학술논문
J-PLUS: Photometric Re-calibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Document Type
Working Paper
Author
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.; Sodre Jr., L.; Ramio, H. Vazquez; Varela, J.
Source
Subject
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Abstract
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.
Comment: ApJS accepted; 21 papes; 20 figures, see main results in Figures 5 and 12
Comment: ApJS accepted; 21 papes; 20 figures, see main results in Figures 5 and 12