The Atacama Large Millimeter/submillimeter Array

Wootten, Alwyn; Thompson, A. Richard

doi:10.48550/arxiv.0904.3739

Cited by 2 publications

(4 citation statements)

References 9 publications

(9 reference statements)

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“…[24]). We will consider angular resolutions between ∼ 0.1 ′′ and 1 ′ , noticing that Planck [11] and ALMA [12,13] could reach resolutions of ∼ 5 ′ and ∼ 1 ′′ , respectively.…”

Section: Jcap02(2010)005mentioning

confidence: 99%

“…The question that we JCAP02(2010)005 address in this paper is whether or not this deviation is observable in light of the contradictory results found by [5][6][7] on the one hand, and by [10] on the other hand. In particular, we investigate whether the Planck satellite [11], which was recently launched, and the ALMA facilities [12,13] will have the sensitivity to detect the SZ signal induced by DM annihilation or decay and could constrain the DM properties.…”

Section: Introductionmentioning

confidence: 99%

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On the Sunyaev-Zel'dovich effect from dark matter annihilation or decay in galaxy clusters

Lavalle

Bœhm

Barthès

2010

J. Cosmol. Astropart. Phys.

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We revisit the prospects for detecting the Sunyaev Zel'dovich (SZ) effect induced by dark matter (DM) annihilation or decay. We show that with standard (or even extreme) assumptions for DM properties, the optical depth associated with relativistic electrons injected from DM annihilation or decay is much smaller than that associated with thermal electrons, when averaged over the angular resolution of current and future experiments. For example, we find: τ DM ∼ 10 −9 − 10 −5 (depending on the assumptions) for m χ = 1 GeV and a density profile ρ ∝ r −1 for a template cluster located at 50 Mpc and observed within an angular resolution of 10 ′′ , compared to τ th ∼ 10 −3 − 10 −2 . This, together with a full spectral analysis, enables us to demonstrate that, for a template cluster with generic properties, the SZ effect due to DM annihilation or decay is far below the sensitivity of the Planck satellite. This is at variance with previous claims regarding heavier annihilating DM particles. Should DM be made of lighter particles, the current constraints from 511 keV observations on the annihilation cross section or decay rate still prevent a detectable SZ effect. Finally, we show that spatial diffusion sets a core of a few kpc in the electron distribution, even for very cuspy DM profiles, such that improving the angular resolution of the instrument, e.g. with ALMA, does not necessarily improve the detection potential. We provide useful analytical formulae parameterized in terms of the DM mass, decay rate or annihilation cross section and DM halo features, that allow quick estimates of the SZ effect induced by any given candidate and any DM halo profile.

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Section: Jcap02(2010)005mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

On the Sunyaev-Zel'dovich effect from dark matter annihilation or decay in galaxy clusters

Lavalle

Bœhm

Barthès

2010

J. Cosmol. Astropart. Phys.

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“…The typical optical depth leading to observable thermal SZ is τ e 10 −3 in galaxy clusters [11], which provides us with a benchmark value useful for further comparisons, while current and coming experiments can reach micro-Kelvin temperature fluctuations, or equivalently τ e ∼ 10 −4 (e.g. [26][27][28]).…”

Section: Sizing the Sz Amplitude: The Electron Optical Depthmentioning

confidence: 99%

“…This value, which roughly sizes the amplitude of the SZ signal expected from high latitudes, is very small, much smaller than the typical optical depth found for Galactic thermal electrons and, more importantly, than the current experimental sensitivities. Indeed, we recall that new generation experiments, like Planck [26] or ALMA [27,28], can hardly constrain electron populations of optical depths 10 −4 . We emphasize that we used a rather light WIMP mass of 1 GeV in this estimate (see e.g.…”

Section: Smooth-halo Contributionmentioning

confidence: 99%

Sunyaev-Zel’dovich effects from annihilating dark matter in the Milky Way: Smooth halo, subhalos, and intermediate-mass black holes

Lavalle

2010

Phys. Rev. D

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We study the Sunyaev-Zel'dovich effect potentially generated by relativistic electrons injected from dark matter annihilation or decay in the Galaxy, and check whether it could be observed by Planck or the Atacama Large Millimeter Array (ALMA), or even imprint the current CMB data as, e.g., the specific fluctuation excess claimed from an recent reanalysis of the WMAP-5 data. We focus on high-latitude regions to avoid contamination of the Galactic astrophysical electron foreground, and consider the annihilation or decay coming from the smooth dark matter halo as well as from subhalos, further extending our analysis to a generic modeling of spikes arising around intermediate-mass black holes. We show that all these dark Galactic components are unlikely to produce any observable Sunyaev-Zel'dovich effect. For a self-annihilating dark matter particle of 10 GeV with canonical properties, the largest optical depth we find is e & 10 À7 for massive isolated subhalos hosting intermediate-mass black holes. We conclude that dark matter annihilation or decay on the Galactic scale cannot lead to significant SunyaevZel'dovich distortions of the CMB spectrum.

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The Atacama Large Millimeter/submillimeter Array

Cited by 2 publications

References 9 publications

On the Sunyaev-Zel'dovich effect from dark matter annihilation or decay in galaxy clusters

On the Sunyaev-Zel'dovich effect from dark matter annihilation or decay in galaxy clusters

Sunyaev-Zel’dovich effects from annihilating dark matter in the Milky Way: Smooth halo, subhalos, and intermediate-mass black holes

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