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Astrophysical Constraints on Inflationary Dark Matter in the Luminogenesis Model
High Energy Physics - Phenomenology · Submitted 5 Aug 2015
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The luminogenesis model is additionally subject to constraints on inflation, and we find an upper bound on the scale of symmetry breaking of the inflaton and the decoupling scale $M_1$ of certain representations of the gauge group.
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The abstract, sentence by sentence
The assumption of collisionless cold dark matter on its own cannot reconcile several astrophysical discrepancies (cusp-vs-core problem, missing satellite problem, too-big-to-fail problem). Self-interacting dark matter provides a promising framework for solving all these problems, and self-interaction cross sections are duly constrained in the literature. Following the work of Tulin, Yu, and Zurek [1], we can constrain the dark matter mass and the mass of a light mediator assuming a generic scalar Yukawa-type interaction. In particular, we constrain the strongly coupled inflationary dark matter of the luminogenesis model, a unification model with the gauge group $SU(3)_C \times SU(6) \times U(1)_Y$, which breaks to the Standard Model with an extra gauge group for dark matter when the inflaton rolls into its true vacuum. The luminogenesis model is additionally subject to constraints on inflation, and we find an upper bound on the scale of symmetry breaking of the inflaton and the decoupling scale $M_1$ of certain representations of the gauge group. We emphasize that the luminogenesis model enables a unique connection between astrophysical constraints, the nature of dark matter, and inflation.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The assumption of collisionless cold dark matter on its own cannot reconcile several astrophysical discrepancies (cusp-vs-core problem, missing satellite problem, too-big-to-fail problem). | background 0.95 | 0.06 | 0.04 | asserted 1.00 |
| s1 | Self-interacting dark matter provides a promising framework for solving all these problems, and self-interaction cross sections are duly constrained in the literature. | background 1.00 | 0.04 | 0.05 | hedged possibility 0.56 |
| s2 | Following the work of Tulin, Yu, and Zurek [1], we can constrain the dark matter mass and the mass of a light mediator assuming a generic scalar Yukawa-type interaction. | method 0.88 | 0.46 | 0.06 | asserted 0.72 |
| s3 | In particular, we constrain the strongly coupled inflationary dark matter of the luminogenesis model, a unification model with the gauge group $SU(3)_C \times SU(6) \times U(1)_Y$, which breaks to the Standard Model with an extra gauge group for dark matter when the inflaton rolls into its true vacuum. | contribution 0.93 | 0.55 | 0.12 | asserted 0.99 |
| s4 | The luminogenesis model is additionally subject to constraints on inflation, and we find an upper bound on the scale of symmetry breaking of the inflaton and the decoupling scale $M_1$ of certain representations of the gauge group. | result 0.98 | 0.94 | 0.28 | asserted 1.00 |
| s5 | We emphasize that the luminogenesis model enables a unique connection between astrophysical constraints, the nature of dark matter, and inflation. | interpretation 0.97 | 0.31 | 0.34 | asserted 0.99 |
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The paper
Original abstract
The assumption of collisionless cold dark matter on its own cannot reconcile several astrophysical discrepancies (cusp-vs-core problem, missing satellite problem, too-big-to-fail problem). Self-interacting dark matter provides a promising framework for solving all these problems, and self-interaction cross sections are duly constrained in the literature. Following the work of Tulin, Yu, and Zurek [1], we can constrain the dark matter mass and the mass of a light mediator assuming a generic scalar Yukawa-type interaction. In particular, we constrain the strongly coupled inflationary dark matter of the luminogenesis model, a unification model with the gauge group $SU(3)_C \times SU(6) \times U(1)_Y$, which breaks to the Standard Model with an extra gauge group for dark matter when the inflaton rolls into its true vacuum. The luminogenesis model is additionally subject to constraints on inflation, and we find an upper bound on the scale of symmetry breaking of the inflaton and the decoupling scale $M_1$ of certain representations of the gauge group. We emphasize that the luminogenesis model enables a unique connection between astrophysical constraints, the nature of dark matter, and inflation.
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What this paper does with the arXiv papers it cites
What it cites · 20 sentences without a confident label
Uses the method or tool of 1 paper
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N-body simulations are needed to accurately analyze the velocity-dependent scattering cross section in the non-classical, resonant regime, but we approximate the transfer cross section by averaging over the initial DM velocities $v⃗_1,2$ with exponential weight, as is done in [ref] , and we apply astrophysical constraints to this velocity-averaged transfer cross section, given by ⟨σ_T ⟩= ∫ d^3 v_1 d^3 v_2/(πv_0^2)^3 e^-v_1^2/v_0^2 e^-v_2^2/v_0^2 σ_T(|v⃗_1 -v⃗_2|) = ∫d^3 v/(2πv_0^2)^3/2 e^-1/2 v^2/v_0^2 σ_T(v) , where $v_0$ is the most probable velocity and $v = |v⃗_1 -v⃗_2|$ is the relative velocity.
Beyond Collisionless Dark Matter: Particle Physics Dynamics for Dark Matter Halo Structure · Introduction · 1.00
Uses data or values from 2 papers
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Since $SU(6)$ breaks at the DUT scale when the inflaton slips into its true vacuum, we specify the DUT scale and therefore the dynamical mass of $χ$ by constraining the parameters of a symmetry-breaking (Coleman-Weinberg) inflaton potential with Planck's constraints on the scalar spectral index and amplitude [ref] .
Planck 2013 results. XVI. Cosmological parameters · Introduction · 0.82
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Since $SU(6)$ breaks at the DUT scale when the inflaton slips into its true vacuum, we specify the DUT scale and therefore the dynamical mass of $χ$ by constraining the parameters of a symmetry-breaking (Coleman-Weinberg) inflaton potential with Planck's constraints on the scalar spectral index and amplitude [ref] .
Planck 2013 results. XXII. Constraints on inflation · Introduction · 0.82
Compares with 2 papers
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For almost all of $m_X < 100$ GeV, we found regions of parameter space that did not grossly disagree with the three astrophysical constraints, similar to the results of the resonant regimes in Fig. 6 of [ref] .
Beyond Collisionless Dark Matter: Particle Physics Dynamics for Dark Matter Halo Structure · Introduction · 0.91
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We will compare these predictions from [ref] to the results from this paper's application of astrophysical constraints to dark matter mass.
Constraining Inflationary Dark Matter in the Luminogenesis Model · Introduction · 1.00
Cites as background 1 paper
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The representations and group structure of the luminogenesis model for each of the three families are given below [ref] .
Luminogenesis from Inflationary Dark Matter · Introduction · 0.80
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