Correlations in molecular content of oxygen-rich AGB and RSG stars Sofia Wallström1, Leen Decin1, Carl Gottlieb2, Holger Müller3, Taïssa Danilovich1, Fabrice Herpin4, and the ATOMIUM collaboration5 1. Institute of Astronomy, KU Leuven, Belgium. 2. Harvard Smithsonian Center for Astrophysics, Cambridge, Massachusetts, USA. 3. I. Physikalisches Institut, Universität zu Köln, Germany. 4. Laboratoire d’astrophysique de Bordeaux, Université Bordeaux, France 5. https://fys.kuleuven.be/ster/research-projects/aerosol/atomium/atomium Background The ATOMIUM ALMA large project aims to establish the dominant physical and chemical processes in the winds of oxygen-rich evolved stars over a range of ini@al stellar masses, pulsa@on behaviours, mass-loss rates, and evolu@onary phases. Through high-resolu@on (~0.025" - 0.05") observa@ons in bands between 214 and 270 GHz, we have detected 286 molecular lines of 23 diﬀerent molecules and their isotopologues, in vibra@onal states up to v=5. The eventual unravelling of the complex chemistry of these sources will provide astrochemical knowledge that will strongly impact research on supernovae, protostars, interstellar clouds, ac@ve galac@c nuclei, etc. — environments in which it is far more diﬃcult to grasp the dust nuclea@on process. As a star@ng point for the chemical analysis, we have calculated Pearson's linear correla@on coeﬃcients between the molecular content of each source and its (circum)stellar parameters: mass-loss rate, expansion velocity, and pulsa@on type. Ini.al results We see some expected correla@ons with mass-loss rate: a higher wind velocity and molecular tracers of dense winds such as H2S, as well as the rarer Al-bearing molecules. Lower wind velocity, conversely, is correlated with the detec@on of H2O and to a lesser extent OH. Mira pulsator sources are correlated with detec@ons of a somewhat random list of molecules: SiS, CS, PO, AlF, and KCl. The metal oxides PO, TiO, and AlO are well correlated, as expected, though TiO2 is not. AlOH is beaer correlated with the metal halides, which are also nicely correlated with each other, with the excep@on of KCl. KCl also shows no correla@on with mass-loss rate, unlike the other metal oxides and halides. However, these outlier molecules tend to have fewer and weaker detected lines, which may explain the observed trends. All results should be treated as preliminary! Note that we also detect more carbonaceous molecules, such as HC3N and SiCC, as well as the nitrogen-bearing SiN, but only in the singular S-type star W Aql and hence they are not included in the correla@on table. VX Sgr and W Aql are the most line rich sources in our sample, with ~5.5 and ~3.8 lines/GHz, respec@vely. Correla.ons between sources: Table of linear correla@on coeﬃcients, colorized by value from green (1.0 = perfect correla@on) to pink (-1.0 = perfect an@-correla@on), calculated using values of mass-loss rate and expansion velocity, and designa@on as 0 or 1 in pulsa@on type (Mira or other) and molecular content (line detec@on at a 3σ level) Source Puls MLR vWind S Pav SRa 8.0E-08 9 T Mic SRb 8.0E-08 4.8 U Del SRb 1.5E-07 7.5 R Hya Mira 2.0E-07 12.5 RW Sco Mira 2.1E-07 11 SV Aqr LPV 3.0E-07 8 V PsA SRb 3.0E-07 14.4 U Her Mira 5.9E-07 15 pi Gru SRb 7.7E-07 30 AH Sco SRc 1.0E-06 23 W Aql Mira 3.0E-06 17.2 R Aql Mira 3.5E-06 8 KW Sgr SRc 5.0E-06 27 GY Aql Mira 6.0E-06 13.6 IRC-10529 Mira 1.0E-05 13 IRC+10011 Mira 1.0E-05 23 VX Sgr SRc 6.1E-05 24.3 Source table: The ATOMIUM sample of AGB and RSG stars, along with their pulsa@on type, mass-loss rate (in solar masses per year) and expansion velocity (in km/s), taken from the literature.