#mnras

Same as Fig. 3 but for the companion star in its preferred position. The arrow indicates the motion of the shadow.

Predicted geometry of the 2026 May 4 event showing the broader ring-occultation shadow region relative to the main-body shadow. A zoomable version of the map is available at https://opop.obspm.fr/media/data/chords/156331/Haumea_4th_May_2026_occultation_map_IAA-CSIC.html. Observations of this event can be reported through the occultation portal at https://opop.obspm.fr/create_report/2518/.

Published in #MNRAS: "Predictions of stellar occultations by Haumea and the event of 2026 May 4", Ortiz et al. These are Figs. 3 & 4: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Selected slices through the reconstructed fields. These slices are one grid cell thick (approximately 10 pc). Please see the paper for the full caption.

Published in #MNRAS: "The radial component of the local Galactic magnetic field in 3D", McCallum et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

The five cubic COLIBRE boxes, which have side lengths ranging from 25 to 400 cMpc. Colour shows total surface density (in 5 Mpc thick faces) at ⁠z = 0. The volumes available at high (m5), intermediate (m6), and low (m7) resolution are indicated. Note, however, that at the time of writing the 50 and 100 Mpc high-resolution simulations have not yet reached redshift ⁠z = 0.

Published in #MNRAS: "The COLIBRE project: cosmological hydrodynamical simulations of galaxy formation and evolution", Schaye et al. Please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Vertical profiles of the Martian atmosphere in the absence of acoustic–gravity waves. Please see the paper for the full caption.

Published in #MNRAS: "Effects of acoustic–gravity waves on the total electron content of the Martian ionosphere", Wang et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

NOT/ALFOSC gri deep stack showing SN 2024cld (circled), embedded in the spiral arm of host galaxy NGC 6004. The panels above show the GOTO discovery/template/difference image for SN 2024cld.

Published in #MNRAS: "SN 2024cld: unveiling the complex mass-loss histories of evolved supergiant progenitors to core collapse supernovae", Killestein et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Top: Roman detector array overlaid on top of our science image input. Bottom: Blown up version of the science image input. Specifically shown is the F160W cutout of the CANDELS COSMOS field at a resolution of 30 mas/pixel. The area of the image is 15’ x 6’ or 0.025 deg⁠^2.

Published in #MNRAS: "ESpRESSO: Modelling realistic crowded scenes for deep Roman Space Telescope grism spectroscopy", Gabrielpillai et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Images obtained from different AIA, HMI, and IRIS-SJI passbands as labelled, showing the region of detailed investigation. Please see the paper for the full caption.

Published in #MNRAS: "Investigating the propagation of small-scale flare energy in the lower and upper atmosphere of solar active region", Gupta et al. This is Fig. 2: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Plot of the two-dimensional surface density for a thin disc around an MBHB with mass ratio q = 1.0 (left) and q = 0.1 (right), accreting from a CBD. The image is from a simulation snapshot, using Sailfish, taken well after the disc is viscously relaxed. The axes show the x-y plane in units of the binary separation a.

Published in #MNRAS: "Unequal mass binary evolution driven by high-Mach circumbinary discs", Clyburn & Zrake. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

he six principal axis views of the final shape model of RS_(11) generated with both optical and radar data in SHAPE. The model has pole solution lambda = 225° and ß = 80°. The average length between the 1500 vertices is 26.9 m. Red shading is applied to facets not viewed by the delay-Doppler radar imaging, while yellow shading is applied to facets viewed only at scattering angles greater than 60° in the delay-Doppler images.

