Bulletin of the American Physical Society
APS April Meeting 2023
Volume 68, Number 6
Minneapolis, Minnesota (Apr 15-18)
Virtual (Apr 24-26); Time Zone: Central Time
Session G13: Dark Matter Constraints |
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Sponsoring Units: DAP Chair: Stephanie Wissel, Pennsylvania State University Room: Marquette IV - 2nd Floor |
Sunday, April 16, 2023 10:45AM - 10:57AM |
G13.00001: Dark Matter Direct Detection Searches with COSINE Experiment Govinda Adhikari COSINE-100 is a direct detection dark matter search experiment that uses Thallium-doped Sodium Iodide, NaI(Tl) as its target detector material. The detector has been collecting data since September 2016 with continuous stable operation. It consists of ~106 kg of low background NaI(Tl) detectors submerged in a 2 tons liquid scintillator veto counter. The basic goal of the experiment is to test the annual modulation signal for Dark Matter - NaI(Tl) recoils reported by the DAMA/LIBRA experiment. In this talk, I will present the status of COSINE-100, including the recent results on WIMP and annual modulation search, and prospects for the next phase, COSINE-200. |
Sunday, April 16, 2023 10:57AM - 11:09AM |
G13.00002: CMB Constraints on Dark Matter Annihilation following an Early Matter-Dominated Era A. Turchaninova, Hwan Bae, Adrienne L Erickcek, Vivian Poulin The evolution of the early universe is largely unconstrained: there is a vast gulf between the possible energy scales of inflation and the onset of Big Bang nucleosynthesis. In many theories, oscillating scalar fields or massive particles come to dominate the Universe during this period, before decaying into Standard Model particles. An early matter-dominated era (EMDE) causes dark matter (DM) to cluster into microhalos earlier than in a standard cosmology, increasing the DM annihilation rate for a given annihilation cross section. Additionally, the decay of the species driving the EMDE dilutes the abundance of thermal relics, allowing for smaller DM annihilation cross sections to produce the observed DM density. An EMDE therefore broadens the range of viable DM candidates while also making more of these candidates accessible to indirect-detection methods, which search for energetic particles produced by DM annihilation. The cosmic microwave background (CMB) is particularly sensitive to the injection of energetic particles close to the time of recombination, well before halo formation occurs in the absence of an EMDE. Furthermore, the impact of DM annihilation on the CMB is clearly distinguishable from known astrophysical signals. We demonstrate the constraining power of the CMB for EMDE scenarios and compare to bounds from the isotropic gamma-ray background. |
Sunday, April 16, 2023 11:09AM - 11:21AM |
G13.00003: Astrophysical Constraints on Warm Dark Matter Kevork N Abazajian In the regime of linear growth of structure, dark matter dominates structure formation at all scales. On small scales, the thermal and kinetic properties of dark matter will alter the growth of structure at a finite scale that depends on the nature of dark matter. I will review the methods for constraining matter clustering on small scales, highlighting those most robust to modeling and data uncertainties. I will also review the impact of these constraints on leading candidate warm dark matter models, including sterile neutrino and gravitino dark matter models, with our work providing more accurate descriptions of structure formation in the case of gravitino warm dark matter. Our other recent work combines strong lensing and galaxy counts to provide among the strongest constraints yet on warm dark matter, with a corresponding significant (greater than 50%) suppression of structure at M < 8 × 106 M?, well below dwarf galaxy scales, requiring thermal warm dark matter particle masses at approximately mth > 9 keV. Ongoing lensing observations by JWST will greatly increase the sensitivities of these methods. |
Sunday, April 16, 2023 11:21AM - 11:33AM |
G13.00004: Constraining bosonic asymmetric dark matter with neutron star mass-radius measurements Nathan Rutherford, Geert Raaijmakers, Chanda Prescod-Weinstein, Anna Watts Neutron stars can accumulate asymmetric dark matter (ADM) in their interiors, which affects the neutron star's measurable properties and makes compact objects prime targets to search for ADM. In this work, we use Bayesian inference to explore potential neutron star mass-radius measurements, from current and future X-ray telescopes, to constrain the bosonic ADM parameters for the case where bosonic ADM has accumulated in the neutron star interior. We find that the high bosonic ADM particle mass (mχ) and low effective self-interaction strength (gχ/mΦ) regime is disfavored due to the observationally and theoretically motivated constraint that neutron stars must have at least a mass of 1 M_sun (solar mass). However, within the remaining parameter space, mχ and gχ/mΦ are individually unconstrained. On the other hand, the ADM mass-fraction, i.e., the fraction of ADM mass inside the neutron star, can be constrained by such neutron star measurements. The inclusion of bosonic ADM in neutron star cores also relaxes the constraints on the baryonic equation of state space. |
