Slices through the kinetic energy dissipation rate (top panels) and the gas density(bottom panels), in the subsonic regime (⁠⁠M = 0.2; left-hand panels) and the supersonic regime (⁠M = 5⁠; right-hand panels). Please see the paper for the full caption.

Published in #MNRAS: "The statistics and structure of dissipation in subsonic and supersonic turbulence", Troccoli & Federrath. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Simulations snapshots of the projected gas at epochs: t = 600 Myr ago (left panel), t = 200 Myr ago (centre) and at the present time (right panel). Streamlines are overlaid to show the projected motion of the hot CGM gas. Please see the paper for the full caption.

Published in #MNRAS: "Temperature asymmetry in the Milky Way’s hot circumgalactic medium induced by the Magellanic Clouds", Oprea et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Continuum image centred at 400 MHz from band 3 (top) and at 685 MHz from band 4 (bottom) of uGMRT. Please read the paper for the full caption (Fig. 1).

Published in #MNRAS: "Detection of non-thermal radio emission components from the Orion Nebula: stellar jets, cloud collision, or feedback from stellar winds?", Rashid et al. Please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

The first ≈0.3" resolution image of the Boötes Deep Field. This image consists of ≈8 billion pixels, contains over 4000 sources, and has a central sensitivity of 33.8 µJy beam^(-1)⁠. The image is 2.5 x 2.5 deg^2 with a restoring beam of 0.50 x 0.34⁠". We highlight three interesting extended sources within this field beneath with the respective locations indicated by arrows. We can now probe radio emission of these sources to a new level thanks to the sub-arcsecond resolution.

Published in #MNRAS: "The sub-arcsecond ILT view of the Boötes Deep Field: a link between low-frequency kiloparsec radio morphology and AGN-driven ionized outflows", Escott et al. This is Fig. 2: please visit academic.oup.com/mnras/articl... @royalastrosoc.bsky.social

Face-on surface density maps of our simulation depicting different stages in the evolution of the bar. Please see the paper for the full caption.

Published in #MNRAS: "Measuring the evolution of stellar bars with the host galaxy’s spin", Joshi et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Density maps showing the time evolution of the 1ms simulation. The energy injection from the central engine inflates a bubble in the centre of the ejecta, filled with high-pressure gas. RT instabilities develop at the edge of the bubble, eventually causing it to rupture at discrete points along its surface. The gas contained in the bubble vents out through these rupture points and leaves behind low-density channels in the remnant.

Published in #MNRAS: "Dynamics and observational signatures of core-collapse supernovae with central engines: hydrodynamics simulations with Monte Carlo post-processing", Eiden & Kasen. This is Fig. 2: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social

Radio continuum image of the TDRG showing its morphology as well as the position of its host galaxy as indicated by the central cross. Background: Pan-STARRS DR1 gri–composite optical image; Contour: MIGHTEE-hi continuum (levels: –3, 3, 5, 10, 15, 25, 30, 35, 40, 50, 75, 100, 150, 200, 250, 300 x sigma_(local) = 5.9 µJy beam^(−1)). The three pairs of lobes are indicated by I (outermost), II (middle) and III (innermost). The scale indicating 100 kpc (12.4 arcsec) and the synthesized beam of MIGHTEE-hi are in the bottom left corner of the image.

Published in #MNRAS: "MIGHTEE: discovery of a triple-double radio galaxy", Rarivoarinoro et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Looking forward to seeing Project Hail Mary? 🚀 🎥

Well, if we ever were forced into travelling to an exoplanet system in search of life, where would be the best place to look? 🪐👽️

That's exactly what a new paper in #MNRAS tried to find out...

⤵️

Left: public PACS-70 µm observations and (middle) SPIRE-500 observations from the Herschel Science Archive. Right: H_2 column density maps from the HGBS (P. André et al. 2010; S. Bontemps et al. 2010; V. Könyves et al. 2015; D. Arzoumanian et al. 2019) (see Section 2). The box shows the region that we focus on in this paper (see e.g. Fig. 2). A 1 parsec scalebar is shown at the upper left corner of each image, and a circle indicating the observational beamsize appears in the lower right.

Published in #MNRAS: "MAJORS II:  HCO+ and HCN abundances in W40", Plume et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

An example of a planet inside the low-density magnetosphere in the stable regime of accretion in model Cav2. Translucent surfaces show two values of density. Lines are sample magnetic field lines. The equatorial slice shows the density distribution.

