The dust content of high-<i>z</i>submillimeter galaxies revealed by<i>Herschel</i>

Santini, P.; Maiolino, R.; Magnelli, B.; Silva, L.; Grazian, A.; Altiéri, B.; Andreani, P.; Aussel, H.; Berta, S.; Bongiovanni, Á.; Brisbin, D.; Calura, F.; Cava, A.; Cepa, J.; Cimatti, A.; Daddi, E.; Dannerbauer, H.; Domínguez-Sánchez, H.; Elbaz, D.; Fontana, A.; Schreiber, N. Förster; Genzel, R.; Granato, G. L.; Gruppioni, C.; Lutz, D.; Magdis, G.; Magliocchetti, M.; Matteuccí, F.; Nordon, R.; García, I. Pérez; Poglitsch, A.; Popesso, P.; Pozzi, F.; Riguccini, L.; Rodighiero, G.; Saintonge, A.; Sánchez‐Portal, M.; Shao, Li; Sturm, E.; Tacconi, L. J.; Valtchanov, I.

doi:10.1051/0004-6361/201014748

Cited by 88 publications

(110 citation statements)

References 54 publications

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“…The stellar masses for these galaxies and with the more topheavy IMFs are in good agreement with observations of galaxies at high-z. Santini et al (2010) and Michałowski et al (2010a) shows that, out of a sample of high-z submillimetre galaxies and local ULIRGs, most of these are assembled at stellar masses around 10 11 M and have dust masses of 10 8−10 M .…”

Section: Discussionmentioning

confidence: 99%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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Aims. The aim is to elucidate the astrophysical conditions required for generating large amounts of dust in massive starburst galaxies at high redshift. Methods. We have developed a numerical galactic chemical evolution model. The model is constructed such that the effect of a wide range of parameters can be investigated. It takes into account results from stellar evolution models, a differentiation between diverse types of core collapse supernovae (CCSN), and the contribution of asymptotic giant branch (AGB) stars in the mass range 3-8 M . We consider the lifetime-dependent yield injection into the interstellar medium (ISM) by all sources, and dust destruction due to supernova (SN) shocks in the ISM. We ascertain the temporal progression of the dust mass and the dust-to-gas and dust-to-metal mass ratios, as well as other physical properties of a galaxy, and study their dependence on the mass of the galaxy, the initial mass function (IMF), dust production efficiencies, and dust destruction in the ISM. Results. The amount of dust and the physical properties of a galaxy strongly depend on the initial gas mass available. Overall, while the total amount of dust produced increases with galaxy mass, the detailed outcome depends on the SN dust production efficiency, the IMF, and the strength of dust destruction in the ISM. Dust masses are higher for IMFs biased towards higher stellar masses, even though these IMFs are more strongly affected by dust destruction in the ISM. The sensitivity to the IMF increases as the mass of the galaxy decreases. SNe are primarily responsible for a significant enrichment with dust at early epochs (<200 Myr). Dust production with a dominant contribution by AGB stars is found to be insufficient to account for dust masses in excess of 10 8 M within 400 Myr after starburst. Conclusions. We find that galaxies with initial gas masses between 1-5 × 10 11 M are massive enough to enable production of dust masses >10 8 M . Our preferred scenario is dominated by SN dust production in combination with top-heavy IMFs and moderate dust destruction in the ISM.

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Section: Discussionmentioning

confidence: 99%

Genesis and evolution of dust in galaxies in the early Universe

Gall

Andersen

Hjorth

2011

A&A

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“…For instance, it has been claimed that ULIRGs show systematically lower metallicities than expected from the mass-metallicity relation (Rupke et al 2008;Caputi et al 2008); but this may simply be a consequence of the fact that in these heavily obscured systems the optical metallicity tracers only probe the outer, less enriched regions. Santini et al (2010) reported that the high dust mass measured in these galaxies disagrees with the metallicity inferred from the optical metallicity diagnostics, suggesting that the optical spectral indices are likely unreliable in these dusty systems.…”

Section: Introductionmentioning

confidence: 90%

ALMA reveals a chemically evolved submillimeter galaxy atz= 4.76

Nagao

Maiolino

Breuck

et al. 2012

A&A

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101

138

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The chemical properties of high-z galaxies provide important information for constraining galaxy evolutionary scenarios. However, widely used metallicity diagnostics based on rest-frame optical emission lines are unusable for heavily dust-enshrouded galaxies (such as submillimeter galaxies; SMGs), especially at z > 3. Here we focus on the flux ratio of the far-infrared fine-structure emis- .008. This is the first measurement of the [N ii]/[C ii]flux ratio in high-z galaxies, and the inferred flux ratio is similar to the ratio observed in the nearby universe (∼0.02−0.07). The velocity-integrated flux ratio and photoionization models suggest that the metallicity in this SMG is consistent with solar, implying that the chemical evolution has progressed very rapidly in this system at z = 4.76. We also obtain a tight upper limit on the CO(12−11) transition, which translates into CO(12−11)/CO(2−1) < 3.8 (3σ). This suggests that the molecular gas clouds in LESS J033229.4-275619 are not significantly affected by the radiation field emitted by the AGN in this system.

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“…Herschel is also probing the coldest phases of dust in high-z galaxies. Santini et al (2010) recently found that the dust content of their high-z submillimeter galaxies appears to be far higher than that expected from their metallicity, probably revealing different dust properties or dust growth mechanism in those environments. We caution the accuracy of dust masses estimates made without rest-frame submm observations.…”

Section: Conditions For Submm Excessmentioning

confidence: 97%

Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz

Madden

Galliano

et al. 2011

A&A

200

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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The dust content of high-zsubmillimeter galaxies revealed byHerschel

Cited by 88 publications

References 54 publications

Genesis and evolution of dust in galaxies in the early Universe

Genesis and evolution of dust in galaxies in the early Universe

ALMA reveals a chemically evolved submillimeter galaxy atz= 4.76

Probing the dust properties of galaxies up to submillimetre wavelengths

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