutaka, additional, Konno, Akira, additional, Koshida, Shintaro, additional, Koyama, Yusei, additional, Kusakabe, Haruka, additional, Leauthaud, Alexie, additional, Lee, Chien-Hsiu, additional, Lin, Lihwai, additional, Lin, Yen-Ting, additional, Lupton, Robert H, additional, Mandelbaum, Rachel, additional, Matsuoka, Yoshiki, additional, Medezinski, Elinor, additional, Mineo, Sogo, additional, Miyama, Shoken, additional, Miyatake, Hironao, additional, Miyazaki, Satoshi, additional, Momose, Rieko, additional, More, Anupreeta, additional, More, Surhud, additional, Moritani, Yuki, additional, Moriya, Takashi J, additional, Morokuma, Tomoki, additional, Mukae, Shiro, additional, Murata, Ryoma, additional, Murayama, Hitoshi, additional, Nagao, Tohru, additional, Nakata, Fumiaki, additional, Niida, Mana, additional, Niikura, Hiroko, additional, Nishizawa, Atsushi J, additional, Obuchi, Yoshiyuki, additional, Oguri, Masamune, additional, Oishi, Yukie, additional, Okabe, Nobuhiro, additional, Okamoto, Sakurako, additional, Okura, Yuki, additional, Ono, Yoshiaki, additional, Onodera, Masato, additional, Onoue, Masafusa, additional, Osato, Ken, additional, Ouchi, Masami, additional, Price, Paul A, additional, Pyo, Tae-Soo, additional, Sako, Masao, additional, Sawicki, Marcin, additional, Shibuya, Takatoshi, additional, Shimasaku, Kazuhiro, additional, Shimono, Atsushi, additional, Shirasaki, Masato, additional, Silverman, John D, additional, Simet, Melanie, additional, Speagle, Joshua, additional, Spergel, David N, additional, Strauss, Michael A, additional, Sugahara, Yuma, additional, Sugiyama, Naoshi, additional, Suto, Yasushi, additional, Suyu, Sherry H, additional, Suzuki, Nao, additional, Tait, Philip J, additional, Takada, Masahiro, additional, Takata, Tadafumi, additional, Tamura, Naoyuki, additional, Tanaka, Manobu M, additional, Tanaka, Masaomi, additional, Tanaka, Masayuki, additional, Tanaka, Yoko, additional, Terai, Tsuyoshi, additional, Terashima, Yuichi, additional, Toba, Yoshiki, additional, Tominaga, Nozomu, additional, Toshikawa, Jun, additional, Turner, Edwin L, additional, Uchida, Tomohisa, additional, Uchiyama, Hisakazu, additional, Umetsu, Keiichi, additional, Uraguchi, Fumihiro, additional, Urata, Yuji, additional, Usuda, Tomonori, additional, Utsumi, Yousuke, additional, Wang, Shiang-Yu, additional, Wang, Wei-Hao, additional, Wong, Kenneth C, additional, Yabe, Kiyoto, additional, Yamada, Yoshihiko, additional, Yamanoi, Hitomi, additional, Yasuda, Naoki, additional, Yeh, Sherry, additional, Yonehara, Atsunori, additional, and Yuma, Suraphong, additional
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- 2017
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34. Robust covariance estimation of galaxy–galaxy weak lensing: validation and limitation of jackknife covariance
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Shirasaki, Masato, primary, Takada, Masahiro, additional, Miyatake, Hironao, additional, Takahashi, Ryuichi, additional, Hamana, Takashi, additional, Nishimichi, Takahiro, additional, and Murata, Ryoma, additional
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- 2017
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35. DETECTION OF THE SPLASHBACK RADIUS AND HALO ASSEMBLY BIAS OF MASSIVE GALAXY CLUSTERS
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More, Surhud, primary, Miyatake, Hironao, additional, Takada, Masahiro, additional, Diemer, Benedikt, additional, Kravtsov, Andrey V., additional, Dalal, Neal K., additional, More, Anupreeta, additional, Murata, Ryoma, additional, Mandelbaum, Rachel, additional, Rozo, Eduardo, additional, Rykoff, Eli S., additional, Oguri, Masamune, additional, and Spergel, David N., additional
