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In the {\Lambda}-CDM paradigm of cosmology, anisotropies larger than 260 Mpc shouldn't exist. However, the existence of the Hercules-Corona Borealis Great Wall (HCB) is purported to challenge this principle by some with an estimated size exceeding 2000 Mpc. Recently, some have challenged the assertion of the existence of the HCB, attributing the anisotropy to sky exposure effects. It has never been explained why the original methods purporting the existence of the HCB produce anisotropies, even if sky-exposure effects are taken into account. In this paper, I apply the methods of the original papers purporting the existence of the HCB in various Monte-Carlo simulations that assume isotropy to analyze the empirical meaning of the significance levels of the original tests used. I find that, although the statistical tests at first glance show significant anisotropies present in the suspect sample, Monte-Carlo simulations can easily reproduce the sample in most cases, and if not, the differences can be accounted for by other statistical considerations. An updated sample raises the probability of drawing the observed clustering from an isotropic sample ten-fold in some cases. Thus the statistical tests used in prior studies overestimate the significance of the observed anisotropy, and an updated sample returns even less significant probabilities. Given the ability to reproduce the observed anisotropy in Monte-Carlo simulations, the new, higher probabilities of being drawn from isotropy for an updated sample, and the work of previous papers attributing anisotropies to sky-selection effects, the existence of the HCB must be treated as doubtful at best., Comment: 6 pages, 5 figures. Accepted for publication in MNRAS

Full list of authors: Christian, Sam; Vanderburg, Andrew; Becker, Juliette; Yahalomi, Daniel A.; Pearce, Logan; Zhou, George ; Collins, Karen A.; Kraus, Adam L.; Stassun, Keivan G.; de Beurs, Zoe; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Winn, Joshua N.; Seager, S.; Jenkins, Jon M.; Abe, Lyu; Agabi, Karim; Amado, Pedro J.; Baker, David; Barkaoui, Khalid; Benkhaldoun, Zouhair; Benni, Paul; Berberian, John; Berlind, Perry; Bieryla, Allyson; Esparza-Borges, Emma; Bowen, Michael; Brown, Peyton; Buchhave, Lars A.; Burke, Christopher J.; Buttu, Marco; Cadieux, Charles; Caldwell, Douglas A.; Charbonneau, David; Chazov, Nikita; Chimaladinne, Sudhish; Collins, Kevin I.; Combs, Deven; Conti, Dennis M.; Crouzet, Nicolas; de Leon, Jerome P.; Deljookorani, Shila; Diamond, Brendan; Doyon, René; Dragomir, Diana; Dransfield, Georgina; Essack, Zahra; Evans, Phil; Fukui, Akihiko; Gan, Tianjun; Esquerdo, Gilbert A.; Gillon, Michaël; Girardin, Eric; Guerra, Pere; Guillot, Tristan; K. Habich, Eleanor Kate; Henriksen, Andreea; Hoch, Nora; Isogai, Keisuke I.; Jehin, Emmanuël; Jensen, Eric L. N.; Johnson, Marshall C.; Livingston, John H.; Kielkopf, John F.; Kim, Kingsley; Kawauchi, Kiyoe; Krushinsky, Vadim; Kunzle, Veronica; Laloum, Didier; Leger, Dominic; Lewin, Pablo; Mallia, Franco; Massey, Bob; Mori, Mayuko; McLeod, Kim K.; Mékarnia, Djamel; Mireles, Ismael; Mishevskiy, Nikolay; Tamura, Motohide; Murgas, Felipe; Narita, Norio; Naves, Ramon; Nelson, Peter; Osborn, Hugh P.; Palle, Enric; Parviainen, Hannu; Plavchan, Peter; Pozuelos, Francisco J.; Rabus, Markus; Relles, Howard M.; Rodríguez López, Cristina; Quinn, Samuel N.; Schmider, Francois-Xavier; Schlieder, Joshua E.; Schwarz, Richard P.; Shporer, Avi; Sibbald, Laurie; Srdoc, Gregor; Stibbards, Caitlin; Stickler, Hannah; Suarez, Olga; Stockdale, Chris; Tan, Thiam-Guan; Terada, Yuka; Triaud, Amaury; Tronsgaard, Rene; Waalkes, William C.; Wang, Gavin; Watanabe, Noriharu; Wenceslas, Marie-Sainte; Wingham, Geof; Wittrock, Justin; Ziegler, Carl.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 au. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation. © 2022. The Author(s). Published by the American Astronomical Society., The IRSF project is a collaboration between Nagoya University and the South African Astronomical Observatory (SAAO) supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (grant Nos. 10147207 and 10147214) and Optical & Near-Infrared Astronomy Inter-University Cooperation Program, from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan and the National Research Foundation (NRF) of South Africa. This work is partly supported by JSPS KAKENHI grant No. JP18H05439, and JST PRESTO grant No. JPMJPR1775, and a University Research Support Grant from the National Astronomical Observatory of Japan (NAOJ). This work is partly supported by Grant-in-Aid for JSPS Fellows, grant No. JP20J21872. This work is partly supported by JSPS KAKENHI grant No. JP17H04574. This work is partly supported by JSPS KAKENHI grant No. JP20K14518, and by Astrobiology Center SATELLITE Research project AB022006. M.T. is supported by MEXT/JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005. This work is partly supported by JSPS KAKENHI grant No. JP21K13955. This work is partly supported by JSPS KAKENHI grant No. 20K14521. C.R.-L. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). M.R. acknowledges support from the Universidad Católica de lo Santísima Concepción grant DI-FIAI 03/2021. P.J.A. acknowledges support from grant AYA2016-79425-C3-3-P of the Spanish Ministry of Economy and Competitiveness (MINECO) and the Centre of Excellence "Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). This paper is based on observations made with the T150 telescope at the Sierra Nevada Observatory (Granada, Spain), operated by the Instituto de Astrofísica de Andalucía (IAA—CSIC). The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liège (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). D.D. acknowledges support from the TESS Guest Investigator Program grant No. 80NSSC19K1727 and NASA Exoplanet Research Program grant No. 18-2XRP18_2-0136. M.G. and E.J. are F.R.S.-FNRS Senior Research Associates. K.K.M. acknowledges support from the New York Community Trust's Fund for Astrophysical Research. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation.

