Spectrophotometric Libraries, Revised Photonic Passbands, and Zero Points for UBVRI, Hipparcos, and Tycho Photometry

By M. Bessell, S. Murphy. 2011

162 citations recorded by the source corpus.

We have calculated improved photonic passbands for the UBVRI, Hipparcos Hp, and Tycho BT and VT standard systems using the extensive spectrophotometric libraries of NGSL and MILES. Using the Hp passband, we adjusted the absolute flux levels of stars in the spectrophotometric libraries so that their synthetic Hp magnitudes matched the precise Hipparcos Catalogue value. Synthetic photometry based on the renormalized fluxes was compared with the standard UBVRI, BT and VT magnitudes, and revised synthetic zero points were determined. The Hipparcos and Tycho photometry system zero points were also compared with the V-magnitude zero points of the SAAO UBVRI system, the homogenized UBV system, and the Walraven VB system. The confusion in the literature concerning broadband magnitudes, fluxes, passbands, and the choice of appropriate mean wavelengths is detailed and discussed in the Appendix.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e374380cac6b1b1a6431979e1c39f880fb3d48ed

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In Astronomy and Astrophysics

1. D. Huber
2. D. Stello
3. N. Smith
4. W. Chaplin
5. T. Bedding
6. D. Kasen
7. A. Miglio
8. M. Pecaut

In Atomic and Molecular Physics, and Optics

1. A. Miglio
2. D. Stello
3. H. Kjeldsen
4. T. Bedding
5. T. White
6. D. Huber
7. V. S. Aguirre
8. W. Chaplin

In Instrumentation

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2. D. Stello
3. W. Chaplin
4. T. Bedding
5. Eric Mamajek
6. A. Miglio
7. C. Bell
8. N. Smith

Citations in the corpus

• PHYSICS OF ECLIPSING BINARIES. II. TOWARD THE INCREASED MODEL FIDELITY (2016, unknown): “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).”
• HIGH-DENSITY CIRCUMSTELLAR INTERACTION IN THE LUMINOUS TYPE IIn SN 2010jl: THE FIRST 1100 DAYS (2013, methodology): “Filter response functions for the JC and SDSS standard systems were adopted from Bessell & Murphy (2012) and Doi et al. (2010).”
• Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, methodology): “Several papers deal with this topic, and excellent discussions on synthetic photometry can be found in e.g., Bessell et al. (1998), Girardi et al. (2002) and Bessell & Murphy (2012).”
• The second data release of the INT Photometric Hα Survey of the Northern Galactic Plane (IPHAS DR2) (2014, background): “These notations follow the definitions by Bessell & Murphy (2012).”
• The long-term evolution of neutron star merger remnants { II. Radioactively powered transients (2013, methodology): “10 shows the broad-band light curves for these two cases, calculated assuming that radiation is emitted with a blackbody spectrum filtered with the standard filter functions for the UBVRI (Bessell & Murphy 2012) and JHK (Cohen et al. 2003) bands.”
• A Test of the Cosmological Principle with Quasars (2020, methodology): “Finally, we calculate the isophotal frequency, at which the flux density Sν equals its mean value within the passband, using Equation A19 in Bessell & Murphy (2012).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “Filter responses and zeropoints were taken from Bessell & Murphy (2012) (UBV RI, BTVT), Cohen et al. (2003) (2MASS), and Bessell et al. (1998) (JHKL).”
• On the age of the β Pictoris moving group (2014, methodology): “For the response functions Rλ we adopt the revised BV bandpasses from Bessell & Murphy (2012).”
• THE Pan-STARRS1 PHOTOMETRIC SYSTEM (2012, unknown): “…are the filter, “net cross section” [m2] for fν=const through this filter at 1.2 airmasses ( ∫ A(ν)d ln ν), filter “pivot” wavelength [nm] described by Bessell & Murphy (2012) ( ∫ λA(ν)d ln ν/〈A〉), bandpass blue and red wavelengths [nm] obtained from a least-squares fit of a square bandpass,…”
• The Absolute Magnitude of the Sun in Several Filters (2018, methodology): “The mean photon wavelength (Bessell & Murphy 2012), also called mean wavelength by (Tokunaga & Vacca 2005) and mean or effective wavelength Rieke et al. (2008) is defined as λmean = ∫ R(λ)λdλ ∫ R(λ)dλ (A1) The mean flux of a source within the band is defined as 〈fλ〉 = ∫ fλR(λ)λdλ ∫ R(λ)λdλ (A2) The…”
• INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, methodology): “To compute the synthetic photometry for the models, we use the updated BV IC normalized photonic bandpasses and zero points from Bessell & Murphy (2012), including the additional zeropoints listed in their Table 5.”
• Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared (2014, background): “The integration is done in photon units (F λλ), because UV/optical/near infrared (NIR) detectors are generally photon-detection devices, rather than total-energy-sensing bolometers, although Bessell & Murphy (2012) demonstrate that counting photons is equivalent to integrating the energy.”
• Spectrophotometric time series of SN 2011fe from the Nearby Supernova Factory (2013, methodology): “After interpolation of those filter responses into 10 Å steps using cubic splines, our integrator agrees at the 0.001 mag level with the colors measured by Bessell & Murphy (2012) using the aforementioned Vega spectrum and the zero-points derived by these authors.”