Dust-to-Gas Ratio in the Extremely Metal Poor Galaxy I ZW 18

Abstract

The blue compact dwarf galaxy I Zw 18 is one of the most metal poor systems known in the local Universe (12 + log(O/H) $=$ 7.17). In this work we study I Zw 18 using data from {\it Spitzer}, {\it Herschel Space Telescope} and IRAM Plateau de Bure Interferometer. Our data set includes the most sensitive maps of I Zw 18, to date, in both, the far infrared and the CO $J=1\to 0$ transition. We use dust emission models to derive a dust mass upper limit of only M${}_{dust}\le 1.1\times 10^4$ M${}_{\odot }$ ($3\sigma$ limit). This upper limit is driven by the non-detection at 160 $\mu$m, and it is a factor of 4-10 times smaller than previous estimates (depending upon the model used). We also estimate an upper limit to the total dust-to-gas mass ratio of M${}_{Dust}$/M${}_{gas}\le 5.0\times 10^{-5}$. If a linear correlation between the dust-to-gas mass ratio and metallicity (measure as O/H) were to hold, we would expect a ratio of 3.9$\times 10^{-4}$. We also show that the infrared SED is similar to that of starbursting systems.

Accepted for publication in ApJ: 8 pages, 4 figures, 1 table

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