Transverse Velocities with the Moving Lens Effect

Hotinli, Selim C.; Meyers, Joel; Dalal, Neal; Jaffe, A. H.; Johnson, Matthew C.; Mertens, James B.; Münchmeyer, Moritz; Smith, Kendrick M.; Engelen, Alexander van

doi:10.1103/physrevlett.123.061301

Cited by 47 publications

(44 citation statements)

References 91 publications

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“…[24,[47][48][49][50], and the transverse velocity fields from the moving lens effect e.g. [51][52][53]. Including these effects in our forecasts, we do not see a significant improvement upon the constraints presented in this work, although we note that using these effects without kSZ can still considerably improve upon past constraints.…”

Section: Discussionmentioning

confidence: 53%

Probing correlated compensated isocurvature perturbations using scale-dependent galaxy bias

et al. 2019

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Compensated isocurvature perturbations (CIPs) are modulations of the relative baryon and dark matter density that leave the total matter density constant. The best current constraints from the primary cosmic microwave background (CMB) are consistent with CIPs some two orders of magnitude larger in amplitude than adiabatic perturbations, suggesting that there may be a huge gap in our knowledge of the early Universe. However, it was recently suggested by Barreira et. al. that CIPs which are correlated with the primordial curvature perturbation, as arises in some versions of the curvaton model, lead to a new observable: scale dependent galaxy bias. Combining a galaxy survey with an unbiased tracer of the density field facilitates a measurement of the amplitude of correlated CIPs that is free from cosmic variance, the main limitation on constraints from the primary CMB. Among the most promising tracers to use for this purpose is the remote dipole field, reconstructed using the technique of kinetic Sunyaev Zel'dovich (kSZ) tomography. In this paper, we evaluate the detection significance on the amplitude of correlated CIPs possible with next-generation CMB and galaxy surveys using kSZ tomography. Our analysis includes all relativistic contributions to the observed galaxy number counts and allows for both CIPs and primordial non-Gaussianity, which also gives rise to a scale dependent galaxy bias. We find that kSZ tomography can probe CIPs of comparable amplitude to the adiabatic fluctuations, representing an improvement of over two orders of magnitude upon current constraints, and an order of magnitude over what will be possible using future CMB or galaxy surveys alone.

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Section: Discussionmentioning

confidence: 53%

Probing correlated compensated isocurvature perturbations using scale-dependent galaxy bias

et al. 2019

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“…The BG effect [58][59][60][61] induces a temperature dipole, of a magnitude comparable to that of the rkSZ effect, with a decrease in CMB temperature following the galaxies' transverse proper motion (and a temperature increase opposite to the transverse proper motion). Regardless of the presence of systematic alignments between the directions of galaxies' spins and their proper motionsinduced, for instance, by filaments [57,[62][63][64]]-, we don't expect any systematic alignment in their sense.…”

Section: Detection Feasibilitymentioning

confidence: 91%

Probing gaseous galactic halos through the rotational kinematic Sunyaev-Zeldovich effect

Matilla

Haiman

2020

Phys. Rev. D

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The rotational kinematic Sunyaev-Zeldovich (rkSZ) signal, imprinted on the cosmic microwave background (CMB) by the gaseous halos (spinning "atmospheres") of foreground galaxies, would be a novel probe of galaxy formation. Although the signal is too weak to detect in individual galaxies, we analyze the feasibility of its statistical detection via stacking CMB data on many galaxies for which the spin orientation can be estimated spectroscopically. We use an "optimistic" model, in which fully ionized atmospheres contain the cosmic baryon fraction and spin at the halo's circular velocity vcirc, and a more realistic model, based on hydrodynamical simulations, with multi-phase atmospheres spinning at a fraction of vcirc. We incorporate realistic noise estimates into our analysis. Using low-redshift galaxy properties from the MaNGA spectroscopic survey (with median halo mass of 6.6 × 10 11 M ), and CMB data quality from Planck, we find that a 3σ detection would require a few×10 4 galaxies, even in the optimistic model. This is too high for current surveys, but upcoming higher-angular resolution CMB experiments will significantly reduce the requirements: stacking CMB data on galaxy spins in a ∼ 10 deg 2 can rule out the optimistic models, and ≈350 deg 2 will suffice for a 3σ detection with ACT. As a proof-of-concept, we stacked Planck data on the position of ≈ 2, 000 MaNGA galaxies, aligned with the galaxies' projected spin, and scaled to their halos' angular size. We rule out average temperature dipoles larger than ≈ 1.9 µK around field spiral galaxies.

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“…Figure taken from Ref. [54]. The signal-to-noise improvement due to a change in angular resolution from 5 to 1.4 is evident, whereas further decreasing the beam size produces only marginal improvement…”

Section: Cosmic Velocity Fields With the Ksz And Moving Lens Effectsmentioning

confidence: 99%

“…However, this signal is proportional to the cluster deflection angle instead of its optical depth, and due to the smallness of the former quantity, it is roughly 10-100 times smaller than the kSZ signal. In spite of that, there are realistic predictions for the detection of the moving lens effect, by constructing an optimized filter for its unique dipole-like pattern, and cross-correlating it with large galaxy catalogs expected from future optical surveys like the Rubin Observatory [54,59]. In particular it has been shown [54] that for a future CMB experiment with sensitivity of ∼ 1 μK-arcmin or better, an improvement of angular resolution from 5 to 1.4 will cause an increase in the signal-to-noise ratio by roughly a factor of 4-5 (Fig.…”

Section: Cosmic Velocity Fields With the Ksz And Moving Lens Effectsmentioning

confidence: 99%

A space mission to map the entire observable universe using the CMB as a backlight

et al. 2021

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This Science White Paper, prepared in response to the ESA Voyage 2050 call for long-term mission planning, aims to describe the various science possibilities that can be realized with an L-class space observatory that is dedicated to the study of the interactions of cosmic microwave background (CMB) photons with the cosmic web. Our aim is specifically to use the CMB as a backlight – and survey the gas, total mass, and stellar content of the entire observable Universe by means of analyzing the spatial and spectral distortions imprinted on it. These distortions result from two major processes that impact on CMB photons: scattering by free electrons and atoms (Sunyaev-Zeldovich effect in diverse forms, Rayleigh scattering, resonant scattering) and deflection by gravitational potential (lensing effect). Even though the list of topics collected in this White Paper is not exhaustive, it helps to illustrate the exceptional diversity of major scientific questions that can be addressed by a space mission that will reach an angular resolution of 1.5 arcmin (goal 1 arcmin), have an average sensitivity better than 1 μK-arcmin, and span the microwave frequency range from roughly 50 GHz to 1 THz. The current paper also highlights the synergy of our Backlight mission concept with several upcoming and proposed ground-based CMB experiments.

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Transverse Velocities with the Moving Lens Effect

Cited by 47 publications

References 91 publications

Probing correlated compensated isocurvature perturbations using scale-dependent galaxy bias

Probing correlated compensated isocurvature perturbations using scale-dependent galaxy bias

Probing gaseous galactic halos through the rotational kinematic Sunyaev-Zeldovich effect

A space mission to map the entire observable universe using the CMB as a backlight

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