Extremely Large Telescope

Abstract:

Abstract We present the architecture, implementation, and on-sky validation of the fully automated acquisition and guiding system (AG) developed for the WEAVE instrument on the William Herschel Telescope. The AG operates in two distinct modes, corresponding to the observing modes of WEAVE. For the large integral field unit (LIFU), an off-axis imaging guider is used, for which we have devised an automatic acquisition method based on pattern recognition of stellar asterisms matched against Gaia predictions. For the multi-object spectrograph (MOS) and the mini-integral field units (mIFU), a multi-fibre guider uses up to eight coherent image guide fibre bundles to derive and apply continuous corrections in azimuth, altitude, and rotation. The system performs complete astrometric calculations, including atmospheric differential refraction and instrument flexure, for each guide frame, enabling accurate target placement and stable closed-loop guiding in all configurations. To support development, commissioning, and operational validation, we have also built a high-fidelity simulation mode that reproduces the behaviour of the telescope control system and of the AG cameras, and we release the standalone camera simulator as open-source software. Using two years of routine WEAVE operations spanning commissioning and early survey phases, we present a statistically robust characterization of AG performance, demonstrating that both modes meet design requirements and are ready for sustained survey operations.

Abstract:

The correlation between optical starlight polarization and polarized thermal dust emission can be used to infer intrinsic dust properties. This correlation is quantified by the ratio R P / p , which has been measured by the Planck Collaboration to be 5.42 ± 0.05 MJy sr −1 at 353 GHz when averaged over large areas of the sky. We investigated this correlation using newly published stellar polarimetric data densely sampling a continuous sky region of about four square degrees at intermediate Galactic latitude. We combined RoboPol optical polarization measurements for 1430 stars with submillimeter data from the Planck satellite at 353 GHz. We performed linear fits between the Planck ( Q s , U s ) and optical ( q v , u v ) Stokes parameters, taking into account the differences in resolution between the two datasets as well as the distribution of clouds along the line of sight. We find in this region of the sky that the R P / p value is 3.67 ± 0.05 MJy sr −1 , indicating a significantly shallower slope than that found previously using different stellar samples. We also find significant differences in the fitted slopes when fitting the Q s – q v and U s – u v data separately. We explore two explanations using mock data: the miscalibration of the polarization angle and the variations in R P / p along the line of sight due to multiple clouds. We show that the former can produce differences in the correlations of Q s – q v and U s – u v , but large miscalibration angles would be needed to reproduce the magnitude of the observed differences. Our simulations favor the interpretation that R P / p differs between the two dominant clouds that overlap on the sky in this region. The difference in R P / p suggests that the two clouds may have distinct dust polarimetric properties. With knowledge from the tomographic decomposition of the stellar polarization, we find that one cloud appears to dominate the correlation of U s – u v , while both clouds contribute to the correlation of the Q s – q v data.

Abstract:

Abstract Supermassive black hole (SMBH) masses can be measured using molecular gas kinematics. Here we present high angular resolution (0.12 arcsec or ≈11 pc) Atacama Large Millimeter/submillimeter Array observations of the 12CO(2–1) line emission of the early-type galaxy NGC 1387. The observations reveal a face-on, regularly-rotating central molecular gas disc with a diameter of ≈18 arcsec (≈1.7 kpc) and a central depression slightly larger than the SMBH sphere of influence. We forward model the CO data cube in a Bayesian framework with the Kinematic Molecular Simulation code, and use Hubble Space Telescope data to constrain the stellar gravitational potential contribution to the molecular gas kinematics. We infer a SMBH mass of $1.10^{+1.71}_{-0.95}[\textrm{stat},3\sigma ]^{+2.45}_{-1.09}[\textrm{sys}]\times 10^8$ M⊙ and a F160W-filter stellar mass-to-light ratio of $0.90^{+0.44}_{-0.35}[\textrm{stat}, 3\sigma ]^{+0.46}_{-0.36}[\textrm{sys}]$ M⊙/L⊙, F160W. This SMBH mass is consistent with the SMBH mass – stellar velocity dispersion relation.