Predicting FIR lines from simulated galaxies

Lupi, Alessandro; Pallottini, Andrea; Ferrara, Andrea; Bovino, S.; Carniani, Stefano; Vallini, L.

doi:10.1093/mnras/staa1842

Cited by 43 publications

(37 citation statements)

References 83 publications

(131 reference statements)

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“…Consistent with our earlier work (Katz et al 2019b ), we find that the [C II ] emission follows the densest gas structures in the galaxy while [O III ] exhibits a different morphology, more coincident with the young star forming regions and mildly lower density gas (see also Pallottini et al 2019b ;Lupi et al 2020 ). With a higher ionization potential and lower critical density compared to C + , such behaviour is expected for O ++ .…”

Section: R E S U Lt Ssupporting

confidence: 90%

“…Like wise, the fe w galaxies simulated in Katz et al ( 2019b ) seem to fall closer to the local [C II ]-SFR relation than those in Pallottini et al ( 2017Pallottini et al ( , 2019a. The origin of these discrepancies can in part be due to g alaxy-to-g alaxy v ariance, in addition to dif ferences in modelling techniques, which are well established to be far from straightforward (Olsen et al 2018 ;Lupi et al 2020 ). Nev ertheless, there hav e been many situations where simulations have agreed on emission-line properties of high-redshift galaxies and provide deep insights into or predictions of the early Univ erse.…”

mentioning

confidence: 78%

“…Furthermore, we employ a constant temperature assumption to account for shocks and SN feedback that are present in the simulation rather than allow CLOUDY to compute the photoionizationequilibrium temperature of the gas. Such an assumption can lead to different line luminosities as Lupi et al ( 2020 ) showed that a variable temperature CLOUDY model can increase the [O III ]/[C II ] ratio by a factor of two. One could also choose a different shape for the input SED than used in this work which can impact both the ionization states of individuals as well as the electron density.…”

Section: Caveatsmentioning

confidence: 99%

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The nature of high [O iii]88 μ m/[C ii]158 μm galaxies in the epoch of reionization: Low carbon abundance and a top-heavy IMF?

Katz

Rosdahl

Kimm

et al. 2022

Monthly Notices of the Royal Astronomical Society

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ALMA observations of z > 6 galaxies have revealed abnormally high [OIII]88μm/[CII]158μm ratios and [CII]158μm deficits compared to local galaxies. The origin of this behaviour is unknown. Numerous solutions have been proposed including differences in C and O abundance ratios, observational bias, and differences in ISM properties, including ionisation parameter, gas density, or photodissociation region (PDR) covering fraction. In order to elucidate the underlying physics that drives this high-redshift phenomenon, we employ SPHINX20, a state-of-the-art, cosmological radiation-hydrodynamics simulation, that resolves detailed ISM properties of thousands of galaxies in the epoch of reionization which has been post-processed with CLOUDY to predict emission lines. We find that the observed z > 6 [OIII]88μm-SFR and [CII]158μm-SFR relations can only be reproduced when the C/O abundance ratio is ∼8 × lower than Solar and the total metal production is ∼4 × higher than that of a Kroupa IMF. This implies that high-redshift galaxies are potentially primarily enriched by low-metallicity core-collapse supernovae with a more top-heavy IMF. As AGB stars and type-Ia supernova begin to contribute to the galaxy metallicity, both the [CII]158μm-SFR and [CII]158μm luminosity functions are predicted to converge to observed values at z ∼ 4.5. While we demonstrate that ionisation parameter, LyC escape fraction, ISM gas density, and CMB attenuation all drive galaxies towards higher [OIII]88μm/[CII]158μm, observed values at z > 6 can only be reproduced with substantially lower C/O abundances compared to Solar. The combination of [CII]158μm and [OIII]88μm can be used to predict the values of ionisation parameter, ISM gas density, and LyC escape fraction and we provide estimates of these quantities for nine observed z > 6 galaxies. Finally, we demonstrate that [OI]63μm can be used as a replacement for [CII]158μm in high-redshift galaxies where [CII]158μm is unobserved and argue that more observation time should be used to target [OI]63μm at z > 6. Future simulations will be needed to self-consistently address the numerous uncertainties surrounding a varying IMF at high redshift and the associated metal returns.

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Section: R E S U Lt Ssupporting

confidence: 90%

mentioning

confidence: 78%

Section: Caveatsmentioning

confidence: 99%

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The nature of high [O iii]88 μ m/[C ii]158 μm galaxies in the epoch of reionization: Low carbon abundance and a top-heavy IMF?

