Standard Photometric Systems

By M. Bessell. 2005

343 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/760cc5f7a00d672034c509f7b62a6ee9cce9bb71

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Citations in the corpus

FURTHER DEFINING SPECTRAL TYPE “Y” AND EXPLORING THE LOW-MASS END OF THE FIELD BROWN DWARF MASS FUNCTION (2012, methodology): “Comparison of this filter curve to the filter curves illustrated in figure 4 of Bessell (2005) shows that it is very similar to the MKO-NIR H-band filter.”
An absolutely calibrated T eff scale from the infrared flux method. Dwarfs and subgiants (2010, methodology): “The core of the present work is to accurately define the zero point of the temperature scale in many standard photometricsystems; we caution however that in some cases real systems might not exactly reproduce standard systems, especially in the cas of the faintest sources (Bessell 2005).”
THE STELLAR-ACTIVITY–ROTATION RELATIONSHIP AND THE EVOLUTION OF STELLAR DYNAMOS (2011, methodology): “3 Conversions provided by Bessell (2005) were used to convert the V −K color of this work onto the 2MASS-based V −Ks color.”
PHYSICS OF ECLIPSING BINARIES. II. TOWARD THE INCREASED MODEL FIDELITY (2016, neutral): “This version is more appropriate for observations where counts are not calibrated (including instrumental and differential photometry, including Kepler data) and passbands are wide (Bessell 2005; Bessell & Murphy 2012; Casagrande & VandenBerg 2014; Brown et al. 2016).”
Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies (2013, neutral): “To good approximation, Ks = K − 0.044 (Carpenter 2001; Bessell 2005), where K is essentially Johnson’s (1962) 2.2 µm bandpass.”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, methodology): “Stromlo Fellow † Email:luca.casagrande@anu.edu.au intermediate-band photometry, a large number of systems exists nowadays, and more are being developed with the advent of extensive photometric surveys (see e.g., Bessell 2005, for a review).”
Accurate fundamental parameters for lower main‐sequence stars (2006, background): “…calibration and the zero-points are expected to be well known and the latest generations of model atmospheres produce realistic fluxes for a wide range of temperatures, gravities and abundances (Bessell 2005) so that the adopted model and calibration are at the best level currently available.”
On the metallicity of open clusters. III. Homogenised sample (2015, methodology): “We note that the standard Johnson UB V system, in particular the (U − B) colour, cannot be reproduced correctly if the instrumental system differs from the originally defined one (see e.g. Sung & Bessell 2000; Bessell 2005).”
Measuring the vertical age structure of the Galactic disc using asteroseismology and SAGA (2015, methodology): “Its y magnitudes are defined to be essentially the same as the Johnson V (e.g. Bessell 2005), and in this work we will refer to the two interchangeably.”
THE Pan-STARRS1 PHOTOMETRIC SYSTEM (2012, background): “Astronomical magnitude systems are based on this concept, as summarized by Bessell (2005).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “The m1 index is designed to measure the depression owing to metal lines around 4100 Å (v band), and hence is suitable to infer the metallicity in a variety ofstars (e.g., Bessell 2005, and references therein).”
An Improved Photometric Calibration of the Sloan Digital Sky Survey Imaging Data (2007, neutral): “The Photometric Model An introduction to photometric calibrations and photometric standard systems may be found in Bessell (2005); we focus on the details relevant to this work below.”