Issue |
A&A
Volume 690, October 2024
|
|
---|---|---|
Article Number | A359 | |
Number of page(s) | 9 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/202451246 | |
Published online | 18 October 2024 |
A high-resolution view of the source-plane magnification near cluster caustics in wave dark matter models
1
Instituto de Física de Cantabria (CSIC-UC). Avda. Los Castros s/n.
39005
Santander,
Spain
2
Department of Physics, The University of Hong Kong,
Pokfulam Road,
Hong Kong
3
Department of Physics, University of the Basque Country UPV/EHU,
48080
Bilbao,
Spain
4
DIPC, Basque Country UPV/EHU,
48080
San Sebastian,
Spain
5
Ikerbasque, Basque Foundation for Science,
48011
Bilbao,
Spain
6
School of Earth and Space Exploration, Arizona State University,
Tempe,
AZ
85287-6004,
USA
7
Physics Department, Ben-Gurion University of the Negev,
PO Box 653,
Be’er-Sheva
84105,
Israel
8
Department of Astronomy, University of California,
Berkeley,
CA
94720-3411,
USA
9
Minnesota Institute for Astrophysics, University of Minnesota,
116 Church Street SE,
Minneapolis,
MN
55455,
USA
10
School of Physics and Astronomy, University of Minnesota,
116 Church Street,
Minneapolis,
MN
55455,
USA
11
Department of Physics, Oklahoma State University,
145 Physical Sciences Bldg,
Stillwater,
OK
74078,
USA
★ Corresponding author; jdiego@ifca.unican.es
Received:
25
June
2024
Accepted:
28
August
2024
We present the highest-resolution images to date of caustics formed by wave dark matter (ψDM) fluctuations near the critical curves of cluster gravitational lenses. We describe the basic magnification features of ψDM in the source plane at high macromodel magnification and discuss specific differences between the ψDM and standard cold dark matter (CDM) models. The unique generation of demagnified counterimages (with respect to the magnification from the smooth macromodel) formed outside the Einstein radius for ψDM is highlighted. Substructure in CDM cannot generate demagnified images with positive parity and thus does not provide a definitive way to distinguish ψDM from CDM. Highly magnified background sources with sizes r ≈ 1 pc, or approximately a factor of ten smaller than the expected de Broglie wavelength of ψDM, offer the best possibility for discriminating between ψDM and CDM. These include objects such as very compact stellar clusters at high redshift, which JWST is finding in abundance.
Key words: gravitational lensing: strong / dark matter
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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