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Jan 24, 2025 | 
academic.oup.com | Instituto de Astronomia |Av. Universidad s
We introduce a novel approach to modelling the nebular emission from star-forming galaxies by combining the contributions from many H ii regions incorporating loose trends in physical properties, random dust attenuation, a predefined Hα luminosity function and a diffuse ionized-gas component.
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Dec 9, 2024 | 
academic.oup.com | Instituto de Astronomia
Recent simulations of Be stars in misaligned binary systems have revealed that misalignment between the disc and binary orbit can cause the disc to undergo Kozai-Lidov (KL) oscillations or disc-tearing. We build on our previous suite of three-dimensional smoothed particle hydrodynamics simulations of equal-mass systems by simulating eight new misaligned Be star binary systems, with mass-ratios of 0.1 and 0.5, or equal-mass systems with varying viscosity.
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Nov 28, 2024 | 
academic.oup.com | Instituto de Astronomia |Universidad Diego Portales |Departamento de Astronomía |Universidad de Chile
We present the discoveries of NGTS-31b(=TOI-2721), and NGTS-32b, two hot Jupiters from the Next Generation Transit Survey (NGTS) transiting slightly evolved stars. The orbital periods, radii, and masses are 4.16 and 3.31 days, 1.61 and 1.42 R , and 1.12 and 0.57 M , respectively. Both planets have an incident stellar flux significantly above the threshold where inflation occurs, with both planets showing signs of inflation.
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Nov 25, 2024 | 
aanda.org | Luis Miranda |Jose Gomez |José Gómez |Christophe Morisset |Instituto de Astronomia
Home All issues Volume 691 (November 2024) A&A, 691 (2024) A321 Full HTML Issue A&A Volume 691, November 2024 Article Number A321 Number of page(s) 11 Section Interstellar and circumstellar matter DOI https://doi.org/10.1051/0004-6361/202451719 Published online 22 November 2024 A&A, 691, A321 (2024) Long- and short-term variability of the possible nascent planetary nebula IRAS 22568+6141: A late thermal pulse? 1★, 1, 1, 2,3, 2, 4 and 2 1 Instituto de Astrofísica de Andalucía IAA–CSIC,...
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Nov 19, 2024 | 
academic.oup.com | Departamento de Astronomía |Universidad de Chile |Universidad Diego Portales |Instituto de Astronomia
In the last few decades planet search surveys have been focusing on solar type stars, and only recently the high-mass regimes. This is mostly due to challenges arising from the lack of instrumental precision, and more importantly, the inherent active nature of fast rotating massive stars. Here we report NGTS-33b (TOI-6442b), a super-Jupiter planet with mass, radius and orbital period of 3.6 ± 0.3 M , 1.64 ± 0.07 R and 2.827972 ± 0.000001 days, respectively.
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Sep 18, 2024 | 
academic.oup.com | Instituto de Astronomia
In this work, we analysed young stellar clusters with spatial and kinematic coherence in the Orion star-forming complex. For this study, we selected a sample of pre-main sequence candidates using parallaxes, proper motions and positions on the colour-magnitude diagram.
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Sep 13, 2024 | 
academic.oup.com | Instituto de Astronomia |Cidade Universitária
Fossil groups have been seen as possible examples of the final stage of evolution of galaxy groups. Not long after Ponman et al. (1994) studied RX J1340.6+4018, it was proposed that they may be the final stage of evolution of a compact group of galaxies and that those galaxies that were close to the centre of the system could have merged in a single elliptical galaxy. Jones et al.
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Aug 15, 2024 | 
academic.oup.com | Instituto de Astronomia
According to the Lambda cold dark matter ( CDM) paradigm, galaxy formation and evolution take place within massive dark matter haloes. A key component of our understanding of galaxy formation and evolution within this context is the stellar-to-halo mass relation (SHMR). The SHMR relates the mass of stars within a galaxy to the mass of its host halo.
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Aug 12, 2024 | 
academic.oup.com | Instituto de Astronomia |Facultad de Ingeniería
The rotational support of the stellar system in galaxies measures the relative magnitude of regular rotation to dispersion and shows important hints on galaxy evolution. The rotational support not only correlates with the galaxy specific angular momentum (Cortese et al. 2016), which is believed to determine the galaxy mass–size relation (Mo, Mao & White 1998; Shen et al.
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Aug 1, 2024 | 
academic.oup.com | Instituto de Astronomia |Argelander-Institut für Astronomie |Departamento de Astronomía |Universidad de Concepcion
Galaxy interaction and merging significantly impact galactic evolution, influencing the morphology and growth of galaxies (Toomre 1977; Conselice et al. 2003; Christensen, Shida & Martin 2009; Kormendy 2013). In addition, galaxy interaction/merging affects star formation, gas recycling, metallicity enrichment, and energy output from supernovae or active galactic nuclei (Kormendy & Kennicutt 2004; Kormendy 2013).
