Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands

Abstract

We have obtained accurate dust reddening from the far-ultraviolet to the mid-infrared for up to 5 million stars by the star-pair algorithm based on LAMOST stellar parameters along with Galaxy Evolution Explorer, Pan-STARRS 1, Gaia, Sloan Digital Sky Survey, Two Micron All Sky Survey, and Wide-field Infrared Survey Explorer photometric data. The typical errors are between 0.01 and 0.03 mag for most colors. We derived the empirical reddening coefficients for 21 colors both in the traditional (single-valued) way and as a function of T eff and E(B − V) by using the largest samples of accurate reddening measurements, together with the extinction values from Schlegel et al. The corresponding extinction coefficients have also been obtained. The results are compared with model predictions and generally in good agreement. Comparisons with measurements in the literature show that the T eff- and E(B − V)-dependent coefficients explain the discrepancies between different measurements naturally, i.e., using sample stars of different temperatures and reddening. Our coefficients are mostly valid in the extinction range of 0–0.5 mag and the temperature range of 4000–10,000 K. We recommend that the new T eff- and E(B − V)-dependent reddening and extinction coefficients should be used in the future. A Python package is also provided for the usage of the coefficients (https://github.com/vnohhf/extinction_coeffcient/).

Improvement of Pan-STARRS Photometric Calibration with LAMOST and Gaia

“…and the metallicity [Fe/H] of the calibration stars. This dependence is probably due to the fact that Zhang & Yuan (2023) used only a secondorder binary function to describe the dependence of reddening coefficients on temperature and reddening to avoid overfitting. Therefore, we use a fourth-order polynomial as a function of E(B − V ) SFD to fit the residuals divided by E(B − V ) SFD .…”

The Preexplosion Environments and the Progenitor of SN 2023ixf from the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX)

“…We also note that the C-rich dust model-derived extinction should be applied with caution, as detailed in Section 9.2 of Van Dyk et al (2023). For the CFHTLS i and z bands, R i =1.799 and R z =1.299 are adopted (Zhang & Yuan 2023). These together give A i ∼ 3.02 mag and A z ∼ 2.18 mag.…”

Internal Calibration of LAMOST and Gaia DR3 GSP-Spec Stellar Abundances

“…Black and gray points also satisfy E(B−V) SFD < 0.02. Their absolute magnitudes and colors are dereddened with the SFD dust map and reddening coefficients as provided in Zhang & Yuan (2023). The red points are member stars of M 67 that can represent the locus of stars having the same metallicity as M 67 on the HRD.…”