The <i>Gaia</i> spectrophotometric standard stars survey – V. Preliminary flux tables for the calibration of <i>Gaia</i> DR2 and (E)DR3

Pancino, E.; Altavilla, G.; Marinoni, S.; Rainer, M.; Cocozza, G.; Ragaini, S.; Galleti, S.; Bellazzini, M.; Bragaglia, A.; Tessicini, G.; Voss, H.; Carrasco, J. M.; Jordi, C.; Harrison, D. L.; Angeli, F. De; Evans, D. W.; Fanari, G.

doi:10.1093/mnras/stab766

Cited by 18 publications

(26 citation statements)

References 73 publications

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“…The typical solution would be to observe a selection of spectro-photometric standard stars with well known spectra -observed or theoretical -spanning the full wavelength range of the filter set in order to calibrate the observed light curves from synthetic photometry. This is the method that will be employed in future works using the Gaia spectro-photometric standard stars (Pancino et al 2012;Altavilla et al 2015;Marinoni et al 2016;Altavilla et al 2021;Pancino et al 2021). Synthetic AB magnitudes of these Gaia spectro-photometric standard stars computed for the ULTRACAM and HiPERCAM Super-SDSS systems are included in appendix A for future reference along with a more thorough analysis of the differences between the Super-SDSS and SDSS photometric systems.…”

Section: Flux Calibrationmentioning

confidence: 99%

“…Table A3. Gaia spectro-photometric standard stars (Pancino et al 2012;Altavilla et al 2015;Marinoni et al 2016;Altavilla et al 2021;Pancino et al 2021) with AB magnitudes computed for the HiPERCAM and ULTRACAM Super-SDSS (𝑢 𝑠 𝑔 𝑠 𝑟 𝑠 𝑖 𝑠 𝑧 𝑠 ) photometric systems using the flux tables of Pancino et al (2021). The 'Type' column indicates the status of a flux standard as either 'Pillar', 'Primary', or 'Secondary' as described in Pancino et al (2012) ('0', '1', and '2' respectively in the table).…”

Section: Wavelength ( å)mentioning

confidence: 99%

“…In order to make flux calibration simpler and more robust in future, we define a set of HiPERCAM standard stars (Table A3). These standard stars are the Gaia spectro-photometric standard stars collated and evaluated by Pancino et al (2012); Altavilla et al (2015); Marinoni et al (2016); Altavilla et al (2021); Pancino et al (2021) who provide high quality spectra of these standards covering the full range of the HiPERCAM photometric system. We again use Equation 2 to produce synthetic AB magnitudes for these stars in both the HiPER-CAM and ULTRACAM systems.…”

Section: Data Availabilitymentioning

confidence: 99%

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Characterising eclipsing white dwarf M dwarf binaries from multi-band eclipse photometry

Brown,

Parsons,

Littlefair

et al. 2022

Preprint

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With the prevalence of wide-field, time-domain photometric sky surveys, the number of eclipsing white dwarf systems being discovered is increasing dramatically. An efficient method to follow these up will be key to determining any population trends and finding any particularly interesting examples. We demonstrate that multi-band eclipse photometry of binaries containing a white dwarf and an M dwarf can be used to determine the masses and temperatures of the white dwarfs to better than 5 per cent. For the M dwarfs we measure their parameters to a precision of better than 6 per cent with the uncertainty dominated by the intrinsic scatter of the M dwarf mass-radius relationship. This precision is better than what can typically be achieved with low-resolution spectroscopy. The nature of this method means that it will be applicable to LSST data in the future, enabling direct characterisation without follow-up spectroscopy. Additionally, we characterise three new post-common-envelope binaries from their eclipse photometry, finding two systems containing hot helium-core white dwarfs with low-mass companions (one near the brown dwarf transition regime) and a possible detached cataclysmic variable at the lower edge of the period gap.

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Section: Flux Calibrationmentioning

confidence: 99%

Section: Wavelength ( å)mentioning

confidence: 99%

Section: Data Availabilitymentioning

confidence: 99%

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Characterising eclipsing white dwarf M dwarf binaries from multi-band eclipse photometry

Brown,

Parsons,

Littlefair

et al. 2022

Preprint

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“…We compared the results from the final photometry with the synthetic photometry of the spectroscopic standard star GD 153. We used the reference spectra from CAL-SPEC 6 (Bohlin et al 2014(Bohlin et al , 2020 and from the Gaia spectrophotometric standard stars (SPSS) survey 7 (Pancino et al 2012(Pancino et al , 2021. GD 153 is one of the three calibration pillars from the…”

