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Official account for Monthly Notices of the Royal Astronomical Society (MNRAS), Geophysical Journal International (GJI) and RAS Techniques and Instruments (RASTI). See also https://academic.oup.com/rasjournals

Projection of the simulated overdensity at ⁠z ≈ 7.5, with distance from the centre of the structure marked in physical kpc and arcseconds. Please see the paper for the full caption.
Map showing the topography, key geological features and the distribution of our MT and GDS stations in central Brazil. Azimuth 125° is a belt of Permo-Triassic and Cretaceous alkaline magmatism (G.M. Gonzaga & L.A. Tompkins 1991; M. Muniswamy 2015; U.G. Cordani et al. 2016). AmC, PBC, SFC and SLC are Amazonian, Paranapanema Block, São Francisco and São Luís cratons, respectively. TBL is the Trans-Brazilian lineament. Inset map shows the location of our current study within South America. The regional geological map is shown in Fig. S1(Supplementary Material).
3D view of the modelled evaporating planetary atmosphere S40 (left) and S40F (right), which have the same stellar wind mass-loss rates, but different stellar XUV fluxes. we show the exoplanet as the black sphere, with total density (⁠⁠rho) displayed in several isosurfaces – these have been cut for z > 0 in the full view panels – and velocity streamlines are coloured by association to an initial planetary outflow (orange) or stellar (blue) wind. the dark blue outer closed isosurface delimits where the gas is made up of mostly planetary material. The insets show a closer view of the planet.
Tectonic setting. AB indicates the GPS profile location; GF: Gardez Fault; KF: Kunar Fault; PF: Panjshir Fault; SF: Sarobi Fault; SGF: Spin Ghar Fault.
False-colour RGB image of The Cliff, illustrating the NIRSpec/IFS FoV. We label a foreground galaxy (ID 24647, at ⁠z_(spec) = 3.05) to the east and a star to the north west. We use publicly available imaging from PRIMER (PID 1837) and MINERVA (PID 7814; A. Muzzin et al. 2025).
The spatial extent of the velocity models chosen for this study. (a) Blue is AKAN (A. Nayak et al. 2020), grey is AKEP (A. Nayak et al. 2020), green is Berg (E.M. Berg et al. 2020), orange is WARD (K.M. Ward & F.-C. Lin 2018), and cyan is YANG (X. Yang & H. Gao 2020). The inverted triangles show the seismic stations (channels BHZ and HHZ) that were active any time from 2019-01-01 to 2024-06-01 for Alaska and western Canada, though we only downloaded data for the broad-band stations. The white line shows the extent of the SPECFEM3D Globe mesh. (b) The mean shear wave velocity at each depth layer that the model is defined at. We have also shown the shear wave velocities used to construct the two FK databases we use in the 1-D moment tensor inversions, SCAK and TACTMOD in magenta. (c) The same as (b), but for P-wave velocity. (WARD does not include P-wave velocity.)
Minimal workflow for reducing OPTICAM data with phoptic. Dashed boxes represent optional, but highly recommended, steps.
Doppler maps of ejecta emitting in [Fe XIV] in SNR 0509, calculated using a rest wavelength of 5308 Å, are shown separately. Left: The red-shifted ejecta, showing lower Doppler velocities along the edges. Right: The blue-shifted component of the ejecta, which also shows lower Doppler velocities in the western region of the remnant, likely linked to a denser ambient medium. H (appearing as the outer shell) is overlaid in magenta to show the full extent of SNR 0509.
Portion of time-series data (2000 s) collected through a turn during AUV Sentry dive 750. (a) Magnetic field in vehicle (XYZ component) reference frame. (b)–(d) Measured, heading corrected and filtered magnetic data in geographic (NED component) reference frame. (e) Vehicle attitude: heading, pitch and roll. Grey shaded area shows turn along survey line.
Monthly average Mount Washington neutron monitor counting rate as a function of time. Rate normalized to 100–2506 in July 1954. The upper panel shows the occurrence and magnitude of FDs with magnitude ≤ 3 per cent as recorded by the Mount Washington neutron monitor [from J. A. Lockwood & W. R. Webber (1984)].
