Vacuum mechatronics

The discipline of vacuum mechatronics is defined as the design and development of vacuum-compatible computer-controlled mechanisms for manipulating, sensing and testing in a vacuum environment. The importance of vacuum mechatronics is growing with an increased application of vacuum in space studies and in manufacturing for material processing, medicine, microelectronics, emission studies, lyophylisation, freeze drying and packaging. The quickly developing field of vacuum mechatronics will also be the driving force for the realization of an advanced era of totally enclosed clean manufacturing cells. High technology manufacturing has increasingly demanding requirements for precision manipulation, in situ process monitoring and contamination-free environments. To remove the contamination problems associated with human workers, the tendency in many manufacturing processes is to move towards total automation. This will become a requirement in the near future for e.g., microelectronics manufacturing. Automation in ultra-clean manufacturing environments is evolving into the concept of self-contained and fully enclosed manufacturing. A Self Contained Automated Robotic Factory (SCARF) is being developed as a flexible research facility for totally enclosed manufacturing. The construction and successful operation of a SCARF will provide a novel, flexible, self-contained, clean, vacuum manufacturing environment. SCARF also requires very high reliability and intelligent control. The trends in vacuum mechatronics and some of the key research issues are reviewed

The TESS-Keck Survey. XI. Mass Measurements for Four Transiting sub-Neptunes orbiting K dwarf TOI-1246

Multi-planet systems are valuable arenas for investigating exoplanet architectures and comparing planetary siblings. TOI-1246 is one such system, with a moderately bright K dwarf (V=11.6, K=9.9) and four transiting sub-Neptunes identified by TESS with orbital periods of 4.31 d, 5.90 d, 18.66 d, and 37.92 d. We collected 130 radial velocity observations with Keck/HIRES and TNG/HARPS-N to measure planet masses. We refit the 14 sectors of TESS photometry to refine planet radii (2.97±0.06 R⊕,2.47±0.08 R⊕,3.46±0.09 R⊕, 3.72±0.16 R⊕), and confirm the four planets. We find that TOI-1246 e is substantially more massive than the three inner planets (8.1±1.1M⊕, 8.8±1.2M⊕, 5.3±1.7M⊕, 14.8±2.3M⊕). The two outer planets, TOI-1246 d and TOI-1246 e, lie near to the 2:1 resonance (Pe/Pd=2.03) and exhibit transit timing variations. TOI-1246 is one of the brightest four-planet systems, making it amenable for continued observations. It is one of only six systems with measured masses and radii for all four transiting planets. The planet densities range from 0.70±0.24 to 3.21±0.44g/cm3, implying a range of bulk and atmospheric compositions. We also report a fifth planet candidate found in the RV data with a minimum mass of 25.6 ± 3.6 M⊕. This planet candidate is exterior to TOI-1246 e with a candidate period of 93.8 d, and we discuss the implications if it is confirmed to be planetary in nature

The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI-1246

Multiplanet systems are valuable arenas for investigating exoplanet architectures and comparing planetary siblings. TOI-1246 is one such system, with a moderately bright K dwarf (V = 11.6, K = 9.9) and four transiting sub-Neptunes identified by TESS with orbital periods of 4.31, 5.90, 18.66, and 37.92 days. We collected 130 radial velocity observations with Keck/HIRES and TNG/HARPS-N to measure planet masses. We refit the 14 sectors of TESS photometry to refine planet radii (2.97 +/- 0.06 R (circle plus), 2.47 +/- 0.08 R (circle plus), 3.46 +/- 0.09 R (circle plus), and 3.72 +/- 0.16 R (circle plus)) and confirm the four planets. We find that TOI-1246 e is substantially more massive than the three inner planets (8.1 +/- 1.1 M (circle plus), 8.8 +/- 1.2 M (circle plus), 5.3 +/- 1.7 M (circle plus), and 14.8 +/- 2.3 M (circle plus)). The two outer planets, TOI-1246 d and TOI-1246 e, lie near to the 2:1 resonance (P (e)/P ( d ) = 2.03) and exhibit transit-timing variations. TOI-1246 is one of the brightest four-planet systems, making it amenable for continued observations. It is one of only five systems with measured masses and radii for all four transiting planets. The planet densities range from 0.70 +/- 0.24 to 3.21 +/- 0.44 g cm(-3), implying a range of bulk and atmospheric compositions. We also report a fifth planet candidate found in the RV data with a minimum mass of 25.6 +/- 3.6 M (circle plus). This planet candidate is exterior to TOI-1246 e, with a candidate period of 93.8 days, and we discuss the implications if it is confirmed to be planetary in nature

NEID Rossiter–McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star

Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other mechanisms (e.g., primordial misalignment or planet-star interactions) are more important in sculpting the obliquity distribution. Here we present the stellar obliquity measurement of TOI-1268 (TIC-142394656, V mag ∼10.9), a young K-type dwarf hosting an 8.2 day period, Saturn-sized planet. TOI-1268's lithium abundance and rotation period suggest the system age between the ages of the Pleiades cluster (∼120 Myr) and the Prasepe cluster (∼670 Myr). Using the newly commissioned NEID spectrograph, we constrain the stellar obliquity of TOI-1268 via the Rossiter-McLaughlin effect from both radial velocity and Doppler tomography signals. The 3σ upper bounds of the projected stellar obliquity λ from both models are below 60°. The large host star separation (a/R ∗ ∼17), combined with the system's young age, makes it unlikely that the planet has realigned its host star. The stellar obliquity measurement of TOI-1268 probes the architecture of a young gas giant beyond the reach of tidal realignment (a/R ∗ ≲10) and reveals an aligned or slightly misaligned system