Published in #MNRAS: "3D MHD simulations of planet migration in cavities and inner discs of magnetized stars", Romanova et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Cluster 001 from the GIZMO_3k run, decomposed into orbiting (yellow–purple) and infalling (black) particles. Please see the paper for the full caption.

Published in #MNRAS: "The Three Hundred Project: deducing the stellar splashback structure of galaxy clusters from their orbiting profiles", Walker et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

^(12)CO J = 3–2 emission distribution integrated (moment 0) between –90 and –70 km s^(-1) (blue), and between – 55 and 5+ km s^(-1)(red). The systemic velocity of the complex is about –64 km s⁠^(-1). The black contour levels are at 5, 8, 12, and 18 mJy beam⁠^(-1). The ALMA continuum emission at 340 GHz is represented in green. The position of the five molecular cores is indicate with the yellow crosses. For more details see M. E. Ortega et al. (2023).

Published in #MNRAS: "Unveiling the collision between molecular outflows: observational evidence and hydrodynamic simulations", Cohen-Arazi et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

HR diagram of the TESS-SPOC FFI sample described in L. Doyle et al. (2024), generated using Gaia DR3 (Gaia Collaboration 2023) colours and parallax, where the colour bar represents the log density of stars. Increasing in MG, the three host stars NGTS-34, TOI-4940, and NGTS-35 are represented by yellow, blue, and pink stars, respectively.

Published in #MNRAS: "A 43 d transiting Neptune and two 25 d Saturns from TESS, NGTS, and ASTEP", Kendall et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social

Visualization of jet activity in the L100m6h simulation at z = 0.2 in proper coordinates. The background image shows the cosmic web using the gas surface density, while particles kicked into jets by BHs are displayed using both information on the elapsed time since when they were kicked into jets (colour) and their surface density (opacity). Side panels zoom in on individual jets of interest, with further zoom-ins on to their host galaxies (except in the case of a cluster and its BCG) displayed using luminosities in the SDSS i, r, and g bands assigned to RGB colours.

Published in #MNRAS: "A hybrid active galactic nucleus feedback model with spinning black holes, winds and jets", Huško et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Optical and peak temperature (⁠⁠T_(peak)) images of NGC7793. Please see the paper for the full caption.

Published in #MNRAS: "The turbulence driving mode in NGC7793 and NGC1313", Miller et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

The face-on surface mass density projection of the stellar discs in the live halo fiducial simulation suite at t = 2.5 Gyr for MW scale. Please see thepaper for the full caption.

Published in #MNRAS: "Formation time-scales for stellar bars in diverse galactic discs", Frosst et al. Please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Example images of ETGs (row 1), LTGs (row 2), galaxies classified as compact (row 3), and those flagged as unclassifiable (row 4). The size of each image is 10 arcsec on a side. The images from different instruments have different orientations – we intentionally keep it this way so that each galaxy is visually inspected at different orientations. In each image the first, second, and third columns show the JWST, HSC, and HST images, respectively. Each individual image has six panels. Within each image the panels in the first row show the original images from the different instruments, while the second row shows their unsharp-masked counterparts.

Published in #MNRAS: "Downsizing does not extend to dwarf galaxies: identifying the stellar mass regimes shaped by supernova and AGN feedback", Lazar et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Isolated DORCHA haloes along with the parent DORCHA _ 00: the subplots show the total projection along the z-direction for the simulations. Please see the paper for the full caption.

Published in #MNRAS: "The DORCHA suite: nature, nurture, and the phase-space distribution of the Milky Way’s high-redshift progenitors today", Balu et al. Please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Earth’s atmospheric composition as an example of comparative biosignatures and habsignatures. Earth, situated within the HZ (green annulus sector), emerges as an outlier. Compared to the abiotic baseline established by Venus and Mars, Earth exhibits significantly lower CO_2 levels (P. van Thienen et al. 2007) and considerably higher O_2 levels (indicated below each planet). All of these gases have plausible abiotic origins, but the abiotic baseline informs our expectation and identifies Earth as anomalous.

Published in #MNRAS: "Comparative biosignatures with systemic retrievals", Constantinou et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Dust surface density of simulated discs with a = 0.1 mm. Please see the paper for the full caption.

Published in #MNRAS: "Dust morphology under changing dust mass ratios in protoplanetary discs", Murray et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Top panel: composite image of GS-9209 obtained by the superposition of F090W, F200W, and F444W NIRCam photometry images. The dotted line is the effective FoV of our NIRSpec observations. A possible satellite is indicated. Bottom panel: zoomed-in portion of the same image, where we highlight the 0.35 arcsec x 0.35 arcsec aperture used for measuring the integrated stellar velocity dispersion. ⁠.

