Cosmological implications of inflaton-mediated dark and visible matter scatterings after reheating

The initial density of dark matter (DM) particles, otherwise secluded from the standard model (SM), may be generated at reheating, with an initial temperature ratio for internal thermalizations, <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:msub><a:mi>ξ</a:mi><a:mi>i</a:mi></a:msub><a:mo>=</a:mo><a:msub><a:mi>T</a:mi><a:mrow><a:mi>DM</a:mi><a:mo>,</a:mo><a:mi mathvariant="normal">i</a:mi></a:mrow></a:msub><a:mo>/</a:mo><a:msub><a:mi>T</a:mi><a:mrow><a:mi>SM</a:mi><a:mo>,</a:mo><a:mi mathvariant="normal">i</a:mi></a:mrow></a:msub></a:math>. This scenario necessarily implies inflaton-mediated scatterings between DM and SM after reheating, with a rate fixed by the relic abundance of DM and the reheat temperature. These scatterings can be important for an inflaton mass and reheat temperature as high as <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi mathvariant="script">O</e:mi><e:mo stretchy="false">(</e:mo><e:msup><e:mn>10</e:mn><e:mn>7</e:mn></e:msup><e:mtext> </e:mtext><e:mtext> </e:mtext><e:mi>GeV</e:mi><e:mo stretchy="false">)</e:mo></e:math> and <j:math xmlns:j="http://www.w3.org/1998/Math/MathML" display="inline"><j:mi mathvariant="script">O</j:mi><j:mo stretchy="false">(</j:mo><j:msup><j:mn>10</j:mn><j:mn>9</j:mn></j:msup><j:mtext> </j:mtext><j:mtext> </j:mtext><j:mi>GeV</j:mi><j:mo stretchy="false">)</j:mo></j:math>, respectively, since the thermally averaged collision terms become approximately independent of the inflaton mass when the bath temperature is larger than the mass. The impact of these scatterings on DM cosmology is studied modeling the perturbative reheating physics by a gauge-invariant set of inflaton interactions up to dimension 5 with the SM gauge bosons, fermions, and the Higgs fields. It is observed that an initially lower (higher) DM temperature will rapidly increase (decrease), even with very small couplings to the inflaton. There is a sharp lower bound on the DM mass below which the relic abundance cannot be satisfied due to faster backscatterings depleting DM quanta to SM particles. For low DM masses, the cosmic microwave background constraints become stronger due to the collisions for <o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:msub><o:mi>ξ</o:mi><o:mi>i</o:mi></o:msub><o:mo><</o:mo><o:mn>1</o:mn></o:math>, probing values as small as <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:mi mathvariant="script">O</q:mi><q:mo stretchy="false">(</q:mo><q:msup><q:mn>10</q:mn><q:mrow><q:mo>−</q:mo><q:mn>4</q:mn></q:mrow></q:msup><q:mo stretchy="false">)</q:mo></q:math>, and weaker for <v:math xmlns:v="http://www.w3.org/1998/Math/MathML" display="inline"><v:msub><v:mi>ξ</v:mi><v:mi>i</v:mi></v:msub><v:mo>></v:mo><v:mn>1</v:mn></v:math>. The big-bang nucleosynthesis constraints become stronger due to the collisions for lower DM masses, probing <x:math xmlns:x="http://www.w3.org/1998/Math/MathML" display="inline"><x:msub><x:mi>ξ</x:mi><x:mi>i</x:mi></x:msub></x:math> as small as <z:math xmlns:z="http://www.w3.org/1998/Math/MathML" display="inline"><z:mi mathvariant="script">O</z:mi><z:mo stretchy="false">(</z:mo><z:mn>0.1</z:mn><z:mo stretchy="false">)</z:mo></z:math>, and weaker for higher DM mass. Thus inflaton-mediated collisions with predictable rates, relevant even for high-scale inflation models, can significantly impact the cosmology of light DM. Published by the American Physical Society 2024