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In 2019, a study based on post-marketing surveillance data in Japan reported that ABT was as effective and safe in elderly patients with rheumatoid arthritis (RA) as non-elderly[1]. However, there were inconsistent reports on the impact of ABT on malignancies which are more common in the elderly and strongly related to prognosis[2-4], and there are still unanswered questions. To evaluate the incidence of malignancy and the efficacy and safety of previous malignancy in RA patients using ABT in our clinical practice. In addition, to explore the predictive risk factors of developing or relapsing malignancy during ABT use. Patients who received ABT for RA at our department from October 2010 to May 2022 were included in the study. Patient background, prior malignancy at starting ABT, disease activity from starting ABT up to 60 months, continuation rates of ABT, and safety, including onset or recurrence of malignancy during ABT use, were retrospectively collected from electronic medical records. The patients were divided into two groups according to the absence or presence of previous malignancy (No previous malignancy: NP group, previous malignancy: PM group), and the collected parameters were compared between the groups. A total of 276 patients were included, of which 61 had previous malignancies when starting ABT. The age of starting ABT was significantly higher in the PM group (72.5 ± 10.6 vs. 68.5 ± 13.0years-old, p = 0.025), and the rate of methotrexate use was significantly lower in the PM group (29.5 vs. 51.2%, p = 0.0028), although there were no significant differences in other patient backgrounds between the groups (Table 1). The disease activity improved significantly at three months after starting ABT in both groups, and DAS28-CRP remission was maintained after that. There was no significant difference in disease activity between the groups from starting ABT to 60 months after. There were no significant differences in the continuation rates for 1-year and 5-year of ABT between the groups (86.3 vs. 86.6%, and 70.5 vs. 65.7%, respectively, Figure 1). There were 14 cases of occurrence and recurrence or progression of malignancy during the observation period. The incidence of malignancy was 1324.6 per 100,000 person-years, and there were no differences in the risk of malignancy in a Japanese national survey of similar age. Despite the significantly older patient population in the PM group, the 5-years incidence rate of malignancy was no significant difference between the groups. Binomial logistic analysis was performed using factors such as age, disease duration, history of previous malignancy, concomitant disease and medications, and disease activity at starting ABT. However, no predictive risk factors were found to be associated with the development or relapse of malignancy during ABT use in this study. In our clinical practice, ABT was effective and safe in both patients with and without previous malignancy. [1] Mod Rheumatol 2019 Sep; 29(5): 747-755. [2] Rheumatology 2019; 58: 683–91. [3] Arthritis Res Ther 2019; 21: 228. [4] Rheumatology 2020; 59: 2360–7. [Display omitted] NIL. Yosuke Kunishita Speakers bureau: AbbVie, Asahi Kasei Pharma, Astellas Pharma, AstraZeneca, Ayumi Pharmaceuticals, Boehringer Ingelheim Pharmaceuticals, Bristol-Myers Squibb, Daiichi Sankyo, Eisai, Eli Lilly, Gilead Sciences, Janssen Pharmaceuticals, Kyowa Kirin, Sanofi, UCB, Paid instructor for: AbbVie, Asahi Kasei Pharma, Astellas Pharma, AstraZeneca, Boehringer Ingelheim Pharmaceuticals, Bristol-Myers Squibb, Eisai, Gilead Sciences, Kyowa Kirin, UCB, Kayo Harita: None declared, Chikara Honda: None declared, Yuji Uzawa: None declared, Masaki Mitsuhashi: None declared, Soichi Ohta: None declared, Toshihisa Igarashi: None declared, Shouhei Nagaoka: None declared. Table 1Patient background at the start of ABT in the groups.NP group (n = 215)PM group (n=61)ρFemale (n, %)182/215 (84.7)49/61 (80.3)0.42Age (y.o.)68.5 ± 13.072.6 ± 10.60.025Disease duration (year)9.7 ± 9.511.8 ± 10.30.13Body weight (kg)53.4 ± 12.052.2 ± 9.60.49RF seropositivity (n, %)181/214 (84.6)52/61 (85.2)0.94Anti-CCP Ab seropositivity (n, %)152/184 (82.6)47/52 (90.4)0.25Complications of CTD (n, %)31/214 (14.5)12/61 (19.7)0.33Interstitial pneumoniae (n, %)47/215 (21.9)9/61 (14.8)0.30b/tsDMARDs naïve (n, %)152/214 (71.0)45/61 (73.8)0.68Concomitant drug　MTX (n, %)110/215 (51.2)18/61 (29.5)0.0028　MTX dose (mg/week)10.4 ± 2.79.9 ± 2.20.43　PSL (n, %)60/213 (28.2)20/61 (32.8)0.48　PSL dose (mg/day)5.8 ± 5.15.2 ± 4.10.65MMP-3 (ng/ml)262.1 ± 278.3294.1 ± 303.80.46DAS28-CRP3.8 ± 1.03.9 ± 1.20.91DAS28-ESR5.3 ± 1.15.3 ± 1.40.86CDAI20.2 ± 11.821.2 ± 12.30.62SDAI22.4 ± 12.923.6 ± 13.20.61

