| Abstract : | We present a multi-wavelength study of the nearby flocculent galaxy NGC 4571 using multi-band observations taken from the Ultra-Violet Imaging Telescope (UVIT) in the F154W and N263M filters, the Sloan Digital Sky Survey (SDSS) in the g and r filters and the Atacama Large Milimeter/Submilimeter Array (ALMA). With the superior spatial resolution of UVIT (FWHM ∼ 1.4′′ ∼ 101.11 pc), we identified 319 bright young star-forming regions in the UVIT FUV and NUV bands throughout the galaxy, with their radii between ∼ 53 − 500 pc. The masses of the identified regions span a range between 103 −106 M⊙ . We observe a trend of decrease in the mass of sources with increasing radial distance. We also studied the associations of FUV-detected Star-forming Regions (SRs) with ALMA-detected Giant Molecular Clouds (GMCs). We find 161 such SR-GMC associations with their separations ranging between ∼ 10 − 200 pc. We observe these SR-GMC associations to trace the flocculent arms of the galaxy. We derived the radial surface brightness profiles in the UV and optical bands and the radial SFR density profile of the galaxy. The radial (F154W - N263M) and the (g - r) color profiles provide further evidence for the presence of younger and bluer sources more towards the outer parts of the galaxy. We estimate the total Star Formation Rate (SFR) of the galaxy using the FUV flux corrected
for galactic and internal extinction. The star forming regions are observed to have a clumpy nature in general, which is also seen in the distribution of molecular gas throughout the galaxy. |
