The X-ray emission in high energy peaked blazars exhibit curved spectral nature and is interpreted in terms of a log-parabola electron distribution, or due to an energy-dependent electron diffusion from the acceleration regions. This unique feature may uncover relevant information about the acceleration mechanisms and the underlying physical conditions in the jet. However, the X-ray emission properties in the extreme class of blazars (termed as "EHBLs") are poorly understood due to insuÿcient data at hard X-ray energies. The broadband coverage blazar monitoring programme of the AstroSat, covering UV to X-ray energy range, has given us unprecedented simultaneous X-ray data from the SXT (0.3-8 keV) and the LAXPC (3-80 keV) instruments. This wide range X-ray data can be used to constrain several model parameters such as synchrotron peak energy, spectral index and the high energy cut off in given electron distribution. In this contribution, we report on a detailed spectral study of the HBL sources 1ES 1741+196 and 1ES 2322-409 using data from AstroSat. The observations of 1ES 1741+196 and 1ES 2322-409 were made as part of AstroSat AO proposals, observed during 2019 and 2020 respectively. We investigate their X-ray spectral nature through spectral fitting using di˙erent curved spectral models and provide a well-constrained measure of the synchrotron peak energies.