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wiki:arxiv [2022/05/19 13:54] Cheng Li |
wiki:arxiv [2023/12/04 22:19] (current) Cheng Li |
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====== My arXiv notes (since 2020) ====== | ====== My arXiv notes (since 2020) ====== | ||
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+ | ==== Userful tools ==== | ||
+ | |||
+ | * RealSim-IFS: [[https://arxiv.org/abs/2205.15335|Realistic synthetic integral field spectroscopy with RealSim-IFS]] | ||
+ | * The RealSim-IFS Python code is publicly available here: https://github.com/cbottrell/realsim_ifs. | ||
+ | * how to referee papers? [[https://arxiv.org/abs/2205.14270|A Referee Primer for Early Career Astronomers]] | ||
+ | * | ||
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+ | ==== Review articles ==== | ||
+ | |||
+ | * [[https://arxiv.org/abs/2206.01548|Dust Formation in Astrophysical Environments: The Importance of Kinetics]] | ||
+ | * [[https://arxiv.org/abs/2206.03510|ALPINE: A Large Survey to Understand Teenage Galaxies]] | ||
+ | |||
+ | ===== 2023 ===== | ||
+ | |||
===== 2022 ===== | ===== 2022 ===== | ||
+ | |||
+ | ==== July ==== | ||
+ | |||
+ | * [[https://arxiv.org/abs/2207.05093|Turbulent Cold Flows Gave Birth to the First Quasars]] | ||
+ | |||
+ | ==== June ==== | ||
+ | |||
+ | * [[https://arxiv.org/abs/2206.04521|The stellar halo in Local Group Hestia simulations I. The in-situ component and the effect of mergers]] | ||
+ | * [[https://arxiv.org/abs/2206.04522|The stellar halo in Local Group Hestia simulations II. The accreted component]] | ||
+ | * [[https://arxiv.org/abs/2206.00681|Pressure-Regulated, Feedback-Modulated Star Formation In Disk Galaxies]] | ||
+ | * [[https://arxiv.org/abs/2206.00662|The Size-Mass Relation of Post-Starburst Galaxies in the Local Universe]]: post-starburst galaxies in SDSS are found to be smaller than quiescent galaxies of same masses. I'm wondering whether the same effect is seen also in the MaNGA-based sample. | ||
+ | * [[https://arxiv.org/abs/2206.00138|PASSAGES: The Large Millimeter Telescope and ALMA Observations of Extremely Luminous High Redshift Galaxies Identified by the Planck]] | ||
+ | * [[https://arxiv.org/abs/2206.00098|AGN Feedback in Groups and Clusters of Galaxies]] a review chapter | ||
+ | * [[https://arxiv.org/abs/2205.15672|Intrinsic shapes of Brightest Cluster Galaxies]] | ||
+ | * We show that these objects are strongly triaxial, with triaxiality parameters 0.39 ≤T≤ 0.72, have on average axis ratios <p(r)>= 0.84 and <q(r)>= 0.68, and are more spherical in the central regions but flatten out at large radii. | ||
+ | * Measured shapes in the outskirts agree well with the shapes found for simulated massive galaxies and their dark matter halos from both the IllustrisTNG and the Magneticum simulations, possibly probing the nature of dark matter. In contrast, both simulations fail to reproduce the observed inner regions of BCGs, producing too flattened objects. | ||
+ | * [[https://arxiv.org/abs/2205.15388|The UV luminosity functions of Bright z>8 Galaxies: Determination from ~0.41 deg2 of HST Observations along ~300 independent sightlines]] | ||
+ | * [[https://arxiv.org/abs/2205.15328|Impact of the cosmic background radiation on the initial mass function of metal-poor stars]] | ||
+ | * [[https://arxiv.org/abs/2205.15325|FIREbox: Simulating galaxies at high dynamic range in a cosmological volume]] | ||
==== May ==== | ==== May ==== | ||
+ | * [[https://arxiv.org/abs/2205.14858|Molecular Gas Structures traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey]] | ||
+ | * [[https://arxiv.org/abs/2205.12169|Investigating the Dominant Environmental Quenching Process in UVCANDELS/COSMOS Groups]] | ||
+ | * [[https://arxiv.org/abs/2205.14899|Close Major Merger Pairs at z=0: Bulge-to-Total Ratio and Star Formation Enhancement]] another paper by Cong Xu on S+S and S+E pairs | ||
+ | * [[https://arxiv.org/abs/2205.14417|The driving mode of shock-driven turbulence]] | ||
+ | * [[https://arxiv.org/abs/2205.14378|Possible Systematic Rotation in the Mature Stellar Population of a z=9.1 Galaxy]] | ||
+ | * [[https://arxiv.org/abs/2205.09087|Three-dimensional extinction maps: Inverting inter-calibrated extinction catalogues]] | ||
+ | * [[https://arxiv.org/abs/2205.09069|Influence of Magnetic Fields on the Gas Rotation in the Galaxy NGC6946]] | ||
+ | * magnetic field causes an ascending rotation curve in the outer radii of the galaxy, by ~7-14 km/s | ||
+ | * so magnetic field is not that important | ||
+ | * [[https://arxiv.org/abs/2205.08799|A sparse regression approach for populating dark matter halos and subhalos with galaxies]] (the Durrum team) | ||
+ | * interesting to compare with Yangyao's model | ||
+ | * [[https://arxiv.org/abs/2205.08554|Resolving the HI in Damped Lyman-α systems that power star-formation]] (Nature) | ||
+ | * [[https://arxiv.org/abs/2205.08552|A trail of dark matter-free galaxies from a bullet dwarf collision]] (Pieter van Dokkum, Nature) | ||
+ | * [[https://arxiv.org/abs/2205.08543|CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5≲z≲1.7 using Hα Emission Line Maps]] | ||
+ | * Ha surface density relative to continuum surface density within 1kpc drops from z~1 to z~0.5. The authors attribute this to inside-out quenching in the wake of inside-out growth. Since galaxy size grows, the lower value at lower redshift could be a result of gradient but not evolution. The 1kpc radius covers out to the disc at z~1 but it is only the central region at lower redshift. Need to check the size-mass relation at different redshifts. | ||
* [[https://arxiv.org/abs/2205.08424|Galaxy cluster aperture masses are more robust to baryonic effects than 3D halo masses]] | * [[https://arxiv.org/abs/2205.08424|Galaxy cluster aperture masses are more robust to baryonic effects than 3D halo masses]] | ||
* [[https://arxiv.org/abs/2205.08241|How well do local relations predict gas-phase metallicity gradients? Results from SDSS-IV MaNGA]] | * [[https://arxiv.org/abs/2205.08241|How well do local relations predict gas-phase metallicity gradients? Results from SDSS-IV MaNGA]] |