Section: Appendix A: Technical Details About the Absolute Color Calibrationmentioning

confidence: 99%

J-PLUS: Systematic impact of metallicity on photometric calibration with the stellar locus

López-Sanjuan

Yuan

Ramió

et al. 2021

A&A

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Aims. We present the photometric calibration of the twelve optical passbands for the Javalambre Photometric Local Universe Survey (J-PLUS) second data release (DR2), comprising 1088 pointings of two square degrees, and study the systematic impact of metallicity on the stellar locus technique. Methods. The [Fe/H] metallicity from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) for 146 184 high-quality calibration stars, defined with signal-to-noise ratio larger than ten in J-PLUS passbands and larger than three in Gaia parallax, was used to compute the metallicity-dependent stellar locus (ZSL). The initial homogenization of J-PLUS photometry, performed with a unique stellar locus, was refined by including the metallicity effect in colors via the ZSL. Results. The variation of the average metallicity along the Milky Way produces a systematic offset in J-PLUS calibration. This effect is well above 1% for the bluer passbands and amounts 0.07, 0.07, 0.05, 0.03, and 0.02 mag in u, J0378, J0395, J0410, and J0430, respectively. We modeled this effect with the Milky Way location of the J-PLUS pointing, also providing an updated calibration for those observations without LAMOST information. The estimated accuracy in the calibration after including the metallicity effect is at 1% for the bluer J-PLUS passbands and below for the rest. Conclusions. Photometric calibration with the stellar locus technique is prone to significant systematic bias in the Milky Way for passbands bluer than λ = 4500 Å. The calibration method for J-PLUS DR2 reaches 1–2% precision and 1% accuracy for 12 optical filters within an area of 2176 square degrees.

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“…1, after an initial preparation step called preprocessing, the internal (or relative) calibration uses only Gaia observations to relate all observations into a common system. After this internal calibration, the external (or absolute) calibration uses a relatively small number of ground-based standard stars (Pancino et al 2012(Pancino et al , 2021Altavilla et al 2021) to get the absolute fluxes and wavelengths. This paper describes the concepts of the internal calibration of Gaia spectrophotometric data, but this is not linked to the particular details used in any of the Fig.…”

Section: Introductionmentioning

confidence: 99%

Internal calibration of Gaia BP/RP low-resolution spectra

Carrasco

Weiler

Jordi

et al. 2021

A&A

Self Cite

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Context. The full third Gaia data release will provide, for the first time, the calibrated spectra obtained with the blue and red Gaia slitless spectrophotometers (BP and RP, respectively). Gaia is a very complex mission and cannot be considered as a single instrument, but rather as many instruments. The two lines of sight with wide fields of view (FoV) introduce strong variations of the observations across the large focal plane with more than one hundred different detectors. The main challenge when facing Gaia spectral calibration is that no lamp spectra or flat fields are available during the mission. Also, the significant size of the line spread function (LSF) with respect to the dispersion of the prisms produces alien photons contaminating neighbouring positions of the spectra. This makes the calibration special and different from standard approaches. Aims. This work gives a detailed description of the internal calibration model for the spectrophotometric data used to obtain the content of the Gaia catalogue. The main purpose of the internal calibration is to bring all the epoch spectra onto a common flux and pixel (pseudo-wavelength) scale, taking into account variations over the focal plane and with time, producing a mean spectrum from all the observations of the same source. Methods. In order to describe all observations on a common mean flux and pseudo-wavelength scale, we constructed a suitable representation of the internally calibrated mean spectra via basis functions, and we described the transformation between non-calibrated epoch spectra and calibrated mean spectra via a discrete convolution, parametrising the convolution kernel to recover the relevant coefficients.Results. The model proposed here for the internal calibration of the Gaia spectrophotometric observations is able to combine all observations into a mean instrument to allow the comparison of different sources and observations obtained with different instrumental conditions along the mission and the generation of mean spectra from a number of observations of the same source. We derived a calibration model that can handle the self-calibrating nature of the problem. The output of this model provides the internal mean spectra, not as a sampled function (flux and wavelength), but as a linear combination of basis functions, although sampled spectra can easily be derived from them.

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The Gaia spectrophotometric standard stars survey – V. Preliminary flux tables for the calibration of Gaia DR2 and (E)DR3

Cited by 18 publications

References 73 publications

Characterising eclipsing white dwarf M dwarf binaries from multi-band eclipse photometry

Characterising eclipsing white dwarf M dwarf binaries from multi-band eclipse photometry

J-PLUS: Systematic impact of metallicity on photometric calibration with the stellar locus

Internal calibration of Gaia BP/RP low-resolution spectra

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