Figure 7.Schematic of an outflow producing double peaked emission lines in the (rotation dominated), inner regions and becomes radially dominated a larger radii producing a blue-shifted absorption profile on the same spectral line. Such dynamic would produce the single line emission with broad absorption shown in Fig. 6.
Schematic diagram of the experimental setup. ⁠P, T⁠, V⁠, R_t and W represent pressure, temperature, ultrasonic wave velocity, resistivity and waveforms, respectively. After T. Liu et al. (2026).
Logarithmic density map of η Car’s nebula. The numerical simulation corresponds to an evolutionary time of t = 161 yr since the Great Eruption of the 1840s. The colour bar on the right is given in units of g cm⁠^(-3), and the axes of the computational domain are in units of cm. A physical description of the figure is provided in the text.
Example of dynamic topography filtering for Model 5A. The full model dynamic topography field is sampled using the observed residual topography data points (M.J. Hoggard et al. 2016, 2017; M.C. Holdt et al. 2022; S.N. Stephenson et al. 2024) to generate synthetic data. A spherical harmonic expansion is then fitted to both observed and synthetic data following M.J. Hoggard et al. (2016). This results in global dynamic topography fields that are directly comparable.
Figure 2: please see the paper for the full caption.
Conceptual schematic of mid-mantle stratification and the ‘density paradox’. This synthesis illustrates the interpretation of the ≈ 800 km discontinuity as a laterally extensive layer of stagnant, eclogitized oceanic crust accumulated near a viscosity barrier at 1000 km depth, thermally equilibrated with the ambient mantle such that chemical and thermal buoyancy approximately cancel. Subducting slab delivers basaltic crust which transforms to eclogite and accumulates as marble-cake remnants.
Images of the clast containing sarcopside (CS) in Martian meteorite Northwest Africa (NWA) 7533. (a) BSE image of clast CS outlined by a dotted line. (b–e) X-ray images of clast CS. (f) BSE image of a sarcopside grain cut through by an impact fracture. Src = sarcopside, Ap = apatite, Pl = plagioclase, Afs = alkali feldspar.
Simplified structural map of the western Alps. Dashed lines represent the directions of the cross-sections: A (Fig. C1) and B (Fig. 4). The study area is represented by the black solid rectangle of the right panel.
Geometrical model of a parabolic reflector antenna showing the segmented surface mesh and the primary feed support structure. The coordinate systems (X, Y, and Z axes) indicate the global and local phase centres for the optical analysis.
The total current (a –d), magnetic field (e–h) and O^+ density (i–l) distributions for the four cases presented in Fig. 5. The plots are sliced in the XY plane at Z = 0 in the VSO coordinate system. Black arrows indicate the directions of the current (a–d), magnetic field (e–h) and ion flow (i–l).
Map highlighting the seismicity and seismic networks of the study region. The area within the brown box indicates the GK region of the Himalayan arc. The seismicity includes earthquakes from 2010 to 2022 with magnitude ranging from 2–5.6 (ISC catalogue). The size and the colour contrast of the circles represent the magnitude and focal depth of the events, respectively. Red and green inverted triangles indicate the station locations of the Tehri Network (TN) and National Center of Seismology, India (IN) networks, respectively. The figure also marks the locations of some major cities (yellow rectangles) and significant faults and thrusts are marked by the blue lines (MFT: Main Frontal Thrust, MBT: Main Boundary Thrust, MT: Munsiari Thrust (MCT-I), VT: Vaikrita Thrust (MCT-II), SAT: South Almora Thrust, NAT: North Almora Thrust, RT: Ramgarh Thrust) within the arc (S. Dasgupta et al. 2000).
The chi-square versus box size plots for nine different EBs are shown. The top row (a, b, c panels) displays three different DEBs with Kepler IDs (KIC): 1026032, 1873513, and 2166200, respectively. The middle row (d, e, f panels) displays three different SDEBs with KIC: 2577756, 5560831, and 5962514, respectively. Lastly, the bottom row (g, h, i panels) displayed three CEBs systems with KIC: 1433410, 2012362, and 2159783, respectively.
