Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II. Spectroscopic and Environmental Analysis of Thorne–Żytkow Object and Super-AGB Star Candidates

• Published in: The Astrophysical journal 2023-01, Vol.943 (1), p.18
• Main Authors: O‘Grady, Anna J. G., Drout, Maria R., Gaensler, B. M., Kochanek, C. S., Neugent, Kathryn F., Doherty, Carolyn L., Speagle, Joshua S., Shappee, B. J., Rauch, Michael, Götberg, Ylva, Ludwig, Bethany, Thompson, Todd A.
• Format: Article
• Language: English
• Subjects: Astrophysics; Asymptotic giant branch stars; Asymptotic properties; Chemically peculiar stars; Heavy elements; Kinematics; Lithium; Lithium stars; Magellanic Clouds; Massive stars; Neutron stars; Nuclear fusion; Peculiar stars; Red giant stars; Spectroscopy; Star & galaxy formation; Star formation; Stars & galaxies; Stellar evolution; Stellar kinematics; Stellar populations; Supergiant stars; Supernovae; Variable stars
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aca655

In previous work, we identified a population of 38 cool and luminous variable stars in the Magellanic Clouds and examined 11 in detail in order to classify them as either Thorne–Żytkow objects (TŻOs; red supergiants with a neutron star cores) or super-asymptotic giant branch (sAGB) stars (the most massive stars that will not undergo core collapse). This population includes HV 2112, a peculiar star previously considered in other works to be either a TŻO or high-mass asymptotic giant branch (AGB) star. Here we continue this investigation, using the kinematic and radio environments and local star formation history of these stars to place constraints on the age of the progenitor systems and the presence of past supernovae. These stars are not associated with regions of recent star formation, and we find no evidence of past supernovae at their locations. Finally, we also assess the presence of heavy elements and lithium in their spectra compared to red supergiants. We find strong absorption in Li and s-process elements compared to RSGs in most of the sample, consistent with sAGB nucleosynthesis, while HV 2112 shows additional strong lines associated with TŻO nucleosynthesis. Coupled with our previous mass estimates, the results are consistent with the stars being massive (∼4–6.5 M ⊙ ) or sAGB (∼6.5–12 M ⊙ ) stars in the thermally pulsing phase, providing crucial observations of the transition between low- and high-mass stellar populations. HV 2112 is more ambiguous; it could either be a maximally massive sAGB star, or a TŻO if the minimum mass for stability extends down to ≲13 M ⊙ .