Rigby J. R

Sep 25, 2024 | academic.oup.com | Brigham Young |Claverton Down |Rigby J. R

The Leavitt law (previously known as the period–luminosity relation) for classical Cepheid variables has been shown to have decreased dispersion at longer wavelengths (Madore & Freedman 1991). As we move beyond the optical region, temperature variation of the stars and extinction due to the interstellar medium become smaller obstacles to obtaining accurate measurements.

Jun 27, 2024 | academic.oup.com | Madingley Road |Space Research |Rigby J. R

The interstellar medium (ISM) of star-forming galaxies is both cradle and grave for the generations of stars embedded within. Throughout their lives, these stars batter the ISM with stellar winds, supernovae, and a flood of photons which leave it chemically enriched and injected with energy (Girichidis et al. 2020; Vogelsberger et al. 2020). While stellar populations shape the ISM, they are also shaped by it.

Apr 16, 2024 | academic.oup.com | Shanghai Jiao Tong |Rigby J. R

Galaxy clusters are the most massive gravitationally bound structures in the Universe, and therefore they are of great use in cosmology and astrophysics. One motivation for the creation of catalogues of clusters is to locate likely areas for observing strongly lensed time-variable phenomena such as gravitationally lensed supernovae and quasars (Meyers et al. 2009).

Jan 23, 2024 | academic.oup.com | Liverpool John Moores |Madingley Road |European Space Agency |Rigby J. R

Understanding the reionization of the Universe is one of the frontier goals of modern astronomy. Several theoretical and observational efforts have been made to answer the related pressing questions, such as when and how first galaxies formed (e.g. Stark 2016) and whether these first galaxies reionized the intergalactic medium (IGM; e.g. Robertson et al. 2010).

May 8, 2023 | academic.oup.com | Colby College |Rigby J. R

There are now several observational results that indicate a co-evolution of supermassive black holes (SMBHs) and their host galaxies. This includes tight correlations between SMBH mass and spheroidal properties (e.g. Magorrian et al. 1998; Gebhardt et al. 2000; Gültekin et al. 2009; Kormendy & Ho 2013) as well as the similar cosmic evolution of SMBH accretion and star formation rate (SFR) density, both of which peak at ‘cosmic noon’ (i.e. z ∼ 2; e.g. Madau & Dickinson 2014; Aird et al. 2015).