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- 2016
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36. First data release of the Hyper Suprime-Cam Subaru Strategic Program
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Aihara, Hiroaki, Armstrong, Robert, Bickerton, Steven, Bosch, James, Coupon, Jean, Furusawa, Hisanori, Hayashi, Yusuke, Ikeda, Hiroyuki, Kamata, Yukiko, Karoji, Hiroshi, Kawanomoto, Satoshi, Koike, Michitaro, Komiyama, Yutaka, Lang, Dustin, Lupton, Robert H, Mineo, Sogo, Miyatake, Hironao, Miyazaki, Satoshi, Morokuma, Tomoki, Obuchi, Yoshiyuki, Oishi, Yukie, Okura, Yuki, Price, Paul A, Takata, Tadafumi, Tanaka, Manobu M, Tanaka, Masayuki, Tanaka, Yoko, Uchida, Tomohisa, Uraguchi, Fumihiro, Utsumi, Yousuke, Wang, Shiang-Yu, Yamada, Yoshihiko, Yamanoi, Hitomi, Yasuda, Naoki, Arimoto, Nobuo, Chiba, Masashi, Finet, Francois, Fujimori, Hiroki, Fujimoto, Seiji, Furusawa, Junko, Goto, Tomotsugu, Goulding, Andy, Gunn, James E, Harikane, Yuichi, Hattori, Takashi, Hayashi, Masao, Hełminiak, Krzysztof G, Higuchi, Ryo, Hikage, Chiaki, Ho, Paul T P, Hsieh, Bau-Ching, Huang, Kuiyun, Huang, Song, Imanishi, Masatoshi, Iwata, Ikuru, Jaelani, Anton T, Jian, Hung-Yu, Kashikawa, Nobunari, Katayama, Nobuhiko, Kojima, Takashi, Konno, Akira, Koshida, Shintaro, Kusakabe, Haruka, Leauthaud, Alexie, Lee, Chien-Hsiu, Lin, Lihwai, Lin, Yen-Ting, Mandelbaum, Rachel, Matsuoka, Yoshiki, Medezinski, Elinor, Miyama, Shoken, Momose, Rieko, More, Anupreeta, More, Surhud, Mukae, Shiro, Murata, Ryoma, Murayama, Hitoshi, Nagao, Tohru, Nakata, Fumiaki, Niida, Mana, Niikura, Hiroko, Nishizawa, Atsushi J, Oguri, Masamune, Okabe, Nobuhiro, Ono, Yoshiaki, Onodera, Masato, Onoue, Masafusa, Ouchi, Masami, Pyo, Tae-Soo, Shibuya, Takatoshi, Shimasaku, Kazuhiro, Simet, Melanie, Speagle, Joshua, Spergel, David N, Strauss, Michael A, Sugahara, Yuma, Sugiyama, Naoshi, Suto, Yasushi, Suzuki, Nao, Tait, Philip J, Takada, Masahiro, Terai, Tsuyoshi, Toba, Yoshiki, Turner, Edwin L, Uchiyama, Hisakazu, Umetsu, Keiichi, Urata, Yuji, Usuda, Tomonori, Yeh, Sherry, and Yuma, Suraphong
- Abstract
The Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) is a three-layered imaging survey aimed at addressing some of the most important outstanding questions in astronomy today, including the nature of dark matter and dark energy. The survey has been awarded 300 nights of observing time at the Subaru Telescope, and it started in 2014 March. This paper presents the first public data release of HSC-SSP. This release includes data taken in the first 1.7 yr of observations (61.5 nights), and each of the Wide, Deep, and UltraDeep layers covers about 108, 26, and 4 square degrees down to depths of i∼ 26.4, ∼26.5, and ∼27.0 mag, respectively (5 σ for point sources). All the layers are observed in five broad bands (grizy), and the Deep and UltraDeep layers are observed in narrow bands as well. We achieve an impressive image quality of 0${^{\prime\prime}_{.}}$6 in the iband in the Wide layer. We show that we achieve 1%–2% point spread function (PSF) photometry (root mean square) both internally and externally (against Pan-STARRS1), and ∼10 mas and 40 mas internal and external astrometric accuracy, respectively. Both the calibrated images and catalogs are made available to the community through dedicated user interfaces and database servers. In addition to the pipeline products, we also provide value-added products such as photometric redshifts and a collection of public spectroscopic redshifts. Detailed descriptions of all the data can be found online. The data release website is https://hsc-release.mtk.nao.ac.jp.
