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Molecular Gas and the Star-Formation Process on Cloud Scales in Nearby Galaxies
E Schinnerer, AK Leroy - Annual Review of Astronomy and …, 2024 - annualreviews.org
Observations that resolve nearby galaxies into individual regions across multiple phases of
the gas–star formation feedback “matter cycle” have provided a sharp new view of molecular …
the gas–star formation feedback “matter cycle” have provided a sharp new view of molecular …
Atomic hydrogen in the milky way: a step** stone in the evolution of galaxies
Atomic hydrogen (Hi) is a critical step** stone in the gas evolution cycle of the interstellar
medium (ISM) of the Milky Way. Hi traces both the cold, premolecular state before star …
medium (ISM) of the Milky Way. Hi traces both the cold, premolecular state before star …
PHANGS–ALMA: Arcsecond CO (2–1) Imaging of Nearby Star-forming Galaxies
AK Leroy, E Schinnerer, A Hughes… - The Astrophysical …, 2021 - iopscience.iop.org
We present PHANGS–ALMA, the first survey to map CO J= 2→ 1 line emission at∼ 1''∼ 100
pc spatial resolution from a representative sample of 90 nearby (d≲ 20 Mpc) galaxies that lie …
pc spatial resolution from a representative sample of 90 nearby (d≲ 20 Mpc) galaxies that lie …
FIRE-2 simulations: physics versus numerics in galaxy formation
ABSTRACT The Feedback In Realistic Environments (FIRE) project explores feedback in
cosmological galaxy formation simulations. Previous FIRE simulations used an identical …
cosmological galaxy formation simulations. Previous FIRE simulations used an identical …
What causes the formation of discs and end of bursty star formation?
As they grow, galaxies can transition from irregular/spheroidal with 'bursty'star formation
histories (SFHs), to discy with smooth SFHs. But even in simulations, the direct physical …
histories (SFHs), to discy with smooth SFHs. But even in simulations, the direct physical …
Pressure-regulated, feedback-modulated star formation in disk galaxies
The star formation rate (SFR) in galactic disks depends on both the quantity of the available
interstellar medium (ISM) gas and its physical state. Conversely, the ISM's physical state …
interstellar medium (ISM) gas and its physical state. Conversely, the ISM's physical state …
Cloud-scale molecular gas properties in 15 nearby galaxies
We measure the velocity dispersion, σ, and surface density, Σ, of the molecular gas in
nearby galaxies from CO spectral line cubes with spatial resolution 45–120 pc, matched to …
nearby galaxies from CO spectral line cubes with spatial resolution 45–120 pc, matched to …
IllustrisTNG in the HSC-SSP: image data release and the major role of mini mergers as drivers of asymmetry and star formation
At fixed galaxy stellar mass, there is a clear observational connection between structural
asymmetry and offset from the star-forming main sequence, ΔSFMS. Herein, we use the …
asymmetry and offset from the star-forming main sequence, ΔSFMS. Herein, we use the …
Theoretical challenges in galaxy formation
Numerical simulations have become a major tool for understanding galaxy formation and
evolution. Over the decades the field has made significant progress. It is now possible to …
evolution. Over the decades the field has made significant progress. It is now possible to …
PDRs4All-III. JWST's NIR spectroscopic view of the Orion Bar
Context. JWST has taken the sharpest and most sensitive infrared (IR) spectral imaging
observations ever of the Orion Bar photodis-sociation region (PDR), which is part of the …
observations ever of the Orion Bar photodis-sociation region (PDR), which is part of the …