Photometric Redshifts for the Hyper Suprime-Cam Subaru Strategic Program Data Release 2

Nishizawa, Atsushi J.; Hsieh, Bau-Ching; Tanaka, Masayuki; Takata, Tadafumi

doi:10.48550/arxiv.2003.01511

Cited by 36 publications

(53 citation statements)

References 34 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We estimate how much stellar mass is changed when including blue galaxies. We first select galaxies from the MIZUKI photometric redshift catalog (Nishizawa et al 2020;Aihara et al 2019;Tanaka et al 2018;Tanaka 2015) with criterion of |z ph − zc| < 0.05(1 + zc) and M * > 10 10 M , where z ph is a photometric redshift. We pick-up galaxies which are not identified in the red galaxy catalog but in the photometric catalog and refer them to as blue galaxies.…”

Section: Blue Galaxies and The Intracluster Lightmentioning

confidence: 99%

“…The Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP; Aihara et al 2018aAihara et al , 2018bMiyazaki et al 2018b;Komiyama et al 2018;Kawanomoto et al 2018;Furusawa et al 2018;Bosch et al 2018;Huang et al 2018b;Coupon et al 2018;Aihara et al 2019;Nishizawa et al 2020) is an on-going wide-field optical imaging survey composed of three layers of different depths (Wide, Deep and UltraDeep). The Wide layer is designed to obtain five-band (grizy) imaging over 1400 deg 2 .…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

HSC-XXL : Baryon budget of the 136 XXL Groups and Clusters

Akino,

Eckert,

Okabe

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

We present our determination of the baryon budget for an X-ray-selected XXL sample of 136 galaxy groups and clusters spanning nearly two orders of magnitude in mass (M 500 ∼ 10 13 − 10 15 M ) and the redshift range 0 < ∼ z < ∼ 1. Our joint analysis is based on the combination of HSC-SSP weak-lensing mass measurements, XXL X-ray gas mass measurements, and HSC and SDSS multiband photometry. We carry out a Bayesian analysis of multivariate mass-scaling relations of gas mass, galaxy stellar mass, stellar mass of brightest cluster galaxies (BCGs), and soft-band X-ray luminosity, by taking into account the intrinsic covariance between cluster properties, selection effect, weak-lensing mass calibration, and observational error covariance matrix. The mass-dependent slope of the gas mass-total mass (M 500 ) relation is found to be 1.29 +0.16 −0.10 , which is steeper than the self-similar prediction of unity, whereas the slope of the stellar mass-total mass relation is shallower than unity, 0.85 +0.12 −0.09 . The BCG stellar mass weakly depends on cluster mass with a slope of 0.49 +0.11 −0.10 . The baryon, gas mass, and stellar mass fractions as a function of M 500 agree with the results from numerical simulations and previous observations. We successfully constrain the full intrinsic covariance of the baryonic contents. The BCG stellar mass shows the larger intrinsic scatter at a given halo total mass, followed in order by stellar mass and gas mass. We find a significant positive intrinsic correlation coefficient between total (and satellite) stellar mass and BCG stellar mass and no evidence for intrinsic correlation between gas mass and stellar mass. All the baryonic components show no redshift evolution.

show abstract

Section: Blue Galaxies and The Intracluster Lightmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

HSC-XXL : Baryon budget of the 136 XXL Groups and Clusters

Akino,

Eckert,

Okabe

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…The HSC-SSP provides several photo-z catalogues 3 (Tanaka et al 2018;Nishizawa et al 2020). We use a photo-z catalogue based on a SED fitting code with Bayesian priors on physical properties of galaxies, called MIZUKI (Tanaka 2015).…”

Section: Photometric Redshift Cataloguementioning

confidence: 99%

A systematic search for galaxy protocluster cores at the transition epoch of their star formation activity

