Rowan J. Smith
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View article: The role of turbulence in setting the phase of the ISM and implications for the star formation rate
The role of turbulence in setting the phase of the ISM and implications for the star formation rate Open
What regulates star formation in different regions of the Galaxy is still debated and especially the role of turbulence is not fully understood. In this work, we explore the link between star formation, turbulence and the thermal state of …
View article: PHANGS-JWST: the largest extragalactic molecular cloud catalog traced by polycyclic aromatic hydrocarbon emission
PHANGS-JWST: the largest extragalactic molecular cloud catalog traced by polycyclic aromatic hydrocarbon emission Open
High-resolution JWST images of nearby spiral galaxies reveal polycyclic aromatic hydrocarbon (PAH) emission structures that trace molecular gas, including CO-dark regions. We identify ISM cloud structures in PHANGS-JWST 7.7 $μ$m PAH maps f…
View article: Azimuthal offsets in spiral arms of nearby galaxies
Azimuthal offsets in spiral arms of nearby galaxies Open
Spiral arms play a central role in disc galaxies, but their dynamical nature remains a long-standing open question. Azimuthal offsets between molecular gas and star formation are expected if gas crosses spiral arms, as predicted by quasi-s…
View article: The dynamical impact of cosmic rays in the Rhea magnetohydrodynamic simulations
The dynamical impact of cosmic rays in the Rhea magnetohydrodynamic simulations Open
This study explores the dynamical impact of cosmic rays (CRs) in Milky Way-like galaxies using the Rhea simulation suite. Cosmic rays, with their substantial energy density, influence the interstellar medium (ISM) by supporting galactic wi…
View article: Reconciling extragalactic star formation efficiencies with theory: Insights from PHANGS
Reconciling extragalactic star formation efficiencies with theory: Insights from PHANGS Open
New extragalactic measurements of the cloud population-averaged star formation efficiency per free-fall time, ϵ ff , from PHANGS show little sign of a theoretically predicted dependence on the gas virial level and weak variation with cloud…
View article: Origin of the IRAS Vela Shell: New Insights from 3D Dust Mapping
Origin of the IRAS Vela Shell: New Insights from 3D Dust Mapping Open
The IRAS Vela Shell (IVS) is a structure of enhanced far-IR (FIR) emission located toward the Gum Nebula, a prominent region of H α emission in the local Milky Way shaped by various galactic stellar feedback over the past several million y…
View article: Simulating nearby disc galaxies on the main star formation sequence
Simulating nearby disc galaxies on the main star formation sequence Open
Recent hydrodynamical simulations of isolated barred disc galaxies have suggested a structural change in the distribution of the interstellar medium (ISM) around a stellar mass M * of 10 10 M ⊙ . In the higher-mass regime ( M ∗ ≥ 10 10 M ⊙…
View article: On the relation between magnetic field strength and gas density in the interstellar medium: a multiscale analysis
On the relation between magnetic field strength and gas density in the interstellar medium: a multiscale analysis Open
The relationship between magnetic field strength B and gas density n in the interstellar medium is of fundamental importance. We present and compare Bayesian analyses of the B–n relation for two comprehensive observational data sets: a Zee…
View article: The impact of spiral arms on the star formation life cycle
The impact of spiral arms on the star formation life cycle Open
The matter cycle between gas clouds and stars in galaxies plays a crucial role in regulating galaxy evolution through feedback mechanisms. In turn, the local and global galactic environments shape the interstellar medium and provide the in…
View article: Correction to: The persistence of high altitude non-equilibrium diffuse ionized gas in simulations of star-forming galaxies
Correction to: The persistence of high altitude non-equilibrium diffuse ionized gas in simulations of star-forming galaxies Open
View article: 3D CMZ. I. Central Molecular Zone Overview
3D CMZ. I. Central Molecular Zone Overview Open
The Central Molecular Zone (CMZ) is the largest reservoir of dense molecular gas in the Galaxy and is heavily obscured in the optical and near-IR. We present an overview of the far-IR dust continuum, where the molecular clouds are revealed…
View article: 3D CMZ. IV. Distinguishing Near versus Far Distances in the Galactic Center Using Spitzer and Herschel
3D CMZ. IV. Distinguishing Near versus Far Distances in the Galactic Center Using Spitzer and Herschel Open
A comprehensive 3D model of the central 300 pc of the Milky Way, the Central Molecular Zone (CMZ) is of fundamental importance in understanding energy cycles in galactic nuclei, since the 3D structure influences the location and intensity …
View article: 3D CMZ. II. Hierarchical Structure Analysis of the Central Molecular Zone
3D CMZ. II. Hierarchical Structure Analysis of the Central Molecular Zone Open
The Central Molecular Zone (CMZ) is the way station at the heart of our Milky Way Galaxy, connecting gas flowing in from Galactic scales with the central nucleus. Key open questions remain about its 3D structure, star formation properties,…
View article: 3D CMZ. III. Constraining the 3D Structure of the Central Molecular Zone via Molecular Line Emission and Absorption
3D CMZ. III. Constraining the 3D Structure of the Central Molecular Zone via Molecular Line Emission and Absorption Open
The Milky Way’s Central Molecular Zone (CMZ) is the largest concentration of dense molecular gas in the Galaxy, the structure of which is shaped by the complex interplay between Galactic-scale dynamics and extreme physical conditions. Unde…
View article: The width of Herschel filaments varies with distance (Corrigendum)
The width of Herschel filaments varies with distance (Corrigendum) Open
Corrigendum to "The width of Herschel filaments varies with distance."
