1. Report on New Physics Subgroup Activities Masaki Asano (Tohoku U.) The 9th general meeting of the ILC physics working group Sorry, we have no progress. This is a quick review of our plan.

2. How to distinguish the dark matter nature in different new physics models @ ILC ? To distinguish the dark matter nature, We concentrate on this process: Charged new particleDark matter

4. arXiv:0901.1081 Eri Asakawa, Masaki Asano, Keisuke Fujii, Tomonori Kusano, Shigeki Matsumoto, Rei Sasaki, Yosuke Takubo, and Hitoshi Yamamoto

5. How to distinguish the dark matter nature in different new physics models @ ILC ? To distinguish the dark matter nature, We concentrate on this process: Charged new particleDark matter

6. Charged new particleDM Properties of DM & associated charged particle in new physics models. We study in these three cases.

7. Our Plan (Next Step) Full sim. @ 500 GeV ILC Quick sim. @ 1 TeV ILC 1. We will Because we have already prepared for BG @ 500GeV in full simulation. M DM = 43.7 GeV M +- = 230 GeV 2. We choice these sample point M DM = 81.9 GeV M +- = 368 GeV @ 500 GeV ILC @ 1 TeV ILC This relation is consistent with three new physics models.

8. Simulation studies Masses – > mass relation between X 0 & X +- Cross section Angular distribution of charged particles – > spin W +- polarization – > the decay vertex structure How accurately can ILC measure

9. 9 Production angle of W H ± Angular distribution of jets from W ± Other parameters W H is spin 1 particle! The dominance of the longitudinal mode! The coupling arises from EWSB!

10. 10 e-e- e+e+ WH+WH+ W+W+ AHAH WH-WH- AHAH W-W- W H ± candidates are reconstructed as corn around W ±. If W H + and W H - are assumed as back-to-back, there are 2 solutions for W H ± candidates. In this mode, however, 2 solutions should be close to true W H ±. W+W+ W-W- WH+WH+ WH-WH- Distribution of production angles of W H +  Production angle of W H ± spin-1 This shape shows W H ± spin as spin-1. Angular distribution of jets W+W+ j1j1 j2j2  j1j1 j2j2 longitudinal W ± helicity as longitudinal mode. Angular distribution of jets in the helicity-frame of the W ± carries information on the polarization of the W ±.

11. 11 Production angle of W H ± Angular distribution of jets from W ± Other parameters W H is spin 1 particle! The dominance of the longitudinal mode! The coupling arises from EWSB! Beam polarization W H has SU(2) L charge, but no U(1) Y charge! 100% RH polarization

12. N. Okada

13. 13 Other parameters Cross section Heavy lepton mass! @ 1 TeV ILC @ 500 GeV ILC Heavy lepton masses depend on Yukawa k_l. k_l can be determined with 22.1% accuracy at 500 GeV, 0.5% accuracy at 1 TeV.

14. Advanced study In these models, there are t-channel process. If the t-channel process is significant big FB asymmetry. Ex. LHT -> W charge ID N. Okada

15. From N. Okada’s slides. Backup

16. N. Okada