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- 2018
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37. Characterization and photometric performance of the Hyper Suprime-Cam Software Pipeline
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Huang, Song, Leauthaud, Alexie, Murata, Ryoma, Bosch, James, Price, Paul, Lupton, Robert, Mandelbaum, Rachel, Lackner, Claire, Bickerton, Steven, Miyazaki, Satoshi, Coupon, Jean, and Tanaka, Masayuki
- Abstract
The Subaru Strategic Program (SSP) is an ambitious multi-band survey using the Hyper Suprime-Cam (HSC) on the Subaru telescope. The Wide layer of the SSP is both wide and deep, reaching a detection limit of i∼ 26.0 mag. At these depths, it is challenging to achieve accurate, unbiased, and consistent photometry across all five bands. The HSC data are reduced using a pipeline that builds on the prototype pipeline for the Large Synoptic Survey Telescope. We have developed a Python-based, flexible framework to inject synthetic galaxies into real HSC images, called SynPipe. Here we explain the design and implementation of SynPipeand generate a sample of synthetic galaxies to examine the photometric performance of the HSC pipeline. For stars, we achieve 1% photometric precision at i∼ 19.0 mag and 6% precision at i∼ 25.0 in the iband (corresponding to statistical scatters of ∼0.01 and ∼0.06 mag respectively). For synthetic galaxies with single-Sérsic profiles, forced CModelphotometry achieves 13% photometric precision at i∼ 20.0 mag and 18% precision at i∼ 25.0 in the iband (corresponding to statistical scatters of ∼0.15 and ∼0.22 mag respectively). We show that both forcedpoint spread function and CModelphotometry yield unbiased color estimates that are robust to seeing conditions. We identify several caveats that apply to the version of HSC pipeline used for the first public HSC data release (DR1) that need to be taking into consideration. First, the degree to which an object is blended with other objects impacts the overall photometric performance. This is especially true for point sources. Highly blended objects tend to have larger photometric uncertainties, systematically underestimated fluxes, and slightly biased colors. Secondly, >20% of stars at 22.5 < i< 25.0 mag can be misclassified as extended objects. Thirdly, the current CModelalgorithm tends to strongly underestimate the half-light radius and ellipticity of galaxy with i> 21.5 mag.
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- 2018
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38. The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey
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Mandelbaum, Rachel, Miyatake, Hironao, Hamana, Takashi, Oguri, Masamune, Simet, Melanie, Armstrong, Robert, Bosch, James, Murata, Ryoma, Lanusse, François, Leauthaud, Alexie, Coupon, Jean, More, Surhud, Takada, Masahiro, Miyazaki, Satoshi, Speagle, Joshua S, Shirasaki, Masato, Sifón, Cristóbal, Huang, Song, Nishizawa, Atsushi J, Medezinski, Elinor, Okura, Yuki, Okabe, Nobuhiro, Czakon, Nicole, Takahashi, Ryuichi, Coulton, William R, Hikage, Chiaki, Komiyama, Yutaka, Lupton, Robert H, Strauss, Michael A, Tanaka, Masayuki, and Utsumi, Yousuke
- Abstract
We present and characterize the catalog of galaxy shape measurements that will be used for cosmological weak lensing measurements in the Wide layer of the first year of the Hyper Suprime-Cam (HSC) survey. The catalog covers an area of 136.9 deg2split into six fields, with a mean i-band seeing of 0${^{\prime\prime}_{.}}$58 and 5σ point-source depth of i∼ 26. Given conservative galaxy selection criteria for first-year science, the depth and excellent image quality results in unweighted and weighted source number densities of 24.6 and 21.8 arcmin−2, respectively. We define the requirements for cosmological weak lensing science with this catalog, then focus on characterizing potential systematics in the catalog using a series of internal null tests for problems with point-spread function (PSF) modeling, shear estimation, and other aspects of the image processing. We find that the PSF models narrowly meet requirements for weak lensing science with this catalog, with fractional PSF model size residuals of approximately 0.003 (requirement: 0.004) and the PSF model shape correlation function ρ1< 3 × 10−7(requirement: 4 × 10−7) at 0${^{\circ}_{.}}$5 scales. A variety of galaxy shape-related null tests are statistically consistent with zero, but star–galaxy shape correlations reveal additive systematics on >1° scales that are sufficiently large as to require mitigation in cosmic shear measurements. Finally, we discuss the dominant systematics and the planned algorithmic changes to reduce them in future data reductions.
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- 2018
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39. The Hyper Suprime-Cam software pipeline
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Bosch, James, Armstrong, Robert, Bickerton, Steven, Furusawa, Hisanori, Ikeda, Hiroyuki, Koike, Michitaro, Lupton, Robert, Mineo, Sogo, Price, Paul, Takata, Tadafumi, Tanaka, Masayuki, Yasuda, Naoki, AlSayyad, Yusra, Becker, Andrew C, Coulton, William, Coupon, Jean, Garmilla, Jose, Huang, Song, Krughoff, K Simon, Lang, Dustin, Leauthaud, Alexie, Lim, Kian-Tat, Lust, Nate B, MacArthur, Lauren A, Mandelbaum, Rachel, Miyatake, Hironao, Miyazaki, Satoshi, Murata, Ryoma, More, Surhud, Okura, Yuki, Owen, Russell, Swinbank, John D, Strauss, Michael A, Yamada, Yoshihiko, and Yamanoi, Hitomi
- Abstract
In this paper, we describe the optical imaging data processing pipeline developed for the Subaru Telescope’s Hyper Suprime-Cam (HSC) instrument. The HSC Pipeline builds on the prototype pipeline being developed by the Large Synoptic Survey Telescope’s Data Management system, adding customizations for HSC, large-scale processing capabilities, and novel algorithms that have since been reincorporated into the LSST codebase. While designed primarily to reduce HSC Subaru Strategic Program (SSP) data, it is also the recommended pipeline for reducing general-observer HSC data. The HSC pipeline includes high-level processing steps that generate coadded images and science-ready catalogs as well as low-level detrending and image characterizations.