View article: The role of magnetic fields in the formation of high-mass star-forming cores
The role of magnetic fields in the formation of high-mass star-forming cores Open
Magnetic fields are often invoked as playing a primary role in star formation and in the formation of high-mass stars. We investigate the effect of magnetic fields on the formation of high-mass cores using the three-dimensional smoothed pa…
View article: The Role of Magnetic Fields in the Formation of High-Mass Star-Forming Cores
The Role of Magnetic Fields in the Formation of High-Mass Star-Forming Cores Open
Magnetic fields are often invoked as playing a primary role in star formation and in the formation of high-mass stars. We investigate the effect of magnetic fields on the formation of high-mass cores using the 3-dimensional smoothed partic…
View article: Introducing the Rhea simulations of Milky-Way-like galaxies I: Effect of gravitational potential on morphology and star formation
Introducing the Rhea simulations of Milky-Way-like galaxies I: Effect of gravitational potential on morphology and star formation Open
The Milky Way is a complex ecosystem, for which we can obtain detailed observations probing the physical mechanisms determining the interstellar medium. For a detailed comparison with observations, and to provide theories for missing obser…
View article: The dynamical impact of cosmic rays in the Rhea magnetohydrodynamics simulations
The dynamical impact of cosmic rays in the Rhea magnetohydrodynamics simulations Open
This study explores the dynamical impact of cosmic rays (CRs) in Milky Way-like galaxies using the Rhea simulation suite. Cosmic rays, with their substantial energy density, influence the interstellar medium (ISM) by supporting galactic wi…
View article: Emergence of high-mass stars in complex fiber networks (EMERGE)
Emergence of high-mass stars in complex fiber networks (EMERGE) Open
Context . Identified as parsec-size, gas clumps at the junction of multiple filaments, hub-filament systems (HFS) play a crucial role during the formation of young clusters and high-mass stars. These HFS still appear to be detached from mo…
View article: Do stars still form in molecular gas within CO-dark dwarf galaxies?
Do stars still form in molecular gas within CO-dark dwarf galaxies? Open
In the Milky Way and other main-sequence galaxies, stars form exclusively in molecular gas, which is traced by CO emission. However, low-metallicity dwarf galaxies are often ‘CO-dark’ in the sense that CO emission is not observable even at…
View article: Evolutionary growth of molecular clouds as traced by their infrared bright fraction
Evolutionary growth of molecular clouds as traced by their infrared bright fraction Open
Understanding how stars form, evolve, and impact molecular clouds is key to understanding why star formation is such an inefficient process globally. In this paper, we use the infrared bright fraction, $f_\text{IRB}$ (the fraction of a giv…
View article: CO Isotopologue-derived Molecular Gas Conditions and CO-to-H<sub>2</sub> Conversion Factors in M51
CO Isotopologue-derived Molecular Gas Conditions and CO-to-H<sub>2</sub> Conversion Factors in M51 Open
Over the past decade, several millimeter interferometer programs have mapped the nearby star-forming galaxy M51 at a spatial resolution of ≤170 pc. This study combines observations from three major programs: the PdBI Arcsecond Whirlpool Su…
View article: Testing kinematic distances under a realistic Galactic potential
Testing kinematic distances under a realistic Galactic potential Open
Context . Obtaining reliable distance estimates to gas clouds within the Milky Way is challenging in the absence of certain tracers. The kinematic distance approach has been used as an alternative, and it is derived from the assumption of …
View article: Emergence of high-mass stars in complex fiber networks (EMERGE) V. From filaments to spheroids: the origin of the hub-filament systems
Emergence of high-mass stars in complex fiber networks (EMERGE) V. From filaments to spheroids: the origin of the hub-filament systems Open
Identified as parsec-size, gas clumps at the junction of multiple filaments, hub-filament systems (HFS) play a crucial role during the formation of young clusters and high-mass stars. These HFS appear nevertheless to be detached from most …
View article: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium Open
We have investigated the possibility of molecular cloud formation via the collision-induced magnetic reconnection (CMR) mechanism of the cold neutral medium (CNM). Two atomic gas clouds with conditions typical of the CNM were set to collid…
View article: CO isotopologue-derived molecular gas conditions and CO-to-H$_2$ conversion factors in M51
CO isotopologue-derived molecular gas conditions and CO-to-H$_2$ conversion factors in M51 Open
Over the past decade, several millimeter interferometer programs have mapped the nearby star-forming galaxy M51 at a spatial resolution of ${\le}170$ pc. This study combines observations from three major programs: the PdBI Arcsecond Whirlp…
View article: 3-D CMZ II: Hierarchical Structure Analysis of the Central Molecular Zone
3-D CMZ II: Hierarchical Structure Analysis of the Central Molecular Zone Open
The Central Molecular Zone (CMZ) is the way station at the heart of our Milky Way Galaxy, connecting gas flowing in from Galactic scales with the central nucleus. Key open questions remain about its 3-D structure, star formation properties…
View article: 3-D CMZ IV: Distinguishing Near vs. Far Distances in the Galactic Center Using Spitzer and Herschel
3-D CMZ IV: Distinguishing Near vs. Far Distances in the Galactic Center Using Spitzer and Herschel Open
A comprehensive 3-D model of the central 300 pc of the Milky Way, the Central Molecular Zone (CMZ) is of fundamental importance in understanding energy cycles in galactic nuclei, since the 3-D structure influences the location and intensit…
View article: 3-D CMZ I: Central Molecular Zone Overview
3-D CMZ I: Central Molecular Zone Overview Open
The Central Molecular Zone (CMZ) is the largest reservoir of dense molecular gas in the Galaxy and is heavily obscured in the optical and near-IR. We present an overview of the far-IR dust continuum, where the molecular clouds are revealed…