We investigate the radio properties of the dwarf galaxy SDSS J133245.62+263449.3 which shows optical signatures of black hole activity. Dwarf galaxies are known to host intermediate mass black holes (IMBHs) with masses MBH ∼ 10 4-6 M⊙, some of them being radio loud. Recently, Reines et al. (2013) found dwarf galaxy candidates which show signatures of being black hole hosts based on optical spectral lines. SDSS J133245.62+263449.3 is one of them; it shows a flux density of ∼ 20 mJy at 1.4 GHz, which corresponds to L 1.4GHz ∼ 10 23 WHz -1. This is much brighter than other black hole host dwarf galaxies. However, star formation activity can contribute to radio continuum emission as well. To understand the nature of the radio emission from SDSS J133245.62 + 263449.3, we imaged this radio loud dwarf galaxy at low frequencies (325 MHz and 610 MHz) using the Giant Metrewave Radio Telescope (GMRT). We present here the high resolution images from our GMRT observations. While we detect no obvious extended emission from radio jets from the central AGN, we do find the emission to be moderately extended and unlikely to be dominated by disk star formation. VLBI observations using the Korean VLBI Network (KVN) are now being planned to understand the emission morphology and radiation mechanism.

Abstract
1. INTRODUCTION
2. OBSERVATIONS AND DATA ANALYSIS
    2.1. Radio Data: GMRT and FIRST
    2.2. Optical Data: Archived SDSS Spectrum
3. RESULTS
    3.1. Results from Radio Observations
    3.2. Star Formation Rate
    3.3. Black Hole Mass and Eddington Ratio
4. DISCUSSION
REFERENCES

• Sanjaya Paudel(Department of Astronomy & Center for Galaxy Evolution Research, Yonsei University)
• Bong Won Sohn(Korea Astronomy and Space Science Institute) Corresponding author
• Chandreyee Sengupta(Yonsei University Observatory, Yonsei University)
• Songyoun Park(Department of Physics and Astronomy, Seoul National University)