Cross-correlation of the thermal Sunyaev–Zel’dovich effect and weak gravitational lensing: Planck and Subaru Hyper Suprime-Cam first-year data

ABSTRACT Cross-correlation analysis of the thermal Sunyaev–Zel’dovich (tSZ) effect and weak gravitational lensing (WL) provides a powerful probe of cosmology and astrophysics of the intracluster medium. We present the measurement of the cross-correlation of tSZ and WL from Planck and Subaru Hyper-Suprime Cam. The combination enables us to study cluster astrophysics at high redshift. We use the tSZ-WL cross-correlation and the tSZ autopower spectrum measurements to place a tight constraint on the hydrostatic mass bias, which is a measure of the degree of non-thermal pressure support in galaxy clusters. With the prior on cosmological parameters derived from the analysis of the cosmic microwave background anisotropies by Planck and taking into account foreground contributions both in the tSZ autopower spectrum and the tSZ-WL cross-correlation, the hydrostatic mass bias is estimated to be $26.9^{+8.9}_{-4.4} {{\ \rm per\ cent}}$ ($68{{\ \rm per\ cent}}$ CL), which is consistent with recent measurements by mass calibration techniques.

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High redshift quasars monitoring campaign

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314004438 ◽

2013 ◽

Vol 9 (S304) ◽

pp. 409-410

Author(s):

Ismael Botti ◽

Paulina Lira ◽

Jorge Martinez ◽

Hagai Netzer ◽

Shai Kaspi

Keyword(s):

Cross Correlation ◽

High Redshift ◽

Mapping Technique ◽

Broad Line ◽

Black Hole Mass ◽

Massive Black Holes ◽

Monitoring Campaign ◽

Reverberation Mapping ◽

Line Region ◽

Cross Correlation Analysis

AbstractWe present an update of the monitoring campaign we have undertaken to probe the most massive black holes in powerful quasars at high redshift through the reverberation mapping technique. Once this campaign has finished, we will be able to directly measure broad line region (BLR) sizes of quasars at z ~ 2−3, improving dramatically the BLR size-luminosity relation, and therefore, black hole mass estimates based on this relationship. So far, we have identified a dozen highly variable sources suitable for future cross-correlation analysis and reverberation measurements.

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Weak Gravitational Lensing of High‐Redshift 21 cm Power Spectra

The Astrophysical Journal ◽

10.1086/505480 ◽

2006 ◽

Vol 647 (2) ◽

pp. 719-736 ◽

Cited By ~ 20

Author(s):

Kaisey S. Mandel ◽

Matias Zaldarriaga

Keyword(s):

Gravitational Lensing ◽

High Redshift ◽

Power Spectra ◽

Weak Gravitational Lensing

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Cosmology with the submillimetre galaxies magnification bias: Proof of concept

Astronomy and Astrophysics ◽

10.1051/0004-6361/202038050 ◽

2020 ◽

Vol 639 ◽

pp. A128

Author(s):

L. Bonavera ◽

J. González-Nuevo ◽

M. M. Cueli ◽

T. Ronconi ◽

M. Migliaccio ◽

...

Keyword(s):

Gravitational Lensing ◽

Cross Correlation ◽

Mass Density ◽

Cosmological Parameters ◽

Monte Carlo Analysis ◽

Model Description ◽

Proof Of Concept ◽

Photometric Redshifts ◽

Density Profiles ◽

Background Sample

Context. As recently demonstrated, high-z submillimetre galaxies (SMGs) are the perfect background sample for tracing the mass density profiles of galaxies and clusters (baryonic and dark matter) and their time-evolution through gravitational lensing. Their magnification bias, a weak gravitational lensing effect, is a powerful tool for constraining the free parameters of a halo occupation distribution (HOD) model and potentially also some of the main cosmological parameters. Aims. The aim of this work is to test the capability of the magnification bias produced on high-z SMGs as a cosmological probe. We exploit cross-correlation data to constrain not only astrophysical parameters (Mmin, M1, and α), but also some of the cosmological ones (Ωm, σ8, and H0) for this proof of concept. Methods. The measured cross-correlation function between a foreground sample of GAMA galaxies with spectroscopic redshifts in the range 0.2 < z < 0.8 and a background sample of H-ATLAS galaxies with photometric redshifts > 1.2 is modelled using the traditional halo model description that depends on HOD and cosmological parameters. These parameters are then estimated by performing a Markov chain Monte Carlo analysis using different sets of priors to test the robustness of the results and to study the performance of this novel observable with the current set of data. Results. With our current results, Ωm and H0 cannot be well constrained. However, we can set a lower limit of > 0.24 at 95% confidence level (CL) on Ωm and we see a slight trend towards H0 > 70 values. For our constraints on σ8 we obtain only a tentative peak around 0.75, but an interesting upper limit of σ8 ≲ 1 at 95% CL. We also study the possibility to derive better constraints by imposing more restrictive priors on the astrophysical parameters.

