ISM properties in low-metallicity environments II. The dust spectral energy distribution of NGC 1569

By F. Galliano, S. Madden, A. Jones, C. Wilson, J. Bernard, F. L. Peintre. 2003

182 citations recorded by the source corpus.

We present new 450 and 850 μ m SCUBA data of the dwarf galaxy NGC 1569. We construct the mid-infrared to millimeter SED of NGC 1569, using ISOCAM, ISOPHOT, IRAS, KAO, SCUBA and MAMBO data, and model the SED in order to explore the nature of the dust in low metallicity environments. The detailed modeling is performed in a self-consistent way, synthesizing the global ISRF of the galaxy using an evolutionary synthesis model with further constraints provided by the observed MIR ionic lines and a photoionisation model. Our results show that the dust properties are different in this low metallicity galaxy compared to other more metal rich galaxies. The results indicate a paucity of PAHs probably due to the destructive effects of the ISRF penetrating a clumpy environment and a size-segregation of grains where the emission is dominated by small grains of size ~$3\;\rm nm$, consistent with the idea of shocks having a dramatic effect on the dust properties in NGC 1569. A significant millimetre excess is present in the dust SED which can be explained by the presence of ubiquitous very cold dust ($T = 5{-}7$ K). This dust component accounts for 40 to 70% of the total dust mass in the galaxy ($1.6{-}3.4 \times 10^5$ $M_\odot$) and could be distributed in small clumps (size $\simeq$ a few pc) throughout the galaxy. We find a gas-to-dust mass ratio of 740-1600, larger than that of the Galaxy and a dust-to-metals ratio of $1/4$ to $1/7$. We generate an extinction curve for NGC 1569, consistent with the modeled dust size distribution. This extinction curve has relatively steep FUV rise and smaller 2175 A bump, resembling the observed extinction curve of some regions in the Large Magellanic Cloud.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2be232b94191afdbfd3ce5ea3ac81d68247f209a

