New Results with TECSA – the d(26Alm,p)27Al experiment, B. T. Roeder1, L. Trache1, T. Davinson2, V. E. Iacob1, M. La Cognata3, G. Lotay2, M. McCleskey1, R. G. Pizzone1,3, G. G. Rapisarda3,4, E. Simmons1, R. Sparta3,4,  A. Spiridon1, C. Spitaleri3,4, R. E. Tribble1, and P. J. Woods2, [1] Cyclotron Institute, Texas A & M University, College Station, Texas, USA; [2] School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom ; [3] INFN Laboratori Nazionali del Sud, 95123 Catania, Italy; [4] Dipartimento di Fisica e Astronomia, Università di Catania, 95123 Catania, Italy − The detection of gamma rays from the decay of the 26Al ground state in the galaxy gives evidence that nucleosynthesis is occurring in present-day stars, but its origin is not yet clear.  This implies that reactions involving 26Al are important for astrophysical processes.  In a recent experiment at the Cyclotron Institute at Texas A & M University, reactions with the ground state and isomeric state of 26Al were investigated with the Texas A & M-Edinburgh-Catania Silicon detector Array (TECSA).  TECSA is a collaborative effort to build a high-efficiency detector Si array useful for measuring reactions of interest for nuclear astrophysics and nuclear structure.  The array consists of up to 16 Micron Semiconductor YY1 detectors that are each 300 um thick.  Each detector has 16 annular ring sectors to measure the energy and the scattering angle of the detected particles.  Using TECSA, we measured d(26Alg,p)27Al and d(26Alm,p)27Al with an 26Al secondary beam prepared in-flight with the MARS spectrometer. First, the composition of the 26Al beam was determined by measuring the ratio of beta-decays to 26Al ions produced.  It was found that at different spectrometer rigidities, beams of 2/3 isomer to ground state ratio or vice-versa could be obtained.  Then, in the second part of the experiment, angular distributions were measured for both reactions at backward angles with TECSA.  The protons were measured in TECSA in coincidence with timing signals from the beam detected by a scintillator and with the cyclotron radio-frequency.  Details of the experiment and results from the analysis of the d(26Alm,p)27Al and d(26Alg,p)27Al data will be presented.  They will give information about the proton capture reactions 26Alm(p,γ)27Si and 26Alg(p,γ)27Si taking place in stars.