The Dust-to-Gas Ratio in the Small Magellanic Cloud Tail

Gordon, K. D.; Bot, Caroline; Müller, Erik; Misselt, K. A.; Bolatto, Alberto D.; Bernard, J.-P.; Reach, W. T.; Engelbracht, C. W.; Babler, B.; Bracker, S.; Block, M.; Clayton, Geoffrey C.; Hora, J. L.; Indebetouw, R.; Israel, F. P.; Li, A.; Madden, S. C.; Meade, M. R.; Meixner, Margaret; Sewiło, M.; Shiao, Bernie; Smith, L. J.; Loon, Jacco Th. van; Whitney, B. A.

doi:10.1088/0004-637x/690/1/l76

Cited by 42 publications

(65 citation statements)

References 40 publications

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“…Bendo et al (2010) also compare radial variations in the D/G with the oxygen abundance gradients and found a good correspondence, although the D/G radial variations seems to be steeper. Recent studies in the low-metallicity Magellanic Clouds have shown that their D/G are lower than that estimated for more metal-rich environments (Bernard et al 2008;Gordon et al 2009), consistent with what should be expected from the previous relation between the D/G and the metallicity. James et al (2002), using JCMT/SCUBA observations at 850 μm observations, concluded that the fraction of metals incorporated into dust was a universal constant, that is to say similar for dwarf and giant galaxies, which was in contradiction to the Lisenfeld & Ferrara (1998) conclusions.…”

Section: Introductionsupporting

confidence: 75%

Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz

Madden

Galliano

et al. 2011

A&A

204

294

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Aims. We are studying the effects of submm observations on the total dust mass and thus dust-to-gas mass ratio measurements. Methods. We gather a wide sample of galaxies that have been observed at submillimeter (submm) wavelengths to model their spectral energy distributions using submm observations (>160 μm) and then without submm observational constraints in order to quantify the error on the dust mass when submm data are not available. Our model does not make strong assumptions on the dust temperature distribution to precisely avoid submm biaises in the study. Our sample includes 52 galaxies observed at submm wavelengths. Out of these, 9 galaxies show an excess in submm which is not accounted for in our fiducial model, most of these galaxies being lowmetallicity dwarfs. We chose to add an independant very cold dust component (T = 10 K) to account for this excess. Results. We find that metal-rich galaxies modelled with submm data often show lower dust masses than when modelled without submm data. Indeed, these galaxies usually have dust SEDs that peaks at longer wavelengths and require constraints above 160 μm to correctly position the peak and sample the submillimeter slope of their SEDs and thus correctly cover the dust temperature distribution. On the other hand, some metal-poor dwarf galaxies modelled with submm data show higher dust masses than when modelled without submm data. Using submm constraints for the dust mass estimates, we find a tightened correlation of the dust-to-gas mass ratio with the metallicity of the galaxies. We also often find that when there is a submm excess present, it occurs preferentially in low-metallicity galaxies. We analyse the conditions for the presence of this excess and find a relation between the 160/850 μm ratio and the submm excess.

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Section: Introductionsupporting

confidence: 75%

Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz

Madden

Galliano

et al. 2011

A&A

204

294

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“…This is the same time at which the SMC tail, a tail of tidal origin located within the Bridge, was stripped from the galaxy (Gordon et al 2009). This means that if the Bridge material were stripped earlier, it did not form stars.…”

Section: Dynamics and The Magellanic Bridgementioning

confidence: 83%

“…The large magellanic cloud (LMC) is a late-type spiral galaxy seen nearly face-on, rich in gas and with active star formation while the small magellanic cloud (SMC) is a highly inclined irregular galaxy with less active star formation. Their dynamical interaction is claimed to be responsible for the various star forming episodes and of the creation of the Magellanic Bridge, connecting the two galaxies, (Gordon et al 2009) and the Stream (Nidever et al 2008). The LMC is probably just a few kpc thick, along the line of sight, but the SMC has a more complex structure that may extend up to 20 kpc.…”

Section: Introductionmentioning

confidence: 99%

The metallicity gradient as a tracer of history and structure: the Magellanic Clouds and M33 galaxies