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Weak gravitational lensing effects on cosmological parameters and dark energy from gamma-ray bursts

Astronomy and Astrophysics ◽

10.1051/0004-6361/201117517 ◽

2011 ◽

Vol 536 ◽

pp. A96 ◽

Cited By ~ 19

Author(s):

F. Y. Wang ◽

Z. G. Dai

Keyword(s):

Dark Energy ◽

Gravitational Lensing ◽

Gamma Ray ◽

Cosmological Parameters ◽

Gamma Ray Bursts ◽

Weak Gravitational Lensing

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XMM-Newton X-ray and HST weak gravitational lensing study of the extremely X-ray luminous galaxy cluster Cl J120958.9+495352 (z = 0.902)

Astronomy and Astrophysics ◽

10.1051/0004-6361/201730913 ◽

2018 ◽

Vol 610 ◽

pp. A71 ◽

Cited By ~ 1

Author(s):

Sophia Thölken ◽

Tim Schrabback ◽

Thomas H. Reiprich ◽

Lorenzo Lovisari ◽

Steven W. Allen ◽

...

Keyword(s):

Temperature Profile ◽

Gravitational Lensing ◽

Mass Fraction ◽

High Redshift ◽

Galaxy Cluster ◽

Cooling Time ◽

Weak Lensing ◽

Imaging Data ◽

Weak Gravitational Lensing ◽

X Ray

Context. Observations of relaxed, massive, and distant clusters can provide important tests of standard cosmological models, for example by using the gas mass fraction. To perform this test, the dynamical state of the cluster and its gas properties have to be investigated. X-ray analyses provide one of the best opportunities to access this information and to determine important properties such as temperature profiles, gas mass, and the total X-ray hydrostatic mass. For the last of these, weak gravitational lensing analyses are complementary independent probes that are essential in order to test whether X-ray masses could be biased. Aims. We study the very luminous, high redshift (z = 0.902) galaxy cluster Cl J120958.9+495352 using XMM-Newton data. We measure global cluster properties and study the temperature profile and the cooling time to investigate the dynamical status with respect to the presence of a cool core. We use Hubble Space Telescope (HST) weak lensing data to estimate its total mass and determine the gas mass fraction. Methods. We perform a spectral analysis using an XMM-Newton observation of 15 ks cleaned exposure time. As the treatment of the background is crucial, we use two different approaches to account for the background emission to verify our results. We account for point spread function effects and deproject our results to estimate the gas mass fraction of the cluster. We measure weak lensing galaxy shapes from mosaic HST imaging and select background galaxies photometrically in combination with imaging data from the William Herschel Telescope. Results. The X-ray luminosity of Cl J120958.9+495352 in the 0.1–2.4 keV band estimated from our XMM-Newton data is LX = (13.4−1.0+1.2) × 1044 erg/s and thus it is one of the most X-ray luminous clusters known at similarly high redshift. We find clear indications for the presence of a cool core from the temperature profile and the central cooling time, which is very rare at such high redshifts. Based on the weak lensing analysis, we estimate a cluster mass of M500 / 1014 M⊙ = 4.4−2.0+2.2(star.) ± 0.6(sys.) and a gas mass fraction of fgas,2500 = 0.11−0.03+0.06 in good agreement with previous findings for high redshift and local clusters.

