Parameters of the super star cluster in our field.
|″||Myr||mag||× 106M⊙||× 1052 s-1||mag|
|HST||−||4.8a||0.8ab||1.2a||−||−||#28 from Table 8 in |
|Keck + VLT||046c||5.7d||−||4.1e||1.3e||15.2f||SSC-C in |
|VLT/SINFONI||06g||<6||0.4||6.0||4.4eh||15.0f||Our work |
estimated from measured E(B − V) = 2.20 and assuming RV = 3.1 extinction curve (Weingartner & Draine 2001),
based on the Brγ equivalent width as an age indicator comparing it with Starburst99 (Leitherer et al. 2010) models,
it is unresolved. The angular size (FWHM) measured from a Gaussian fit corresponds to the size of the seeing disk,
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