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Summary of AS and NAS methylation tests on the 2.2 million CpGs tested across any of the datasets. This file contains a file of tab-separated values (.txt text file) with the following columns: (1) CpG chromosome, (2) CpG location, (3) corrected GIT p value, (4) corrected mQTL p value, (5) corrected ASM p value, (6) ChromHMM state. (ZIP 19804 kb)

Excel file (.xlsx) containing list of over-expressed transcripts (107 genes) in WI/Ma and WI/Ut contrasts. (XLSX 26Â kb)

Video S1. Example of “resident stays”. Bee Y67 landed on a flower occupied by bee W58 and left spontaneously. In this example, the flower was “not-emptied” as bee W58 fed on the flower for less than 8 s before the interaction occurred. (AVI 461 kb)

Related Article: Paul Chatelain, Abhijit Sau, Christopher N. Rowley, Joseph Moran|2019|Angew.Chem.,Int.Ed.|58|14959|doi:10.1002/anie.201908336 Related Article: Paul Chatelain, Abhijit Sau, Christopher N. Rowley and Joseph Moran|2019|CSD Communication|||

Related Article: Marc‐Antoine Stoeckel, Yoann Olivier, Marco Gobbi, Dmytro Dudenko, Vincent Lemaur, Mohamed Zbiri, Anne A. Y. Guilbert, Gabriele D'Avino, Fabiola Liscio, Andrea Migliori, Luca Ortolani, Nicola Demitri, Xin Jin, Young‐Gyun Jeong, Andrea Liscio, Marco‐Vittorio Nardi, Luca Pasquali, Luca Razzari, David Beljonne, Paolo Samorì, Emanuele Orgiu|2021|Adv.Mater.|33|2007870|doi:10.1002/adma.202007870

We present Herschel SPIRE and PACS maps of the Cepheus Flare clouds L1157, L1172, L1228, L1241, and L1251, observed by the Herschel Gould Belt Survey of nearby star-forming molecular clouds. Through modified blackbody fits to the SPIRE and PACS data, we determine typical cloud column densities of (0.5-1.0)x1021/cm^2^ and typical cloud temperatures of 14-15K. Using the getsources identification algorithm, we extract 832 dense cores from the SPIRE and PACS data at 160-500{mu}m. From placement in a mass versus size diagram, we consider 303 to be candidate prestellar cores, and 178 of these to be "robust" prestellar cores. From an independent extraction of sources at 70{mu}m, we consider 25 of the 832 dense cores to be protostellar. The distribution of background column densities coincident with candidate prestellar cores peaks at (2-4)x1021/cm^2^. About half of the candidate prestellar cores in Cepheus may have formed as a result of the widespread fragmentation expected to occur within filaments of "transcritical" line mass. The lognormal robust prestellar core mass function (CMF) drawn from all five Cepheus clouds peaks at 0.56M{sun} and has a width of ~0.5dex, similar to that of Aquila's CMF. Indeed, the width of Cepheus's aggregate CMF is similar to the stellar system initial mass function (IMF). The similarity of CMF widths in different clouds and the system IMF suggests a common, possibly turbulent origin for seeding the fluctuations that evolve into prestellar cores and stars. Cone search capability for table J/ApJ/904/172/table1 (Details of Herschel observations) Cone search capability for table J/ApJ/904/172/tablec1 (Observed properties of dense cores in Cepheus) Cone search capability for table J/ApJ/904/172/tablec2 (Derived properties of dense cores in Cepheus)

Experimental demonstration of spatial Talbot amplification of a periodic binary amplitude grating. The spatial phase modulation is turned on and off, switching between the 3rd integer Talbot image and the q=3 Talbot amplification regimes; the difference in brightness between both regimes can be clearly observed.

IPTA DR2 common red noise, MCMC output These files are the primary output from a Markov chain Monte Carlo (MCMC) sampling process. They are samples from the posterior probability distribution for a particular model described in the companion paper. Each zipped tarball contains four files. The "chain" file has several tab-separated columns, each of which corresponds to a model parameter, except the last four which are metadata. The parameter names (including metadata) are listed in the companion "params" file. The frequencies used in the common red noise models are listed in the "crn_frequencies" file. Additional information is provided in a README file. Each row of the chain file is one sample from the model posterior. The first samples at the beginning of the MCMC are the "burn-in" phase, before the chain has converged to the posterior. We recommend discarding the first ~25% of samples before using them to make inferences.