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One of the most remarkable properties of massive stars is that almost all of them are found in binaries or higher-order multiple systems. Observations that cover the full companion mass ratio and separation regime are essential to constrain massive star and binary formation theories. We used VLT/SPHERE to characterise the multiplicity properties of 20 OB stars in the active star-forming region Sco OB1. We simultaneously observed with the IFS and IRDIS instruments, obtaining high-contrast imaging observations that cover a field of view of 1\".73 x 1\".73 in YJH bands and 11\" x 12\".5 in \\(K_1\\) and \\(K_2\\) bands, respectively, corresponding to a separation range between \\(\\)200 and 9000 AU. The observations reach contrast magnitudes down to \\( K_1 13\\), allowing us to detect companions at the stellar-substellar boundary. In total, we detect 789 sources, most of which are likely background or foreground objects. We obtain SPHERE companion fractions of \\(2.3 0.4\\) and \\(4.2 0.8\\) for O- and B-type stars, respectively. Including all previously detected companions, we find a total multiplicity fraction of \\(0.890.07\\) for our sample in the range of \\(\\)0-12000 AU. In conclusion, SPHERE explores an as of yet uncharted territory of companions around massive stars, which is crucial to ultimately improve our understanding of massive star and binary formation.

The formation of massive stars remains one of the most intriguing questions in astrophysics today. The main limitations result from the difficulty to obtain direct observational constraints on the formation process itself. In this context, the Carina High-contrast Imaging Project of massive Stars (CHIPS) aims to observe all 80+ O stars in the Carina nebula using the new VLT 2nd-generation extreme-AO instrument SPHERE. This instrument offers unprecedented imaging contrast allowing us to detect the faintest companions around massive stars. These novel observational constraints will help to discriminate between the different formation scenarios by comparing their predictions for companion statistics and properties.

Most massive stars belong to multiple systems, yet the formation process leading to such high multiplicity remains insufficiently understood. To help constrain the different formation scenarios that exist, insights on the low-mass end of the companion mass function of such stars is crucial. However, this is a challenging endeavour as (sub-)solar mass companions at angular separations (\\(\\rho\\)) below 1\" (corresponding to 1000-3000 au in nearby young open clusters and OB associations) are difficult to detect due to the large brightness contrast with the central star. With the Carina High-contrast Imaging Project of massive Stars (CHIPS), we aim to obtain statistically significant constraints on the presence and properties of low-mass companions around massive stars at a previously unreachable observing window (\\(\\Delta \\mathrm{mag} \\gtrsim 10\\) at \\(\\rho \\lesssim\\) 1\"). In this second paper in the series, we focus on the Trumpler 14 cluster, which harbours some of the youngest and most massive O-type stars in the Milky Way. We obtained VLT-SPHERE observations of seven O-type objects in Trumpler 14 using the IRDIFS_EXT mode. These allow us to search for companions at separations larger than 0.\"15 (approx. 360 au) and down to magnitude contrast \\(>10 \\mathrm{mag}\\) in the near-infrared. We used angular and spectral differential imaging along with PSF fitting to detect sources and measure their flux relative to that of the central object. We detected 211 sources with near-infrared magnitude contrast in the range of 2 to 12. The closest companion, at only 0.\"26, is characterised as a 1.4M\\(_{\\odot}\\) stars with an age of 0.6Myr, in excellent agreement with previous age estimates for Tr 14. The mass function peaks at about 0.4M\\(_{\\odot}\\) and presents a dearth of stars in the 0.5 to 0.8M\\(_{\\odot}\\) mass range compared to previous estimates of the initial mass function in Tr 14.