Sunday, April 16, 2023 11:33AM - 11:45AM |
G13.00005: The Sensitivity Floor for Primordial Black Holes Neutrino Searches Qishan Liu Primordial black holes(PBHs) are a well-motivated dark matter (DM) candidate over a wide range of masses. Light, asteroid-mass primordial black holes could be detected using neutrinos produced via Hawking radiation. We discuss using neutrino to search for non-rotating PBHs with monochromatic mass distributions, spanning from 5 × 1014 g to 1016 g. We consider the null observations of antineutrino flux from several neutrino detectors and set new constraints on the PBHs as a dark matter candidate. We also set the constraint using data from forecasts on JUNO detectors. In addition, we note that the Diffuse Supernova Neutrino Background(DSNB) is an unavoidable isotropic background, we thus estimate the sensitivity floor up to mass about 1016 g caused by DSNB on PBHs dark matter. |
Sunday, April 16, 2023 11:45AM - 11:57AM |
G13.00006: Primordial Black-Hole Dark Matter from Warm Natural Inflation Grant J Mathews, Miguel Correa, Mayukh R Gangopadhyay, Nur Jaman We describe a study of the natural warm inflationary paradigm (WNI). We show two important new results arise in this model. One is that the observational constraints on the primordial power spectrum from the cosmic microwave background (CMB) can be satisfied without going beyond the Planck scale of the effective field theory. The second is that WNI can inevitably provide perfect conditions for the production of primordial black holes (PBHs) in the golden window of black-hole mass range (10−16 − 10−11MSol) where it can account for all of the the dark matter content of the universe while satisfying observational constraints. |
Sunday, April 16, 2023 11:57AM - 12:09PM |
G13.00007: Dark matter properties from universal scaling laws and energy cascade in dark matter flow Zhijie Xu We present a new approach to estimate dark matter particle mass, size, density, and many other properties based on a cascade theory for the flow of dark matter, similar to the cascade in hydrodynamic turbulence. The energy cascade from small to large scales with a constant rate εu≈-4.6x10-7m2/s3 is a fundamental feature of dark matter flow. Energy cascade leads to a two-thirds law for kinetic energy vr2 ≈(εur)2/3 on scale r, as confirmed by N-body simulations. This is equivalent to a four-thirds law for mean halo density ρs enclosed in the halo scale radius rs such that ρs ≈εu2/3G-1rs-4/3, as confirmed by galaxy rotation curves. The smallest length scale in dark matter flow is dependent on the nature of dark matter. For collisionless dark matter, particle mass is estimated to be mX≈(-εuh5G4)1/9≈1012GeV with a size of rη ≈(-εuhG)1/3≈10-13m, where h is the Planck constant. An uncertainty principle for momentum and acceleration fluctuations is also postulated to explain the physical origin of the rate of energy cascade εu. For self-interacting dark matter, the smallest structure has a sale rη ≈εu2G-3(σ/m)3, where σ/m is the cross-section. On halo scale, the energy cascade leads to an asymptotic density slope γ=-4/3 for fully virialized halos with a vanishing radial flow, which might explain the nearly universal halo density. A modified Einasto density profile is proposed accordingly. Accompanying slides and datasets for this work can be found at https://doi.org/10.5281/zenodo.6569901. |
Sunday, April 16, 2023 12:09PM - 12:21PM |
G13.00008: Search for Solar Dark Matter Particles with Crystal micro-pendulum. IGOR OSTROVSKII We report the direct detection of dark neutral massive particles (MP) emitted by the Sun. The estimated rest mass is (3.15 ±1) PeV/C2 and the local mass-energy density is (0.64 ±0.2) GeV/cm3. They were detected by using a novel mechano-optical method, which does not require any electromagnetic or nuclear interaction of MP with detector elements. The sensor is a crystal pendulum (CP) with a microgram crystalline bob. It starts to oscillate when MP carrying momentum knocks CP. The Laser-Doppler-Vibrometer (LDV) detects these oscillations. A laser beam of LDV is focused on the crystal-bob and is reflected to LDV optical sensor. It allows for measuring the speed, amplitude, and frequency of CP oscillations. Theoretical calculations of CP oscillations are then compared to experimental data registered by LDV. The solar MP was detected by 8 CP with different quartz crystals in 30 runs of the experiments completed at different seasons. The data obtained allowed us to estimate the rest mass and local mass-energy density of solar MP. The MP particles do not interact with electromagnetic radiation and are dark to contemporary astrophysical and particle physics detectors. That is why detected MP is a part of dark matter by definition, despite MP are not a part of matter produced during the Big Bang period. Discovered MP is a new part of solar/star wind. They contribute their mass to the total mass of the galaxy and universe. Possibly, other stars also can emit similar MP and it may shed light on astrophysical problems in mass distribution in the universe. |
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