Collisional impacts between asteroid-sized objects have been common throughout the history of our solar system and have significantly contributed to the formation of asteroid families (Nesvorný et al., 2015). Of particular interest are the low-albedo (geometric albedo < 0.10) and low-inclination (i ≤ 15°) asteroid families situated within the inner main belt (IMB), between the v6 secular resonance at ~ 2.15 au and the 3:1 mean-motion resonance with Jupiter at ~2.5 au. These families are proposed to be significant sources of carbonaceous near-Earth asteroids (NEAs) such as asteroids Ryugu and Bennu (Bottke et al. 2015; Granvik et al. 2016; Dykhuis and Greenberg, 2015). Carbonaceous NEAs contain abundant water- and carbon-rich materials, which are essential elements for understanding the origin of life on Earth and provide valuable historical records of the early solar system. Exploring the relationships between carbonaceous NEAs and these IMB families also enhances the scientific value of the sample return missions (see this meeting abstract # 678 by Takir et al.). Studying the IMB also has broader implications for the formation of exoplanetary systems, such as PDS 70. The discovery of water vapor by JWST MIRI in the inner part of PDS 70's protoplanetary disk (Perotti et al. 2023) suggests that water is playing a crucial role in the formation of this young exoplanetary system.As part of the JWST SAMBA3 (Spectral Analysis of Main Belt Asteroids in the 3-µm region) program (Cycle 3 GO; #6384), we are conducting observations of asteroids from seven collisional low-albedo and low-inclination families located in the IMB. The studied families include New Polana, Eulalia, Erigone, Sulamitis, Clarissa, Chaldaea, and Klio. We have selected nine asteroids from these families to investigate potential links with carbonaceous NEAs (see Table 1). Our study focuses on the parent bodies of six asteroid families. For the New Polana family, we are observing three fragments. We will compare these fragments with one another and with the parent body asteroid (142) Polana (Arredondo et al. 2024) to determine whether the fragments from the same family exhibit similar or differing hydration states (e.g., Michel et al. 2020). For our observations, we are utilizing the NIRSpec instrument, which covers a spectral range of~ 0.6 to 5.2 µm. This range includes essential diagnostic absorption features characteristic of primitive and carbonaceous materials, such as H2O/hydroxyl (OH), carbonates, and organics.Table 1. Current JWST observation status of the SAMBA3 program (Cycle 3 GO; #6384).As of this writing, JWST has executed observations for seven asteroids. The observation of asteroid (6769) Brokoff faced an issue and was not fully executed; therefore, it has been rescheduled for the next cycle. Le Pivert-Jolivet et al. (this meeting abstract #359) will discuss the analysis and interpretation of asteroid (84) Klio. Harvison et al. (this meeting abstract #1004) will focus on asteroids (302) Clarissa and (163) Erigone. Additionally, McClure et al. (this meeting abstract #404) will examine asteroids (2441) Hibbs, (6712) Hornstein, and (495) Eulalia. We also expect to observe asteroids (752) Sulamitis and (313) Chladaea before the meeting. Acknowledgements: We would like to acknowledge the support of the Space Telescope Science Institute (JWST-GO-06384.001-A). JdL, TPJ, and JL acknowledge support from the Agencia Estatal de Investigacion del Ministerio de Ciencia e Innovación (AEI-MCINN) under grant "Hydrated Minerals and Organic Compounds in Primitive Asteroids" with reference PID2020-120464GB-100. References: Arredondo, A. et al., 2024. AAS DPS, Abstract##411.02.Bottke, W.F et al., 2015. Icarus 247, 191e217.Dykhuis, M., Greenberg, R., 2015. Icarus 252, 199e211.Granvik, M. et al., 2016. Icarus 312, 181-207.Michel, P. et al., 2020. Nature Communications 11, 2655 (2020.Nesvorný, D. et al., 2015. Asteroids IV 297e321.Perotti, G. et al., 2023 et al. Nature 620, 516-520.