TY - JOUR
T1 - LHC Dark Matter Working Group
T2 - Next-generation spin-0 dark matter models
AU - Abe, Tomohiro
AU - Afik, Yoav
AU - Albert, Andreas
AU - Anelli, Christopher R.
AU - Barak, Liron
AU - Bauer, Martin
AU - Behr, J. Katharina
AU - Bell, Nicole F.
AU - Boveia, Antonio
AU - Brandt, Oleg
AU - Busoni, Giorgio
AU - Carpenter, Linda M.
AU - Chen, Yu Heng
AU - Doglioni, Caterina
AU - Elliot, Alison
AU - Fujiwara, Motoko
AU - Genest, Marie Helene
AU - Gerosa, Raffaele
AU - Gori, Stefania
AU - Gramling, Johanna
AU - Grohsjean, Alexander
AU - Gustavino, Giuliano
AU - Hahn, Kristian
AU - Haisch, Ulrich
AU - Henkelmann, Lars
AU - Hisano, Junji
AU - Huitfeldt, Anders
AU - Ippolito, Valerio
AU - Kahlhoefer, Felix
AU - Landsberg, Greg
AU - Lowette, Steven
AU - Maier, Benedikt
AU - Maltoni, Fabio
AU - Muehlleitner, Margarete
AU - No, Jose M.
AU - Pani, Priscilla
AU - Polesello, Giacomo
AU - Price, Darren D.
AU - Robens, Tania
AU - Rovelli, Giulia
AU - Rozen, Yoram
AU - Sanderson, Isaac W.
AU - Santos, Rui
AU - Sevova, Stanislava
AU - Sperka, David
AU - Sung, Kevin
AU - Tait, Tim M.P.
AU - Terashi, Koji
AU - Ungaro, Francesca C.
AU - Vryonidou, Eleni
AU - Yu, Shin Shan
AU - Wu, Sau Lan
AU - Zhou, Chen
N1 - Funding Information:
T. Abe’s work is supported by JSPS KAKENHI Grant Number 16K17715 . The research of Y. Afik and Y. Rozen was supported by a grant from the United States–Israel Binational Science Foundation, Jerusalem, Israel , and by a grant from the Israel Science Foundation . A. Albert receives support from the German Federal Ministry of Education and Research under grant 05H15PACC1 . J. K. Behr acknowledges the support of the Helmholtz Foundation . The research of A. Boveia and L. M. Carpenter is supported by the U.S. DOE grant DE-SC0011726 . C. Doglioni has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation program (grant agreement 679305 ) and from the Swedish Research Council . S. Gori is supported by the NSF CAREER grant PHY-1654502 and grateful to the Kavli Institute for Theoretical Physics in Santa Barbara, supported in part by the NSF under Grant No. NSF PHY11-25915, as well as the Aspen Center for Physics, supported by the National Science Foundation Grant No. PHY-1066293 , for hospitality. U. Haisch acknowledges the hospitality and support of the CERN Theoretical Physics Department . J. Hisano’s work is supported by Grant-in-Aid for Scientific research from the Ministry of Education, Science, Sports, and Culture (MEXT), Japan , No. 16H06492 , and also by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan . The work of J. M. No was partially supported by the European Research Council under the European Union’s Horizon 2020 program (grant agreement 648680 ) and by the Programa Atraccion de Talento de la Comunidad de Madrid under grant n. 2017-T1/TIC-5202 . DDP is supported by STFC under grant ST/M005437/1 . The work of T. M. P. Tait is supported in part by NSF grant PHY-1316792 . T. Robens is supported in part by the National Science Centre, Poland , the HARMONIA project under contract UMO-2015/18/M/ST2/00518 (2016–2019) , and by grant K 25105 of the National Research, Development and Innovation Fund in Hungary . We gratefully acknowledge the support by the U.S. DOE .
