Dark matter search results from the complete exposure of the PICO-60 
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 bubble chamber

Amole, C.; Ardid, M.; Arnquist, I. J.; Asner, D. M.; Baxter, Daniel; Behnke, E.; Bressler, M.; Broerman, B.; Cao, G.; Chen, C. J.; Chowdhury, U.; Clark, K.; Collar, J. I.; Cooper, P. S.; Coutu, C. B.; Cowles, C.; Crisler, M.; Crowder, Gavin; Cruz-Venegas, N. A.; Dahl, C. E.; Das, Mala; Fallows, S.; Farine, J.; Felis, I.; Filgas, R.; Girard, François; Giroux, G.; Hall, J.; Hardy, Corentin; Harris, Orin; Hillier, Teresa A.; Hoppe, E. W.; Jackson, C. M.; Jin, M.; Klopfenstein, Lorenz Cuno; Kozynets, Tetiana; Krauss, C. B.; Laurin, Mathias; Lawson, I.; Leblanc, Alexandre; Levine, I.; Licciardi, C.; Lippincott, W. H.; Loer, B.; Mamedov, F.; Mitra, P.; Moore, C.; Nania, T.; Neilson, R.; Noble, A. J.; Oedekerk, P.; Ortega, A. Diago; Piro, M.‐C.; Plante, A.; Podviyanuk, R.B.; Priya, Shashank; Robinson, Alan; Sahoo, Sunita; Scallon, O.; Seth, S.; Sonnenschein, A.; Starinski, N.; Štekl, I.; Sullivan, T.; Tardif, F.; Vázquez‐Jáuregui, E.; Walkowski, N.; Weima, E.; Wichoski, U.; Wierman, K.; Yan, Y. L.; Zacek, V.; Zhang, J.

doi:10.1103/physrevd.100.022001

Cited by 264 publications

(248 citation statements)

References 58 publications

(48 reference statements)

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“…3. Further, the densest part of the outer crust is 1 − 2 orders of magnitude less dense than the inner crust on average, while of comparable thickness; therefore its optical depth (and hence cross section sensitivity in Figure 4 directly compares our net crust sensitivity to constraints from underground experiments searching for dark matter in nuclear recoils, for both spin-independent and spin-dependent scattering [85][86][87][88][89]. We also show the xenon neutrino floor, which denotes the cross section sensitivity below which irreducible neutrino backgrounds are expected to confound direct detection searches.…”

Section: E Results and Discussionmentioning

confidence: 90%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

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Neutron stars serve as excellent next-generation thermal detectors of dark matter, heated by the scattering and annihilation of dark matter accelerated to relativistic speeds in their deep gravitational wells. However, the dynamics of neutron star cores are uncertain, making it difficult at present to unequivocally compute dark matter scattering in this region. On the other hand, the physics of an outer layer of the neutron star, the crust, is more robustly understood. We show that dark matter scattering solely with the low-density crust still kinetically heats neutron stars to infrared temperatures detectable by forthcoming telescopes. We find that for both spin-independent and spin-dependent scattering on nucleons, the crust-only cross section sensitivity is 10 −43 − 10 −41 cm 2 for dark matter masses of 100 MeV − 1 PeV, with the best sensitivity arising from dark matter scattering with a crust constituent called nuclear pasta (including gnocchi, spaghetti, and lasagna phases). For dark matter masses from 10 eV to 1 MeV, the sensitivity is 10 −39 − 10 −34 cm 2 , arising from exciting collective phonon modes in a neutron superfluid in the inner crust. Furthermore, for any s-wave or p-wave annihilating dark matter, we show that dark matter will efficiently annihilate by thermalizing just with the neutron star crust, regardless of whether the dark matter ever scatters with the neutron star core. This implies efficient annihilation in neutron stars for any electroweakly interacting dark matter with inelastic mass splittings of up to 200 MeV, including Higgsinos. We conclude that neutron star crusts play a key role in dark matter scattering and annihilation in neutron stars. *

