We present results from the first application of the G rid of R ed Supergiant and A symptotic Giant Branch M odel S ( GRAMS ) model grid to the entire evolved stellar population of the Large Magellanic Cloud ( LMC ) .
GRAMS is a pre-computed grid of 80 843 radiative transfer ( RT ) models of evolved stars and circumstellar dust shells composed of either silicate or carbonaceous dust .
We fit GRAMS models to \sim 30 000 Asymptotic Giant Branch ( AGB ) and Red Supergiant ( RSG ) stars in the LMC , using 12 bands of photometry from the optical to the mid-infrared .
Our published dataset consists of thousands of evolved stars with individually determined evolutionary parameters such as luminosity and mass-loss rate .
The GRAMS grid has a greater than 80 % accuracy rate discriminating between Oxygen- and Carbon-rich chemistry .
The global dust injection rate to the interstellar medium ( ISM ) of the LMC from RSGs and AGB stars is on the order of 1.5 \times 10 ^ { -5 } M _ { \odot } yr ^ { -1 } , equivalent to a total mass injection rate ( including the gas ) into the ISM of \sim 5 \times 10 ^ { -3 } M _ { \odot } yr ^ { -1 } .
Carbon stars inject two and a half times as much dust into the ISM as do O-rich AGB stars , but the same amount of mass .
We determine a bolometric correction factor for C-rich AGB stars in the K _ { s } band as a function of J – K _ { s } color , BC _ { K _ { s } } = -0.40 ( J - K _ { s } ) ^ { 2 } +1.83 ( J - K _ { s } ) +1.29 .
We determine several IR color proxies for the dust mass-loss rate ( Ṁ _ { d } ) from C-rich AGB stars , such as \log \dot { M _ { d } } = \frac { -18.90 } { ( K _ { s } - [ 8.0 ] ) +3.37 } -5.93 .
We find that a larger fraction of AGB stars exhibiting the ‘ long-secondary period ’ phenomenon are O-rich than stars dominated by radial pulsations , and AGB stars without detectable mass-loss do not appear on either the first-overtone or fundamental-mode pulsation sequences .