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

Olsen, Karen P.; Greve, T. R.; Narayanan, Desika; Thompson, Raymond H.; Davé, Romeel; Rios, Luis Niebla; Stawinski, Stephanie M. Urbano

doi:10.3847/1538-4357/aa86b4

Cited by 103 publications

(102 citation statements)

References 111 publications

(221 reference statements)

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“…The top row shows face-on maps of total gas column density, H 2 column density, density weighted temperature, metal surface mass density, dust surface mass density, and stellar mass surface density in a 5kpc cube surrounding the galaxy. Similarly, face-on images for nine IR lines and twelve of the nebular lines listed in works that have modelled these systems Pallottini et al 2017a,b;Olsen et al 2017;Vallini et al 2015), while [OIII] 88.33µm is picking out individual star forming regions (see also Katz et al 2017;Moriwaki et al 2018). In these images, we are showing the emergent emission rather than the intrinsic emission as in practice, these lines are observed against and modulated by the background CMB (Chatzikos et al 2013;Lagache et al 2018).…”

Section: Results -General Propertiesmentioning

confidence: 51%

Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST

Katz

Galligan

Kimm

et al. 2019

Monthly Notices of the Royal Astronomical Society

110

133

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Infrared and nebular lines provide some of our best probes of the physics regulating the properties of the interstellar medium (ISM) at high-redshift. However, interpreting the physical conditions of high-redshift galaxies directly from emission lines remains complicated due to inhomogeneities in temperature, density, metallicity, ionisation parameter, and spectral hardness. We present a new suite of cosmological, radiation-hydrodynamics simulations, each centred on a massive Lyman-break galaxy that resolves such properties in an inhomogeneous ISM. Many of the simulated systems exhibit transient but well defined gaseous disks that appear as velocity gradients in [CII] 157.6µm emission. Spatial and spectral offsets between [CII] 157.6µm and [OIII] 88.33µm are common, but not ubiquitous, as each line probes a different phase of the ISM. These systems fall on the local [CII]-SFR relation, consistent with newer observations that question previously observed [CII] 157.6µm deficits. Our galaxies are consistent with the nebular line properties of observed z ∼ 2 − 3 galaxies and reproduce offsets on the BPT and mass-excitation diagrams compared to local galaxies due to higher star formation rate (SFR), excitation, and specific-SFR, as well as harder spectra from young, metal-poor binaries. We predict that local calibrations between Hα and [OII] 3727Å luminosity and galaxy SFR apply up to z > 10, as do the local relations between certain strong line diagnostics (R23 and [OIII] 5007Å/Hβ) and galaxy metallicity. Our new simulations are well suited to interpret the observations of line emission from current (ALMA and HST) and upcoming facilities (JWST and ngVLA).

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Section: Results -General Propertiesmentioning

confidence: 51%

Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST

Katz

Galligan

Kimm

et al. 2019

Monthly Notices of the Royal Astronomical Society

110

133

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“…Our model galaxy suite is generated from the MUFASA-zoom simulation series, which are zoomed galaxies from the MUFASA cosmological simulation (Davé et al , 2017a. This zoom simulation methodology has been described in detail in Olsen et al (2017), Narayanan et al (2018), Abruzzo et al (2018), and Privon et al (2018). We therefore refer the reader to those works for details, and summarize the salient points here.…”

