Determination of luminosity function of main sequence stars in the solar neighborhood by gaia data

In this study, we are aimed to obtain the space density and luminosity function of the main- sequence stars at the Solar neighborhood. For this purpose, 41,848,305 stars with relative parallax errors and σϖ/ϖ≤0.10 distances from the Sun within 1 kpc were selected from the Gaia satellite early third data release (Gaia EDR3) catalogue. Dust maps of the Milky Way were used to calculate the extinction values of the Gaia photometric magnitudes of the stars. PARSEC isochrones of the thin-disc population calibrated on the MG×(GBP-GRP) diagram was taken into account in the selection of main-sequence stars. The isochrones are extended to include the binary-star effect. On the MG×(GBP-GRP) diagram, 39,131,320 objects in the main-sequence band were selected as main-sequence stars. Main-sequence stars with absolute magnitudes of 0 < MG ≤ 15 are in the spectral class A1 to M6. The space density the Solar neighborhood was calculated as 0.072±0.001 star/pc3, from the main-sequence stars at a distance of 25 ≤ d ≤ 300 pc from the Sun. Three different relative parallax error values at different distance intervals were taken into account in obtaining the luminosity functions of the main-sequence stars at the Solar neighborhood. The analyses showed that the luminosity functions with the relative parallax error σϖ/ϖ≤0.10 and calculated up to 175pc are compatible with the luminosity function given for the distance value of 100 pc in the literature.