The Far-infrared Emission of the First Massive Galaxies

Rossi, M. E. De; Rieke, G. H.; Shivaei, Irene; Lyu, Jianwei

doi:10.3847/1538-4357/aaebf8

Cited by 41 publications

(67 citation statements)

References 118 publications

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“…, where the uncertainty is only from fitting. Some recent works suggest that the relatively lowmetallicity galaxy template Haro 11 could provide a better fit to the IR SED of high-redshift quasar (Lyu et al 2016;De Rossi et al 2018). As a comparison, we also fit the observed data with the Haro 11 template and a AGN template from Lyu et al (2016), which results in a 1.6 times higher TIR luminosity, consistent with the systematic difference between the optically thin graybody model and Haro 11 template (De Rossi et al 2018).…”

Section: Continuum Emission and Infrared (Ir) Luminositysupporting

confidence: 82%

Far-infrared Properties of the Bright, Gravitationally Lensed Quasar J0439+1634 at z = 6.5

Yang

Venemans

Wang

et al. 2019

ApJ

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We present IRAM NOrthern Extended Millimeter Array, James Clerk Maxwell Telescope/Submillimetre Common-User Bolometer Array-2 and Very Large Array (VLA) observations of the most distant known gravitationally lensed quasar, J0439+1634 at z=6.5. We detect strong dust emission, [C II] 158 μm, [C I] 369 μm, [O I] 146 μm, CO(6-5), CO(7-6), CO(9-8), CO(10-9), H 2 O 3 1,2 −2 2,1 , and H 2 O 3 2,1 −3 1,2 lines, as well as a weak radio continuum. The strong [C II] line yields a systemic redshift of the host galaxy to be z=6.5188±0.0002. The magnification makes J0439+1634 the far-infrared (FIR) brightest quasar at z>6 known, with the brightest [C II] line yet detected at this redshift. The FIR luminosity is (3.4±0.2)×10 13 μ −1 L e , where μ ∼2.6-6.6 is the magnification of the host galaxy, estimated based on the lensing configuration from HST imaging. We estimate the dust mass to be (2.2±0.1)×10 9 μ −1 ☉ M. The CO spectral line energy distribution using four CO lines are best fit by a two-component model of the molecular gas excitation. The estimates of molecular gas mass derived from CO lines, and atomic carbon mass are consistent, in the range of (3.9-8.9)×10 10 μ −1 ☉ M. The [C II]/[C I], [C II]/CO, and [O I]/[C II] line luminosity ratios suggest a photodissociation region model with more than one component. The ratio of H 2 O 3 2,1 −3 1,2 line luminosity to L TIR is consistent with values in local and high-redshift ultra-/hyper-luminous infrared galaxies. The VLA observations reveal an unresolved radio continuum source, and indicate that J0439+1634 is a radio-quiet quasar with R=0.05-0.17.

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Section: Continuum Emission and Infrared (Ir) Luminositysupporting

confidence: 82%

Far-infrared Properties of the Bright, Gravitationally Lensed Quasar J0439+1634 at z = 6.5

Yang

Venemans

Wang

et al. 2019

ApJ

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“…De Rossi & Bromm (2017) analyses the role of silicate rich dust, that is expected from a Pop III dominated enrichment: the work shows that a warmer FIR SED can naturally arise because of the emission properties of silicates, that typically emit at higher wavelength with respect to the carbonaceous grains. Further, in De Rossi et al (2018) it is shown that a combination of silicate and small amount of carbonaceous grains can reproduce the SED observed in Haro 11, a local lowmetallicity starburst, thought to be an analogue of high-z galaxies: this entails that assuming a simplified dust models can possibly modify the properties inferred from high-z observations (cfr. Behrens et al 2018).…”