Section: Cosmological Zoom Galaxy Formation Simulationsmentioning

confidence: 99%

A Theory for the Variation of Dust Attenuation Laws in Galaxies

Narayanan

Conroy

Davé

et al. 2018

ApJ

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132

173

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In this paper, we provide a physical model for the origin of variations in the shapes and bump strengths of dust attenuation laws in galaxies by combining a large suite of cosmological "zoom-in" galaxy formation simulations with 3D Monte Carlo dust radiative transfer calculations. We model galaxies over 3 orders of magnitude in stellar mass, ranging from Milky Way like systems through massive galaxies at high-redshift. Critically, for these calculations we employ a constant underlying dust extinction law in all cases, and examine how the role of geometry and radiative transfer effects impact the resultant attenuation curves. Our main results follow. Despite our usage of a constant dust extinction curve, we find dramatic variations in the derived attenuation laws. The slopes of normalized attenuation laws depend primarily on the complexities of star-dust geometry. Increasing fractions of unobscured young stars flatten normalized curves, while increasing fractions of unobscured old stars steepen curves. Similar to the slopes of our model attenuation laws, we find dramatic variation in the 2175Å ultraviolet (UV) bump strength, including a subset of curves with little to no bump. These bump strengths are primarily influenced by the fraction of unobscured O and B stars in our model, with the impact of scattered light having only a secondary effect. Taken together, these results lead to a natural relationship between the attenuation curve slope and 2175Å bump strength. Finally, we apply these results to a 25 Mpc/h box cosmological hydrodynamic simulation in order to model the expected dispersion in attenuation laws at integer redshifts from z = 0 − 6. A significant dispersion is expected at low redshifts, and decreases toward z = 6. We provide tabulated results for the best fit median attenuation curve at all redshifts.

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“…For example, some simulations calculate abundances of specific elements on the fly, whereas others only contain one number for the metallicity and an abundance table must be adopted. Including several elements separately instead of a fixed abundance table, has been shown to make a significant difference for modeling of the fine-structure [C II] line [124].…”

Section: From Cloud To Galaxy Scale Simulationsmentioning

confidence: 99%

Challenges and Techniques for Simulating Line Emission

et al. 2018

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Modeling emission lines from the millimeter to the UV and producing synthetic spectra is crucial for a good understanding of observations, yet it is an art filled with hazards. This is the proceedings of "Walking the Line", a 3-day conference held in 2018 that brought together scientists working on different aspects of emission line simulations, in order to share knowledge and discuss the methodology. Emission lines across the spectrum from the millimeter to the UV were discussed, with most of the focus on the interstellar medium, but also some topics on the circumgalactic medium. The most important quality of a useful model is a good synergy with observations and experiments. Challenges in simulating line emission are identified, some of which are already being worked upon, and others that must be addressed in the future for models to agree with observations. Recent advances in several areas aiming at achieving that synergy are summarized here, from micro-physical to galactic and circum-galactic scale.2 of 29 us to characterize the mass, composition, and chemical state of the ISM, as well as to trace galaxy properties such as star formation rate (SFR), metallicity and dynamics. For example, the emission from major cooling lines, such as Hα or [C II], is sensitive to the physical conditions (densities, radiation field) and dynamics of the ISM. In addition, emission lines work on all physical scales, from galaxy dynamics and inflows to turbulent and collapse motions in star-forming clouds and cores. By systematically comparing spectral-line signatures of different physical models, one can correctly identify the physical processes occurring in these regions. Furthermore, the emission from ionized interstellar gas contains particularly valuable information about the nature of the ionizing radiation sources in a galaxy. In fact, prominent optical emission lines are routinely used to estimate whether ionization is dominated by young massive stars (tracing SFR), an AGN or evolved, post-asymptotic giant branch (post-AGB) stars. Three of the most widely used line-ratio diagnostic "BPT" diagrams 1 , relate the [OIII]/Hβ ratio to the [NII]/Hα, [SII]/Hα and [OI]/Hα ratios. These diagrams have proven useful in identifying the nature of the ionizing radiation in large samples of galaxies in the local Universe [2,3]. Complementary to line emission are the observations of absorption lines of the circumgalactic medium (CGM), which can give key information on the history of the feedback, in terms of chemical, ionization, and thermodynamical state of the outflowing/inflowing gas, that regulates the star formation process. Gas kinematics, from both emission and absorption, give information about large scale gas flows. Thus galactic outflows, from active galactic nuclei (AGN) and starbursts, can be combined with CGM absorption line observations, to study the star formation history, AGN activity history, and feedback processes that regulate both the evolution of the galaxy and its environment.Looking back on the past three decades, t...

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

Cited by 103 publications

References 111 publications

Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST

Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST

A Theory for the Variation of Dust Attenuation Laws in Galaxies

Challenges and Techniques for Simulating Line Emission

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