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

• Main Authors: Xiao, Kai, Yuan, Haibo, Lopez-Sanjuan, C, Huang, Yang, Huang, Bowen, Beers, Timothy C, Xu, Shuai, Wang, Yuanchang, Yang, Lin, Alcaniz, J, Galarza, Carlos Andrés, Angulo, R. E, Cenarro, A. J, Cristobal-Hornillos, D, Dupke, R. A, Ederoclite, A, Hernandez-Monteagudo, C, Marn-Franch, A, Moles, M, SodreJr, L, Ramio, H. Vazquez, Varela, J
• Format: Journal Article
• Language: English
• Published: 20.09.2023
• Subjects: Physics - Solar and Stellar Astrophysics
• DOI: 10.48550/arxiv.2309.11225

We employ the corrected Gaia Early Data Release 3 (EDR3) 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 validated the J-PLUS DR3 photometry, and uncovered significant systematic errors: up to 15 mmag in the results of Stellar Locus (SL) method, and up to 10 mmag mainly caused by magnitude-, color-, and extinction-dependent errors of the Gaia XP spectra with the Gaia BP/RP (XP) Synthetic Photometry (XPSP) method. We have also further developed the XPSP method using the corrected Gaia XP spectra by Huang et al. (2023) and applied it to the J-PLUS DR3 photometry. This resulted in an agreement of 1-5 mmag with the SCR method, and a two-fold 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 tiles outside this footprint relying on the improved XPSP method. The re-calibrated J-PLUS DR3 photometric data establishes a solid data foundation for conducting research that depends on high-precision photometric calibration.