Searching for low-mass dark matter particles with a massive Ge bolometer operated above-ground. (arXiv:1901.03588v1 [astro-ph.GA])

Searching for low-mass dark matter particles with a massive Ge bolometer operated above-ground. (arXiv:1901.03588v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Armengaud_E/0/1/0/all/0/1">E. Armengaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Augier_C/0/1/0/all/0/1">C. Augier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benoit_A/0/1/0/all/0/1">A. Beno&#xee;t</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benoit_A/0/1/0/all/0/1">A. Benoit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berge_L/0/1/0/all/0/1">L. Berg&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Billard_J/0/1/0/all/0/1">J. Billard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Broniatowski_A/0/1/0/all/0/1">A. Broniatowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Camus_P/0/1/0/all/0/1">P. Camus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cazes_A/0/1/0/all/0/1">A. Cazes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chapelier_M/0/1/0/all/0/1">M. Chapelier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charlieux_F/0/1/0/all/0/1">F. Charlieux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ducimetiere_D/0/1/0/all/0/1">D. Ducimeti&#xe8;re</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dumoulin_L/0/1/0/all/0/1">L. Dumoulin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eitel_K/0/1/0/all/0/1">K. Eitel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Filosofov_D/0/1/0/all/0/1">D. Filosofov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gascon_J/0/1/0/all/0/1">J. Gascon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giuliani_A/0/1/0/all/0/1">A. Giuliani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gros_M/0/1/0/all/0/1">M. Gros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jesus_M/0/1/0/all/0/1">M. De J&#xe9;sus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jin_Y/0/1/0/all/0/1">Y. Jin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juillard_A/0/1/0/all/0/1">A. Juillard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kleifges_M/0/1/0/all/0/1">M. Kleifges</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maisonobe_R/0/1/0/all/0/1">R. Maisonobe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marnieros_S/0/1/0/all/0/1">S. Marnieros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Misiak_D/0/1/0/all/0/1">D. Misiak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Navick_X/0/1/0/all/0/1">X.-F. Navick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nones_C/0/1/0/all/0/1">C. Nones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olivieri_E/0/1/0/all/0/1">E. Olivieri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oriol_C/0/1/0/all/0/1">C. Oriol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pari_P/0/1/0/all/0/1">P. Pari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paul_B/0/1/0/all/0/1">B. Paul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poda_D/0/1/0/all/0/1">D. Poda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Queguiner_E/0/1/0/all/0/1">E. Queguiner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rozov_S/0/1/0/all/0/1">S. Rozov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanglard_V/0/1/0/all/0/1">V. Sanglard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siebenborn_B/0/1/0/all/0/1">B. Siebenborn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vagneron_L/0/1/0/all/0/1">L. Vagneron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weber_M/0/1/0/all/0/1">M. Weber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yakushev_E/0/1/0/all/0/1">E. Yakushev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zolotarova_A/0/1/0/all/0/1">A. Zolotarova</a>, (EDELWEISS Collaboration), <a href="http://arxiv.org/find/astro-ph/1/au:+Kavanagh_B/0/1/0/all/0/1">B. J. Kavanagh</a>

The EDELWEISS collaboration has performed a search for dark matter particles
with masses below the GeV-scale with a 33.4-g germanium cryogenic detector
operated in a surface lab. The energy deposits were measured using a
neutron-transmutation-doped Ge thermal sensor with a 17.7 eV (RMS) baseline
heat energy resolution leading to a 60 eV analysis energy threshold. Despite a
moderate lead shielding and the high-background environment, the first sub-GeV
spin-independent dark matter limit based on a germanium target has been
achieved. The experiment provides the most stringent, nuclear recoil based,
above-ground limit on spin-independent interactions above 600 MeV/c$^{2}$. The
dark matter search results were also studied in the context of Strongly
Interacting Massive Particles, taking into account Earth-shielding effects, for
which new regions of the available parameter space have been excluded. Finally,
the dark matter search has also been extended to interactions via the Migdal
effect, resulting for the first time in the exclusion of particles with masses
between 45 and 150 MeV/c$^{2}$ with cross sections ranging from $10^{-29}$ to
$10^{-26}$ cm$^2$.

The EDELWEISS collaboration has performed a search for dark matter particles
with masses below the GeV-scale with a 33.4-g germanium cryogenic detector
operated in a surface lab. The energy deposits were measured using a
neutron-transmutation-doped Ge thermal sensor with a 17.7 eV (RMS) baseline
heat energy resolution leading to a 60 eV analysis energy threshold. Despite a
moderate lead shielding and the high-background environment, the first sub-GeV
spin-independent dark matter limit based on a germanium target has been
achieved. The experiment provides the most stringent, nuclear recoil based,
above-ground limit on spin-independent interactions above 600 MeV/c$^{2}$. The
dark matter search results were also studied in the context of Strongly
Interacting Massive Particles, taking into account Earth-shielding effects, for
which new regions of the available parameter space have been excluded. Finally,
the dark matter search has also been extended to interactions via the Migdal
effect, resulting for the first time in the exclusion of particles with masses
between 45 and 150 MeV/c$^{2}$ with cross sections ranging from $10^{-29}$ to
$10^{-26}$ cm$^2$.

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