Spectral energy distributions of H ii regions in M 33 (HerM33es)

Relaño, M.; Verley, S.; Pérez, I.; Krämer, C.; Calzetti, Daniela; Xilouris, E. M.; Boquien, M.; Abreu-Vicente, J.; Combes, F.; Israel, F. P.; Tabatabaei, F. S.; Braine, J.; Buchbender, C.; González, M.; Gratier, P.; Lord, S. D.; Mookerjea, B.; Quintana-Lacaci, G.; Werf, P. van der

doi:10.1051/0004-6361/201220073

Cited by 19 publications

(28 citation statements)

References 69 publications

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“…Pohlen et al 2010;Engelbracht et al 2010;Fritz et al 2012). The corresponding T c values in HII regions agree with those derived by Relano et al (2013) using the Draine & Li (2007) models and following the prescription of Galametz et al (2012). Warm dust temperatures of T w 50 K are found in the spiral arms and star-forming regions with a maximum of 60 ± 10 K in NGC 604, NGC 595, and IC 133.…”

Section: Cold and Warm Dust Temperaturessupporting

confidence: 77%

Variation in the dust emissivity index across M 33 withHerschelandSpitzer(HerM 33es)

Tabatabaei¹,

Braine²,

Xilouris³

et al. 2014

A&A

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We study the wavelength dependence of the dust emission as a function of position and environment across the disk of M 33 using Spitzer and Herschel photometric data. M 33 is a Local Group spiral with slightly subsolar metallicity, which makes it an ideal stepping-stone to less regular and lower-metallicity objects such as dwarf galaxies and, probably, young-universe objects. Expressing the emissivity of the dust as a power law, the power-law exponent (β) was estimated from two independent approaches designed to properly treat the degeneracy between β and the dust temperature (T ). Both β and T are higher in the inner than in the outer disk, contrary to reported β − T anti-correlations found in other sources. In the cold + warm dust model, the warm component and the ionized gas (Hα) have a very similar distribution across the galaxy, demonstrating that the model separates the components in an appropriate way. Both cold-and warm-dust column densities are high in star-forming regions and reach their maxima toward the giant star-forming complexes NGC 604 and NGC 595. β declines from close to 2 in the center to about 1.3 in the outer disk. β is positively correlated with star formation and with the molecular gas column, as traced by the Hα and CO emission. The lower dust-emissivity index in the outer parts of M 33 is most likely related to the reduced metallicity (different grain composition) and possibly to a different size distribution. It is not due to the decrease in stellar radiation field or temperature in a simple way because the far-infrared-bright regions in the outer disk also have a low β. Like most spirals, M 33 has a (decreasing) radial gradient in star formation and molecular-to-atomic gas ratio such that the regions bright in Hα or CO tend to trace the inner disk, which makes it difficult to distinguish between their effects on the dust. The assumption of a constant emissivity index β is obviously not appropriate.

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Section: Cold and Warm Dust Temperaturessupporting

confidence: 77%

Variation in the dust emissivity index across M 33 withHerschelandSpitzer(HerM 33es)

Tabatabaei¹,

Braine²,

Xilouris³

et al. 2014

A&A

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“…That could be the case for instance in a region where recently formed clusters have blown away much of the dust and the gas of their parent clouds. Such regions were found by Relaño et al (2013), especially in the outskirts of M33.…”

Section: Limits On the Determination Of The Attenuationmentioning

confidence: 80%

Measuring star formation with resolved observations: the test case of M 33

Boquien

Calzetti

Aalto

et al. 2015

A&A

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Context. Measuring star formation on a local scale is important to constrain star formation laws. It is not clear yet, however, whether and how the measure of star formation is affected by the spatial scale at which a galaxy is observed. Aims. We wish to understand the impact of the resolution on the determination of the spatially resolved star formation rate (SFR) and other directly associated physical parameters such as the attenuation. Methods. We carried out a multi-scale, pixel-by-pixel study of the nearby galaxy M 33. Assembling FUV, Hα, 8 µm, 24 µm, 70 µm, and 100 µm maps, we have systematically compared the emission in individual bands with various SFR estimators from a resolution of 33 pc to 2084 pc. Results. There are strong, scale-dependent, discrepancies of up to a factor 3 between monochromatic SFR estimators and Hα+24 µm. The scaling factors between individual IR bands and the SFR show a strong dependence on the spatial scale and on the intensity of star formation. Finally, strong variations of the differential reddening between the nebular emission and the stellar continuum are seen, depending on the specific SFR (sSFR) and on the resolution. At the finest spatial scales, there is little differential reddening at high sSFR. The differential reddening increases with decreasing sSFR. At the coarsest spatial scales the differential reddening is compatible with the canonical value found for starburst galaxies. Conclusions. Our results confirm that monochromatic estimators of the SFR are unreliable at scales smaller than 1 kpc. Furthermore, the extension of local calibrations to high-redshift galaxies presents non-trivial challenges because the properties of these systems may be poorly known.

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“…The dust emission in M33 has already been the subject of several works (e.g. Tabatabaei et al 2014, Relaño et al 2013, Xilouris et al 2012, Boquien et al 2011, Verley et al 2010. In Relaño et al (2013; hereafter R13) they studied the dust properties of HII regions in M33 that they detected in Hα emission.…”

Section: Introductionmentioning

confidence: 91%

“…Tabatabaei et al 2014, Relaño et al 2013, Xilouris et al 2012, Boquien et al 2011, Verley et al 2010. In Relaño et al (2013; hereafter R13) they studied the dust properties of HII regions in M33 that they detected in Hα emission. The sources were classified based on their Hα morphology and, for each source, they measured the FIR colours and dust parameters.…”

Section: Introductionmentioning

confidence: 99%

A multiwavelength analysis of the clumpy FIR-bright sources in M33

Natale

Foyle

Wilson

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present a multiwavelength study of a sample of far-infrared (FIR) sources detected on the Herschel broad-band maps of the nearby galaxy M33. We perform source photometry on the FIR maps as well as mid-infrared (MIR), Hα, far-ultraviolet and integrated HI and CO line emission maps. By fitting MIR/FIR dust emission spectra, the source dust masses, temperatures and luminosities are inferred. The sources are classified based on their Hα morphology (substructured versus not-substructured) and on whether they have a significant CO detection (S/N >3σ). We find that the sources have dust masses in the range 10 2 -10 4 M ⊙ and that they present significant differences in their inferred dust/star formation/gas parameters depending on their Hα morphology and CO detection classification. The results suggests differences in the evolutionary states or in the number of embedded HII regions between the subsamples. The source background-subtracted dust emission seems to be predominantly powered by local star formation, as indicated by a strong correlation between the dust luminosity and the dust-corrected Hα luminosity and the fact that the extrapolated young stellar luminosity is high enough to account for the observed dust emission. Finally, we do not find a strong correlation between the dust-corrected Hα luminosity and the dust mass of the sources, consistent with previous results on the breakdown of simple scaling relations at sub-kpc scales. However, the scatter in the relation is significantly reduced by correcting the Hα luminosity for the age of the young stellar populations in the star-forming regions.

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Spectral energy distributions of H ii regions in M 33 (HerM33es)

Cited by 19 publications

References 69 publications

Variation in the dust emissivity index across M 33 withHerschelandSpitzer(HerM 33es)

Variation in the dust emissivity index across M 33 withHerschelandSpitzer(HerM 33es)

Measuring star formation with resolved observations: the test case of M 33

A multiwavelength analysis of the clumpy FIR-bright sources in M33

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