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We have imaged over 35 years of archival Very Large Array (VLA) observationsof the nearby (d$_{\rm{L}}$ $=$ 3.15 Mpc) Type Ia supernovae SN\,1972E andSN\,1895B between 9 and 121 years post-explosion. No radio emission isdetected, constraining the 8.5 GHz luminosities of SN\,1972E and SN\,1895B tobe L$_{\nu,8.5\rm{GHz}}$ $<$ 6.0 $\times$ 10$^{23}$ erg s$^{-1}$ Hz$^{-1}$ 45years post-explosion and L$_{\nu,8.5\rm{GHz}}$ $<$ 8.9 $\times$ 10$^{23}$ ergs$^{-1}$ Hz$^{-1}$ 121 years post-explosion, respectively. These limits imply aclean circumstellar medium (CSM), with $n$ $<$ 0.9 cm$^{-3}$ out to radii of afew $\times$ 10$^{18}$ cm, if the SN blastwave is expanding into uniformdensity material. Due to the extensive time coverage of our observations, wealso constrain the presence of CSM shells surrounding the progenitor ofSN\,1972E. We rule out essentially all medium and thick shells with masses of0.05$-$0.3 M$_\odot$ at radii between $\sim$10$^{17}$ and 10$^{18}$ cm, andthin shells at specific radii with masses down to $\lesssim$0.01 M$_\odot$.These constraints rule out swaths of parameter space for a range of single anddouble degenerate progenitor scenarios, including recurrent nova,core-degenerate objects, ultra-prompt explosions and white dwarf (WD) mergerswith delays of a few hundred years between the onset of merger and explosion.Allowed progenitors include WD-WD systems with a significant ($>$ 10$^{4}$years) delay from the last episode of common envelope evolution and singledegenerate systems undergoing recurrent nova, provided that the recurrencetimescale i short and the system has been in the nova phase for$\gtrsim$10$^{4}$ yr, such that a large ($>$ 10$^{18}$ cm) cavity has beenevacuated. Future multi-epoch observations of additional intermediate-aged TypeIa SNe will provide a comprehensive view of the large-scale CSM environmentsaround these explosions.

Thirty Years of Radio Observations of Type Ia SN 1972E and SN 1895B: Constraints on Circumstellar Shells