ISM properties in low-metallicity environments. III. The dust spectral energy distributions of II Zw 40, He 2-10 and NGC 1140

By F. Galliano, S. Madden, A. Jones, C. Wilson, Jean-Philippe Bernard. 2005

176 citations recorded by the source corpus.

We present new 450 and 850μm SCUBA data and 1.3 mm MAMBO data of the dwarf galaxies II Zw 40, He 2-10 and NGC 1140. Additional ISOCAM, IRAS as well as ground based data are used to construct the observed mid-infrared to millimeter spectral energy distribution of these galaxies. These spectral energy distributions are modeled in a self-consistent way, as was achieved with NGC 1569 (Galliano et al. 2003, AA (ii) a very small (∼3-4nm) average size of grains, consistent with the fragmentation and erosion of dust particles by the numerous shocks; (iii) a significant millimetre excess in the dust spectral energy distribution which can be explained by the presence of ubiquitous very cold dust (T = 5-9 K) accounting for 40 to 80% of the total dust mass, probably distributed in small clumps. We derive a range of gas-to-dust mass ratios between 300 and 2000, larger than the Galactic values and dust-to-metals ratios of 1/30 to 1/2. The modeled dust size distributions are used to synthesize an extinction curve for each galaxy. The UV slopes of the extinction curves resemble that observed in some regions in the Large Magellanic Cloud. The 2175 A bumps of the modeled extinction curves are weaker than that of the Galaxy, except in the case of II Zw 40 where we are unable to accurately constrain the 2175 A bump carrier.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/55c1dbfe0d1b165fb0903bc497f9ec3e1ae56b86

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An Ultraviolet-to-Radio Broadband Spectral Atlas of Nearby Galaxies (2006, background): “Low metallicity systems, for example, are known to be deficient in PAH emission (e.g., Dale et al. 2005; Engelbracht et al. 2005; Galliano et al. 2005; Walter et al. 2006).”
Mid-Infrared Properties of Low-Metallicity Blue Compact Dwarf Galaxies from the Spitzer Infrared Spectrograph (2005, methodology): “It has a very small average size of grains (Galliano et al. 2003, 2005) and an LIR of 4:3 ; 10 9 L .”
THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, background): “A hard ionizing radiation field has been linked with low metallicity in star forming galaxies (e.g., Campbell et al. 1986; Galliano et al. 2005; Madden et al. 2006; Hunt et al. 2010; Levesque et al. 2010).”
ISM properties in low-metallicity environments I. mid-infrared spectra of dwarf galaxies (2005, methodology): “In support of this hypothesis, to account for the observed FIR to submm SEDs in dwarf galaxies, Galliano et al. (2005b) invoked a scenario of small dense clumps, with size scales on the order of a few tens of pc, having a small volume factor of 10−4 to 10−3.”
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)…”
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).”
HERSCHEL FAR-INFRARED AND SUBMILLIMETER PHOTOMETRY FOR THE KINGFISH SAMPLE OF NEARBY GALAXIES (2011, unknown): “3 (e.g., Bolatto et al. 2000; Galliano et al. 2005; Bot et al. 2010; Gordon et al. 2010; Ade et al. 2011a,b; Galametz et al. 2011; Galliano et al. 2011).”
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.”
Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy’s Evolution (SAGE). I. Overview and Initial Results (2006, unknown): “…IRAC mapping of the lowermetallicity LMCwill yield high-resolution insight into recent work on the paucity of PAH emission in low-metallicity galaxies (Madden 2000, 2006; Houck et al. 2004; Engelbracht et al. 2005; Galliano et al. 2005; Dale et al. 2005; Wu et al. 2006; O’Halloran et al. 2006).”
Spitzer’s perspective of polycyclic aromatic hydrocarbons in galaxies (2020, background): “Madden et al.128 performed a more systematic investigation of the ISOCAM CVF mid-IR spectra of a large number of metal-poor dwarf galaxies and found that the PAH features are substantially suppressed.”
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.”
PAH and Mid-Infrared Luminosities as Measures of Star Formation Rate in Spitzer First Look Survey Galaxies (2005, background): “PAH features can be strong in moderate UV radiation fields such as photodissociation regions, but the PAH carriers could be destroyed in a hard radiation field (Galliano et al. 2005).”
The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, background): “…of knots of star formation (Roussel et al. 2001; Förster-Schreiber et al. 2004; Calzetti et al. 2005) and of the overall star-formation activity of star-forming galaxies (e.g. Wu et al. 2005), except in low-luminosity galaxies with intense ultraviolet (UV) radiation fields (Galliano et al. 2005).”
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).”
The Behavior of the Aromatic Features in M101 H II Regions: Evidence for Dust Processing (2008, background): “…do weaken significantly in active galactic nuclei (Roche et al. 1991; Lutz et al. 1998; Smith et al. 2007b) and star bursting galaxies with fairly low metallicities (Roche et al. 1991; Engelbracht et al. 2005; Galliano et al. 2005; Madden et al. 2006; Wu et al. 2006; Engelbracht et al. 2008).”
The Calibration of Mid-Infrared Star Formation Rate Indicators (2007, background): “The deficiency is far more pronounced in the case of S8µm, dust, a fact already noted in a number of previous investigations (e.g., Engelbracht et al. 2005; Galliano et al. 2005; Hogg et al. 2005; Rosenberg et al. 2006; Draine et al. 2007).”
An Overview of the Dwarf Galaxy Survey (2013, methodology): “Possible explanations put forth to explain the submm excess include: (1) very cold dust component (e.g., Galliano et al. 2005; Galametz et al. 2011); (2) unusual dust emissivity properties (e.g., Lisenfeld et al. 2002;Meny et al. 2007; Galliano et al. 2011; Paradis et al. 2011); (3) anomalous…”
Infrared Spectral Energy Distributions of Nearby Galaxies (2005, result): “Some of the low-metallicity objects lie dramatically below the canonical star-forming galaxy curves, consistent with the Engelbracht et al. (2005) and Galliano et al. (2005) empirical finding that low-metallicity galaxies show relatively low 8.0 m emission.”
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.”
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).”