Katz

Rosdahl

Kimm

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Following cooling from individual metal species can modify the thermodynamics of the low density ISM (Gnedin & Hollon 2012;Capelo et al 2018), since the cooling function typically changes by a factor < ∼ 2 (Bovino et al 2016). Such effect might be important to correctly compute emission lines strengths, particularly for some lines (Lupi et al 2020).…”

Section: Gas Thermodynamicsmentioning

confidence: 99%

A survey of high-$z$ galaxies: SERRA simulations

Pallottini,

Ferrara,

Gallerani

et al. 2022

Preprint

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We introduce serra, a suite of zoom-in high-resolution (∼ 10 pc) cosmological simulations including non-equilibrium chemistry and on-the-fly radiative transfer. The outputs are post-processed to derive galaxy UV+FIR continuum and emission line properties. Results are compared with available multi-wavelength data to constrain the physical properties (e.g., star formation rates, stellar/gas/dust mass, metallicity) of high-redshift 6 < ∼ z < ∼ 15 galaxies. This flagship paper focuses on the z = 7.7 sub-sample, including 207 galaxies with stellar mass 10 7 M < ∼ M < ∼ 5×10 10 M , and specific star formation ranging from sSFR ∼ 100 Gyr −1 in young, low-mass galaxies to ∼ 10 Gyr −1 for older, massive ones. At this redshift, serra galaxies are typically bursty, i.e. they are located above the Schmidt-Kennicutt relation by a factor κ s = 3.03 +4.9 −1.8 , consistent with recent findings for [O III] and [C II] emitters at high-z. They also show relatively large IRX = L FIR /L UV values as a result of their compact/clumpy morphology effectively blocking the stellar UV luminosity. Note that this conclusion might be affected by insufficient spatial resolution at the molecular cloud level. We confirm that early galaxies lie on the standard [C II]−SFR relation; their observed L [OIII] /L [CII] 1−10 ratios are reproduced without the need of a top-heavy IMF and/or anomalous C/O abundances. [O I] line intensities are similar to local ones, making ALMA high-z detections challenging but feasible (∼ 6 hr for an SFR of 50 M yr −1 ).

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“…The version used for this work includes the common cooling and star formation models described in Paper II while stellar feedback is based on the mechanical feedback model described in Hopkins et al (2018), i.e., both kinetic and thermal energy are distributed among gas cells lying within each star particle kernel according to the evolutionary stage of the SN blast wave (energy or momentum conserving). The SN rate used in this work is described by a piecewise function, where we assume the decaying power-law fit in Lupi et al (2020) for star particles older than 5.089 Myr, and a constant rate equal to the power-law maximum value for younger stars, aimed at modeling early feedback by massive stars. For consistency, the integrated number of SN events is normalized to ensure one SN per 91 M e , while the injected energy is set to 5 × 10 51 erg/SN in order to reproduce the desired stellar mass at z = 4.…”

Section: Gizmomentioning

confidence: 99%

The AGORA High-resolution Galaxy Simulations Comparison Project. III. Cosmological Zoom-in Simulation of a Milky Way–mass Halo

Roca-Fàbrega¹,

Kim

Hausammann

et al. 2021

ApJ

Self Cite

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We present a suite of high-resolution cosmological zoom-in simulations to z = 4 of a 10 12 M e halo at z = 0, obtained using seven contemporary astrophysical simulation codes (ART-I, ENZO, RAMSES, CHANGA, GADGET-3, GEAR, and GIZMO) widely used in the numerical galaxy formation community. The physics prescriptions for gas cooling and heating and star formation are the same as the ones used in our previous Assembling Galaxies of Resolved Anatomy (AGORA) disk comparison but now account for the effects of cosmological processes such as the expansion of the universe, intergalactic gas inflow, and the cosmic ultraviolet background radiation emitted by massive stars and quasars. In this work, we introduce the most careful comparison yet of galaxy formation simulations run by different code groups, together with a series of four calibration steps each of which is designed to reduce the number of tunable simulation parameters adopted in the final run. In the first two steps, we methodically calibrate the gas physics, such as cooling and heating, in simulations without star formation. In the third step, we seek agreement on the total stellar mass produced with the common star formation prescription used in the AGORA disk comparison, in stellar-feedback-free simulations. In the last calibration step, we activate stellar feedback, where each code group is asked to set the feedback prescription to as close to the most widely used one in its code community as possible, while aiming for convergence in the stellar mass at z = 4 to the values predicted by semiempirical models. After all the participating code groups successfully complete the calibration steps, we achieve a suite of cosmological simulations with similar mass assembly histories down to z = 4. With numerical accuracy that resolves the internal structure of a target halo (100 physical pc at z = 4), we find that the codes overall agree well with one another, e.g., in gas and stellar properties, but also show differences, e.g., in circumgalactic medium (CGM) properties. We argue that, if adequately tested in accordance with our proposed calibration steps and common parameters, high-resolution cosmological zoom-in simulations can have robust and reproducible results. New code groups are invited to join and enrich this comparison by generating equivalent models or to test the code's compatibility on their own, by adopting the common initial conditions, the common easy-to-implement physics package, and the proposed calibration steps. Further analyses of the zoom-in

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Predicting FIR lines from simulated galaxies

Cited by 43 publications

References 83 publications

The nature of high [O iii]88 μ m/[C ii]158 μm galaxies in the epoch of reionization: Low carbon abundance and a top-heavy IMF?

The nature of high [O iii]88 μ m/[C ii]158 μm galaxies in the epoch of reionization: Low carbon abundance and a top-heavy IMF?

A survey of high-$z$ galaxies: SERRA simulations

The AGORA High-resolution Galaxy Simulations Comparison Project. III. Cosmological Zoom-in Simulation of a Milky Way–mass Halo

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