Obtained the results by using Calo-VQ for dataset2 (ATLAS detector);
Xbb Calibration:
Checked with Rachel and Kosuke the Ttbar process with $f_{top}=0$
Plan:
ssWWjj:
Push the codes to the main branch of the easyjet framework (after splitting the mc20 and mc23);
Added the chargeflip to the fastframe framework;
HWW QE:
Check the status with Castein and Steffen;
Fast Simulation for Dark SHINE:
Check the results with Qibin;
Change the structure of the network to allow Calo-VQ to be used in our DarkSHINE experiment;
Xbb Calibration:
Check the trigger list with Rachel and Elisabeth;
Derive the mu_post-tag fitting with systematics;
10:30
→
10:40
Status10m
Speaker:
Xuliang Zhu(TDLI, SJTU)
10:40
→
10:50
Status10m
Speaker:
Zhiyu Zhao(TDLI, SJTU)
DarkSHINE
We found that the SiPM signal attenuates at high frequencies (from 1 kHz to 1 MHz, the signal attenuates by a factor of 9). Through communication with HAMAMATSU, the main reason is determined to be the peripheral circuit design. After updating the circuit design, the situation improved significantly, but there is still a 10% amplitude reduction at 1MHz, which still need to be further investigated.
Anylyze the results from b1.0 and b1.6, and compare the differences in their signal and background efficiencies.
10:50
→
11:00
Status10m
Speaker:
Ngoc Khanh Vu(TDLI, SJTU)
Run 3 ggHyyd:
cross-check the fit results of the Run-3 ggF channel obtained by the combination FW with ones obtained by trex-fitter.
1st EB meeting on Sep 1st (next Monday).
ATLAS+CMS HH combination: 1st paper draft ready, next EB meeting is being scheduled.