This work presents the 12CO emission of HD121617's debris disk. We used ALMA data to investigate the dynamics of the gas and produce a dynamical mass estimate to compare it with stellar evolutionary models. This disk is well-suited for radiative transfer modeling of the Keplerian motion of the gas in the disk. We pair the radiative modeling of the disk with an affine-invariant MCMC methods.

We used radiative transfer code, DISKMODEL3, to fit the ALMA 12CO channel maps for HD121617. With new, precise distance measurements for this source, we are able to make high precision direct measurements of HD121617's mass. The mass measurement is no longer limited by the distance as in previous studies. We find that HD121617 has a mass of 1.70+/-0.02 (solar units) Comparing with stellar masses estimated using the MESA stellar evolutionary database, we find that our dynamical mass estimate for HD121617 is not in agreement with the model. The large discrepancy for this may be caused due to the large uncertainties on metallicity estimates which has the effect of shifting our dynamical mass estimate through a large region on the HR diagram.

Future studies should leverage the synergy of ALMA, Gaia, and detailed radiative transfer disk modeling as this will enable precise mass measurements of dynamical masses for a large number of stars ultimately allowing for the evaluation of our stellar evolutionary models.

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