Cioni¹

2009

A&A

134

154

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Context. The stellar metallicity and its gradient place constraints on the formation and evolution of galaxies. Aims. This is a study of the metallicity gradient of the LMC, SMC and M33 galaxies derived from their asymptotic giant branch (AGB) stars. Methods. The [Fe/H] abundance was derived from the ratio between C-and M-type AGB stars and its variation analysed as a function of galactocentric distance. Galaxy structure parameters were adopted from the literature.Results. The metallicity of the LMC decreases linearly as −0.047± 0.003 dex kpc −1 out to ∼8 kpc from the centre. In the SMC, [Fe/H] has a constant value of ∼−1.25 ± 0.01 dex up to ∼12 kpc. The gradient of the M33 disc, until ∼9 kpc, is −0.078 ± 0.003 dex kpc −1 while the outer disc/halo, out to ∼25 kpc, has [Fe/H] ∼ −1.7 dex. Conclusions. The metallicity of the LMC, as traced by different populations, bears the signature of two major star forming episodes: the first one constituting a thick disc/halo population and the second one a thin disc and bar due to a close encounter with the Milky Way and SMC. The [Fe/H] of the recent episode supports an LMC origin for the Stream. The metallicity of the SMC supports star formation, ∼3 Gyr ago, as triggered by LMC interaction and sustained by the bar in the outer region of the galaxy. The SMC [Fe/H] agrees with the present-day abundance in the Bridge and shows no significant gradient. The metallicity of M33 supports an "insideout" disc formation via accretion of metal poor gas from the interstellar medium.

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“…In order to quantify in a more objective way the detection of these three structures we followed the approach adopted by Gordon et al (2009) who, to this aim, used the correlation expected between hydrogen column density and foreground subtracted FIR maps. We have looked for such correlations in regions E, F and G, between the high resolution hydrogen map, and SPIRE images.…”

Section: Far-infrared Structuresmentioning

confidence: 99%

TheHerschelExploitation of Local Galaxy Andromeda (HELGA)

Fritz

Gentile

Smith

et al. 2012

A&A

Self Cite

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Context. We have obtained Herschel images at five wavelengths from 100 to 500 μm of a ∼5.5 × 2.5 degree area centred on the local galaxy M 31 (Andromeda), our nearest neighbour spiral galaxy, as part of the Herschel guaranteed time project "HELGA". The main goals of HELGA are to study the characteristics of the extended dust emission, focusing on larger scales than studied in previous observations of Andromeda at an increased spatial resolution, and the obscured star formation. Aims. In this paper we present data reduction and Herschel maps, and provide a description of the far-infrared morphology, comparing it with features seen at other wavelengths. Methods. We used high-resolution maps of the atomic hydrogen, fully covering our fields, to identify dust emission features that can be associated to M 31 with confidence, distinguishing them from emission coming from the foreground Galactic cirrus. Results. Thanks to the very large extension of our maps we detect, for the first time at far-infrared wavelengths, three arc-like structures extending out to ∼21, ∼26 and ∼31 kpc respectively, in the south-western part of M 31. The presence of these features, hosting ∼2.2 × 10 6 M of dust, is safely confirmed by their detection in HI maps. Overall, we estimate a total dust mass of ∼5.8 × 10 7 M , about 78% of which is contained in the two main ring-like structures at 10 and 15 kpc, at an average temperature of 16.5 K. We find that the gas-to-dust ratio declines exponentially as a function of the galacto-centric distance, in agreement with the known metallicity gradient, with values ranging from 66 in the nucleus to ∼275 in the outermost region. Conclusions. Dust in M 31 extends significantly beyond its optical radius (∼21 kpc) and what was previously mapped in the farinfrared. An annular-like segment, located approximately at R 25 , is clearly detected on both sides of the galaxy, and two other similar annular structures are undoubtedly detected on the south-west side even further out.

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The Dust-to-Gas Ratio in the Small Magellanic Cloud Tail

Cited by 42 publications

References 40 publications

Probing the dust properties of galaxies up to submillimetre wavelengths

Probing the dust properties of galaxies up to submillimetre wavelengths

The metallicity gradient as a tracer of history and structure: the Magellanic Clouds and M33 galaxies

TheHerschelExploitation of Local Galaxy Andromeda (HELGA)

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