Heating up the Galaxy with hidden photons

Dubovsky, Sergei; Hernández-Chifflet, Guzmán

doi:10.1088/1475-7516/2015/12/054

Cited by 59 publications

(94 citation statements)

References 27 publications

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“…For the range of dark photon masses coinciding with the SM photon plasma mass in this redshift range, m A ∼ 10 −13 eV, this bound is stronger than previous cosmological limits [11] by 5 orders of magnitude and stronger than bounds on local collapsed objects [29,30] by 4 orders of magnitude. We note that these bounds will scale quadratically in , so the bound for ∆ρ A ≤ 0.5 eV ×n b is trivially obtained by rescaling our HeII limit by √ 2.…”

Section: Helium II Reionizationmentioning

confidence: 52%

Cosmological evolution of light dark photon dark matter

McDermott

Witte

2020

Phys. Rev. D

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Light dark photons are subject to various plasma effects, such as Debye screening and resonant oscillations, which can lead to a more complex cosmological evolution than is experienced by conventional cold dark matter candidates. Maintaining a consistent history of dark photon dark matter requires ensuring that the super-thermal abundance present in the early Universe (i) does not deviate significantly after the formation of the CMB, and (ii) does not excessively leak into the Standard Model plasma after BBN. We point out that the role of non-resonant absorption, which has previously been neglected in cosmological studies of this dark matter candidate, produces strong constraints on dark photon dark matter with mass as low as 10 −22 eV. Furthermore, we show that resonant conversion of dark photons after recombination can produce excessive heating of the IGM which is capable of prematurely reionizing hydrogen and helium, leaving a distinct imprint on both the Ly−α forest and the integrated optical depth of the CMB. Our constraints surpass existing cosmological bounds by more than five orders of magnitude across a wide range of dark photon masses.

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Section: Helium II Reionizationmentioning

confidence: 52%

Cosmological evolution of light dark photon dark matter

McDermott

Witte

2020

Phys. Rev. D

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“…In the medium it is decomposed into longitudinal and transverse components, Im Π L,T , as shown in Eq. (12) in the main text. The factor I νσ is the 2-body final state integrated over its phase space,…”

Section: Full Expression Of χ-Pair Production Ratementioning

confidence: 99%

“…However, a decoupling of stellar constraints as 2 m 2 V [5] when m V arises from a Stuckelberg mechanism, opens the opportunity to explore a vast parameter region through direct, laboratory searches, in particular if V is the dark matter (DM), see, e.g. [6][7][8][9][10][11][12][13][14][15][16][17][18][19][20].…”

Section: Introductionmentioning

confidence: 99%

Stellar probes of dark sector-photon interactions

et al. 2019

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Electromagnetically neutral dark sector particles may directly couple to the photon through higher dimensional effective operators. Considering electric and magnetic dipole moment, anapole moment, and charge radius interactions, we derive constraints from stellar energy loss in the Sun, horizontal branch and red giant stars, as well as from cooling of the proto-neutron star of SN1987A. We provide the exact formula for in-medium photon-mediated pair production to leading order in the dark coupling, and compute the energy loss rates explicitly for the most important processes, including a careful discussion on resonances and potential double counting between the processes. Stringent limits for dark states with masses below 3 keV (40 MeV) arise from red giant stars (SN1987A), implying an effective lower mass-scale of approximately 10 9 GeV (10 7 GeV) for mass-dimension five, and 100 GeV (2.5 TeV) for mass-dimension six operators as long as dark states stream freely; for the proto-neutron star, the trapping of dark states is also evaluated. Together with direct limits previously derived by us in Chu et al. (2018), this provides the first comprehensive overview of the viability of effective electromagnetic dark-state interactions below the GeV mass-scale.

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“…Such collisions will lead to the same kinetic energy of A and ψ, thus cool ψ due to the large number of A . However, there could also be absorption of A which could heat the plasma [76], where the rate of absorption is roughly the collision rate of ψ themselves. In Fig.…”

Section: Discussionmentioning

confidence: 99%

Co-interacting dark matter

2019

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We propose a novel mechanism with two component dark matter models. The subdominant dark matter can thermalize the dominant one in galaxies, and leads to core density profiles. Using ultralight dark photons and GeV-TeV Dirac fermions as an example, we couple the two dark matter candidates with a U (1) interaction. This mechanism differs from self-interacting dark matter, due to three effects: (1) higher occupation numbers, (2) forward-backward scattering cancellation, and (3) the multiple scatterings required for the heavy dark matter. Furthermore, the Bullet Cluster bound is evaded due to the reduced Bose enhancement factor. Unlike the fuzzy dark matter solution to the small structure problems which have tension with Lyman-α, the ultralight dark photons with mass 10 −21 eV can have a core profile through interactions with ψ and are not constrained by other astrophysical observations.

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Heating up the Galaxy with hidden photons

Cited by 59 publications

References 27 publications

Cosmological evolution of light dark photon dark matter

Cosmological evolution of light dark photon dark matter

Stellar probes of dark sector-photon interactions

Co-interacting dark matter

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