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Cosmology with weak lensing surveys

Philosophical Transactions of The Royal Society A Mathematical Physical and Engineering Sciences ◽

10.1098/rsta.2005.1672 ◽

2005 ◽

Vol 363 (1837) ◽

pp. 2675-2691 ◽

Cited By ~ 6

Author(s):

Dipak Munshi ◽

Patrick Valageas

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Gravitational Lensing ◽

Large Scale ◽

High Redshift ◽

Cosmological Parameters ◽

Power Spectra ◽

Weak Lensing ◽

Satellite Mission ◽

The Universe

Weak gravitational lensing is responsible for the shearing and magnification of the images of high-redshift sources due to the presence of intervening mass. Since the lensing effects arise from deflections of the light rays due to fluctuations of the gravitational potential, they can be directly related to the underlying density field of the large-scale structures. Weak gravitational surveys are complementary to both galaxy surveys and cosmic microwave background observations as they probe unbiased nonlinear matter power spectra at medium redshift. Ongoing CMBR experiments such as WMAP and a future Planck satellite mission will measure the standard cosmological parameters with unprecedented accuracy. The focus of attention will then shift to understanding the nature of dark matter and vacuum energy: several recent studies suggest that lensing is the best method for constraining the dark energy equation of state. During the next 5 year period, ongoing and future weak lensing surveys such as the Joint Dark Energy Mission (JDEM; e.g. SNAP) or the Large-aperture Synoptic Survey Telescope will play a major role in advancing our understanding of the universe in this direction. In this review article, we describe various aspects of probing the matter power spectrum and the bispectrum and other related statistics with weak lensing surveys. This can be used to probe the background dynamics of the universe as well as the nature of dark matter and dark energy.

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The mass–richness relation of optically selected clusters from weak gravitational lensing and abundance with Subaru HSC first-year data

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/psz092 ◽

2019 ◽

Vol 71 (5) ◽

Cited By ~ 19

Author(s):

Ryoma Murata ◽

Masamune Oguri ◽

Takahiro Nishimichi ◽

Masahiro Takada ◽

Rachel Mandelbaum ◽

...

Keyword(s):

Gravitational Lensing ◽

Signal To Noise Ratio ◽

High Redshift ◽

First Year ◽

Model Parameters ◽

Redshift Range ◽

Photometric Redshift ◽

Related Science ◽

The Mean ◽

Log Normal

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 ≤ zcl ≤ 1.0 with N ≥ 15 using the HSC first-year shear catalog covering ∼140 deg2. The exquisite depth and image quality of the HSC survey allow us to measure lensing signals around high-redshift clusters at 0.7 ≤ zcl ≤ 1.0 with a signal-to-noise ratio of 19 within the comoving radius range $0.5\lesssim R\lesssim 15\, h^{-1}\:{\rm Mpc}$. We constrain the richness–mass relations P(ln N ∣ M, z) of 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 proportional to ln (1 + z) and [ln (1 + z)]2 in 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 redshift. We show that constraints on the mean relation 〈M ∣ N〉 are consistent between the Planck and WMAP models, whereas the scatter values σln 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.

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Cosmological Applications of Gravitational Lensing

Symposium - International Astronomical Union ◽

10.1017/s0074180900110095 ◽

1996 ◽

Vol 168 ◽

pp. 209-217

Author(s):

Peter Schneider

Keyword(s):

Gravitational Lensing ◽

High Redshift ◽

Cosmological Parameters ◽

Gravitational Lens ◽

Mass Determination ◽

Gravitational Lenses ◽

Distant Object ◽

The Many ◽

The Universe

It was recognized very early that the gravitational lens effect can be used as an efficient cosmological tool. Of the many researchers who foresaw the use of lensing, F. Zwicky and S. Refsdal should be explicitly mentioned. The perhaps most accurate predictions and foresights by these two authors are as follows: Zwicky estimated the probability that a distant object is multiply imaged to be about 1/400, and thus that the observation of this effect is “a certainty” [73] – his value, which was obtained by a very crude reasoning, is in fact very close to current estimates of the lensing probability of high-redshift QSOs. He predicted that the magnification caused by gravitational light deflection will allow a “deeper look” into the universe –in fact, the spectroscopy of very faint galaxies which are imaged into giant luminous arcs have yielded spectral information which would be very difficult to obtain without these ‘natural telescopes’. And third, Zwicky saw that gravitational lenses may be used to determine the mass of distant extragalactic objects[72] – in fact, the mass determination of clusters masses from giant luminous arcs is as least as accurate as other methods, but does not rely on special assumptions (like spherical symmetry, virial or thermal equilibrium) inherent in other methods, and the determination of the mass within the inner 0.9 arcseconds of the lensing galaxy in the quadruple QSO 2237+0305 to within 2% [52] is the most accurate extragalactic mass determination known. Refsdal predicted the use of gravitational lenses for determining cosmological parameters and for testing cosmological theories [48][49] – we shall return to these issues below.

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