Additional file 1: Figure S1. Fab fragment expression patterns obtained via western blot analysis for comparison of the soluble and IB fractions of different cultivations. Table S1. Loading scheme for the western blots shown in Figure S1. Table S2. Extracellular DNA content at fermentation end. Figure S2. Elution profiles for ProteinG affinity chromatography (a) and CIEX chromatography (b). Figure S3. Elution profiles of the HPLC amino acid quantification. (a) shows a low norleucin sample (B, Reference, at fermentation end) and (b) shows a high norleucin sample (H, Scale-down, fermentation end).

Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 AU) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia EDR3 and the TESS mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there appears to be a statistically significant difference in the inclination distribution of wide-binary stars with transiting planets compared to a control sample (p=0.0048). This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 AU. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion is the most promising explanation., {"references":["Batygin, K. 2012, Nature, 491, 418, doi: 10.1038/nature11560","El-Badry, K., & Rix, H.-W. 2018, MNRAS, 480, 4884, doi: 10.1093/mnras/sty2186","Pearce, L. A., Kraus, A. L., Dupuy, T. J., et al. 2020, ApJ, 1774 894, 115, doi: 10.3847/1538-4357/ab8389","Roisin, A., Teyssandier, J., & Libert, A.-S. 2021, arXiv e-prints, arXiv:2107.06832.1793"]}