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Citations in the corpus

An Overview of the Dwarf Galaxy Survey (2013, methodology): “…our Galaxy (Reach et al. 1995) and has been detected in low-metallicity dwarf galaxies using ground-based telescopes observing 850=870 μm with SCUBA on the JCMT and with LABOCAonAPEX (e.g., Galliano et al. 2003, 2005; Bendo et al. 2006; Galametz et al. 2009; Zhu et al. 2009; Galametz et al. 2011).”
Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. IV. The Controlling Parameters of the Starburst SED (2007, background): “The French group (Galliano et al. 2003) take the simplest approach of approximating the starburst by a spherical H II region and clumpy dust shell around the central star forming region.”
Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range (2013, background): “…show that the G/D of some low-metallicity dwarf galaxies deviate from this reference trend, with a higher G/D than expected for their metallicity (Lisenfeld & Ferrara 1998; Galliano et al. 2003, 2005, 2008, 2011; Hunt et al. 2005; Bernard et al. 2008; Engelbracht et al. 2008; Galametz et al. 2011).”
Luminous Infrared Galaxies with the Submillimeter Array. I. Survey Overview and the Central Gas to Dust Ratio (2008, background): “The ideal procedure for determing dust mass would be to fit a detailed physical model to the full infrared spectral energy distribution, as has been done by Galliano et al. (2003) for the dwarf galaxy NGC 1569 or Regan et al. (2004) for NGC 7331.”
Mid-Infrared Properties of Low-Metallicity Blue Compact Dwarf Galaxies from the Spitzer Infrared Spectrograph (2005, background): “It has a very small average size of grains (Galliano et al. 2003, 2005) and an LIR of 4:3 ; 10 9 L .”
ISM properties in low-metallicity environments I. mid-infrared spectra of dwarf galaxies (2005, methodology): “…new MIR ISOCAM spectra for the 3 dwarf galaxies, NGC 1569, NGC 1140 and II Zw 40, whose full infrared (IR) SEDs have been succesfully modeled by Galliano et al. (2003, 2005b), as well as the MIR spectra toward 30 Dor in the LMC. Additionally, we add to our study other low metallicity sources…”
Metallicity Effects on Mid-Infrared Colors and the 8 μm PAH Emission in Galaxies (2005, background): “…dramatically from their higher metallicity cousins in their IR properties, with hotter large-grain dust emission and weak PAH emission (Sauvage et al. 1990; Roche et al. 1991; Thuan et al. 1999; Calzetti et al. 2000; Contursi et al. 2000; Madden 2002; Galliano et al. 2003; Houck et al. 2004b).”
Stellar Evolutionary Effects on the Abundances of Polycyclic Aromatic Hydrocarbons and Supernova-Condensed Dust in Galaxies (2007, background): “The first suggests that the trend reflects an increase in the destruction efficiency of PAHs in low-metallicity environments (Galliano et al. 2003, 2005; Madden et al. 2006).”
Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey (2014, background): “A very cold dust component was proposed by Galliano et al. (2003, 2005), showing that it would need to lie in a small number of dense parsec scale clumps, but Galliano et al. (2011) showed that this hypothesis was not verified in the LMC, where they had the spatial resolution to test it.”
Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample (2007, background): “…from the very cold (<10 K) dust that has been reported by Krugel et al. (1998) for the spiral galaxies NGC 6156 and NGC 6918, or the 5Y9 K dust that Galliano et al. (2003, 2005) reported for low-metallicity dwarf galaxies, or the 4Y6K dust that Dumke et al. (2004) reported for the edge-on spiral…”
Metallicity Effects on Dust Properties in Starbursting Galaxies (2008, methodology): “Spectra obtained with the Infrared Space Observatory (ISO) showed that they are significantly weaker in a number of low-metallicity galaxies (Thuan et al. 1999; Madden 2000; Galliano et al. 2003, 2005).”
Variations of the Mid-IR Aromatic Features inside and among Galaxies (2008, background): “Indeed, PAHs are underabundant in low-metallicity galaxies (e.g., Galliano et al. 2003, 2005, 2008; Draine et al. 2007).”
The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types (2014, background): “In low-metallicity objects, small grain sizes (<∼3 nm) start to dominate the 24 µm emission compared to larger dust grains (Lisenfeld et al. 2002; Galliano et al. 2003, 2005), due to the fragmentation of these larger dust grains through shocks experienced in the turbulent ISM.”
Far-infrared to millimeter astrophysical dust emission. I. A model based on physical properties of a (2007, methodology): “For instance, by combining JCMT data at 450 and 850 µm, IRAM 30 m data at 1.2 mm with ISO and IRAS measurements in the IR and FIR, Galliano et al. (2003, 2005) prove a strong millimeter excess towards a set of four blue-compact galaxies (NGC1569, II Zw40, He 2-10, and NGC 1140).”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, background): “…competition, for the origin of this excess: (i) very cold dust, in dense clumps, accounting for a large fraction of the dust budget of the galaxy (Galliano et al., 2003, 2005; Galametz et al., 2009; O’Halloran et al., 2010); (ii) temperature dependent submm emissivity (Meny et al., 2007); (iii)…”
Probing the dust properties of galaxies up to submillimetre wavelengths. II. Dust-to-gas mass ratio trends with metallicity and the submm excess in dwarf galaxies (2011, methodology): “Galliano et al. (2003, 2005) also showed that taking the very cold dust traced in some low metallicity galaxies by SCUBA or MAMBO, the dust-tometals ratios are closer to the Galactic value.”
ISM properties in low-metallicity environments. III. The dust spectral energy distributions of II Zw 40, He 2-10 and NGC 1140 (2005, methodology): “Compared to the Galaxy, there is an obvious dearth of PAHs and the mass spectrum is dominated by grains of small sizes (radius a ≃ 3 − 4nm) as shown in Fig.”