2025

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Left: stacked 42 epoch total intensity (contours) and linear polarization (color) of the VLBA imacge at 0.8mas resolution of the z=0.6 neutrino blazar PKS1424+340. The position angle of the electric vectors are shown as line segments. Right: the magnetic field direction in a linear integral convolution projection (Kovalev et al. 2025, A&A 700, L12).

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Upper limits (95% confidence) on the number density of FFOs for different mass ranges in the vicinity of 10 of the longest timed pulsars in the NANOgrav dataset. The combined upper limits on the FFO number density from all 68 pulsars are also shown with black squares (Dey et al. 2025 arXiv:2507.19475).

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Two examples of offset AGN identified through cross correlation of the VLASS and the SDSS. In these cases, the radio AGN has an optical counterpart. Color frames are SDSS g+r+I and the grayscale image is the VLASS. The scale bars are 10’’ (Barrows & Comerford 2025, arXiv:2509.09768).

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Left: VLA images of the off-nuclear TDE at z = 0.045 before and after the advent of the radio source. Right: Radio light curves showing the double peak and the unprecedented fast temporal evolution (Margutti et al. ApJ 992, L18).

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ALMA images of Callisto after subtracting mean model disk emission (in K), at 0.09’’ to 0.24’’ resolution. The images are scaled such that the horizontal and vertical axes span -3500 km to +3500 km (Cordiner et al. arXiv:2508.05925).

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ALMA emission maps of H2O and HDO in comet 12P/Pons-Brooks at 1” resolution. Insets show the spectra (Camarca et al. arXiv:2507.12671).

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Left: Hα image of solar prominence taken with Cerro Tololo optical telescope on December17, 2015, with PR boundaries (red contours). Right: Concurrent ALMA Band 3 total power image. The blue circle is the ALMA Band 3 single dish beam size (Matkovic et al. arXiv:2509.08605).

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Green Bank Ammonia Survey in the Perseus molecular cloud at 32’’ resolution (Black contours, Pineda et al. arXiv:2510.0607). The color scale shows N(H2) derived from Herschel.

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Left: VLA image of the region around the massive protostar IRAS 18162–2048 at 5 GHz, 6” resolution (Cheriyan et al. 2025 ApJ 988, L9). Right: color scale now shows the stokes V circular polarization

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ALMA observations of linearly polarized emission from aligned dust grains at 230 GHz in protostellar cores and clumps in NGC6334, down to 0.4” resolution (Zhang et al. 2025, ApJ 992, 103).

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The seven-ring PAH Cyanocoronene structure and GBT GOTHAM (black) + laboratory (orange) spectra. This is the largest PAH discovered outside the solar system to date (Wenzel et al. 2025 ApJ 984, L36).

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ALMA [OIII] image of a z = 11.1 galaxy pair at 0.8” resolution at 280 GHz (red contours), plus the JWST near-IR images (Witstok et al. 2025, arXiv:2507.22888).

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ALMA + JWST images of the stars and [CII] 158um line emission from a z = 7.9 merging galaxy cluster (Fudamoto et al. arXiv:2510.11770), elucidating the details of massive galaxy formation in the early Universe.

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Left: ALMA observations of the dust continuum and [CII] 158 um emission from a z = 5.85 massive galaxy pair at 70mas resolution (contours), plus the JWST near-IR images (Akins et al. arXiv:2508.06607). Right: the velocity fields of the galaxies measured with the [CII] line, plus best-fit rotation curves.

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Left: Chandra image of the X-ray emitting hot gas plus the HST image of the stars in a z = 0.5 brightest cluster galaxy and cooling flow cluster. Center: the JVLA L band image at 1” resolution, and the VLBA 5 GHz image at 1.4mas x 4.3mas resolution. Right: the HST image of the stars and the JVLA image at 1.4 GHz of the parent galaxy (Ubertosi et al. 2025, ApJ 989, 128).

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Left: ALMA image CO 2-1 velocity field at 75mas (7pc) resolution of the barred lenticular galaxy NGC1574, which hosts a supermassive black hole. Center: the velocity field along the major axis, plus the best fit model including a SMBH. Right: separating the mass contributions from the galaxy and the SMBH, indicating a black hole mass of 6.2x107 M⊙ (Zhang et al. arXiv:2507.10662).

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