tokens: 1. Hipparcos AGB stars. This list is biased toward nearer stars, mostly within 1 kpc. McDonald et al. ( 2012 ) obtained effective temperatures and luminosities of 107,619 Hipparcos stars (ESA Publications Division 1997 ) based on photometric data covering from the UV to the far-IR. Our search was limited to Hipparcos stars restricted to T eff 3500 K and 1000 ( L / L ⊙ ) 54,000, which eventually reduced the number of candidates to 801 objects. The maximum temperature and minimum luminosity (Salaris Cassisi 1997 ) are criteria intended to reduce the contamination of the sample by RGB stars, while the upper limit of luminosity corresponds to the tip of the AGB ( M bol = − 7.1; Wood et al. 1983 ) that separates massive, evolved AGB stars from supergiants in the HR diagram. Eventually, the spectral classifications of the selected stars were examined in the SIMBAD database to exclude symbiotics, CVs, and other stars that had their temperature and/or luminosity miscalculated by McDonald et al. ( 2012 ). 2. Mass-losing AGB stars. In order to include stars with a circumstellar dust shell ( yr −1 ), a sample of 563 mass-losing AGB stars detected with the Japanese experiment IRTS (Murakami et al. 1996 ) was selected (Le Bertre et al. 2003 ). 3. S-type AGB stars. This class of objects represents the link between O- and C-rich AGB stars and includes two distinct subcategories: (i) the intrinsic S stars are genuine AGB that have their atmosphere enriched by s-process elements brought from the bottom of the convective shell by the third dredge-up process; (ii) the extrinsic S stars have accreted mass from a former AGB companion (now a WD) and generally do not show overabundances of s-process elements. We used the 2nd. edition of the General Catalog of S Stars (Stephenson 1984 ), that contains 1347 stars exhibiting ZrO or LaO bands in their spectra, obtained after various sky surveys. 4. C-rich AGB stars. C-rich stars are the result of the third dredge-up during the thermal-pulse AGB phase, which causes the abundance of carbon to exceed that of oxygen. We adopted a corrected, machine-readable version of the original General Catalog of Galactic Carbon Stars by Stephenson et al. ( 2001 ) available on the Vizier platform, containing 6891 objects. 3. AGB Counterparts in the 4XMM Catalog We cross-correlated the sample of AGB stars described above with the 4XMM-DR9 catalog 3 3 http://xmm-catalog.irap.omp.eu and assumed an X-ray source in this catalog to be a candidate counterpart of an AGB star if their angular distance is within three times the individual positional uncertainty (i.e., 3 × σ pos ). After discarding symbiotic systems, other X-ray emitters, and misclassified AGB stars, we were left with a sample of 19 AGB stars with candidate X-ray counterparts. We then proceeded to download all available XMM-Newton EPIC data of these sources from the XMM-Newton Science Archive (XSA). 4 4 http://nxsa.esac.esa.int/nxsa-web/#home A preliminary inspection revealed that
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