We present results from a dual narrowband imaging survey targeting the CL1604 supercluster at z = 0.9 using the Subaru Telescope. By combining the NB921 filter on Hyper Suprime-Cam and the NB1244 filter on SWIMS, we can detect redshifted Hα and Hβ emission lines from the supercluster. This unique technique allows us to measure both star formation

Context. Free-floating planetary-mass objects (FFPs) have been detected through direct imaging in several young, nearby star-forming regions. The properties of circumstellar disks around these objects may provide a valuable probe into their origin but are currently limited by the small sample sizes explored. Aims. We aim to perform a statistical

Gamma-ray bursts (GRBs), particularly those detected by wide-field instruments such as the Fermi/GBM, pose challenges for optical follow-up because of their large initial localization regions, leaving many GRBs without identified afterglows. The Gravitational-wave Optical Transient Observer (GOTO), with its wide field of view, dual-site coverage

The Deep Extragalactic VIsible Legacy Survey (DEVILS) is a deep, high-completeness multiwavelength survey based around spectroscopic observations using the Anglo-Australian Telescope's AAOmega spectrograph. The survey covers $\sim 4.5$ deg $^{2}$ over three extragalactic fields to Y $_{\mathrm{ AB}}< 21.2$ mag and probes sources at $0< z< 1.2$

We present a cosmological analysis of the third-order aperture mass statistic using Dark Energy Survey Year 3 (DES Y3) data. We perform a complete tomographic measurement of the three-point correlation function of the Y3 weak lensing shape catalog with the four fiducial source redshift bins. Building upon our companion methodology paper, we apply a

We measure galaxy sizes from 2 < z < 10 using COSMOS-Web, the largest-area JWST imaging survey to date, covering ∼0.54 deg 2. We analyze the rest-frame optical (∼5000 Å) size evolution and its scaling relation with stellar mass ( R e ∝ M * α ) for star-forming and quiescent galaxies. For star-forming galaxies, the slope α remains approximately 0.20