In this study, we conduct a multi-frequency analysis of the gamma-ray bright blazar 1308+326 from February 2013 to March 2020, using the Korean VLBI Network at 22 and 43 GHz and gamma-ray data from the Fermi Large Area Telescope (LAT). Our findings reveal spectral variations around the 2014 gamma-ray flare, aligning with the shock-in-jet model. A strong correlation is observed between gamma-ray and 43 GHz emissions, with a 27-day lag in the VLBI core light curve, indicating a 50-day delay from the beginning of a specific radio flare to the gamma-ray peak. This radio flare correlates with a new jet component, suggesting the 2014 gamma-ray flare resulted from its interaction with a stationary component. Our analysis indicates the 2014 gamma-ray flare originated 40–63 parsecs from the central engine, with seed photons for the gamma-ray emission unlikely from the broad-line region.

Introduction
Observations and Data Acquisition
    KVN Data
        KVN Single-Dish Observations
        KVN VLBI Data
    Multi-Frequency Data
        OVRO 15 GHz and Metsähovi 37 GHz
        Gamma-Ray Data
        VLBA Data
Results and Analysis
    Multi-Frequency Light Curves
        Radio Light Curves
        Gamma-Ray Light Curve
    Spectral Indices
    Cross-Correlation Analysis
    Variability Time Scales
        Radio Flare Decomposition
        Physical Parameters
Discussion
    Variability of the Spectral Index
    Connection between Gamma-Ray Emission and Radio Flares
    Location of Gamma-Ray Emission Region
    Seed Photon Candidates
    Brightness Temperature and Emission Region
Summary
Acknowledgments
References
Comparison of the Measurements from the KVN Single-Dish Observations

• Shan Li(Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea, University of Science and Technology, Daejeon 34113, Republic of Korea)
• Sang-Sung Lee(Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea, University of Science and Technology, Daejeon 34113, Republic of Korea) Corresponding author
• Whee Yeon Cheong(Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea, University of Science and Technology, Daejeon 34113, Republic of Korea)