Spectrophotometric Libraries, Revised Photonic Passbands, and Zero Points for<i>UBVRI</i>,<i>Hipparcos</i>, and Tycho Photometry

Bessell, M. S.; Murphy, Simon J.

doi:10.1086/664083

Cited by 191 publications

(224 citation statements)

References 49 publications

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“…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).…”

Section: Synthetic Photometrymentioning

confidence: 99%

“…The latter must be taken into account in the response function of the overall system because, in all instances, the flux is evaluated after entering the detector. Because of this, one must distinguish between photon-counting (e.g., CCD) and energy-integration (e.g., photo-multiplier) detectors (e.g., Bessell 2000;Maíz Apellániz 2006;Bessell & Murphy 2012).…”

Section: Photon Counting Versus Energy Integrationmentioning

confidence: 99%

“…-1: Bessell (1990). -2: Bessell & Murphy (2012): notice that the formalism introduced in that paper for the U BV(RI) C system is in terms of AB magnitudes, although the system is actually VEGA based; ζ values are obtained from their tables 3 and 5 (but with the opposite sign, following our definition of ζ ). -3: Cohen et al (2003); ζ values from Casagrande et al (2010).…”

Section: Bolometric Correctionsmentioning

confidence: 99%

“…The novel approach of Bessell & Murphy (2012) is that the Johnson-Cousins system is formulated in terms of AB magnitudes, despite being on the VEGA system. We have named these magnitudes ubvri12.…”

Section: Johnson-cousins U Bv(ri) C and 2mass Jhk Smentioning

confidence: 99%

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Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Casagrande¹,

VandenBerg²

2014

Monthly Notices of the Royal Astronomical Society

257

321

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After a pedagogical introduction to the main concepts of synthetic photometry, colours and bolometric corrections in the Johnson-Cousins, 2MASS, and HST-ACS/WFC3 photometric systems are generated from MARCS synthetic fluxes for various [Fe/H] and [α/Fe] combinations, and virtually any value of E(B − V) 0.7. The successes and failures of model fluxes in reproducing the observed magnitudes are highlighted. Overall, extant synthetic fluxes predict quite realistic broad-band colours and bolometric corrections, especially at optical and longer wavelengths: further improvements of the predictions for the blue and ultraviolet spectral regions await the use of hydrodynamic models where the microturbulent velocity is not treated as a free parameter. We show how the morphology of the colour-magnitude diagram (CMD) changes for different values of [Fe/H] and [α/Fe]; in particular,how suitable colour combinations can easily discriminate between red giant branch and lower main sequence populations with different [α/Fe], due to the concomitant loops and swings in the CMD. We also provide computer programs to produce tables of synthetic bolometric corrections as well as routines to interpolate in them. These colour-T eff -metallicity relations may be used to convert isochrones for different chemical compositions to various bandpasses assuming observed reddening values, thus bypassing the standard assumption of a constant colour excess for stars of different spectral type. We also show how such an assumption can lead to significant systematic errors. The MARCS transformations presented in this study promise to provide important constraints on our understanding of the multiple stellar populations found in globular clusters (e.g., the colours of lower main sequence stars are predicted to depend strongly on [α/Fe]) and of those located towards/in the Galactic bulge.

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“…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).…”

Section: Synthetic Photometrymentioning

confidence: 99%

Section: Photon Counting Versus Energy Integrationmentioning

confidence: 99%

Section: Bolometric Correctionsmentioning

confidence: 99%

Section: Johnson-cousins U Bv(ri) C and 2mass Jhk Smentioning

confidence: 99%

See 2 more Smart Citations

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Casagrande¹,

VandenBerg²

2014

Monthly Notices of the Royal Astronomical Society

257

321

View full text Add to dashboard Cite

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“…Synthetic photometry is the process by which the apparent magnitudes in a bandpass is obtained from a spectrum by convolution with the filter quantum efficiency curve (Bessell 2005). Following Bessell & Murphy (2012) and Casagrande & VandenBerg (2014) we calculate the synthetic AB magnitudes using…”

Section: Absolute Magnitudesmentioning

confidence: 99%

An X-Shooter composite of bright 1 <z< 2 quasars from UV to infrared

Selsing

Fynbo

Christensen

et al. 2015

A&A

160

180

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Quasi-stellar object (QSO) spectral templates are important both to QSO physics and for investigations that use QSOs as probes of intervening gas and dust. However, combinations of various QSO samples obtained at different times and with different instruments so as to expand a composite and to cover a wider rest frame wavelength region may create systematic effects, and the contribution from QSO hosts may contaminate the composite. We have constructed a composite spectrum from luminous blue QSOs at 1 < z < 2.1 selected from the Sloan Digital Sky Survey (SDSS). The observations with X-Shooter simultaneously cover ultraviolet (UV) to nearinfrared (NIR) light, which ensures that the composite spectrum covers the full rest-frame range from Lyβ to 11 350 Å without any significant host contamination. Assuming a power-law continuum for the composite we find a spectral slope of α λ = 1.70 ± 0.01, which is steeper than previously found in the literature. We attribute the differences to our broader spectral wavelength coverage, which allows us to effectively avoid fitting any regions that are affected either by strong QSO emissions lines (e.g., Balmer lines and complex [Fe II] blends) or by intrinsic host galaxy emission. Finally, we demonstrate the application of the QSO composite spectrum for evaluating the reddening in other QSOs.

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