Context. We report the discovery of TOI 263.01 (TIC 120916706), a transiting substellar object (R = 0.87 R Jup ) orbiting a faint M3.5 V dwarf (V = 18.97) on a 0.56 d orbit.Aims. We set out to determine the nature of the TESS planet candidate TOI 263.01 using ground-based multicolour transit photometry. The host star is faint, which makes RV confirmation challenging, but the large transit depth makes the candidate suitable for validation through multicolour photometry.Methods. Our analysis combines three transits observed simultaneously in r , i , and z s bands using the MuSCAT2 multicolour imager, three LCOGT-observed transit light curves in g , r , and i bands, a TESS light curve from Sector 3, and a low-resolution spectrum for stellar characterisation observed with the ALFOSC spectrograph. We model the light curves with PyTransit using a transit model that includes a physics-based light contamination component that allows us to estimate the contamination from unresolved sources from the multicolour photometry. This allows us to derive the true planet-star radius ratio marginalised over the contamination allowed by the photometry, and, combined with the stellar radius, gives us a reliable estimate of the object's absolute radius. Results. The ground-based photometry strongly excludes contamination from unresolved sources with a significant colour difference to TOI 263. Further, contamination from sources of same stellar type as the host is constrained to levels where the true radius ratio posterior has a median of 0.217 and a 99 percentile of 0.286. The median and maximum radius ratios correspond to absolute planet radii of 0.87 and 1.41 R Jup , respectively, which confirms the substellar nature of the planet candidate. The object is either a giant planet or a brown dwarf (BD) located deep inside the socalled "brown dwarf desert". Both possibilities offer a challenge to current planet/BD formation models and makes TOI 263.01 an object deserving of in-depth follow-up studies.

The present study evaluates the treatment acceptability and preference for behavioral interventions for feeding problems with parents of children with Autism Spectrum Disorder and other developmental disabilities. The impact of behavioral severity on acceptability and preference was also evaluated by comparing results of parents who responded with respect to a vignette of a child with food refusal with those who responded to a vignette of a child with food selectivity. Overall, parents rated differential reinforcement of alternative behavior as the most preferred and most acceptable strategy across both food selectivity and food refusal groups. Escape extinction was the least acceptable and least preferred across both groups, and the severity of the behavior had no impact on acceptability or preference scores. Implications for future research on the social validity of feeding interventions are provided.

We report the analysis of additional multiband photometry and spectroscopy and new adaptive optics (AO) imaging of the nearby planetary microlensing event TCPJ05074264+2447555 (Kojima-1), which was discovered toward the Galactic anticenter in 2017 (Nucita et al.). We confirm the planetary nature of the light-curve anomaly around the peak while finding no additional planetary feature in this event. We also confirm the presence of apparent blending flux and the absence of significant parallax signal reported in the literature. The AO image reveals no contaminating sources, making it most likely that the blending flux comes from the lens star. The measured multiband lens flux, combined with a constraint from the microlensing model, allows us to narrow down the previously unresolved mass and distance of the lens system. We find that the primary lens is a dwarf on the K/M boundary (0.581 ± 0.033 M e) located at 505±47 pc, and the companion (Kojima-1Lb) is a Neptune-mass planet (20.0 ± 2.0 M ⊕) with a semimajor axis of-+ 1.08 0.18 0.62 au. This orbit is a few times smaller than those of typical microlensing planets and is comparable to the snow-line location at young ages. We calculate that the a priori