Descriptive maps of the Corkscrew Galaxy. Please see the paper for the full caption.
Dynamic rupture modelling domain: (a) The Hellenic Arc megathrust by A. Scala et al. (2020) and R. Basili et al. (2021) used in this study. The dark red color indicates deeper fault depths. Note that the tsunami modelling computational domain extends beyond the dynamic rupture modelling domain (Figs. 3 and 4). (b) Zoom into the Hellenic Arc region with 5.4 earthquakes (red stars) related to the Hellenic Arc subduction or surrounding tectonics (R. Mallet 1853; J. Antonopoulos 1973; G. Papadopoulos 2000; E. Guidoboni et al. 2005; G.A. Papadopoulos et al. 2010; G.M. Bocchini et al. 2020; A. Cirella et al. 2020; K.H. Coban & N. Sayil 2020). Plate boundaries are indicated by black lines (P. Bird 2003), and the convergent subduction margin is marked by a black saw-toothed line.
Schematic of the iBridge method as developed for this application. The system is divided into two parts: a star cluster and a planetary system, with one star being common for both parts. The acceleration caused by the cluster on the planetary system is calculated and used to update the velocities of the bodies in the planetary system. Then the planets and central star are evolved, and the state of the central star in the cluster is updated with that of the planetary system. Afterwards, the cluster is evolved and the state of the centre of mass of the planetary system is updated using the latest cluster information. This process is repeated at every step.
The magnitude of spatial separation between a pair of CR trajectories are shown as a function of time. Please see the paper for the full caption.
Radio luminosity (1.4 GHz) vs X-ray luminosity (2–10 keV) for the combined Boötes and COSMOS sample, where a detection in both radio and X-ray is required to be displayed. Please see the paper for the full caption.
From top to bottom: rest-frame FUV, NUV and optical PYSERSIC fits for a galaxy in our sample, probed by the NIRCam filters F090W, F200W, and F356W at ⁠z ≈ 5.2. In each band, the galaxy (left) is modelled with a PSF (FWHM shown with the red circle)-convolved one-component Sérsic profile (middle), and contaminants are masked during the fitting. The residual images (right) show that a single Sérsic profile does not fully capture the galaxy’s surface brightness, most likely due to the excess flux in the top region of this system. However, the overall size (effective radius) of the galaxy is well measured by the model.
This year's winner: Daisaburo Kido from the University of Tokyo.
Figure 2 from the winning paper. Please see the paper for the full caption.
Four examples of the comparisons of the FFI and the SAP. In each sub-figure, the top panel is the FFI photometry, and the bottom panel is the concatenated SAP LC. In the FFI photometry, the green squares, blue triangles, black circles, and red diamonds indicate the four quarters of an year, the same with those figures of Montet et al. (2017).
Occurrence rates of planet candidates around TESS-SPOC FGK main-sequence stars. Each cell displays the average occurrence as a percentage (number of planets per 100 stars), along with the corresponding uncertainties (the difference between the 16th and 84th percentiles and the median). For clarity, text in cells with an occurrence rate below 0.01 per cent is displayed in white. The colour of each cell encodes the occurrence rate density, ⁠, per 100 stars. The logarithmic colour scale is truncated at 0.5 to enhance visibility. We also provide an online interactive plot that allows users to easily select any region and obtain its total occurrence rate.
Transit light curves of NGTS-7Ab. Top: Phase-folded NGTS light curve (as in Fig. 1) with the best-fitting model overlaid in red. Middle: Primary transit light curve from SAAO in I band, with the best-fitting model in green. Bottom: Primary transit light curve from EulerCam in V band, with the best-fitting model in magenta. Residuals for each fit are shown underneath each plot.