Published in #MNRAS: "The shape and spin state of (275677) 2000 RS11 from ground-based radar and optical observations", Cannon et al. This is Fig. 4: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

(a) unWISE 12.0 µm image of the G351 cloud overlaid with the positions of YSOs (red circles) identified using [5.8]-[4.5] versus [3.6]-[4.5] CCD (see the text for more details). The white dashed box highlights the area shown in Figs 3(a)–(d). (b) An overlay of SMGPS 1.3 GHz continuum emission contours (in blue) on ATLASGAL 870 µm contours (in red). The red contour levels are 0.14, 0.24, 0.38, 0.48, 0.94, 1.41, 2.35, 3.30, 4.71, 9.42, 14.12, 18.83, 23.54, 37.66, and 42.37 mJy beam⁠^(-1). The blue contour levels are 0.44, 0.88, 2.6, 4.4, 6.2, 8.8, 18, 26, 35, 44, 70, and 79 mJy beam⁠^(-1). (c) Herschel 250 µm image of the G351 cloud. (d) Spitzer 4.5 µm/3.6 µm ratio map of the G351 cloud overlaid with the 870 µm emission contour level at 0.14 mJy beam^(-1)⁠. The cyan arrows are used to highlight the bright regions where star formation activity is prominent. The diamonds show the positions of ATLASGAL clumps. The scale bar corresponds to 3 pc at a distance of 2.0 kpc.

Published in #MNRAS: "Unveiling an hourglass-shaped magnetic field toward IRDC G351.77–0.53", Jadhav et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Left: MeerKAT 816 MHz image of Abell 4067 at ROBUST 0.0, with a resolution of 11.7 arcsec x 11.7 arcsec, position angle 0.0° and rms noise, sigma = 6.20 µJy beam⁠^(-1). The labels S1–S10 indicate the compact sources within the cluster region (dashed circle) and those near the extended source labelled ‘Relic’ are A, B, C and FRII. The X-ray cluster centre is marked by ‘X’. The synthesized beam is shown in cyan in the lower-left corner. The residual calibration artefacts seen in the image stem from a complex southern source with a total flux density of ≈Jy at 816 MHz, which remain despite extensive peeling and direction-dependent calibration attempts. Right: DESI Legacy Survey grz -image of the region of the labelled sources with the MeerKAT 816 MHz contours overlaid. Contour levels are drawn at [5, 9, 13, 17] x 1⁠ sigma, where sigma = 6.20 µJy beam⁠^(-1).

Published in #MNRAS: "Discovery of a nearby radio relic in the low-mass, merging cluster Abell 4067", Magolego et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Metallicity constraints on QSO1 inferred from the observed emission-line ratios. Please see the paper for the full caption.

Published in #MNRAS: "A black hole in a near pristine galaxy 700 Myr after the big bang", Maiolino et al. This is Fig. 1: please visit academic.oup.com/mnras/articl... to read the paper.
@royalastrosoc.bsky.social @academic.oup.com

The AR observed in AIA showing the SJI 1400 Å  FOV and the sub-FOV shown in Fig. 5. The rain trajectory is plotted in white as ‘original spline’.

Published in #MNRAS: "Compression, impact, and hot rebound flows from coronal rain downflows", Wachira and Antolin. This is Fig. 2: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

Surface accelerations (i.e. gravitational and rotational accelerations combined) for two representative asteroids.

Published in #MNRAS: "Modelling and characterizing spacecraft–surface interactions on small Solar system bodies", Fodde et al. This is Fig. 1: for the caption & to read the paper please visit academic.oup.com/mnras/articl... @royalastrosoc.bsky.social @academic.oup.com

The left, middle, and right panels show the HST/ACS F814W, JWST/NIRCam F277W and JWST/MIRI F770W images of three of the dwarf galaxies (from top to bottom: IDs 5, 120, and 232) presented in this paper. The contours on the MIRI images in the right panel represent the F814W emission from the HST/ACS images in the left panel. The horizontal bar shows the physical 1 kpc scale and the circle in the bottom left shows the PSF (FWHM) of the respective images. The potential emission from the dust becomes clearly visible in the MIRI images, which are otherwise absent in the HST images. See Section 4.1 for further details.

Published in #MNRAS: "Multiwavelength morphology and dust emission in low-redshift dwarf galaxies in COSMOS-Web with HST and JWST", Kakkad et al. This is Fig. 2: please visit academic.oup.com/mnras/articl... to read the paper. @royalastrosoc.bsky.social @academic.oup.com

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