XMASS-I年度调制揭示暗物质新边界：排除DAMA/LIBRA区域
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本文主要探讨了利用单相液态氙探测器XMASS进行暗物质搜索的方法，特别是通过观察地球围绕太阳运动引起的年度调制信号。XMASS-I项目收集了359.2个工作日的数据，涵盖了2013年11月至2015年3月期间累计的832公斤氙气曝光量。研究团队假设暗物质可能是弱相互作用质量粒子(WIMP)，并考虑了它们在目标原子核上的弹性散射过程。通过这一假设，他们设定了一个WIMP的排除上限，即在8 GeV/c²的能量下，WIMP与核子的横截面限制为4.3×10^-41 cm²，这比之前DAMA/LIBRA实验的结果更为严格，几乎排除了16至16 GeV/c²能量范围内的大部分DAMA/LIBRA允许区域，尤其是低于10^-40 cm²的区域。
文章没有假设特定的暗物质模型，而是进行了简单的调制分析，结果显示出轻微的负振幅。通过两次独立分析，得到的p值分别为0.014和0.068，这表明观察到的效应具有一定的统计显著性。此外，该研究给出了90%的置信水平(C.L.)上限，这对于检验不同的暗物质模型提供了有价值的数据。这是第一次广泛开展的年度调制搜索，其探测能力与DAMA/LIBRA相当，进一步推动了对暗物质性质的探索。
参与研究的团队来自多个机构，包括日本的 Kamioka天文台、东京大学宇宙射线研究所以及韩国的韩国基础科学研究所等，显示了国际合作在此类前沿科学研究中的重要性。这项工作不仅展示了技术上的突破，也对暗物质研究领域提出了新的限制和可能性，为未来的研究方向提供了宝贵的参考。
Physics Letters B 759 (2016) 272–276
Contents lists available at ScienceDirect
Physics Letters B
www.elsevier.com/locate/physletb
Direct dark matter search by annual modulation in XMASS-I
XMASS Collaboration
K. Abe
a,e
, K. Hiraide
a,e
, K. Ichimura
a,e
, Y. Kishimoto
a,e
, K. Kobayashi
a,e
, M. Kobayashi
a,e
,
S. Moriyama
a,e
, M. Nakahata
a,e
, T. Norita
a
, H. Ogawa
a,e
, H. Sekiya
a,e
, O. Takachio
a
,
A. Takeda
a,e
, M. Yamashita
a,e
, B.S. Yang
a,e
, N.Y. Kim
b
, Y.D. Kim
b
, S. Tasaka
c,1
,
K. Fushimi
d
, J. Liu
e,2
, K. Martens
e
, Y. Suzuki
e
, B.D. Xu
e
, R. Fujita
g
, K. Hosokawa
g
,
K. Miuchi
g
, Y. Onishi
g
, N. Oka
g
, Y. Takeuchi
g,e
, Y.H. Kim
h,b
, J.S. Lee
h
, K.B. Lee
h
,
M.K. Lee
h
, Y. Fukuda
i
, Y. Itow
j,f
, R. Kegasa
j
, K. Kobayashi
j
, K. Masuda
j
, H. Takiya
j
,
K. Nishijima
k
, S. Nakamura
l
a
Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan
b
Center of Underground Physics, Institute for Basic Science, 70 Yuseong-daero 1689-gil, Yuseong-gu, Daejeon, 305-811, South Korea
c
Information and Multimedia Center, Gifu University, Gifu 501-1193, Japan
d
Institute of Socio-Arts and Sciences, The University of Tokushima, 1-1 Minamijosanjimacho Tokushima city, Tokushima, 770-8502, Japan
e
Kavli Institute for the Physics and Mathematics of the Universe (WPI), the University of Tokyo, Kashiwa, Chiba, 277-8582, Japan
f
Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8602, Japan
g
Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
h
Korea Research Institute of Standards and Science, Daejeon 305-340, South Korea
i
Department of Physics, Miyagi University of Education, Sendai, Miyagi 980-0845, Japan
j
Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8602, Japan
k
Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan
l
Department of Physics, Faculty of Engineering, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
a r t i c l e i n f o a b s t r a c t
Article history:
Received
3 March 2016
Received
in revised form 11 April 2016
Accepted
25 May 2016
Available
online 30 May 2016
Editor:
S. Dodelson
Keywords:
Dark
matter
Annual
modulation
Liquid
xenon
A search for dark matter was conducted by looking for an annual modulation signal due to the Earth’s
rotation around the Sun using XMASS, a single phase liquid xenon detector. The data used for this analysis
was 359.2 live days times 832 kg of exposure accumulated between November 2013 and March 2015.
When we assume Weakly Interacting Massive Particle (WIMP) dark matter elastically scattering on the
target nuclei, the exclusion upper limit of the WIMP–nucleon cross section 4.3 × 10
−41
cm
2
at 8 GeV/c
2
was obtained and we exclude almost all the DAMA/LIBRA allowed region in the 6 to 16 GeV/c
2
range
at ∼10
−40
cm
2
. The result of a simple modulation analysis, without assuming any specific dark matter
model but including electron/γ events, showed a slight negative amplitude. The p-values obtained with
two independent analyses are 0.014 and 0.068 for null hypothesis, respectively. We obtained 90% C.L.
upper bounds that can be used to test various models. This is the first extensive annual modulation
search probing this region with an exposure comparable to DAMA/LIBRA.
© 2016 The Author(s). Published by Elsevier B.V. This is an open access article under the CC BY license
(http://creativecommons.org/licenses/by/4.0/). Funded by SCOAP
3
.
E-mail address: xmass.publications2@km.icrr.u-tokyo.ac.jp.
1
Now at Kamioka Observatory, Institute for Cosmic Ray Research, the University
of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu, 506-1205, Japan.
2
Now at Department of Physics, the University of South Dakota, Vermillion, SD
57069, USA.
1. Introduction
There is strong evidence that about 5 times more dark matter
exists in the universe than ordinary matter. Despite its prominence,
we do not yet know what dark matter is [1]. Among many can-
didates
for dark matter particles, WIMPs are well motivated and
have received the most attention to date. However, collider experi-
ments
at the LHC do not show any indication for such particles so
far [1]. And no experimental indication for a standard WIMP was
http://dx.doi.org/10.1016/j.physletb.2016.05.081
0370-2693/
© 2016 The Author(s). Published by Elsevier B.V. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/4.0/). Funded by
SCOAP
3
.
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