We have developed a test setup to measure frequency up-conversion gain in superconductor–insulator–superconductor (SIS) junctions at W band (75–110 GHz). A conventional SIS mixer with Nb/AlO x /Nb tunnel junctions was used as a frequency up-converter. An up-converted signal is measured by a room-temperature down-converter system. We observed distinct intermediate frequency responses to signal inputs from a continuous microwave source. The measured single-sideband up-conversion gain in SIS junctions was clearly positive (> 0 dB) with input frequency less than 2 GHz, which was well-calibrated by using an input from the continuous-wave source.

We report here the effect of film qualities in superconductors on the properties of Microwave Kinetic Inductance Detectors (MKIDs). The sensitivity of MKIDs between crystal aluminum films and amorphous aluminum films is compared. The good quality and crystallized aluminum films have been prepared by using molecular beam epitaxy. We have confirmed that epitaxial Al(111) films were grown on Si(111) substrates with X-ray diffraction and in-situ reflection high-energy electron diffraction measurements. The amorphous aluminum films on the Si(111) wafers have been deposited by electron beam evaporation. We have measured transmission losses of MKIDs, noise spectrum and relaxation time against optical pulses, changing MKIDs’ bath temperature from 0.11 K to 0.55 K in a dilution refrigerator. Despite of the improvement in normal resistivity, the quasiparticle decay time of both films are equivalent and 450 μs at 0.11 K. The electrical noise equivalent power of the both MKIDs are also comparable and around . Fabrication details and performance data of both films are presented.

We study on the electric transport properties of epitaxial NbTiN ultrathin films in a range from 2 to 8nm. The films with 4 nm thick shows superconductivity of which mean-field superconducting transition temperature is TC0 = 9.43 K The excess conductance due to superconducting fluctuations was measured at temperatures above TC0. The paraconductivity shows a two-dimensional like behaviour at close to TC0. Experimental results are in good agreement with the sum of Aslamazov − Larkin and Maki − Thompson term for superconducting fluctuation theory. Decreasing temperature below TC0, the current-voltage characteristic shows a crossover from linear to nonlinear behaviour. The exponent α of current-voltage relation, V ∼ Iα showed universal jump at TCBKT = 9.33 K As results, we find that there is a consistency between the parametrization of the2D characteristics of fluctuation paraconductivity above TC0 and Berezinskii-Kosterlitz-Thouless type behaviour below TC0.

The optics of a 900-GHz HEB receiver for the ASTE telescope have been analyzed by quasi-optical analysis and Physical Optics simulations in combination with beam pattern measurements. The disagreement between simulations and measurements has motivated an extensive campaign of Monte Carlo analyses to find out the cause of such a difference in results. Monte Carlo analyses have considered fabrication and assembly tolerances in all components in the RF chain, as well as some non-expected fabrication errors. This strategy has allowed determining the defective component. In short, the use of all available analyses techniques together with measurements has allowed singling out an underperforming element in an astronomical receiver. The change of this component will improve the optical efficiency and ease astronomical observations. These ideas can be of interest for any quasi-optical receiver at THz frequencies.

Microwave kinetic inductance detectors (MKIDs) are being developed at the National Astronomical Observatory of Japan to enable precise measurements of the cosmic microwave background. One of the features of MKIDs is scalability using a frequency-division multiplexing (FDMUX) readout scheme. A digital fast fourier transform spectrometer (FFTS) is a good way to read out a number of resonance frequencies simultaneously and fully utilize the advantage of FDMUX of MKIDs. We have developed FFTS readout electronics using an ADC/DAC with 1 Gsps (sample per second) sampling rate and 270 MHz bandwidth. We measured the noise characteristics of a single MKID in the frequency range of 60 Hz–30 kHz with this readout system, and found the noise was almost equivalent to the noise measured by ordinary analog IQ down-converter readout. This indicates our FFTS electronics do not add any additional noise to the MKID readout system over the frequency range.