Section: Coupling With Gas and Dustmentioning

confidence: 98%

Deep into the structure of the first galaxies: SERRA views

Pallottini

Ferrara

Decataldo

et al. 2019

Monthly Notices of the Royal Astronomical Society

144

193

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We study the formation and evolution of a sample of Lyman Break Galaxies in the Epoch of Reionisation by using high-resolution (∼ 10 pc), cosmological zoom-in simulations part of the serra suite. In serra, we follow the interstellar medium (ISM) thermo-chemical non-equilibrium evolution, and perform on-the-fly radiative transfer of the interstellar radiation field (ISRF). The simulation outputs are post-processed to compute the emission of far infrared lines ([C II], [N II], and [O III]). At z = 8, the most massive galaxy, "Freesia", has an age t 409 Myr, stellar mass M 4.2 × 10 9 M , and a star formation rate SFR 11.5 M yr −1 , due to a recent burst. Freesia has two stellar components (A and B) separated by 2.5 kpc; other 11 galaxies are found within 56.9 ± 21.6 kpc. The mean ISRF in the Habing band is G = 7.9 G 0 and is spatially uniform; in contrast, the ionisation parameter is U = 2 +20 −2 × 10 −3 , and has a patchy distribution peaked at the location of star-forming sites. The resulting ionising escape fraction from Freesia is f esc 2%. While [C II] emission is extended (radius 1.54 kpc), [O III] is concentrated in Freesia-A (0.85 kpc), where the ratio Σ [OIII] /Σ [CII] 10. As many high-z galaxies, Freesia lies below the local [C II]-SFR relation. We show that this is the general consequence of a starburst phase (pushing the galaxy above the Kennicutt-Schmidt relation) which disrupts/photodissociates the emitting molecular clouds around star-forming sites. Metallicity has a sub-dominant impact on the amplitude of [C II]-SFR deviations.

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“…For example, does dust at z = 5.85 have the same absorptive properties as local Universe dust, even if it might have a very different origin and composition (e.g. de Rossi et al 2018)? What CO-to-H 2 conversion factor holds for Mambo-9?…”

Section: Mass Budget and Halo Mass Raritymentioning

confidence: 99%

Physical Characterization of an Unlensed, Dusty Star-forming Galaxy at z = 5.85

Casey

Zavala

Aravena

et al. 2019

ApJ

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We present a physical characterization of MM J100026.36+021527.9 (a.k.a. "Mambo-9"), a dusty star-forming galaxy (DSFG) at z = 5.850 ± 0.001. This is the highest redshift unlensed DSFG (and fourth most distant overall) found to-date, and is the first source identified in a new 2 mm blank-field map in the COSMOS field. Though identified in prior samples of DSFGs at 850µm-1.2 mm with unknown redshift, the detection at 2 mm prompted further follow-up as it indicated a much higher probability that the source was likely to sit at z > 4. Deep observations from the Atacama Large Millimeter and submillimeter Array (ALMA) presented here confirm the redshift through the secure detection of 12 CO(J =6→5) and p-H 2 O(2 1,1 →2 0,2 ). Mambo-9 is comprised of a pair of galaxies separated by 6 kpc with corresponding star-formation rates of 590 M yr −1 and 220 M yr −1 , total molecular hydrogen gas mass of (1.7±0.4)×10 11 M , dust mass of (1.3±0.3)×10 9 M and stellar mass 2 Casey et al.of (3.2 +1.0 −1.5 )×10 9 M . The total halo mass, (3.3±0.8)×10 12 M , is predicted to exceed > 10 15 M by z = 0. The system is undergoing a merger-driven starburst which will increase the stellar mass of the system tenfold in τ depl = 40 − 80 Myr, converting its large molecular gas reservoir (gas fraction of 96 +1 −2 %) into stars. Mambo-9 evaded firm spectroscopic identification for a decade, following a pattern that has emerged for some of the highest redshift DSFGs found. And yet, the systematic identification of unlensed DSFGs like Mambo-9 is key to measuring the global contribution of obscured star-formation to the star-formation rate density at z > ∼ 4, the formation of the first massive galaxies, and the formation of interstellar dust at early times ( < ∼ 1 Gyr).

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The Far-infrared Emission of the First Massive Galaxies

Cited by 41 publications

References 118 publications

Far-infrared Properties of the Bright, Gravitationally Lensed Quasar J0439+1634 at z = 6.5

Far-infrared Properties of the Bright, Gravitationally Lensed Quasar J0439+1634 at z = 6.5

Deep into the structure of the first galaxies: SERRA views

Physical Characterization of an Unlensed, Dusty Star-forming Galaxy at z = 5.85

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