Bibcode
Elmegreen, D. M.; Elmegreen, B. G.; Sánchez Almeida, J.; Muñoz-Tuñón, C.; Mendez-Abreu, Jairo; Gallagher, John S.; Rafelski, Marc; Filho, M.; Ceverino, Daniel
Bibliographical reference
The Astrophysical Journal, Volume 825, Issue 2, article id. 145, pp. (2016).
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7
2016
Journal
Citations
14
Refereed citations
12
Description
The tadpole galaxy Kiso 5639 has a slowly rotating disk with a drop in
metallicity at its star-forming head, suggesting that star formation was
triggered by the accretion of metal-poor gas. We present
multi-wavelength Hubble Space Telescope Wide Field Camera 3 images of UV
through I band plus Hα to search for peripheral emission and
determine the properties of various regions. The head has a mass in
young stars of ∼ {10}6 {M}ȯ and an
ionization rate of 6.4× {10}51 s‑1,
equivalent to ∼2100 O9-type stars. There are four older star-forming
regions in the tail, and an underlying disk with a photometric age of
∼1 Gyr. The mass distribution function of 61 star clusters is a
power law with a slope of ‑1.73 ± 0.51. Fourteen young
clusters in the head are more massive than {10}4
{M}ȯ , suggesting a clustering fraction of
30%–45%. Wispy filaments of Hα emission and young stars
extend away from the galaxy. Shells and holes in the head H ii region
could be from winds and supernovae. Gravity from the disk should limit
the expansion of the H ii region, although hot gas might escape through
the holes. The star formation surface density determined from Hα
in the head is compared to that expected from likely pre-existing and
accreted gas. Unless the surface density of the accreted gas is a factor
of ∼3 or more larger than what was in the galaxy before, the star
formation rate has to exceed the usual Kennicutt–Schmidt rate by a
factor of ≥slant 5.