A merger in the dusty,<i>z</i>= 7.5 galaxy A1689-zD1?

Knudsen, K. K.; Watson, Derrick G.; Frayer, David; Christensen, L.; Gallazzi, Anna; Michałowski, M. J.; Richard, Johan; Zavala, Jesús

doi:10.1093/mnras/stw3066

Cited by 94 publications

(102 citation statements)

References 69 publications

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“…These are predominantly LAEs with SFR < 30 M yr −1 , except for two notable high-SFR sources (Ouchi et al 2013;Inoue et al 2016). Since the majority of these sources have in fact only upper limit constraints on their [C II] luminosity (Kanekar et al 2013;Ota et al 2014;Maiolino et al 2015;Knudsen et al 2017) ) for local metal-poor dwarf galaxies (grey dashed line) and local starburst galaxies (grey dotted line); grey dashed and dotted lines, respectively, with the shaded regions indicating the r.m.s. scatter of these relations).…”

Section: Gas Kinetic Temperaturementioning

confidence: 99%

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Olsen

Greve

Narayanan

et al. 2017

ApJ

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Of the almost 40 star forming galaxies at z > ∼ 5 (not counting QSOs) observed in [C II] to date, nearly half are either very faint in [C II], or not detected at all, and fall well below expectations based on locally derived relations between star formation rate and [C II] luminosity. This has raised questions as to how reliable [C II] is as a tracer of star formation activity at these epochs and how factors such as metallicity might affect the [C II] emission. Combining cosmological zoom simulations of galaxies with SÍGAME (SImulator of GAlaxy Millimeter/submillimeter Emission) we have modeled the multi-phased interstellar medium ( We find that the [C II] emission is dominated by the diffuse ionized gas phase and molecular clouds, which on average contribute ∼ 66% and ∼ 27%, respectively. The molecular gas, which constitutes only ∼ 10% of the total gas mass is thus a more efficient emitter of [C II] than the ionized gas, which makes up ∼ 85% of the total gas mass. A principal component analysis shows that the [C II] luminosity correlates with the star formation activity of a galaxy as well as its average metallicity. The low metallicities of our simulations together with their low molecular gas mass fractions can account for their [C II]-faintness, and we suggest these factors may also be responsible for the [C II]-faint normal galaxies observed at these early epochs.

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Section: Gas Kinetic Temperaturementioning

confidence: 99%

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Olsen

Greve

Narayanan

et al. 2017

ApJ

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“…An exception to the above scenario is the puzzling case of A1689-zD1 (Watson et al 2015;Knudsen et al 2016), a z = 7.5 ± 0.2 gravitationally-lensed LBG for which the thermal dust emission has been detected by ALMA. The large FIR flux LFIR = (6.2 ± 0.8) × 10 10 L is indicative of considerable amounts of dust, consistent with a Milky Way dust-to-gas ratio.…”

Section: Motivationmentioning

confidence: 98%

The infrared-dark dust content of high redshift galaxies

Ferrara

Hirashita

Ouchi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present a theoretical model aimed at explaining the IRX-β relation for high redshift (z > ∼ 5) galaxies. Recent observations (Capak et al. 2015;Bouwens et al. 2016) have shown that early Lyman Break Galaxies, although characterized by a large UV attenuation (e.g. flat UV β slopes), show a striking FIR deficit, i.e. they are "infrareddark". This marked deviation from the local IRX-β relation can be explained by the larger molecular gas content of these systems. While dust in the diffuse ISM attains relatively high temperatures (T d 45 K for typical size a = 0.1µm; smaller grains can reach T d > ∼ 60 K), a sizable fraction of the dust mass is embedded in dense gas, and therefore remains cold. If confirmed, the FIR deficit might represent a novel, powerful indicator of the molecular content of high-z galaxies which can be used to pre-select candidates for follow-up deep CO observations. Thus, high-z CO line searches with ALMA might be much more promising than currently thought.

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“…In Figure 6 we summarise spectral and spatial offset from literature studies observing SMG (SFR>1000 M yr −1 ) z >4 De Breuck et al 2014) and primeval galaxies with SFR< 100 M yr −1 and z>4 (Mallery et al 2012;Carilli et al 2013;Williams et al 2014;Maiolino et al 2015;Willott et al 2015;Capak et al 2015;Knudsen et al 2016Knudsen et al , 2017Pentericci et al 2016;Inoue et al 2016;Bradač et al 2017). Since this work does not focus on determining a correlation between the offsets and the galaxy properties, we also report the positional offset revealed in in high-z galaxies whose redshifts have not been spectroscopically confirmed in the optical yet ).…”

Section: Spatial and Spectral Offsetsmentioning

confidence: 99%

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

Carniani

Maiolino

Pallottini

et al. 2017

A&A

187

237

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We present new ALMA observations of the [Oiii]88µm line and high angular resolution observations of the [Cii]158µm line in a normal star forming galaxy at z=7.1. Previous [Cii] observations of this galaxy had detected [Cii] emission consistent with the Lyα redshift but spatially slightly offset relative to the optical (UV-rest frame) emission. The new [Cii] observations reveal that the [Cii] emission is partly clumpy and partly diffuse on scales larger than about 1kpc.[Oiii] emission is also detected at high significance, offset relative to the optical counterpart in the same direction as the [Cii] clumps, but mostly not overlapping with the bulk of the [Cii] emission. The offset between different emission components (optical/UV and different far-IR tracers) is similar to that which is observed in much more powerful starbursts at high redshift. We show that the [Oiii] emitting clump cannot be explained in terms of diffuse gas excited by the UV radiation emitted by the optical galaxy, but it requires excitation by in-situ (slightly dust obscured) star formation, at a rate of about 7 M yr −1 . Within 20 kpc from the optical galaxy the ALMA data reveal two additional [Oiii] emitting systems, which must be star forming companions. We discuss that the complex properties revealed by ALMA in the z∼7.1 galaxy are consistent with expectations by recent models and cosmological simulations, in which differential dust extinction, differential excitation and different metal enrichment levels, associated with different subsystems assembling a galaxy, are responsible for the various appearance of the system when observed with distinct tracers.

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A merger in the dusty,z= 7.5 galaxy A1689-zD1?

Cited by 94 publications

References 69 publications

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

The infrared-dark dust content of high redshift galaxies

Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

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