Dr. Sehgal et al reply

Sehgal, Rahul; Ernste, Floranne C.; Eckloff, Sara

doi:10.3899/jrheum.211190

Cited by 10 publications

(13 citation statements)

References 7 publications

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“…For both models, the average redshift of all the clusters, z = 0.78, is used. tion et al 2011;Draper et al 2012;Sehgal et al 2013;Saro et al 2017), and we explore that possibility here. For example, Saro et al (2017) [S17] used a sample of DES redMaPPer clusters and measured their SZ signal by stacking in SPT (South Pole Telescope) data in multiple richness bins.…”

Section: Richness To Mass Scalingmentioning

confidence: 81%

“…The SZ signals of low-richness, optically-selected clus-ters are smaller than expected from mass-richness relationships, which are usually calibrated with high-richness clusters (Planck Collaboration et al 2011;Draper et al 2012;Sehgal et al 2013;Saro et al 2017). Several possible explanations for this discrepancy are: radio or infrared point source contamination of the SZ signal, line-of-sight projections contaminating richness measurements, cluster miscentering, variable gas mass fractions in optically selected clusters, or more fundamentally, a lower amplitude for the massrichness relation.…”

Section: Introductionmentioning

confidence: 99%

“…Although studies of low mass halos using the SZ effect will become more common as CMB telescopes become more sensitive, for now we depend on stacking, or averaging, multiple clusters that have been detected by other means. Spatially coherent stacking allows the use of the SZ effect to extend to lower masses, as it averages out contributions from the CMB, atmosphere, and detector noise (Saro et al 2017;Sehgal et al 2013;Planck Collaboration et al 2011;Hand et al 2011).…”

Section: Introductionmentioning

confidence: 99%

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The Atacama Cosmology Telescope: SZ-based masses and dust emission from IR-selected cluster candidates in the SHELA survey

Fuzia,

Kawinwanichakij,

Mehrtens

et al. 2020

Preprint

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We examine the stacked thermal Sunyaev-Zel'dovich (SZ) signals for a sample of galaxy cluster candidates from the Spitzer-HETDEX Exploratory Large Area (SHELA) Survey, which are identified in combined optical and infrared SHELA data using the redMaPPer algorithm. We separate the clusters into three richness bins, with average photometric redshifts ranging from 0.70 to 0.80. The richest bin shows a clear temperature decrement at 148 GHz in the Atacama Cosmology Telescope data, which we attribute to the SZ effect. All richness bins show an increment at 220 GHz, which we attribute to dust emission from cluster galaxies. We correct for dust emission using stacked profiles from Herschel Stripe 82 data, and allow for synchrotron emission using stacked profiles created by binning source fluxes from NVSS data. We see dust emission in all three richness bins, but can only confidently detect the SZ decrement in the highest richness bin, finding M 500 = 8.7 +1.7 −1.3 × 10 13 M . Neglecting the correction for dust depresses the inferred mass by 26 percent, indicating a partial fill-in of the SZ decrement from thermal dust and synchrotron emission by the cluster member galaxies. We compare our corrected SZ masses to two redMaPPer mass-richness scaling relations and find that the SZ mass is lower than predicted by the richness. We discuss possible explanations for this discrepancy, and note that the SHELA richnesses may differ from previous richness measurements due to the inclusion of IR data in redMaPPer.

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Section: Richness To Mass Scalingmentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Atacama Cosmology Telescope: SZ-based masses and dust emission from IR-selected cluster candidates in the SHELA survey

Fuzia,

Kawinwanichakij,

Mehrtens

et al. 2020

Preprint

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“…The lensing potential can be reconstructed using a minimum-variance quadratic estimator [7,8] using both CMB temperature and polarization maps. Ongoing and upcoming experiments, including Advanced ACT [9], SPT-3G [10], and Simons Observatory (SO) [11], have sensitivities for which temperature maps provide most of the statistical weight for lensing reconstruction; proposed future experiments such as CMB-S4 [12] and CMB-HD [13] will have high enough sensitivity so that polarization becomes the dominant channel for lensing reconstruction.…”

