α-element enhancements in the ISM of the LMC and SMC: Evidence of recent star formation

¹ European Southern Observatory, Karl-Schwarzschild Str. 2, 85748 Garching bei München, Germany
e-mail: adecia@eso.org
² Department of Astronomy, University of Geneva, Chemin Pegasi 51, 1290 Versoix, Switzerland
³ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁴ Franco-Chilean Laboratory for Astronomy, IRL 3386, CNRS and Dep. de Astonomía, Universidad de Chile, Santiago, Chile
⁵ Institut d’Astrophysique de Paris, UMR 7095, CNRS and Sorbonne Université, 98bis bd Arago, 75014 Paris, France
⁶ Institute of Astronomy, Kharkiv National University, 4 Svobody Sq., Kharkiv 61022, Ukraine
⁷ AURA for ESA, 3700 San Martin Drive, Space Telescope Science Institute, Baltimore, MD 21218, USA
⁸ Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA
⁹ European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Vitacura, Santiago, Chile
¹⁰ Cosmic Dawn Center (DAWN), Denmark
¹¹ DTU-Space, National Space Institute, Technical University of Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark
¹² Observatoire de Lyon, 9 avenue Charles André, 69561 St. Genis Laval, France
¹³ Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon (CRAL) UMR5574, 69230 Saint-Genis-Laval, France

Received: 6 April 2023
Accepted: 20 January 2024

Abstract

Context. Important questions regarding the chemical composition of the neutral interstellar medium (ISM) in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are still open. It is usually assumed that their metallicity is uniform and equal to that measured in hot stars and H II regions, but direct measurements of the neutral ISM metallicity had not been performed until now. Deriving the metallicity from the observed metal abundances is not straightforward because the abundances depend on the depletion of metals into dust and on nucleosynthesis effects such as α-element enhancement.

Aims. Our aim is to measure the metallicity of the neutral ISM in the LMC and SMC, dust depletion, and any nucleosynthesis effects.

Methods. We collected literature column densities of Ti II, Ni II, Cr II, Fe II, Mn II, Si II, Cu II, Mg II, S II, P II, Zn II, and O I in the neutral ISM towards 32 hot stars in the LMC and 22 in the SMC. We determined dust depletion from the relative abundances of different metals because they deplete with different strengths. This includes a ‘golden sample’ of sightlines where Ti and other α-elements are available. We fit linear relations to the observed abundance patterns so that the slopes determined the strengths of dust depletion and the normalizations determined the metallicities. We investigated α-element enhancements in the gas from the deviations from the linear fits and compared them with stars.

Results. In our golden sample we find α-element enhancement in the neutral ISM in most systems, on average 0.26 dex (0.35 dex) for the LMC (SMC), and an Mn underabundance in the SMC (on average −0.35 dex). Measurements of Mn II are not available for the LMC. These are higher than for stars at similar metallicities. We find total neutral ISM metallicities that are mostly consistent with hot star metallicity values, on average [M/H]_tot = −0.33 (−0.83), with standard deviations of 0.30 (0.30), in the LMC (the SMC). In six systems, however, we find significantly lower metallicities, 2 out of 32 in the LMC (with ~16% solar) and 4 out of 22 in the SMC (3 and 10% solar), two of which are in the outskirts of the SMC near the Magellanic Bridge, a region known for having a lower metallicity.

Conclusions. The observed a-element enhancements and Mn underabundance are likely due to bursts of star formation, more recently than ~1 Gyr ago, that enriched the ISM from core-collapse supernovae. With the exception of lines of sight towards the Magellanic Bridge, the neutral gas in the LMC and SMC appears fairly well mixed in terms of metallicity.