A high-resolution view of the source-plane magnification near cluster caustics in wave dark matter models

J. M. Diego; Alfred Amruth; Jose M. Palencia; Tom Broadhurst; Sung Kei Li; Jeremy Lim; Rogier A. Windhorst; Adi Zitrin; Alexei V. Filippenko; Liliya L.R. Williams; Ashish K. Meena; Wenlei Chen; Patrick L. Kelly

doi:https://doi.org/10.1051/0004-6361/202451246

A high-resolution view of the source-plane magnification near cluster caustics in wave dark matter models

J. M. Diego, Alfred Amruth, Jose M. Palencia, Tom Broadhurst, Sung Kei Li, Jeremy Lim, Rogier A. Windhorst, Adi Zitrin, Alexei V. Filippenko, Liliya L.R. Williams, Ashish K. Meena, Wenlei Chen, Patrick L. Kelly

Department of Physics

Ben-Gurion University of the Negev

Research output: Contribution to journal › Article › peer-review

Abstract

We present the highest-resolution images to date of caustics formed by wave dark matter (ÏÃ Â DM) fluctuations near the critical curves of cluster gravitational lenses. We describe the basic magnification features of ÏÃ Â DM in the source plane at high macromodel magnification and discuss specific differences between the ÏÃ Â DM 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 ÏÃ Â DM is highlighted. Substructure in CDM cannot generate demagnified images with positive parity and thus does not provide a definitive way to distinguish ÏÃ Â DM from CDM. Highly magnified background sources with sizes r âÃ Â Ã Â 1 pc, or approximately a factor of ten smaller than the expected de Broglie wavelength of ÏÃ Â DM, offer the best possibility for discriminating between IDM and CDM. These include objects such as very compact stellar clusters at high redshift, which JWST is finding in abundance.

Original language	American English
Article number	A359
Journal	Astronomy and Astrophysics
Volume	690
DOIs	https://doi.org/10.1051/0004-6361/202451246
State	Published - 1 Oct 2024

Keywords

Dark matter
Gravitational lensing: strong

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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https://doi.org/10.1051/0004-6361/202451246

Cite this

Diego, J. M., Amruth, A., Palencia, J. M., Broadhurst, T., Li, S. K., Lim, J., Windhorst, R. A., Zitrin, A., Filippenko, A. V., Williams, L. L. R., Meena, A. K., Chen, W., & Kelly, P. L. (2024). A high-resolution view of the source-plane magnification near cluster caustics in wave dark matter models. Astronomy and Astrophysics, 690, Article A359. https://doi.org/10.1051/0004-6361/202451246

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title = "A high-resolution view of the source-plane magnification near cluster caustics in wave dark matter models",

abstract = "We present the highest-resolution images to date of caustics formed by wave dark matter ({\"I}{\~A} {\^A} DM) fluctuations near the critical curves of cluster gravitational lenses. We describe the basic magnification features of {\"I}{\~A} {\^A} DM in the source plane at high macromodel magnification and discuss specific differences between the {\"I}{\~A} {\^A} DM 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 {\"I}{\~A} {\^A} DM is highlighted. Substructure in CDM cannot generate demagnified images with positive parity and thus does not provide a definitive way to distinguish {\"I}{\~A} {\^A} DM from CDM. Highly magnified background sources with sizes r {\^a}{\~A} {\^A} {\~A} {\^A} 1 pc, or approximately a factor of ten smaller than the expected de Broglie wavelength of {\"I}{\~A} {\^A} DM, offer the best possibility for discriminating between IDM and CDM. These include objects such as very compact stellar clusters at high redshift, which JWST is finding in abundance.",

keywords = "Dark matter, Gravitational lensing: strong",

author = "Diego, {J. M.} and Alfred Amruth and Palencia, {Jose M.} and Tom Broadhurst and Li, {Sung Kei} and Jeremy Lim and Windhorst, {Rogier A.} and Adi Zitrin and Filippenko, {Alexei V.} and Williams, {Liliya L.R.} and Meena, {Ashish K.} and Wenlei Chen and Kelly, {Patrick L.}",

note = "Publisher Copyright: {\textcopyright} The Authors 2024.",

year = "2024",

month = oct,

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doi = "https://doi.org/10.1051/0004-6361/202451246",

language = "American English",

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journal = "Astronomy and Astrophysics",

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T1 - A high-resolution view of the source-plane magnification near cluster caustics in wave dark matter models

AU - Diego, J. M.

AU - Amruth, Alfred

AU - Palencia, Jose M.

AU - Broadhurst, Tom

AU - Li, Sung Kei

AU - Lim, Jeremy

AU - Windhorst, Rogier A.

AU - Zitrin, Adi

AU - Filippenko, Alexei V.

AU - Williams, Liliya L.R.

AU - Meena, Ashish K.

AU - Chen, Wenlei

AU - Kelly, Patrick L.

PY - 2024/10/1

Y1 - 2024/10/1

N2 - We present the highest-resolution images to date of caustics formed by wave dark matter (ÏÃ Â DM) fluctuations near the critical curves of cluster gravitational lenses. We describe the basic magnification features of ÏÃ Â DM in the source plane at high macromodel magnification and discuss specific differences between the ÏÃ Â DM 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 ÏÃ Â DM is highlighted. Substructure in CDM cannot generate demagnified images with positive parity and thus does not provide a definitive way to distinguish ÏÃ Â DM from CDM. Highly magnified background sources with sizes r âÃ Â Ã Â 1 pc, or approximately a factor of ten smaller than the expected de Broglie wavelength of ÏÃ Â DM, offer the best possibility for discriminating between IDM and CDM. These include objects such as very compact stellar clusters at high redshift, which JWST is finding in abundance.

AB - We present the highest-resolution images to date of caustics formed by wave dark matter (ÏÃ Â DM) fluctuations near the critical curves of cluster gravitational lenses. We describe the basic magnification features of ÏÃ Â DM in the source plane at high macromodel magnification and discuss specific differences between the ÏÃ Â DM 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 ÏÃ Â DM is highlighted. Substructure in CDM cannot generate demagnified images with positive parity and thus does not provide a definitive way to distinguish ÏÃ Â DM from CDM. Highly magnified background sources with sizes r âÃ Â Ã Â 1 pc, or approximately a factor of ten smaller than the expected de Broglie wavelength of ÏÃ Â DM, offer the best possibility for discriminating between IDM and CDM. These include objects such as very compact stellar clusters at high redshift, which JWST is finding in abundance.

KW - Dark matter

KW - Gravitational lensing: strong

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U2 - https://doi.org/10.1051/0004-6361/202451246

DO - https://doi.org/10.1051/0004-6361/202451246

M3 - Article

SN - 0004-6361

VL - 690

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A359

ER -

A high-resolution view of the source-plane magnification near cluster caustics in wave dark matter models

Abstract

Keywords

All Science Journal Classification (ASJC) codes

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