Funding Information:
T. Abe's work is supported by JSPS KAKENHI Grant Number 16K17715. The research of Y. Afik and Y. Rozen was supported by a grant from the United States–Israel Binational Science Foundation, Jerusalem, Israel, and by a grant from the Israel Science Foundation. A. Albert receives support from the German Federal Ministry of Education and Research under grant 05H15PACC1. J. K. Behr acknowledges the support of the Helmholtz Foundation. The research of A. Boveia and L. M. Carpenter is supported by the U.S. DOE grant DE-SC0011726. C. Doglioni has received funding from the European Research Council under the European Union's Horizon 2020 research and innovation program (grant agreement 679305) and from the Swedish Research Council. S. Gori is supported by the NSF CAREER grant PHY-1654502 and grateful to the Kavli Institute for Theoretical Physics in Santa Barbara, supported in part by the NSF under Grant No. NSF PHY11-25915, as well as the Aspen Center for Physics, supported by the National Science Foundation Grant No. PHY-1066293, for hospitality. U. Haisch acknowledges the hospitality and support of the CERN Theoretical Physics Department. J. Hisano's work is supported by Grant-in-Aid for Scientific research from the Ministry of Education, Science, Sports, and Culture (MEXT), Japan, No. 16H06492, and also by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. The work of J. M. No was partially supported by the European Research Council under the European Union's Horizon 2020 program (grant agreement 648680) and by the Programa Atraccion de Talento de la Comunidad de Madrid under grant n. 2017-T1/TIC-5202. DDP is supported by STFC under grant ST/M005437/1. The work of T. M. P. Tait is supported in part by NSF grant PHY-1316792. T. Robens is supported in part by the National Science Centre, Poland, the HARMONIA project under contract UMO-2015/18/M/ST2/00518 (2016–2019), and by grant K 25105 of the National Research, Development and Innovation Fund in Hungary. We gratefully acknowledge the support by the U.S. DOE.
Publisher Copyright:
© 2019 The Authors
PY - 2020/1
Y1 - 2020/1
N2 - Dark matter (DM) simplified models are by now commonly used by the ATLAS and CMS Collaborations to interpret searches for missing transverse energy (ET miss). The coherent use of these models sharpened the LHC DM search program, especially in the presentation of its results and their comparison to DM direct-detection (DD) and indirect-detection (ID) experiments. However, the community has been aware of the limitations of the DM simplified models, in particular the lack of theoretical consistency of some of them and their restricted phenomenology leading to the relevance of only a small subset of ET miss signatures. This document from the LHC Dark Matter Working Group identifies an example of a next-generation DM model, called 2HDM+a, that provides the simplest theoretically consistent extension of the DM pseudoscalar simplified model. A comprehensive study of the phenomenology of the 2HDM+a model is presented, including a discussion of the rich and intricate pattern of mono-X signatures and the relevance of other DM as well as non-DM experiments. Based on our discussions, a set of recommended scans are proposed to explore the parameter space of the 2HDM+a model through LHC searches. The exclusion limits obtained from the proposed scans can be consistently compared to the constraints on the 2HDM+a model that derive from DD, ID and the DM relic density.
AB - Dark matter (DM) simplified models are by now commonly used by the ATLAS and CMS Collaborations to interpret searches for missing transverse energy (ET miss). The coherent use of these models sharpened the LHC DM search program, especially in the presentation of its results and their comparison to DM direct-detection (DD) and indirect-detection (ID) experiments. However, the community has been aware of the limitations of the DM simplified models, in particular the lack of theoretical consistency of some of them and their restricted phenomenology leading to the relevance of only a small subset of ET miss signatures. This document from the LHC Dark Matter Working Group identifies an example of a next-generation DM model, called 2HDM+a, that provides the simplest theoretically consistent extension of the DM pseudoscalar simplified model. A comprehensive study of the phenomenology of the 2HDM+a model is presented, including a discussion of the rich and intricate pattern of mono-X signatures and the relevance of other DM as well as non-DM experiments. Based on our discussions, a set of recommended scans are proposed to explore the parameter space of the 2HDM+a model through LHC searches. The exclusion limits obtained from the proposed scans can be consistently compared to the constraints on the 2HDM+a model that derive from DD, ID and the DM relic density.
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U2 - 10.1016/j.dark.2019.100351
DO - 10.1016/j.dark.2019.100351
M3 - Article
AN - SCOPUS:85070383963
SN - 2212-6864
VL - 27
JO - Physics of the Dark Universe
JF - Physics of the Dark Universe
M1 - 100351
ER -