LiteBIRD is a next-generation satellite mission to measure the polarization of the cosmic microwave background (CMB) radiation. On large angular scales the B-mode polarization of the CMB carries the imprint of primordial gravitational waves, and its precise measurement would provide a powerful probe of the epoch of inflation. The goal of LiteBIRD is to achieve a measurement of the characterizing tensor to scalar ratio r to an uncertainty of δ r = 0.001 . In order to achieve this goal we will employ a kilo-pixel superconducting detector array on a cryogenically cooled sub-Kelvin focal plane with an optical system at a temperature of 4 K. We are currently considering two detector array options; transition edge sensor (TES) bolometers and microwave kinetic inductance detectors. In this paper we give an overview of LiteBIRD and describe a TES-based polarimeter designed to achieve the target sensitivity of 2  μ K arcmin over the frequency range 50–320 GHz.

Inflation is the leading theory of the first instant of the universe. Inflation, which postulates that the universe underwent a period of rapid expansion an instant after its birth, provides convincing explanation for cosmological observations. Recent advancements in detector technology have opened opportunities to explore primordial gravitational waves generated by the inflation through “B-mode” (divergent-free) polarization pattern embedded in the cosmic microwave background anisotropies. If detected, these signals would provide strong evidence for inflation, point to the correct model for inflation, and open a window to physics at ultra-high energies. LiteBIRD is a satellite mission with a goal of detecting degree-and-larger-angular-scale B-mode polarization. LiteBIRD will observe at the second Lagrange point with a 400 mm diameter telescope and 2622 detectors. It will survey the entire sky with 15 frequency bands from 40 to 400 GHz to measure and subtract foregrounds. The US LiteBIRD team is proposing to deliver sub-Kelvin instruments that include detectors and readout electronics. A lenslet-coupled sinuous antenna array will cover low-frequency bands (40–235 GHz) with four frequency arrangements of trichroic pixels. An orthomode-transducer-coupled corrugated horn array will cover high-frequency bands (280–402 GHz) with three types of single frequency detectors. The detectors will be made with transition edge sensor (TES) bolometers cooled to a 100 milli-Kelvin base temperature by an adiabatic demagnetization refrigerator. The TES bolometers will be read out using digital frequency multiplexing with Superconducting QUantum Interference Device (SQUID) amplifiers. Up to 78 bolometers will be multiplexed with a single SQUID amplifier. We report on the sub-Kelvin instrument design and ongoing developments for the LiteBIRD mission.

ALMA has been operating since 2011, but has not yet been populated with the full suite of intended frequency bands. In particular, ALMA Band 2 (67-90 GHz) is the final band in the original ALMA band definition to be approved for production. We aim to produce a wideband, tuneable, sideband-separating receiver with 28 GHz of instantaneous bandwidth per polarisation operating in the sky frequency range 67-116 GHz. Our design anticipates new ALMA requirements following the recommendations in the 2030 ALMA Development Roadmap. The cryogenic cartridge is designed to be compatible with the ALMA Band 2 cartridge slot, where the coldest components -- the feedhorns, orthomode transducers, and cryogenic low noise amplifiers -- operate at a temperature of 15 K. We use multiple simulation methods and tools to optimise our designs for both the passive optics and the active components. The cryogenic cartridge interfaces with a room temperature cartridge hosting the local oscillator (LO) and the downconverter module. This warm cartridge is largely based on GaAs semiconductor technology and is optimised to match the cryogenic receiver bandwidth with the required instantaneous LO tuning range. Our collaboration has designed, fabricated, and tested multiple technical solutions for each of the components, producing a state-of-the-art receiver covering the full ALMA Band 2 & 3 atmospheric window. The receiver is suitable for deployment on ALMA in the coming years, and is capable of dual-polarisation, sideband-separating observations in intermediate frequency bands spanning 4-18 GHz, for a total of 28 GHz on-sky bandwidth per polarisation channel. We conclude that the 67-116 GHz wideband implementation for ALMA Band 2 is now feasible, and this receiver is a compelling instrumental upgrade that will enhance observational capabilities and scientific reach.