MNRAS 000, 1–14 (0000) Preprint 15 November 2022 Compiled using MNRAS L A T E X style file v3.0 Discovery of  Sct Components in Eclipsing Binary Systems IQ CMa, AW Men and W Vol Burak Ulaş 1 ★ , Ceren Ulusoy 2 1 Department of Space Sciences and Technologies, Faculty of Sciences, Çanakkale Onsekiz Mart University, Terzioˇ glu Campus, Çanakkale, TR-17100,Turkey 2 Department of Physics and Astronomy, Botswana International University of Science and Technology (BIUST), Plot 10017, Private Bag 16, Palapye, Botswana Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We present the first evidence on the  Sct type pulsations of the primary components of three eclipsing binaries IQ CMa, AW Men and W Vol in the TESS field. A comprehensive investigation of the binary properties is conducted. The light curves of the systems are analysed and the frequency analyses are performed to residual data. The systems are compared to the binaries of the same morphological types, and the primaries are examined in contrast to the  Sct type pulsators. The results show that the systems are oscillating eclipsing Algol-type systems. Key words: (stars:) binaries: eclipsing – stars: oscillations (including pulsations) – stars: individual: IQ CMa, AW Men, W Vol 1 INTRODUCTION Scientific research on Eclipsing Binary Systems (EBs) constitutes the backbone of astrophysics in many respects. First and foremost, EBs play a vital role in studying the fundamental stellar parameters and distances that can be determined more precisely than the data obtained for single stars. EBs with pulsating components are the most advantageous targets for direct measurement of component masses and radii in the case of high-mass short period binaries (e.g. Ribas et al. 2000; Torres et al. 2010). Thus, these targets are critical to uncovering the physical phenomena of massive pulsating stars in EBs (Lampens et al. 2022; Tkachenko et al. 2020; Johnston 2021; Southworth & Bowman 2022; Simón-Díaz et al. 2017). Pulsating components can be found in a broad range of spectral types and in the various group of instability strips ( Sct and  Cep stars) across the HR diagram (Liakos & Niarchos 2017). Over the last decade, our understanding of binary stars has remarkably improved since a large number of EBs with pulsating stars were discovered in the  Sct Scuti regime by the Kepler/K2 (Borucki et al. 2010; Gilliland et al. 2010; Howell et al. 2014) and TESS (Ricker et al. 2015) missions.  Sct stars are Population I stars situated on the main-sequence at the extension of the Cepheid instability strip with A0-F5 spectral types and effective temperatures of 6700–8900K (Samadi Ghadim et al. 2018; Chang et al. 2013). Their masses are between 1.5 and 2.5 M⊙, which correspond to the main sequence stage of core hydrogen or shell burning. The oscillations of this type of pulsators are driven by - mechanism in radial and non-radial pressure and gravity modes or both (Grigahcène et al. 2010; Uytterhoeven et al. 2011). The periods vary between about 0. d 008-0. d 42. (Catelan & Smith 2015). The study of EBs with  Sct components can provide accurate asteroseismic models which are linked to the short-term stellar evo- ★ E-mail: burak.ulas@comu.edu.tr lution dynamic because they undergo a series of several physical phenomena such as tidal interactions between the components, mass transfer stages and pulsations (Samadi Ghadim et al. 2018; Lamp- ens 2021; Lampens et al. 2022). Particularly, in close binary systems, tidally-excited non-radial pulsations can also be involved in the stellar evolution process (Aerts 2021). The literature has very limited information about the systems and all targets are mainly published in several catalogue studies such as Gaia DR2, DR3 (Gaia Collaboration et al. 2018; Brandt 2021), the binary star catalogue of Avvakumova et al. (2013) and the TESS eclipsing binary catalogue of Mortensen et al. (2021). Wright et al. (2003) indicated an effective temperature value, 7580 K, for IQ CMa based on the spectral type, A8V. Sharma et al. (2018) listed temper- ature and log  (7250 K and 3.8) values for W Vol based on high resolution spectroscopy. The radial velocity limit for the target was catalogued by Reiners & Zechmeister (2020) and the mid-infrared flux and diameter were given by Cruzalèbes et al. (2019). The lack of detailed studies, although the light curves show evident oscillation- like effects, motivated us to investigate the systems. This is the first report that presents the first evidence on pulsation characteristics of primary components, as well as the first comprehensive binary modeling in the literature. 2 LIGHT CURVE DATA The TESS light curves of three eclipsing binary systems were col- lected through Mikulski Archive for Space Telescopes (MAST) por- tal 1 . The data from sectors 6 and 33 for IQ CMa, 2, 4 and 5 for AW Men, and 2, 5 and 6 for W Vol were used. Data files cover datapoints of 32308, 52304 and 51324 for IQ CMa, AW Men and W Vol, respectively, with no NULL data. Since the Per-search Data 1 https://mast.stsci.edu/portal/Mashup/Clients/Mast/ Portal.html © 0000 The Authors arXiv:2211.07529v1 [astro-ph.SR] 14 Nov 2022