Methanol (MeOH) synthesis at low temperature in a liquid medium presents the possibility of achieving full syngas conversion per pass. The Low temperature MeOH synthesis (LTMS) process is advantageous over the current technology for MeOH production since the former is thermodynamically favourable and gives a high yield per pass. The LTMS involves two main steps, (i) MeOH carbonylation to form methyl formate and (ii) hydrogenolysis of methyl formate to form MeOH. The initial aim of the present work was to develop, characterize and evaluate the catalyst system involved in the LTMS process. A once-through catalyst system involving copper (II) acetate and methoxide was used to obtain up to 92 % conversion (> 94 % selectivity to MeOH) per batch at 20 bar syngas pressure and 100 oC temperature within 2 h. XRD and TEM characterization of the slurry catalyst system revealed that about 10 ± 5 nm Cu2O/Cu0 nanoparticles were involved in the catalytic process. Decreasing Cu nanoparticles sizes led to increased MeOH production due to an increase in active Cu surface area, which enhanced methyl formate hydrogenolysis. Agglomeration of the Cu nanoparticles in the course of MeOH production was identified as a major cause for the deactivation of the Cu nanoparticle component of the LTMS catalyst system. Furthermore, with the aim of investigating the role of solvents polarity on the LTMS, MeOH production maximized for solvents with dielectric constant (ɛ) around 7.2, similar to the polarity of diglyme. A probe of possible side reactions of the main intermediate revealed that, in the presence of methoxide, low polar solvents enhanced decarbonylation of methyl formate while high polar solvents enhanced a nucleophilic substitution to form dimethyl ether and sodium formate. Relatively moderate polar solvents such as diglyme appeared to give a good balance in minimizing possible side reactions of methyl formate and therefore enhanced MeOH production. In addition, the spinning disk reactor (SDR) was used to synthesize on-purpose Cu nanoparticles with predefined particle sizes for catalysing the LTMS reaction. By maintaining the same chemical recipe, Cu nanoparticle sizes were tuned down to 3 nm when physical conditions were varied to shorten for example micromixing time, mean residence time and relative residence time distribution. This subsequently led to uniform nucleation and ultimately formation of smaller Cu nanoparticle sizes with narrow particle size distribution. At the end, a model was proposed for a complete LTMS process with the help of Aspen HYSYS simulation tool, using an air-blown autothermal reformer, for a full conversion per pass at 60 bar syngas (0.31 CO: 0.62 H2: 0.07 N2) and 100 oC MeOH synthesis temperature.

We present the discovery and characterization of five hot and warm Jupiters -- TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960) -- based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the $TESS$ Follow-up Observing Program (TFOP) Working Group. The planets are all Jovian size (R$_{\rm P}$ = 1.01-1.77 R$_{\rm J}$) and have masses that range from 0.85 to 6.33 M$_{\rm J}$. The host stars of these systems have F and G spectral types (5595 $\le$ T$_{\rm eff}$ $\le$ 6460 K) and are all relatively bright (9 $ 1.7R$_{\rm J}$, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive hot Jupiter discovered to date by $TESS$ with a measured mass of $6.31^{+0.28}_{-0.30}$ M$_{\rm J}$ and a statistically significant, non-zero orbital eccentricity of e = $0.074^{+0.021}_{-0.022}$. This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-Solar analogue. NASA's $TESS$ mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals., Comment: 25 Pages, 7 Figures, 5 Tables, Accepted to The Astronomical Journal

Acetylcholine is a neurochemical that has a wide variety of functions in the brain and other organ systems of the body. Specifically, it is a neurotransmitter that acts as a chemical message that is released by neurons and allows them to communicate with one another and other specialized cells such as myocytes and cells found in glandular tissues. The name "acetylcholine" is derived from its chemical structure, as it is an ester of acetic acid and choline. Tissues of the body that use this chemical messenger or are responsive to it are referred to as cholinergic. There is a class of chemicals called anticholinergics that interfere with acetylcholine's action on tissues as well.  While ACh operates as a neurotransmitter in many parts of the body, it is most commonly associated with the neuromuscular junction. The neuromuscular junction is where motor neurons located in the ventral spinal cord synapse with muscles in the body to activate them. Acetylcholine also functions as a neurotransmitter in the autonomic nervous system, acting both as the neurotransmitter between preganglionic and postganglionic neurons as well as being the final release product from parasympathetic postganglionic neurons.[1], (Copyright © 2022, StatPearls Publishing LLC.)