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Oct 8, 2024 | 
academic.oup.com | Max-Planck-Institut für Astronomie
Cosmological simulations have greatly improved our understanding of the physics of galaxy formation and are widely used to guide the interpretation of observations and the design of new observational campaigns and instruments. Simulations are useful for testing how different physical processes affect galaxy formation, which can then be compared with observations in order to develop a more complete understanding of the Universe.
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Sep 28, 2024 | 
academic.oup.com | Max-Planck-Institut für Astronomie |Burnaby Road
Bars are expected to impact the distribution of stellar populations both during bar formation, as they rearrange stars into new orbits, and afterwards, due to the redistribution of star-formation-fuelling gas and transfer of angular momentum. We study the impact of stellar bars on the azimuthal variation of stellar population age, metallicity and mass surface density in ∼1 000 nearby barred galaxies from the SDSS-IV/MaNGA survey.
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Aug 20, 2024 | 
academic.oup.com | Universidad Adolfo Ibáñez |Max-Planck-Institut für Astronomie |Departamento de Astronomía |Universidad de Chile
Brown dwarfs are substellar objects that canonically fall within the 13–80 mass range (Burrows & Liebert 1993; Baraffe et al. 2002; Burgasser 2008). They are not quite massive enough to burn hydrogen in their cores, but some can burn deuterium (Bate, Bonnell & Bromm 2002; Whitworth 2018). As they age, they cool, progressing through the M-L-T-Y spectral types, and their radii contract. The first confirmed brown dwarfs were Gliese 229B (Nakajima et al.
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Jun 26, 2024 | 
iopscience.iop.org | Bingjie Wang |Joel Leja |Anna de Graaff |Max-Planck-Institut für Astronomie
In the cores of the most massive galaxies in the local Universe, stars have inferred stellar age of ∼13 Gyr and high α-element abundance, suggesting that their stellar components are formed at z ≳ 5 in a spectacular and short burst of star formation (e.g., Thomas et al. 2005).
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Apr 13, 2024 | 
academic.oup.com | Max-Planck-Institut für Radioastronomie |Max-Planck-Institut für Astronomie |Ludwig Maximilian
This is a correction to: A. G. Pazukhin, I. I. Zinchenko, E. A. Trofimova, C. Henkel, D. A.
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Mar 6, 2024 | 
academic.oup.com | Abu Dhabi |Space science |Max-Planck-Institut für Astronomie
In a dark energy-cold dark matter (ΛCDM) dominated hierarchical Universe, galaxy evolution is a complex interplay between gravitational and baryonic processes (White & Rees 1978; White & Frenk 1991). With most of the baryons in galaxies found in their central parts (at the minimum of the gravitational potential), the mass budget of all galaxies is DM dominated in the outskirts.
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Feb 20, 2024 | 
academic.oup.com | Three Gorges |Max-Planck-Institut für Astronomie |Hangzhou Dianzi
The stellar initial mass function (IMF) describes the distribution of the number of stars formed as a function of their mass. Originally proposed by Salpeter (1955) and further studied by seminal works like Miller & Scalo (1979) and Kroupa (2001), the IMF is typically described as a power-law distribution. At high masses, the IMF follows a power-law slope of around −2.3, while slopes of around −1.3 and −0.3 are seen at intermediate and low masses, respectively.
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Oct 1, 2023 | 
academic.oup.com | Max-Planck-Institut für Radioastronomie |Max-Planck-Institut für Astronomie |Ludwig Maximilian
We use spectra and maps of the J = 1 − 0 and J = 2 − 1 DCO+, DCN, DNC, |$\rm N_2D^+$| lines and 1 − 1 ortho- and para-NH D lines, obtained with the IRAM-30m telescope, as well as observations of their hydrogenated isotopologues to study deuteration processes in five high-mass star-forming regions.
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Aug 25, 2023 | 
academic.oup.com | Universität Heidelberg |Max-Planck-Institut für Astronomie
Due to ram-pressure stripping, jellyfish galaxies are thought to lose large amounts, if not all, of their interstellar medium. Nevertheless, some, but not all, observations suggest that jellyfish galaxies exhibit enhanced star formation compared to control samples, even in their ram pressure-stripped tails.
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Jul 26, 2023 | 
academic.oup.com | Max-Planck-Institut für Astronomie
Lyman α emitters (LAEs) are excellent probes of the reionization process, as they must be surrounded by large ionized bubbles in order to be visible during the reionization era. Large ionized regions are thought to correspond to overdense regions and may be protoclusters, making them interesting test-beds for early massive structures. Close associations containing several LAEs are often assumed to mark overdense, ionized bubbles.
