Light Dark Matter Search with a High-Resolution Athermal Phonon Detector Operated Above Ground. (arXiv:2007.14289v4 [hep-ex] UPDATED)
<a href="http://arxiv.org/find/hep-ex/1/au:+Alkhatib_I/0/1/0/all/0/1">I. Alkhatib</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Amaral_D/0/1/0/all/0/1">D. W. P. Amaral</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Aralis_T/0/1/0/all/0/1">T. Aralis</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Aramaki_T/0/1/0/all/0/1">T. Aramaki</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Arnquist_I/0/1/0/all/0/1">I. J. Arnquist</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Langroudy_I/0/1/0/all/0/1">I. Ataee Langroudy</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Azadbakht_E/0/1/0/all/0/1">E. Azadbakht</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Banik_S/0/1/0/all/0/1">S. Banik</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Barker_D/0/1/0/all/0/1">D. Barker</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bathurst_C/0/1/0/all/0/1">C. Bathurst</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bauer_D/0/1/0/all/0/1">D. A. Bauer</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bezerra_L/0/1/0/all/0/1">L. V. S. Bezerra</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bhattacharyya_R/0/1/0/all/0/1">R. Bhattacharyya</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Binder_T/0/1/0/all/0/1">T. Binder</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bowles_M/0/1/0/all/0/1">M. A. Bowles</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Brink_P/0/1/0/all/0/1">P. L. Brink</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Bunker_R/0/1/0/all/0/1">R. Bunker</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cabrera_B/0/1/0/all/0/1">B. Cabrera</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Calkins_R/0/1/0/all/0/1">R. Calkins</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cameron_R/0/1/0/all/0/1">R. A. Cameron</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cartaro_C/0/1/0/all/0/1">C. Cartaro</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cerdeno_D/0/1/0/all/0/1">D. G. Cerde&#xf1;o</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Chang_Y/0/1/0/all/0/1">Y.-Y. Chang</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Chaudhuri_M/0/1/0/all/0/1">M. Chaudhuri</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Chen_R/0/1/0/all/0/1">R. Chen</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Chott_N/0/1/0/all/0/1">N. Chott</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cooley_J/0/1/0/all/0/1">J. Cooley</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Coombes_H/0/1/0/all/0/1">H. Coombes</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Corbett_J/0/1/0/all/0/1">J. Corbett</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Cushman_P/0/1/0/all/0/1">P. Cushman</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Brienne_F/0/1/0/all/0/1">F. De Brienne</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Vacri_M/0/1/0/all/0/1">M. L. di Vacri</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Diamond_M/0/1/0/all/0/1">M. D. Diamond</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Fascione_E/0/1/0/all/0/1">E. Fascione</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Figueroa_Feliciano_E/0/1/0/all/0/1">E. Figueroa-Feliciano</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Fink_C/0/1/0/all/0/1">C. W. Fink</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Fouts_K/0/1/0/all/0/1">K. Fouts</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Fritts_M/0/1/0/all/0/1">M. Fritts</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Gerbier_G/0/1/0/all/0/1">G. Gerbier</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Germond_R/0/1/0/all/0/1">R. Germond</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Ghaith_M/0/1/0/all/0/1">M. Ghaith</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Golwala_S/0/1/0/all/0/1">S. R. Golwala</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Harris_H/0/1/0/all/0/1">H. R. Harris</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Herbert_N/0/1/0/all/0/1">N. Herbert</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hines_B/0/1/0/all/0/1">B. A. Hines</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hollister_M/0/1/0/all/0/1">M. I. Hollister</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hong_Z/0/1/0/all/0/1">Z. Hong</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hoppe_E/0/1/0/all/0/1">E. W. Hoppe</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hsu_L/0/1/0/all/0/1">L. Hsu</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Huber_M/0/1/0/all/0/1">M. E. Huber</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Iyer_V/0/1/0/all/0/1">V. Iyer</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Jardin_D/0/1/0/all/0/1">D. Jardin</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Jastram_A/0/1/0/all/0/1">A. Jastram</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kashyap_V/0/1/0/all/0/1">V. K. S. Kashyap</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kelsey_M/0/1/0/all/0/1">M. H. Kelsey</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kubik_A/0/1/0/all/0/1">A. Kubik</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kurinsky_N/0/1/0/all/0/1">N. A. Kurinsky</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lawrence_R/0/1/0/all/0/1">R. E. Lawrence</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Li_A/0/1/0/all/0/1">A. Li</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Loer_B/0/1/0/all/0/1">B. Loer</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Asamar_E/0/1/0/all/0/1">E. Lopez Asamar</a>, et al. (63 additional authors not shown)

We present limits on spin-independent dark matter-nucleon interactions using
a $10.6$ $mathrm{g}$ Si athermal phonon detector with a baseline energy
resolution of $sigma_E=3.86 pm 0.04$ $(mathrm{stat.})^{+0.19}_{-0.00}$
$(mathrm{syst.})$ $mathrm{eV}$. This exclusion analysis sets the most
stringent dark matter-nucleon scattering cross-section limits achieved by a
cryogenic detector for dark matter particle masses from $93$ to $140$
$mathrm{MeV}/c^2$, with a raw exposure of $9.9$ $mathrm{g}cdotmathrm{d}$
acquired at an above-ground facility. This work illustrates the scientific
potential of detectors with athermal phonon sensors with eV-scale energy
resolution for future dark matter searches.

We present limits on spin-independent dark matter-nucleon interactions using
a $10.6$ $mathrm{g}$ Si athermal phonon detector with a baseline energy
resolution of $sigma_E=3.86 pm 0.04$ $(mathrm{stat.})^{+0.19}_{-0.00}$
$(mathrm{syst.})$ $mathrm{eV}$. This exclusion analysis sets the most
stringent dark matter-nucleon scattering cross-section limits achieved by a
cryogenic detector for dark matter particle masses from $93$ to $140$
$mathrm{MeV}/c^2$, with a raw exposure of $9.9$ $mathrm{g}cdotmathrm{d}$
acquired at an above-ground facility. This work illustrates the scientific
potential of detectors with athermal phonon sensors with eV-scale energy
resolution for future dark matter searches.

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