J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method

Abstract

We employ the corrected Gaia Early Data Release 3 photometric data and spectroscopic data from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) DR7 to assemble a sample of approximately 0.25 million FGK dwarf photometric standard stars for the 12 J-PLUS filters using the stellar color regression (SCR) method. We then independently validate the J-PLUS DR3 photometry and uncover significant systematic errors: up to 15 mmag in the results from the stellar locus method and up to 10 mmag primarily caused by magnitude-, color-, and extinction-dependent errors of the Gaia XP spectra as revealed by the Gaia BP/RP (XP) synthetic photometry (XPSP) method. We have also further developed the XPSP method using the corrected Gaia XP spectra by B. Huang et al. and applied it to the J-PLUS DR3 photometry. This resulted in an agreement of 1–5 mmag with the SCR method and a twofold improvement in the J-PLUS zero-point precision. Finally, the zero-point calibration for around 91% of the tiles within the LAMOST observation footprint is determined through the SCR method, with the remaining approximately 9% of the tiles outside this footprint relying on the improved XPSP method. The recalibrated J-PLUS DR3 photometric data establish a solid data foundation for conducting research that depends on high-precision photometric calibration.

A Comprehensive Correction of the Gaia DR3 XP Spectra

“…Modest changes have been observed only in the C3 term and within the 336-400 nm range. The corrected Gaia XP spectra with version v0.1 have been employed in the photometric recalibration of the Javalambre Photometric Local Universe Survey (Cenarro et al 2019) and the Southern Photometric Local Universe Survey (Mendes de Oliveira et al 2019), and the corrections have been confirmed (Xiao et al 2023a(Xiao et al , 2023b.…”

S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method

“…In principle, the spectroscopy-based SCR method could provide accurate calibrations of zero-points of S-PLUS photometry, just as we have done for the J-PLUS data recently (Xiao et al 2023c). However, corrections of spatial-related systematics for S-PLUS require a large number of stars targeted by spectroscopic surveys in the southern sky, which is unfortunately not available at present.…”

“…For each source, we obtain a linear function for the Gaia XP spectra's flux density with wavelength through fitting of the Gaia XP spectral data over the range of 336 nm to 382 nm for individual stars. This approach has been proposed and validated in the process of recalibration of J-PLUS photometry, after evaluation of multiple extrapolation methods (Xiao et al 2023c).…”

“…First, we select calibration samples with the same constraints on photometric recalibration as those of J-PLUS, as in Xiao et al (2023c), by requiring stars with magnitude errors smaller than 0.02 mag for the uJAVA, J0378, and J0395 bands, and less than 0.01 mag for the remainder; a phot_bp_rp_excess_ factor smaller than…”

“…In addition, Xiao & Yuan (2022) and Xiao et al (2023b) applied the SCR method to the Pan-STARRS1 (PS1; Tonry et al 2012) data, effectively correcting for significant largescale and small-scale spatial variations in the magnitude offsets and magnitude-dependent systematic errors. Other applications include that of Xiao et al (2023c), who used the SCR method to perform recalibration on the J-PLUS Data Release 3 (DR3) photometric data, accurately measuring and correcting for PS1 systematic errors and metallicity-dependent systematic errors present in the data. Xiao et al (2023a) also performed photometric calibration of the Nanshan 1 m wide-field telescope gri-band imaging data of the Stellar Abundance and Galactic Evolution Survey (SAGES; Zheng et al 2018Zheng et al , 2019 using the SCR method, achieving 1-2 mmag precision in the zero-points.…”