Left: Host galaxy stellar mass versus galaxy age for the sample used by S25. Galaxy ages are taken from C. Chung et al. (2025) and are strongly correlated with host galaxy stellar mass. Centre: Hubble residual before bias correction and mass standardization, versus galaxy age. Hubble residuals are taken from the Pantheon + analysis. We recover a somewhat smaller slope than C. Chung et al. (2025), and with lower significance; Right: Hubble residuals after a bias correction and standardization for stellar mass. The relationship between Hubble residual and host galaxy age is smaller, and not significant.
The long term X-ray light curve of GRB 250702B compared to all 177 1 traces from our MCMC fit using a WD-IMBH model (blue solid lines). The vertical grey lines mark the times of the Fermi triggers. Note the first plotted WXT point is excluded from our fitting.
Flowchart outlining the methodology used in our work. The blue box (upper left) describes the BPASS framework and the steps taken to generate simple stellar population models (Section 2). Different IMF and stellar spectral libraries are applied during the population and spectral synthesis steps, respectively, to generate models with varying underlying assumptions. The yellow box (lower left) represents our simulated galaxy sample from the EAGLE project and the data acquired to generate mock observations (Section 3.1). This data is combined with the default BPASS v2.2.1 framework to construct mock galaxy observations in the orange box (centre, Section 3.2). Comparison between the mock galaxy observations and all BPASS templates is performed using the BAGPIPES SED fitting software, highlighted in the green box (upper right, Section 3.3). The process from simple to composite stellar populations is outlined with the assumptions being varied highlighted. This generates the inferred galaxy properties in the purple box (lower right).
Schematic of a nested sampling run. Each dead point defines an iso-likelihood contour in the parameter space (left), which then encloses a certain fractional prior volume (right). As the points compress towards the peak of the likelihood, they enclose smaller and smaller fractional volumes.
Top panel: Sky density of the ≈ 33,000 known white dwarfs before Gaia DR2 (Gentile Fusillo et al. 2015b; Kilkenny et al. 2015; Kepler et al. 2016b; Dufour et al. 2017; Gentile Fusillo et al. 2017; Hollands et al. 2017). Bottom panel: Sky density of Gaia DR2 white dwarf candidates with P_(WD) > 0.75 from the catalogue presented in this article.
C IV emission space for the SDSS-IV quasar sample presented in A. L. Rankine et al. (2020, 2021) (grey) and the subset of this sample that was part of the CORE SDSS quasar targeting programmes (blue; see Section 3). The contours encircle 11.8, 39.3, 67.5 and 86.4 per cent of the objects in each sample. The marginalized distributions have been renormalized. The C IV distance reference line is the black curve, with the direction of increasing C IV distance indicated. The optical selection that constitutes the CORE sample does not bias the SDSS-IV comparison sample towards a particular part of the parameter space. The X-ray selected SDSS-V sample (orange; discussed in Section 3) is shifted towards lower blueshifts and larger C IV EWs but spectra with significant blueshifts are still apparent in the sample.
Bi′K image of cluster field CVB6. Please visit the paper for the full caption.
POL-2 magnetic field vectors (grey) and SMA magnetic field vectors (red), overlaid on an HST 658 nm image of OH231.8. For the SMA data, the positions of each vector are shown as dots, and the average magnetic field direction is shown as a vector. The most extreme position angles of the bullets in the explosive outflow (the ‘outflow cone angles’) are marked with dotted magenta lines. The JCMT and SMA beams are shown as an open grey circle and a filled red ellipse, respectively.
Top: [Mg IV] flux map showing the annulus considered and directionality of the angles. The colour scaling has been cut to three times below the maximum value to highlight the edges of the ionization cone. Bottom: average flux as a function of angle throughout the annulus for the [Mg IV] flux with the cone edge regions shaded and the positive peak identified as the red circle, and the negative peak identified as the orange circle. The dashed and solid black lines enclose the angular regions where we expect the cone edge to lie on both plots, with the dashed showing the inside of the edge and solid showing the outer extent of the edge. The two unmarked peaks beyond ±100° correspond to the edges of the eastern cone which is obscured by the disc.
Near-IR to millimetre images of 6 x 6 arcsec size centred on AC-2168. Please see the paper for the full caption.