Section: Introductionmentioning

confidence: 99%

The Bias to Cosmic Microwave Background Lensing Reconstruction from the Kinematic Sunyaev-Zel'dovich Effect at Reionization

Cai,

Madhavacheril,

Hill

et al. 2021

Preprint

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The power spectrum of reconstructed cosmic microwave background (CMB) lensing maps is a powerful tool for constraints on cosmological parameters like the sum of the neutrino masses and the dark energy equation of state. One possible complication is the kinematic Sunyaev-Zel'dovich (kSZ) effect, due to the scattering of CMB photons by moving electrons, which can bias the reconstruction of the CMB lensing power spectrum through both kSZ-lensing correlations and the non-Gaussianity of the kSZ temperature anisotropies. We investigate for the first time the bias to CMB lensing reconstruction from temperature anisotropies due to the reionization-induced kSZ signal and show that it is negligible for both ongoing and upcoming experiments based on current numerical simulations of reionization. We also revisit the bias induced by the late-time kSZ field, using more recent kSZ simulations. We find that it is potentially twice as large as found in earlier studies, reaching values as large as several percent of the CMB lensing power spectrum signal, indicating that this bias will have to be mitigated in upcoming data analyses.

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“…Along with the large angular scale measurements of the CMB signal, observations from the ongoing and upcoming high resolution ground-based CMB experiments (such as the Atacama Cosmology Telescope (ACTPol) (Thornton et al 2016), South Pole Telescope (SPT) (Benson et al 2014), Simons Observatory (Aguirre et al 2018), and CMB-S4 (Abazajian et al 2019)), can also explore the small angular scale anisotropies in CMB temperature and polarization field. Proposed CMB mission concepts (such as Probe of Inflation and Cosmic Origins (PICO) (Hanany et al 2019), CMB-Bharat 1 , CMB-HD (Sehgal et al 2020), and the proposal submitted to Voyage-2050 (Delabrouille et al 2019)) are also capable to probe secondary anisotropies in the CMB with high angular resolution. The small angular scale CMB anisotropies are rich source of information about secondary CMB anisotropies which are generated after the surface last scattering which is around z ∼ 1080.…”

Section: Introductionmentioning

confidence: 99%

Inevitable imprints of patchy reionization on the cosmic microwave background anisotropy

Paul,

Mukherjee,

Choudhury

2020

Preprint

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Reionization of the cosmic neutral hydrogen by the first stars in the Universe is an inhomogeneous process which produces spatial fluctuations in free electron density. These fluctuations lead to observable signatures in cosmological probes like the cosmic microwave background (CMB). We explore the effect of the electron density fluctuations on CMB using photon-conserving semi-numerical simulations of reionization named SCRIPT. We show that the amplitude of the kinematic Sunyaev-Zeldovich (kSZ) and B-mode polarization signal depends on the electron density fluctuations along with the dependence on mid-point and extent of the reionization history. Motivated by this finding, we provide new scaling relations for the amplitude of kSZ and B-mode polarization signal which can capture the effects arising from the mean optical depth, width of reionization, and spatial fluctuations in the electron density. We show that the amplitude of the kSZ and B-mode polarization signal exhibits different dependency on the width of reionization and spatial fluctuations, and hence a joint study of these CMB probes will be able to break the degeneracy. By combining external datasets from 21 cm measurements, the degeneracy can be further lifted by directly exploring the sizes of the ionized regions.

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Dr. Sehgal et al reply

Abstract: We appreciate the interest of Wang et al1 in our case.2 We agree with several of their comments and would like to clarify a few details here.

Cited by 10 publications

References 7 publications

The Atacama Cosmology Telescope: SZ-based masses and dust emission from IR-selected cluster candidates in the SHELA survey

The Atacama Cosmology Telescope: SZ-based masses and dust emission from IR-selected cluster candidates in the SHELA survey

The Bias to Cosmic Microwave Background Lensing Reconstruction from the Kinematic Sunyaev-Zel'dovich Effect at Reionization

Inevitable imprints of patchy reionization on the cosmic microwave background anisotropy

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