Computing Natural Magnitudes in the Photometric Systems of Astronomical Plates using Gaia DR3 SEDs

TL;DR

This paper introduces a method to derive accurate natural magnitudes for astronomical photographic plates using Gaia DR3 spectral data, improving calibration accuracy and correcting systematic errors in historical data.

Contribution

It presents a novel synthetic photometry approach leveraging Gaia DR3 SEDs to calibrate photographic plates, outperforming previous color term methods.

Findings

Systematic errors in existing photographic plate data are revealed.

The method effectively corrects atmospheric reddening effects.

Achieves improved calibration accuracy over traditional methods.

Abstract

Context. Accurate photometric calibration of astronomical photographic plates remains a fundamental challenge in astronomy, especially when bridging historical photographic data with modern observations due to the mismatch of spectral sensitivities of photographic plates and passbands of modern calibration catalogs. Aims. We intend to derive consistent natural magnitudes for celestial sources within the intrinsic photometric systems of astronomical photographic plates by using Gaia Data Release 3 (DR3) blue photometer (BP) and red photometer (RP) low-resolution spectral data and to show its superiority to former methods. Methods. We compiled spectral characteristic data for emulsions and filters applied in photometric observations using glass plates. The collected color sensitivities, modified by atmospheric reddening depending on the air mass, are then used to compute accurate natural magnitudes and fluxes of objects in the photographic plates through synthetic photometry, utilizing a catalog of Gaia spectral energy distributions (SEDs) over the wavelength range 330 nm to 1050 nm (XP spectra). This process uses GaiaXPy, a Python library designed to handle Gaia DR3 spectral data. These natural magnitudes are then compared with results from the color term method used to compile the data in existing photoplate archives. Results. Comparing the synthetic magnitudes with those existing in the Archives of Photographic PLates for Astronomical USE (APPLAUSE), we were able to reveal systematic errors of the existing data in the range of +/-0.3 mag and higher. In addition, the presented method allows for an accommodation of stars with similar color index but of different luminosity classes as well as an effective correction of atmospheric reddening at higher air masses, approximately 0.2 mag.