Warm dust and spatially variable polycyclic aromatic hydrocarbon emission in the dwarf starburst galaxy NGC 1705

J.M. M. Cannon, J.D.T. D.T. Smith, F. Walter, G.J. J. Bendo, D. Calzeti, D.A. A. Dale, B.T. T. Draine, C.W. W. Engelbracht, K.D. D. Gordon, G. Helou, R.C. C. Kennicutt, C. Leitherer, L. Armus, B.A. A. Buckalew, D.J. J. Hollenbach, T.H. H. Jarrett, A. Li, Martin Meyer, E.J. J. Murfhy, M.W. W. ReganG.H. H. Rieke, M.J. J. Rieke, H. Roussel, K. Sheth, M.D. D. Thornley

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36 Citations (Scopus)


We present Spitzer observations of the nearby dwarf starburst galaxy NGC 1705 obtained as part of the Spitzer Infrared Nearby Galaxies Survey. The galaxy morphology is very different shortward and longward of ~5 µm: optical and short-wavelength IRAC imaging shows an underlying red stellar population, with the central super star cluster (SSC) dominating the luminosity; longer wavelength IRAC and MIPS imaging reveals warm dust emission arising from two off-nuclear regions that are offset by ~250 pc from the SSC and that dominate the far-IR flux of the system. These regions show little extinction at optical wavelengths. The galaxy has a relatively low global dust mass (~2 × 105 A?, implying a global dust-to-gas mass ratio ~2-4 times lower than the Milky Way average, roughly consistent with the metallicity decrease). The off-nuclear dust emission appears to be powered by photons from the same stellar population responsible for the excitation of the observed Ha emission; these photons are unassociated with the SSC (although a contribution from embedded sources to the IR luminosity of the off-nuclear regions cannot be ruled out). Low-resolution IRS spectroscopy shows moderate-strength PAH emission in the 11.3 µm band in the more luminous eastern peak; no PAH emission is detected in the SSC or the western dust emission complex. There is significant diffuse emission in the IRAC 8 µm band after starlight has been removed by scaling shorter wavelength data; the fact that IRS spectroscopy shows spatially variable PAH emission strengths compared to the local continuum within this diffuse gas suggests caution in the interpretation of IRAC diffuse 8 µm emission as arising from PAH carriers alone. The nebular metallicity of NGC 1705 falls at the transition level of ~0.35 Z? found by Engelbracht and collaborators, below which PAH emission is difficult to detect; the fact that a system at this metallicity shows spatially variable PAH emission demonstrates the complexity of interpreting diffuse 8 mu;m emission in galaxies. NGC 170
Original languageEnglish
Pages (from-to)293-302
Number of pages10
JournalThe Astrophysical Journal
Issue number1 I
Publication statusPublished - 2006


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