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- 2018
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40. The Hyper Suprime-Cam SSP Survey: Overview and survey design
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Aihara, Hiroaki, Arimoto, Nobuo, Armstrong, Robert, Arnouts, Stéphane, Bahcall, Neta A, Bickerton, Steven, Bosch, James, Bundy, Kevin, Capak, Peter L, Chan, James H H, Chiba, Masashi, Coupon, Jean, Egami, Eiichi, Enoki, Motohiro, Finet, Francois, Fujimori, Hiroki, Fujimoto, Seiji, Furusawa, Hisanori, Furusawa, Junko, Goto, Tomotsugu, Goulding, Andy, Greco, Johnny P, Greene, Jenny E, Gunn, James E, Hamana, Takashi, Harikane, Yuichi, Hashimoto, Yasuhiro, Hattori, Takashi, Hayashi, Masao, Hayashi, Yusuke, Hełminiak, Krzysztof G, Higuchi, Ryo, Hikage, Chiaki, Ho, Paul T P, Hsieh, Bau-Ching, Huang, Kuiyun, Huang, Song, Ikeda, Hiroyuki, Imanishi, Masatoshi, Inoue, Akio K, Iwasawa, Kazushi, Iwata, Ikuru, Jaelani, Anton T, Jian, Hung-Yu, Kamata, Yukiko, Karoji, Hiroshi, Kashikawa, Nobunari, Katayama, Nobuhiko, Kawanomoto, Satoshi, Kayo, Issha, Koda, Jin, Koike, Michitaro, Kojima, Takashi, Komiyama, Yutaka, Konno, Akira, Koshida, Shintaro, Koyama, Yusei, Kusakabe, Haruka, Leauthaud, Alexie, Lee, Chien-Hsiu, Lin, Lihwai, Lin, Yen-Ting, Lupton, Robert H, Mandelbaum, Rachel, Matsuoka, Yoshiki, Medezinski, Elinor, Mineo, Sogo, Miyama, Shoken, Miyatake, Hironao, Miyazaki, Satoshi, Momose, Rieko, More, Anupreeta, More, Surhud, Moritani, Yuki, Moriya, Takashi J, Morokuma, Tomoki, Mukae, Shiro, Murata, Ryoma, Murayama, Hitoshi, Nagao, Tohru, Nakata, Fumiaki, Niida, Mana, Niikura, Hiroko, Nishizawa, Atsushi J, Obuchi, Yoshiyuki, Oguri, Masamune, Oishi, Yukie, Okabe, Nobuhiro, Okamoto, Sakurako, Okura, Yuki, Ono, Yoshiaki, Onodera, Masato, Onoue, Masafusa, Osato, Ken, Ouchi, Masami, Price, Paul A, Pyo, Tae-Soo, Sako, Masao, Sawicki, Marcin, Shibuya, Takatoshi, Shimasaku, Kazuhiro, Shimono, Atsushi, Shirasaki, Masato, Silverman, John D, Simet, Melanie, Speagle, Joshua, Spergel, David N, Strauss, Michael A, Sugahara, Yuma, Sugiyama, Naoshi, Suto, Yasushi, Suyu, Sherry H, Suzuki, Nao, Tait, Philip J, Takada, Masahiro, Takata, Tadafumi, Tamura, Naoyuki, Tanaka, Manobu M, Tanaka, Masaomi, Tanaka, Masayuki, Tanaka, Yoko, Terai, Tsuyoshi, Terashima, Yuichi, Toba, Yoshiki, Tominaga, Nozomu, Toshikawa, Jun, Turner, Edwin L, Uchida, Tomohisa, Uchiyama, Hisakazu, Umetsu, Keiichi, Uraguchi, Fumihiro, Urata, Yuji, Usuda, Tomonori, Utsumi, Yousuke, Wang, Shiang-Yu, Wang, Wei-Hao, Wong, Kenneth C, Yabe, Kiyoto, Yamada, Yoshihiko, Yamanoi, Hitomi, Yasuda, Naoki, Yeh, Sherry, Yonehara, Atsunori, and Yuma, Suraphong
- Abstract
Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2-m Subaru telescope on the summit of Mauna Kea in Hawaii. A team of scientists from Japan, Taiwan, and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400 deg2in five broad bands (grizy), with a 5 σ point-source depth of r≈ 26. The Deep layer covers a total of 26 deg2in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5 deg2). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey.
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- 2018
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