Published in #MNRAS: "When relics were made: vigorous stellar rotation and low dark matter content in the massive ultra-compact galaxy GS-9209 at z = 4.66", Pascalau et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

The metallicity distribution of NGC 1385, computed using the O_3N_2 metallicity diagnostic of M. Curti et al. (2017). In this Figure, both a large scale trend in decreasing metallicity (corresponding to a negative metallicity gradient) and small-scale (sub-kpc) fluctuations (which we argue correspond to face-on superbubbles) can be seen.

Published in #MNRAS: "The ‘bubbly’ interstellar medium as origin for the inhomogeneous internal metallicity distributions in large disc galaxies", Metha et al. This is Fig. 2: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Spitzer/IRAC mosaic of the Ser OB2 region in the 3.6 µ (blue), 5.8 µm (green), and 8.0 µm (red) bands. The yellow contours indicate the surface–density distribution of cluster members (Section 4), with the 60 x 60 pc box used for this analysis indicated (green rectangle). Several sub-regions are labelled.

Published in #MNRAS: "On the origin of kinematic structure in the young association Serpens OB", Kuhn et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

High-resolution LOFAR HBA image of the tailed radio galaxy (C) in the galaxy cluster MACS J1354.6+7715, observed at 144 MHz. A and B denotes two compact radio sources, while D marks an additional radio source detected in the field. Please see the paper for the full caption.

Composite image of the cluster combining optical, radio, and X-ray data. Please see the paper for the full caption.

Published in #MNRAS: "Wiggling through the ICM: multiresolution radio imaging of a tailed radio galaxy in MACS J1354.6+7715", Gani et al. These are Figs. 1 & 6: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

A comparison of the locations of four global 21 cm experiments with the maximal declination of the moon over a period of approximately 40 yr. Maximal lunar declination is shown as a continuous blue line, and the shaded blue area describes all possible lunar declinations over the course of a tropical month. The red band indicates a declination of ±0.5° around Sagittarius A*, describing the galactic bulge. Site latitudes are indicated by a grey line with varying styles. For this work, we chose to look at the MIST Deep Springs Valley site as it is the closest of the MIST sites to the equator, though it should be noted that MIST is an experiment designed to be mobile and is not fixed in one locale.

Published in #MNRAS: "Quantifying the impact of lunar and planetary occultation on experimental global 21 cm cosmology", Pattison et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

The evolution of the spatial distribution of GES stars with different infall orbital energies. Please see the paper for the full caption.

Published in #MNRAS: "From order to chaos: the blurred out metallicity gradient of the Gaia-Enceladus/Sausage progenito", Carrillo et al. This is Fig. 4: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

The peak main beam temperature maps of the CMZ before smoothing for the transitions and isotopologues of CO. Please see the paper for the full caption.

Published in #MNRAS: "CHIMPS2: the physical properties and star formation efficiency of molecular gas in the central molecular zone", King et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

The most distant and most primitive object ever explored by a spacecraft, the ultra-red, 4 billion-year-old body known as Arrokoth, which is shaped like a snowman.

Snowmen in space? ⛄️ 🌌🤔

Yes, you read that correctly! A new study published in #MNRAS has uncovered evidence as to why so many icy objects in the outer solar system are shaped like two connected spheres – much like a snowman.

Read more at 👉️ ras.ac.uk/news-and-pre...

An overview of the three impulsive quiet Sun events (labelled Events 1–3) captured with NuSTAR on 2020 February 21. Top row: AIA 211 Å images of the flaring regions, with NuSTAR FPMA + FPMB contours shown in green. The AIA light curves were found over the grey dashed boxes. Bottom row: NuSTAR and AIA light curves showing the X-ray and EUV evolution of the events. Shaded regions represent the time intervals used for NuSTAR spectral fitting.

Published in #MNRAS: "Quiet Sun impulsive events observed with NuSTAR during solar minimum", Paterson et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

False-colour RGB (F277W/F200W/F115W) images for the 20 largest LSBs in the sample, by effective radii. Each cut-out is 50 x 50 pixels (1.5 x 1.5 arcsec), and each object is normalised by its individual cut-out’s brightest pixel. Each object’s JADES catalogue ID and photometric redshift are shown in the lower left corners, while the physical scale corresponding to 0.3 arcsec is provided in the top right corners.

Published in #MNRAS: "JADES: low surface brightness galaxies at 0.4 < z < 0.8 in GOODS-S", Shields et al. This is Fig. 4: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com