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Chiu, Chih‐Chou; Shao, Yuehjen E.; Lee, Tian–Shyug; Lee, Ker-Ming

doi:10.1023/a:1024657911399

Cited by 52 publications

(7 citation statements)

References 26 publications

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“…Thus the extended emission in halos is correlated with the mass of the dark matter halo that provides the gravitational potential well in which the galaxies reside (White & Frenk 1991;Kereš et al 2005;van de Voort et al 2011;Correa et al 2018). Studies show that even the stellar mass in galaxies is correlated with the host dark matter halo mass (e.g., Moster et al 2010;Shankar et al 2014;Chiu et al 2016). Observations suggest that pointed X-ray emission in galaxies too are correlated with stellar luminosity and stellar mass thereof (e.g., Forman et al 1985;Trinchieri & Fabbiano 1985;Canizares et al 1987;Sarazin et al 2000;Strickland et al 2002;Kim & Fabbiano 2003;Sivakoff et al 2003;Fab-FIG.…”

Section: Discussionmentioning

confidence: 99%

X-Ray Surface Brightness Profiles of Optically Selected Active Galactic Nuclei: Comparison with X-Ray AGNs

Mukherjee

Bhattacharjee²,

Chatterjee

et al. 2019

ApJ

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We use data from the All Wavelength Extended Groth Strip International Survey to construct stacked X-ray maps of optically bright active galaxies (AGN) and an associated control sample of galaxies at high redshift (z ∼ 0.6). From our analysis of the surface brightness profiles obtained from these X-ray maps, we find evidence of feedback from the active nuclei. We find that excluding galaxies and AGN, residing in group environments, from our samples enhances the significance of our detection. Our results support the tentative findings of Chatterjee et al. who use X-ray selected AGN for their analysis. We discuss the implications of these results in the context of quantifying AGN feedback and show that the current method can be used to extract X-ray source population in high redshift galaxies.

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Section: Discussionmentioning

confidence: 99%

X-Ray Surface Brightness Profiles of Optically Selected Active Galactic Nuclei: Comparison with X-Ray AGNs

Mukherjee

Bhattacharjee²,

Chatterjee

et al. 2019

ApJ

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“…We briefly introduce the likelihood and fitting framework below and refer the reader to previous publications for more details (Liu et al 2015;Chiu et al 2016c). This likelihood is designed to obtain the parameters of the targeted X-ray observable-mass-redshift scaling relation (e.g., r X ) for a given sample that is selected using another observable (e.g., the SPT signal-to-noise ξ), for which the observable-mass-redshift relation is already known (e.g., equation (3) used in this work).…”

Section: Fitting Proceduresmentioning

confidence: 99%

“…We have verified that this likelihood recovers unbiased scaling relation parameters by testing it against large mocks (> 1300 clusters). Moreover, it has been further optimized in the goal of obtaining the parameters of scaling relations in a high dimensional space (Chiu et al 2016c). We note that in each iteration of the chain we use the current value of R 500 for each cluster to recalculate the M ICM (see Section 3.2).…”

Section: Fitting Proceduresmentioning

confidence: 99%

X-Ray Properties of SPT-selected Galaxy Clusters at 0.2 < z < 1.5 Observed with XMM-Newton

Bulbul

Chiu

Mohr

et al. 2019

ApJ

118

173

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We present measurements of the X-ray observables of the intra-cluster medium (ICM), including luminosity L X , ICM mass M ICM , emission-weighted mean temperature T X , and integrated pressure Y X , that are derived from XMM-Newton X-ray observations of a Sunyaev-Zel'dovich Effect (SZE) selected sample of 59 galaxy clusters from the South Pole Telescope SPT-SZ survey that span the redshift range of 0.20 < z < 1.5. We constrain the best-fit power law scaling relations between X-ray observables, redshift, and halo mass. The halo masses are estimated based on previously published SZE observable to mass scaling relations, calibrated using information that includes the halo mass function. Employing SZE-based masses in this sample enables us to constrain these scaling relations for massive galaxy clusters (M 500 ≥ 3 × 10 14 M ) to the highest redshifts where these clusters exist without concern for X-ray selection biases. We find that the mass trends are steeper than self-similarity in all cases, and with ≥ 2.5σ significance in the case of L X and M ICM . The redshift trends are consistent with the self-similar expectation, but the uncertainties remain large. Core-included scaling relations tend to have steeper mass trends for L X . There is no convincing evidence for a redshift-dependent mass trend in any observable. The constraints on the amplitudes of the fitted scaling relations are currently limited by the systematic uncertainties on the SZE-based halo masses, however the redshift and mass trends are limited by the X-ray sample size and the measurement uncertainties of the X-ray observables. −0.16 7 3 0.28 +0.07 −0.09 0.02 +0.48 −0.58 0.76 +0.76 −0.71 III with fixed SZE params 9.93 +0.58 −0.49 1.90 +0.13 −0.18 7 3 0.25 +0.07 −0.06 −0.18 +0.48 −0.32 0.80 +0.93 −0.57

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“…Specifically, we assume an underlying N-M relation characterized by its log-normal intrinsic scatter at fixed mass and evaluate the probability of observing the weak-lensing magnification signal for a given richness. This method has been widely used in previous work to calibrate the observable-to-mass relation of a cluster sample with a well-defined selection function (Chiu et al 2016b;Chiu et al 2018a;Bulbul et al 2018). In addition, the effects of Malmquist and Eddington bias are fully accounted for in this approach.…”

Section: Modelling Of the Scaling Relationmentioning

confidence: 99%

The richness-to-mass relation of CAMIRA galaxy clusters from weak-lensing magnification in the Subaru Hyper Suprime-Cam survey

Chiu

Umetsu

Murata

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a statistical weak-lensing magnification analysis on an optically selected sample of 3029 CAMIRA galaxy clusters with richness N > 15 in the Subaru Hyper Suprime-Cam (HSC) survey. The CAMIRA sample spans a wide redshift range of 0.2 z < 1.1. We use two distinct populations of color-selected, flux-limited background galaxies, namely the low-z and high-z samples at mean redshifts of ≈ 1.1 and ≈ 1.4, 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 CAMIRA sample is detected at a significance level of 8.29σ , which is dominated by the high-z background. We forward-model the observed magnification data to constrain the richness-to-mass (N-M) relation for the CAMIRA sample. In this work, we can only constrain the normalization of the N-M relation by employing informative priors on the mass and redshift trends, and on the intrinsic scatter at fixed mass. The resulting scaling relation is N ∝ M 500 0.91±0.14 (1 + z) −0.45±0.75 , with a characteristic richness of N = (19.63 ± 3.16) and intrinsic log-normal scatter of 0.14 ± 0.07 at M 500 = 10 14 h −1 M . With the derived N-M relation, we provide magnification-calibrated mass estimates of individual CAMIRA clusters, with the typical uncertainty of ≈ 38% and ≈ 30% at richness≈ 20 and ≈ 40, respectively. We further compare our magnification-inferred N-M relation with those from the shear-based results in the literature, finding good agreement.

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Untitled

Cited by 52 publications

References 26 publications

X-Ray Surface Brightness Profiles of Optically Selected Active Galactic Nuclei: Comparison with X-Ray AGNs

X-Ray Surface Brightness Profiles of Optically Selected Active Galactic Nuclei: Comparison with X-Ray AGNs

X-Ray Properties of SPT-selected Galaxy Clusters at 0.2 < z < 1.5 Observed with XMM-Newton

The richness-to-mass relation of CAMIRA galaxy clusters from weak-lensing magnification in the Subaru Hyper Suprime-Cam survey

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