TY - JOUR

T1 - Postinflationary production of particle dark matter: Hilltop and Coleman-Weinberg inflation

AU - Ghoshal, Anish

AU - Khlopov, Maxim Yu

AU - Lalak, Zygmunt

AU - Porey, Shiladitya

N1 - The authors appreciate the insightful exchanges with Qaisar Shafi. Work of S.\u2009P. is funded by RSF Grant No. 19-42-02004. The research by M.\u2009K. was carried out at Southern Federal University with financial support of the Ministry of Science and Higher Education of the Russian Federation (State Contract No. GZ0110/23-10-IF). Z.\u2009L. has been supported by the Polish National Science Center Grant No. 2017/27/B/ ST2/02531. Postinflationary production of particle dark matter: Hilltop and Coleman-Weinberg inflation / A. Ghoshal, M. Yu. Khlopov, Z. Lalak, Sh. Porey // Physical Review D. – 2024. – Vol. 109, No. 6. – P. 063037. – DOI 10.1103/physrevd.109.063037.

PY - 2024/3/15

Y1 - 2024/3/15

N2 - We investigate the production of nonthermal dark matter (DM), χ, during the postinflationary reheating era. For inflation, we consider two slow roll single field inflationary scenarios - generalized version of Hilltop (GH) inflation, and Coleman-Weinberg (CW) inflation. Using a set of benchmark values that comply with the current constraints from cosmic microwave background radiation (CMBR) data for each inflationary model, we explored the parameter space involving mass of dark matter particles, mχ, and coupling between inflaton and χ, yχ. For these benchmarks, we find that tensor-to-scalar ratio r can be as small as 2.69×10-6 for GH and 1.91×10-3 for CW inflation, both well inside 1-σ contour on scalar spectral index versus r plane from Planck2018+BICEP3+Keck Array2018 dataset, and testable by future cosmic microwave background (CMB) observations, e.g., Simons Observatory. For the production of χ from the inflaton decay satisfying CMB and other cosmological bounds and successfully explaining total cold dark matter density of the present universe, we find that yχ should be within this range O(10-4) yχ O(10-20) for both inflationary scenarios. We also show that, even for the same inflationary scenario, the allowed parameter space on reheating temperature versus mχ plane alters with inflationary parameters including scalar spectral index, r, and energy scale of inflation.

AB - We investigate the production of nonthermal dark matter (DM), χ, during the postinflationary reheating era. For inflation, we consider two slow roll single field inflationary scenarios - generalized version of Hilltop (GH) inflation, and Coleman-Weinberg (CW) inflation. Using a set of benchmark values that comply with the current constraints from cosmic microwave background radiation (CMBR) data for each inflationary model, we explored the parameter space involving mass of dark matter particles, mχ, and coupling between inflaton and χ, yχ. For these benchmarks, we find that tensor-to-scalar ratio r can be as small as 2.69×10-6 for GH and 1.91×10-3 for CW inflation, both well inside 1-σ contour on scalar spectral index versus r plane from Planck2018+BICEP3+Keck Array2018 dataset, and testable by future cosmic microwave background (CMB) observations, e.g., Simons Observatory. For the production of χ from the inflaton decay satisfying CMB and other cosmological bounds and successfully explaining total cold dark matter density of the present universe, we find that yχ should be within this range O(10-4) yχ O(10-20) for both inflationary scenarios. We also show that, even for the same inflationary scenario, the allowed parameter space on reheating temperature versus mχ plane alters with inflationary parameters including scalar spectral index, r, and energy scale of inflation.

UR - http://./https://www.scopus.com/record/display.uri?eid=2-s2.0-85189470769&origin=inward&txGid=a86ad21f4b2dca77673ecb0ad03acd40

UR - https://www.mendeley.com/catalogue/eae5275d-7b94-30be-a8fe-d08cc95b5446/

UR - https://elibrary.ru/item.asp?id=66812428

U2 - 10.1103/PhysRevD.109.063037

DO - 10.1103/PhysRevD.109.063037

M3 - Article

VL - 109

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 6

M1 - 063037

ER -