分类： 天文学 >> 天文学 提交时间： 2023-02-19
Markus Michael Rau
Roohi Dalal
Tianqing Zhang
Xiangchong Li
Atsushi J. Nishizawa
Surhud More
Rachel Mandelbaum
Michael A. Strauss
Masahiro Takada
摘要： We present posterior sample redshift distributions for the Hyper Suprime-Cam Subaru Strategic Program Weak Lensing three-year (HSC Y3) analysis. Using the galaxies' photometry and spatial cross-correlations, we conduct a combined Bayesian Hierarchical Inference of the sample redshift distributions. The spatial cross-correlations are derived using a subsample of Luminous Red Galaxies (LRGs) with accurate redshift information available up to a photometric redshift of $z < 1.2$. We derive the photometry-based constraints using a combination of two empirical techniques calibrated on spectroscopic- and multiband photometric data that covers a spatial subset of the shear catalog. The limited spatial coverage induces a cosmic variance error budget that we include in the inference. Our cross-correlation analysis models the photometric redshift error of the LRGs to correct for systematic biases and statistical uncertainties. We demonstrate consistency between the sample redshift distributions derived using the spatial cross-correlations, the photometry, and the posterior of the combined analysis. Based on this assessment, we recommend conservative priors for sample redshift distributions of tomographic bins used in the three-year cosmological Weak Lensing analyses.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Hung-Yu Jian
Lihwai Lin
Bau-Ching Hsieh
Kai-Yang Lin
Keiichi Umetsu
Carlos Lopez-Coba
Yusei Koyama
Chin-Hao Hsu
Yung-Chau Su
Yu-Yen Chang
Tadayuki Kodama
Yutaka Komiyama
Surhud More
Atsushi J. Nishizawa
Masamune Oguri
Ichi Tanaka
摘要： We utilize the Hyper Suprime-Cam (HSC) Wide Survey to explore the properties of galaxies located in the voids identified from the Baryon Oscillation Spectroscopic Survey (BOSS) up to z~0.7. The HSC reaches i~25, allowing us to characterize the void galaxies down to 10$^{9.2}$ solar mass. We find that the revised void galaxy densities, when including faint galaxies in voids defined by bright galaxies, are still underdense compared to the mean density from the entire field. In addition, we classify galaxies into star-forming, quiescent, and green valley populations, and find that void galaxies tend to have slightly higher fractions of star-forming galaxies under the mass and redshift control, although the significance of this result is only moderate (2$\sigma$). However, when we focus on the star-forming population, the distribution of the specific star formation rate (sSFR) of void galaxies shows little difference from that of the control galaxies. Similarly, the median sSFR of star-forming void galaxies is also in good agreement with that of the star-forming control galaxies. Moreover, the effective green valley fraction of void galaxies, defined as the number of green valley galaxies over the number of nonquiescent galaxies, is comparable to that of the control ones, supporting the suggestion that void and control galaxies evolve under similar physical processes and quenching frequencies. Our results thus favor a scenario of the galaxy assembly bias.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Wenting Wang
Xiangchong Li
Jingjing Shi
Jiaxin Han
Naoki Yasuda
Yipeng Jing
Surhud More
Masahiro Takada
Hironao Miyatake
Atsushi J. Nishizawa
摘要： Using photometric galaxies from the HSC survey, we measure the stellar mass density profiles for satellite galaxies as a function of the projected distance, $r_p$, to isolated central galaxies (ICGs) selected from SDSS/DR7 spectroscopic galaxies at $z\sim0.1$. By stacking HSC images, we also measure the projected stellar mass density profiles for ICGs and their stellar halos. The total mass distributions are further measured from HSC weak lensing signals. ICGs dominate within $\sim$0.15 times the halo virial radius ($0.15R_{200}$). The stellar mass versus total mass fractions drop with the increase in $r_p$ up to $\sim0.15R_{200}$, beyond which they are less than 1\% while stay almost constant, indicating the radial distribution of satellites trace dark matter. The total stellar mass in satellites is proportional to the virial mass of the host halo, $M_{200}$, for ICGs more massive than $10^{10.5}M_\odot$, i.e., $M_{\ast,\mathrm{sat}} \propto M_{200}$, whereas the relation between the stellar mass of ICGs $+$ stellar halos and $M_{200}$ is close to $M_{\ast,\mathrm{ICG+diffuse}}\propto M_{200}^{1/2}$. Below $10^{10.5}M_\odot$, the change in $M_{200}$ is much slower with the decrease in $M_{\ast,\mathrm{ICG+diffuse}}$. At fixed stellar mass, red ICGs are hosted by more massive dark matter halos and have more satellites. At $M_{200}\sim10^{12.7}M_\odot$, both $M_{\ast,\mathrm{sat}}$ and the fraction of stellar mass in satellites versus total stellar mass, $f_\mathrm{sat}$, tend to be slightly higher around blue ICGs, perhaps implying the late formation of blue galaxies. $f_\mathrm{sat}$ increases with the increase in both $M_{\ast,\mathrm{ICG+diffuse}}$ and $M_{200}$, and scales more linearly with $M_{200}$. We provide best-fitting formulas for these scaling relations and for red and blue ICGs separately.
分类： 天文学 >> 天文学 提交时间： 2023-02-19
Xiangchong Li
Hironao Miyatake
Wentao Luo
Surhud More
Masamune Oguri
Takashi Hamana
Rachel Mandelbaum
Masato Shirasaki
Masahiro Takada
Robert Armstrong
Arun Kannawadi
Satoshi Takita
Satoshi Miyazaki
Atsushi J. Nishizawa
Andrés A. Plazas Malagón
Michael A. Strauss
Masayuki Tanaka
Naoki Yoshida
摘要： We present the galaxy shear catalog that will be used for the three-year cosmological weak gravitational lensing analyses using data from the Wide layer of the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) Survey. The galaxy shapes are measured from the $i$-band imaging data acquired from 2014 to 2019 and calibrated with image simulations that resemble the observing conditions of the survey based on training galaxy images from the Hubble Space Telescope in the COSMOS region. The catalog covers an area of 433.48 deg$^2$ of the northern sky, split into six fields. The mean $i$-band seeing is 0.59 arcsec. With conservative galaxy selection criteria (e.g., $i$-band magnitude brighter than 24.5), the observed raw galaxy number density is 22.9 arcmin$^{-2}$, and the effective galaxy number density is 19.9 arcmin$^{-2}$. The calibration removes the galaxy property-dependent shear estimation bias to a level: $|\delta m|1$ degree scales and will require mitigation during the inference of cosmological parameters using cosmic shear measurements.
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