TOI-677 b is part of an emerging class of "tidally detached" gas giants (a/Ra. 11) that exhibit large orbital eccentricities and yet low stellar obliquities. Such sources pose a challenge for models of giant planet formation, which must account for the excitation of high eccentricities without large changes in the orbital inclination. In this work, we present a new Rossiter-McLaughlin measurement of the tidally detached warm Jupiter TOI-677 b, obtained using high-precision radial velocity observations with Magellan's Planet Finder Spectrograph (PFS). Combined with previously published observations from the Very Large Telescope's ESPRESSO spectrograph, we derive one of the most precisely constrained sky-projected spin-orbit angle measurements to date for an exoplanet. The combined fit offers a refined set of self-consistent parameters, including a low sky-projected stellar obliquity of l =. 3 2+ 1. 51. 6.. and a moderately high eccentricity of = e 0.460+ 0.0180.019, which further constrain the puzzling architecture of this system. We examine several potential scenarios that may have produced the current TOI-677 orbital configuration, ultimately concluding that TOI-677 b most likely had its eccentricity excited through diskplanet interactions. This system adds to a growing population of aligned warm Jupiters on eccentric orbits around hot (Teff > 6100 K) stars. Unified Astronomy Thesaurus concepts: Planetary theory (1258); Exoplanet tides (497); Exoplanet migration (2205); Planetary dynamics (2173); Exoplanets (498); Hot Jupiters (753); Exoplanet systems ( 484); Star-planet interactions (2177); Planetary alignment (1243); Exoplanet evolution (491); Exoplanet astronomy (486); Exoplanet dynamics (490)

We investigate the group-scale environment of 15 luminous quasars (luminosity L-3000 > 10(46) erg s(-1)) from the Cosmic Ultraviolet Baryon Survey (CUBS) at redshift z approximate to 1. Using the Multi Unit Spectroscopic Explorer integral field spectrograph on the Very Large Telescope, we conduct a deep galaxy redshift survey in the CUBS quasar fields to identify group members and measure the physical properties of individual galaxies and galaxy groups. We find that the CUBS quasars reside in diverse environments. The majority (11 out of 15) of the CUBS quasars reside in overdense environments with typical halo masses exceeding 10(13 )M(circle dot), while the remaining quasars reside in moderate-size galaxy groups. No correlation is observed between overdensity and redshift, black hole (BH) mass, or luminosity. Radio-loud quasars (5 out of 15 CUBS quasars) are more likely to be in overdense environments than their radio-quiet counterparts in the sample, consistent with the mean trends from previous statistical observations and clustering analyses. Nonetheless, we also observe radio-loud quasars in moderate groups and radio-quiet quasars in overdense environments, indicating a large scatter in the connection between radio properties and environment. We find that the most UV luminous quasars might be outliers in the stellar mass-to-halo mass relations or may represent departures from the standard single-epoch BH relations.