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Section: E Results and Discussionmentioning

confidence: 90%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

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“…The last row shows the upper limits on the DM-nucleon cross section for both the spin-dependent and spin-independent cases for four different decay length for the long-lived mediator L = R , 0.1, 1 and 5 AU. The plots also show the limits at 90% CL from the PICO-60 experiment [40] in the case of spin-dependent (SD) scattering (cyan line) and from the XENON1T experiment [41] in the case of spin-independent (SI) scattering (blue line).…”

Section: Resultsmentioning

confidence: 99%

“…6, together with the recent HAWC and Fermi [44] results obtained with gamma rays constraints, i.e., for the two cases in which the mediator decays into 2 γ (4γ case), and the case as the one discussed in this work of mediator decaying into e ± and where γs are produced via FSR (i.e., 2 e ± FSR γ case). The plot also shows the PICO-60 limit at 90% CL [40]. In Fig.…”

Section: Discussionmentioning

confidence: 95%

Search for dark matter cosmic-ray electrons and positrons from the Sun with the Fermi Large Area Telescope

et al. 2020

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We use 7 years of electron and positron Fermi-LAT data to search for a possible excess in the direction of the Sun in the energy range from 42 GeV to 2 TeV. In the absence of a positive signal we derive flux upper limits which we use to constrain two different dark matter (DM) models producing e + e − fluxes from the Sun. In the first case we consider DM model being captured by the Sun due to elastic scattering and annihilation into e + e − pairs via a long-lived light mediator that can escape the Sun. In the second case we consider instead a model where DM density is enhanced around the Sun through inelastic scattering and the DM annihilates directly into e + e − pairs. In both cases we perform an optimal analysis, searching specifically for the energy spectrum expected in each case, i.e., a box-like shaped and line-like shaped spectrum respectively. No significant signal is found and we can place limits on the spin-independent cross-section in the range from 10 −46 cm 2 to 10 −44 cm 2 and on the spin-dependent cross-section in the range from 10 −43 cm 2 to 10 −41 cm 2 . In the case of inelastic scattering the limits on the cross-section are in the range from 10 −43 cm 2 to 10 −41 cm 2 . The limits depend on the life time of the mediator (elastic case) and on the mass splitting value (inelastic case), as well as on the assumptions made for the size of the deflections of electrons and positrons in the interplanetary magnetic field. PACS numbers: 95.35.+d, 95.85.Ry

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“…Figure 1: Regions of the parameter space allowing Ω χ 0 1 h 2 ≤ Ω obs DM h 2 in the decoupling limit (equivalent to a SM Higgs sector). All the plotted points fulfill the bounds from XENON1T [27,28] and PICO-60 [29]. Moreover the condition |M D | > 100 GeV has been required to satisfy the LEP limits [31] on charged fermions, in this case the charged components of the D−fields.…”

Section: Alignment From Decouplingmentioning

confidence: 87%

Generalized blind spots for dark matter direct detection in the 2HDM

Cabrera

Casas

Delgado

et al. 2020

J. High Energ. Phys.

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In this paper we study the presence of generalized blind spots, i.e. regions of the parameter space where the spin-independent cross section for dark matter direct detection is suppressed, in the context of a generic 2HDM and a minimal fermionic Higgs-portal dark sector. To this end, we derive analytical expressions for the couplings of the dark matter to the light and heavy Higgses, and thus for the blind spot solutions. Unlike the case of a standard Higgs sector, blind spots can occur even without a cancellation between different contributions, while keeping unsuppressed and efficient the annihilation processes in the early Universe involving Higgs states. As a consequence, the allowed parameter space is dramatically enhanced.

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Dark matter search results from the complete exposure of the PICO-60 C3F8 bubble chamber

Cited by 264 publications

References 58 publications

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Search for dark matter cosmic-ray electrons and positrons from the Sun with the Fermi Large Area Telescope

Generalized blind spots for dark matter direct detection in the 2HDM

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