Ando,

Shimasaku,

Momose

et al. 2022

Preprint

View full text Add to dashboard Cite

The redshift of 𝑧 ∼ 1.5 is the transition epoch of protoclusters (PCs) from the star-forming phase into the quenching phase, and hence an appropriate era to investigate the build up of the quenched population. We define a 'core' as the most massive halo in a given PC, where environmental effects are likely to work most effectively, and search for cores at 1 < 𝑧 < 1.5. We use a photometric redshift catalogue of a wide (effective area of ∼ 22.2 deg 2 ) and deep (𝑖 ∼ 26.8 mag) optical survey with Subaru Hyper-Suprime Cam. Regarding galaxies with log(𝑀 * /𝑀 ) > 11.3 as the central galaxies of PC cores, we estimate their average halo mass by clustering analysis and find it to be log(𝑀 h /𝑀 ) ∼ 13.7. An expected mass growth by the Illustris TNG simulation and the observed overdensities around them suggest that the PC cores we find are progenitors of present-day clusters. Classifying our galaxy sample into red and blue galaxies, we calculate the stellar mass function (SMF) and the red galaxy fraction. The SMFs in the PC cores are more-top heavy than field, implying early high-mass galaxy formation and disruption of low-mass galaxies. We also find that the red fraction increases with stellar mass, consistent with stellar-mass dependent environmental quenching recently found at 𝑧 > 1. Interestingly, although the cores with red and blue centrals have similar halo masses, only those with red centrals show a significant red fraction excess compared to the field, suggesting a conformity effect. Some observational features of PC cores may imply that the conformity is caused by assembly bias.

show abstract

“…Since the survey depth is not uniform across the HSC survey, for a low stellar mass limit, some patches remain complete while others may not. Therefore, we use HSC-SSP PDR2 deep field catalog and DEmP photo-z (Nishizawa et al 2020) to study the completeness of galaxies for different stellar mass. We select galaxies with photo-z between 0.5 and 0.7 and calculate the physical properties for these galaxies with five bands grizy using the SED code CIGALE (Boquien et al 2019).…”

Section: Observational Datamentioning

confidence: 99%

“…However, without precise redshift measurement, the usefulness of image surveys is limited. People attempt to infer the photometric redshift from their broad band magnitudes in the image surveys (Ilbert et al 2006(Ilbert et al , 2009Sánchez et al 2014;Nishizawa et al 2020). Photo-z has been used to measure SMF (Fontana et al 2006;Pérez-González et al 2008;Ilbert et al 2010;Bielby et al 2012;McLeod et al 2021) and GC (Crocce et al 2016;Ishikawa et al 2020;Wang et al 2021b), though one has to be very careful about the error and systematics of photo-z especially for faint galaxies.…”

Section: Introductionmentioning

confidence: 99%

Photometric Objects around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. I. Methods

Xu,

Zheng,

Jing

2021

Preprint

View full text Add to dashboard Cite

We provide a method for estimating the projected density distribution n2 w p (r p ) of photometric objects around spectroscopic objects in a redshift survey. This quantity describes the distribution of Photometric sources with certain physical properties (e.g. luminosity, mass, color etc) Around Cosmic webs (PAC) traced by the spectroscopic objects. The method can make full use of current and future deep and wide photometric surveys to explore the formation of galaxies up to medium redshift (z s < 2) a) , with the aid of cosmological redshift surveys that sample only a fairly limited species of objects (e.g. Emission Line Galaxies). As an example, we apply the PAC method to the CMASS spectroscopic and HSC-SSP PDR2 photometric samples to explore the distribution of galaxies for a wide range of stellar mass from 10 9.0 M to 10 12.0 M around massive ones at z s ≈ 0.6. Using the abundance matching method, we model n2 w p (r p ) in N-body simulation using MCMC sampling, and accurately measure the stellar-halo mass relation (SHMR) and stellar mass function (SMF) for the whole mass range. We can also measure the conditional stellar mass function (CSMF) of satellites for central galaxies of different mass. The PAC method has many potential applications for studying the evolution of galaxies.

show abstract

Photometric Redshifts for the Hyper Suprime-Cam Subaru Strategic Program Data Release 2

Cited by 36 publications

References 34 publications

HSC-XXL : Baryon budget of the 136 XXL Groups and Clusters

HSC-XXL : Baryon budget of the 136 XXL Groups and Clusters

A systematic search for galaxy protocluster cores at the transition epoch of their star formation activity

Photometric Objects around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. I. Methods

Contact Info

Product

Resources

About