Ixekizumab for patients with non-radiographic axial spondyloarthritis (COAST-X): a randomised, placebo-controlled trial

Background: Ixekizumab, a high-affinity interleukin-17A (IL-17A) monoclonal antibody, has previously shown efficacy in radiographic axial spondyloarthritis (also known as ankylosing spondylitis). We aimed to evaluate the efficacy and safety of ixekizumab, an IL-17 inhibitor, in non-radiographic axial spondyloarthritis. Here, we report the primary results of COAST-X. Methods: COAST-X was a 52-week, randomised, double-blind, placebo-controlled, parallel-group study done at 107 sites in 15 countries in Europe, Asia, North America, and South America. Eligible participants were adults (aged ≥18 years) with active axial spondyloarthritis without definite radiographic sacroiliitis (non-radiographic axial spondyloarthritis), objective signs of inflammation (via MRI or C-reactive protein), and an inadequate response or intolerance to non-steroidal anti-inflammatory drugs (NSAIDs). Patients were randomly assigned (1:1:1) to receive subcutaneous 80 mg ixekizumab every 4 weeks (Q4W) or every 2 weeks (Q2W), or placebo. Changing background medications or switching to open-label ixekizumab Q2W, or both, was allowed after week 16 at investigator discretion. Primary endpoints were Assessment of SpondyloArthritis international Society-40 (ASAS40) response (defined as an improvement of 40% or more and an absolute improvement from baseline of 2 units or more [range 0–10] in at least three of the four domains [patient global, spinal pain, function, and inflammation] without any worsening in the remaining one domain) at weeks 16 and 52. Patients who switched to open-label ixekizumab were imputed as non-responders in logistic regression analysis. This trial is registered with ClinicalTrials.gov, number NCT02757352. Findings: Between Aug 2, 2016, and Jan 29, 2018, 303 patients were enrolled (105 to placebo, 96 to ixekizumab Q4W, and 102 to ixekizumab Q2W). Both primary endpoints were met: ASAS40 at week 16 (ixekizumab Q4W: 34 [35%] of 96, p=0·0094 vs placebo; ixekizumab Q2W: 41 [40%] of 102, p=0·0016; placebo: 20 [19%] of 105) and ASAS40 at week 52 (ixekizumab Q4W: 29 [30%] of 96, p=0·0045; ixekizumab Q2W: 32 [31%] of 102, p=0·0037; placebo: 14 [13%] of 105). 60 (57%) of 104 patients in the placebo group, 63 (66%) of 96 in the ixekizumab Q4W group, and 79 (77%) of 102 in the ixekizumab Q2W group had at least one treatment-emergent adverse event. The most common treatment-emergent adverse events in the ixekizumab groups were nasopharyngitis and injection site reaction. Of the treatment-emergent adverse events of special interest, there was one case of serious infection in the ixekizumab Q4W group. The frequency of serious adverse events was low (four [1%] of 302) and similar across the three groups. There were no malignancies or deaths. No new safety signals were identified. Interpretation: Ixekizumab was superior to placebo for improving signs and symptoms in patients with non-radiographic axial spondyloarthritis at weeks 16 and 52. Reports of adverse events were similar to those of previous ixekizumab studies. Ixekizumab offers a potential therapeutic option for patients with non-radiographic axial spondyloarthritis who had an inadequate response or were intolerant to NSAID therapy. Funding: Eli Lilly and Company

Validation of 13 Hot and Potentially Terrestrial TESS Planets

The James Webb Space Telescope will be able to probe the atmospheres and surface properties of hot, terrestrial planets via emission spectroscopy. We identify 18 potentially terrestrial planet candidates detected by the Transiting Exoplanet Survey Satellite (TESS) that would make ideal targets for these observations. These planet candidates cover a broad range of planet radii (Rp ~ 0.6-2.0R⊕) and orbit stars of various magnitudes (Ks = 5.78-10.78, V = 8.4-15.69) and effective temperatures (Teff ~ 3000-6000 K). We use ground-based observations collected through the TESS Follow-up Observing Program (TFOP) and two vetting tools-DAVE and TRICERATOPS-to assess the reliabilities of these candidates as planets. We validate 13 planets: TOI-206 b, TOI-500 b, TOI-544 b, TOI-833 b, TOI-1075 b, TOI-1411 b, TOI-1442 b, TOI-1693 b, TOI-1860 b, TOI-2260 b, TOI-2411 b, TOI-2427 b, and TOI-2445 b. Seven of these planets (TOI-206 b, TOI-500 b, TOI-1075 b, TOI-1442 b, TOI-2260 b, TOI-2411 b, and TOI-2445 b) are ultra-short-period planets. TOI-1860 is the youngest (133 ± 26 Myr) solar twin with a known planet to date. TOI-2260 is a young (321 ± 96 Myr) G dwarf that is among the most metal-rich ([Fe/H] = 0.22 ± 0.06 dex) stars to host an ultra-short-period planet. With an estimated equilibrium temperature of ~2600 K, TOI-2260 b is also the fourth hottest known planet with Rp < 2 R⊕