Indirect probe of electroweak-interacting particles at the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>μ</mml:mi><mml:mi>TRISTAN</mml:mi></mml:mrow></mml:math> <mml:math xmlns:mml="http://www.w3.org/199

A novel collider, called <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>μ</a:mi><a:mi>TRISTAN</a:mi></a:math>, was recently proposed, offering the capability to achieve high-energy collisions of antimuons. This high-energy collider presents an exceptional opportunity for the discovery of electroweak-interacting massive particles (EWIMPs), which are predicted by various new physics models. In a lepton collider like <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mi>μ</c:mi><c:mi>TRISTAN</c:mi></c:math>, the potential for discovering EWIMPs extends beyond their direct production. Quantum corrections arising from EWIMP loops can significantly enhance our prospects for discovery by precise measurement of Standard Model processes. This study focuses on the indirect detection method within the <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>μ</e:mi><e:mi>TRISTAN</e:mi></e:math> experiment, with a specific emphasis on TeV-scale EWIMP dark matter scenarios that yield the correct thermal relic density. At collision energies for <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:mrow><g:msqrt><g:mrow><g:mi>s</g:mi></g:mrow></g:msqrt><g:mo>=</g:mo><g:mi>O</g:mi><g:mo stretchy="false">(</g:mo><g:mn>1</g:mn><g:mi>–</g:mi><g:mn>10</g:mn><g:mo stretchy="false">)</g:mo><g:mtext> </g:mtext><g:mtext> </g:mtext><g:mi>TeV</g:mi></g:mrow></g:math>, these EWIMPs introduce noticeable effects, typically in the range of <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:mrow><k:mi>O</k:mi><k:mo stretchy="false">(</k:mo><k:mn>0.1</k:mn><k:mi>–</k:mi><k:mn>1</k:mn><k:mo stretchy="false">)</k:mo><k:mo>%</k:mo></k:mrow></k:math>. Our findings indicate that at <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:msqrt><o:mi>s</o:mi></o:msqrt><o:mo>=</o:mo><o:mn>2</o:mn><o:mo stretchy="false">(</o:mo><o:mn>10</o:mn><o:mo stretchy="false">)</o:mo><o:mtext> </o:mtext><o:mtext> </o:mtext><o:mi>TeV</o:mi></o:math>, with an integrated luminosity of <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" display="inline"><s:mrow><s:mn>10</s:mn><s:mtext> </s:mtext><s:mtext> </s:mtext><s:msup><s:mrow><s:mi>ab</s:mi></s:mrow><s:mrow><s:mo>−</s:mo><s:mn>1</s:mn></s:mrow></s:msup></s:mrow></s:math>, <u:math xmlns:u="http://www.w3.org/1998/Math/MathML" display="inline"><u:mi>μ</u:mi><u:mi>TRISTAN</u:mi></u:math> can detect Higgsinos at a mass of 1.3 (3.0) TeV and winos at a mass of 1.9 (4.4) TeV, assuming an optimistic level of systematic uncertainty in the observation of the Standard Model processes. Published by the American Physical Society 2024