The electoral scene in the period from 133 to 129 b.c.e. was doubtless unpredictable, even in the centuriate assembly, and any prosopographical modelling based on the available data would be adventurous. The report that Appius Claudius Pulcher (cos. 143 and bitter opponent to Scipio Aemilianus) ran in 133 for a second consulship is not implausible, and the possibility of a thwarted candidature, whatever its duration and the reason for its termination, should be registered. The successful candidates were P. Popillius Laenas and P. Rupilius, the latter a close associate of Scipio. The unsuccessful consular candidacy of Rupilius’ brother Lucius should be dated to 132, 131 or 130. The elimination of the first of those options by F.X. Ryan (CQ 45 [1995], 263–5) is challenged.

Nearly all intragroup (IGL) and intracluster light (ICL) comes from stars that are not bound to any single galaxy but were formed in galaxies and later unbound from them. Kinematic information on these very low surface brightness structures mostly comes from discrete tracers such as planetary nebulae and globular clusters, showing highly unrelaxed velocity distributions. Cosmological hydrodynamical simulations provide key predictions for the dynamical state of IGL and ICL and find that most IC stars are dissolved from galaxies that subsequently merge with the central galaxy. The increase of the measured velocity dispersion with radius in the outer halos of bright galaxies is a key feature to identify IGL and ICL components. In the local groups and clusters, IGL and ICL are more centrally concentrated than the galaxies, with their typical fractions that are few to ten percent, i.e. significantly lower than the average values in more evolved clusters. The properties of ICPNe, their luminosity functions and specific frequencies were key to further constraint the age (10 Gyr) and the metallicity ([M / Fe]< −1.0) of the IC/IGL. The results in the nearby clusters are briefly illustrated.

I have performed numerical hydrodynamical calculations of outflows driven by the evaporation of a pseudo-barotropic ring around a luminous central star. The outflow shapes and internal structures resemble known cylindrical nebulae. Some of the corresponding synthetic spectra show ‘Hubble’ type outflow.

The tilt of the bipolar magnetic region (BMR) is crucial in the Babcock-Leighton process for the generation of the poloidal magnetic field in the Sun. We extend the work of Jha et al. (2020) and analyze the recently reported tracked BMR catalogue based on AutoTAB (Sreedevi et al. 2023) from Michelson Doppler Imager (1996–2011) and Helioseismic and Magnetic Imager (2010–2018). Using the tracked information of BMRs based on AutoTAB, we confirm that the distribution of Bmax reported by Jha et al. (2020) is not because of the BMRs are picked multiple times at the different phases of their evolution instead it is also present if we consider each BMRs only once. Moreover, we find that the slope of Joy’s law (〈γ0〉) initially increases slowly with the increase of Bmax. However, when Bmax >2.5 kG, γ0 decreases. The decrease of observed γ0 with Bmax provides a hint to a nonlinear tilt quenching in the Babcock-Leighton process.

This paper argues that despite recent tendencies to minimize the differences between Posidonius and the Early Stoics, there are some important aspects of Stoic ethics in which Posidonius deviated from the orthodox doctrine. According to two passages in Diogenes Laertius, Posidonius counted health and wealth among the goods and held that virtue alone is insufficient for happiness. While Kidd in his commentary dismissed this report as spurious, there are good reasons to take Diogenes’ remarks seriously. Through a careful analysis of the sources, in particular of Galen's De placitis Hippocratis et Platonis, this article offers a new interpretation of Posidonius’ ethics. It sheds light on Posidonius’ theory of virtues and shows that Posidonius must have granted a special status to things like health and wealth even if he did not regard them as genuine goods.

A high sensitivity and high-angular resolutions infrared space telescope, the James Webb Space Telescope (JWST), allowed us to study dust and molecules in unprecedented details. This contribution highlights the first year of JWST’s scientific operation, and reports prospects of dust and molecular studies in the coming future.

Observations of super flare occurrence (with energy 1033–1036 erg)s in low mass stars like M dwarfs still remains as a puzzle. In this paper we have inferred the typical sizes and characteristics of magnetic fields associated with active regions in M dwarfs responsible for these super flares. This is done by extrapolation of physical conditions associated with largest solar flares. The average poloidal and toroidal magnetic fields near the surface of selected M dwarfs will be also inferred in this context.

A quarter of a century has passed since the observing technique of integral field spectroscopy (IFS) was first applied to planetary nebulae (PNe). Progress after the early experiments was relatively slow, mainly because of the limited field-of-view (FoV) of first generation instruments. With the advent of MUSE at the ESO Very Large Telescope, this situation has changed. MUSE is a wide field-of-view, high angular resolution, one-octave spanning optical integral field spectrograph with high throughput. Its major science mission has enabled an unprecedented sensitive search for Lyα emitting galaxies at redshift up to z=6.5. This unique property can be utilized for faint objects at low redshift as well. It has been demonstrated that MUSE is an ideal instrument to detect and measure extragalactic PNe with high photometric accuracy down to very faint magnitudes out to distances of 30 Mpc, even within high surface brightness regions of their host galaxies. When coupled with a differential emission line filtering (DELF) technique, MUSE becomes far superior to conventional narrow-band imaging, and therefore MUSE is ideal for accurate Planetary Nebula Luminosity Function (PNLF) distance determinations. MUSE enables the PNLF to become a competitive tool for an independent measure of the Hubble constant, and stellar population studies of the host galaxies that present a sufficiently large number of PNe.

My thanks to the reviewers for their insightful comments and to the editors of Church History, most especially Jon Butler, for shepherding the reviews. Having once served as a Church History editor, I appreciate his labors even more.