Localizing SN 2023ixf in the pre-explosion HST/ACS image using Keck/NIRC2 adaptive optics imaging. The left panel shows a contrast-enhanced cutout of the post-explosion Keck/NIRC2 Ks-band image (middle panel, in north-up, east-left orientation), centred at the heavily saturated SN. The SN location is precisely determined by fitting the positions of diffraction spikes (data points with error bars) using a simple linear pattern (lines). The middle panel shows the astrometric reference stars (circles) detected in the Keck/NIRC2 image, while the right panel shows the same field of the three-band combined HST/ACS image. Fitting an astrometric solution with these stars, the SN can be localized with a total uncertainty of 19.5 mas in the HST/ACS image. Arrows indicate the residual error of the best-fitting astrometric solution, which dominates the error budget.
Properties of the flow in the forced convection regime. Please see the paper for the full caption.
Radial velocities and metallicities in Sextans. Please see the paper for the full caption.
Top: distribution of galaxies in our toy model library across the E(B-V) – A_V plane, colour coded by their projected dust surface mass density. Bottom: median properties of toy models located in each region of the E(B-V) – A_V diagram. Parameters are sorted based on their impact on the effective total-over-selective attenuation, R_V (see the text for details). Regions 1, 2, and 3 contain 31.5 per cent, 25.5 per cent, and 43.0 per cent of the toy models within our SKIRT library, respectively.
Illustration of ⁠ΔV⋆ − g. Please see the paper for the full caption.
Example SED fits to NIRCam imaging for candidates in our sample, along with posterior probability distributions for the redshift and sSFR parameters. Please see the paper for the full caption.
Comparison of the inclination angle and apparent speed distributions of XRB and AGN jets. Please see the paper for the full caption.
Unfolded XMM–Newton ObsIDs 0724060701 (left) and 0724060801 (middle) and Chandra ObsID 16276 (right) spectra fit with the single-component model tbabs(tbabs(powerlaw)) (top row) and the two-component model tbabs(tbabs(diskbb + diskbb)) (bottom row). In each panel, the best-fitting total model is shown by the solid line and the residuals are shown in the lower segment. In the bottom row, the dashed and dotted lines represent two diskbb model components. Note the XMM–Newton panels show only the data and residuals from the EPIC-PN detector, but the plotted models were obtained through simultaneous spectral fitting to the data from all three EPIC detectors.
The field of view of Chandra ObsID 16 276 in which our PULX candidate, 4XMM J132542.2–425943, is identifiable as an X-ray point source. The PULX candidate lies close to the axis of the jet emitted from the active nucleus of Centaurus A (South-West of 4XMM J132542.2–425943 in this image, circle).
Measurement of the amplitude of the clustering bias of GW sources (⁠⁠B) by cross-correlating different pairs of GWs detectors and radio surveys. Please see the paper for the full caption.
Composite RGB image of MACS0647-JD1 obtained by super- posing F115W, F200W and F444W NIRCam photometry images. Please see the paper for the full caption.
2D histogram of the effective radius versus photometric stellar mass, colour-coded by the gas-phase metallicity for the MaNGA survey. Please see the paper for the full caption.
Disc modelling and subtraction for NGC 5728. Please see the paper for the full caption.
The first four principal components of the 3.3 μm PAH for NGC 7582. Please see the paper for the full caption.
Density contours for the (U, V) plane of 13 518 objects from the GCS smoothed to a scale of ∼12 km s^(−1) via a stationary wavelet transform. The five major structures are identified by red points: 1. Hercules, 2. Hyades, 3. Pleiades, 4. Coma Berenice, 5. Sirius.
CMD of our Solar neighbourhood sample. The colour shows the number density of sources. We exclude bins with N < 5 stars in them.
Comparison of our refined PECs of NiH to those from Havalyova et al. (2021). Darker shades of colours correspond to the curves from Havalyova et al. (2021). Lighter shades of colours correspond to our refined curves. The horizontal dashed line shows where the first of higher lying electronic states with allowed transitions start according to Zou & Liu (2007). The right display zooms in on the spectroscopically important region.