Yang et al. 2020: Evolved Massive Stars at Low-metallicity II. Red Supergiant Stars in the Small Magellanic Cloud

Evolved Massive Stars at Low-metallicity II. Red Supergiant Stars in the Small Magellanic Cloud

Ming Yang, Alceste Z. Bonanos, Bi-Wei Jiang, Jian Gao, Panagiotis Gavras, Grigoris Maravelias, Shu Wang, Xiao-Dian Chen, Frank Tramper, Yi Ren, Zoi T. Spetsieri, Meng-Yao Xue


We present the most comprehensive RSG sample for the SMC up to now, including 1,239 RSG candidates. The initial sample is derived based on a source catalog for the SMC with conservative ranking. Additional spectroscopic RSGs are retrieved from the literature, as well as RSG candidates selected from the inspection of CMDs. We estimate that there are in total ∼ 1,800 or more RSGs in the SMC. We purify the sample by studying the infrared CMDs and the variability of the objects, though there is still an ambiguity between AGBs and RSGs. There are much less RSGs candidates (∼4%) showing PAH emission features compared to the Milky Way and LMC (∼15%). The MIR variability of RSG sample increases with luminosity. We separate the RSG sample into two subsamples (“risky” and “safe”) and identify one M5e AGB star in the “risky” subsample. Most of the targets with large variability are also the bright ones with large MLR. Some targets show excessive dust emission, which may be related to previous episodic mass loss events. We also roughly estimate the total gas and dust budget produced by entire RSG population as ∼1.9(+2.4/−1.1)×10<sup>−6</sup> M⊙/yr in the most conservative case. Based on the MIST models, we derive a linear relation between Teff and observed J−KS color with reddening correction for the RSG sample. By using a constant bolometric correction and this relation, the Geneva evolutionary model is compared with our RSG sample, showing a good agreement and a lower initial mass limit of ∼7 M⊙ for the RSG population. Finally, we compare the RSG sample in the SMC and the LMC. Despite the incompleteness of LMC sample in the faint end, the result indicates that the LMC sample always shows redder color (except for the IRAC1−IRAC2 and WISE1−WISE2 colors due to CO absorption) and larger variability than the SMC sample.

Fig. 8. IRAC4 versus IRAC1−IRAC4 (left) and MIPS24 versus MLR (right) diagrams color coded with WISE1-band variability (same below). The IRAC1−IRAC4 color is converted to the MLR by using a modified algorithm from Groenewegen & Sloan (2018), where the insert panel shows the comparison between the new (red solid line) and old (black dashed line) algorithms (x-axis is the IRAC1−IRAC4 color and y-axis is the MLR). The error bars show typical error of 0.35 dex. Most of the targets appear to have MLR below ∼10−6.5 M⊙/yr (vertical dashed line; for convenience, two targets showing substantial MLR, e.g.~10−6.0 M⊙/yr, are not shown in the IRAC4 versus IRAC1−IRAC4 diagram). There is a linear relation (dashed line) between MIPS24 magnitude and MLR, while the dotted lines and dashed-dotted lines indicate the 1σ and 3σ uncertainties, respectively. Moreover, a bunch of targets lying above the upper limit of 3σ may be related to episodic mass loss events during the RSGs phase.

NASA/ADS: 2020A&A…639A.116Y

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