Large and small-scale structure of the Intermediate and High Velocity Clouds towards the LMC and SMC

TL;DR

This study uses CaII K and NaI D absorption spectroscopy of stars in the Magellanic Clouds to explore the detailed structure and composition of foreground Intermediate and High Velocity Clouds on various spatial scales.

Contribution

It provides extensive observational data on the small- and large-scale structure of I/HVCs, revealing significant variations in absorption features and ratios, and offers insights into their composition and physical conditions.

Findings

CaII K equivalent width varies by factors >10 over 20 arcsec scales.

No molecular gas detected at high velocities, but molecular absorption present at LMC velocities.

CaII/NaI ratio varies from -0.45 to +1.5 dex, indicating dust or ionisation effects.

Abstract

We employ CaII K and NaI D interstellar absorption-line spectroscopy of early-type stars in the Large and Small Magellanic Clouds to investigate the large- and small-scale structure in foreground Intermediate and High Velocity Clouds (I/HVCs). These data include FLAMES-GIRAFFE CaII K observations of 403 stars in four open clusters, plus FEROS or UVES spectra of 156 stars in the LMC and SMC. The FLAMES observations are amongst the most extensive probes to date of CaII structures on 20 arcsec scales From the FLAMES data within a 0.5 degree field-of-view, the CaII K equivalent width in the I/HVC components towards three clusters varies by factors of >10. There are no detections of molecular gas in absorption at intermediate or high velocities, although molecular absorption is present at LMC and Galactic velocities towards some sightlines. The sightlines show variations in EW exceeding a factor 7 in CH+ towards NGC 1761 over scales of less than 10 arcminutes. The FEROS/UVES data show CaII K I/HVC absorption in $\sim$60 per cent of sightlines. No NaI D is found at non-Magellanic HVC velocities aside from a tentative detection towards the star LHA 120-S 93. The range in the CaII/NaI ratio in I/HVCs is from -0.45 to +1.5 dex, similar to previous measurements for I/HVCs. In ten sightlines we find CaII/OI ratios in I/HVC gas ranging from 0.2 to 1.5 dex below the solar value, indicating either dust or ionisation effects. In nine sightlines I/HVC gas is detected in both HI and CaII, and shows similar CaII/HI ratios to typical I/HVCs, and similar velocities, implying that in these sightlines the two elements form part of the same structure.