This ratio is called phot_bp_rp_excess_factor. One can appreciate that the faint sources have flux ratios larger than the bright set. One can also notice that the excess factor is larger in the ecliptic plane area indicating an under-subtraction of the sky background.
phot_bp_rp_excess_factor : BP/RP excess factor (float) BP/RP excess factor estimated from the comparison of the sum of integrated BP and RP fluxes with respect to the flux in the G band. This measures the excess of flux in the BP and RP integrated photometry with respect to.
phot_bp_rp_excess_factor : BP/RP excess factor (float) BP/RP excess factor estimated from the comparison of the sum of integrated BP and RP fluxes with respect to the flux in the G band. This measures the excess of flux in the BP and RP integrated photometry with respect to the G band. This excess is believed to be caused by background and …
phot_bp_rp_excess_factor : BP/RP excess: BP/RP excess factor estimated from the comparison of the sum of integrated BP and RP fluxes with respect to the flux in the G band. This measures the excess of flux in the BP and RP integrated photometry with respect to the G band. This excess is believed to be caused by background and contamination …
10/20/2020 · The latter, phot_bp_rp_excess_factor, is an estimation of background and contamination issues affecting the Gaia BP and RP photometry (Riello et al. 2018). Both of these criteria are found in the main gaia_source table. Iorio & Belokurov also enforced a constraint that the reddening must be low (E(B ? V) < 0.8).phot_bp_rp_excess_factor : BP/RP excess: BP/RP excess factor estimated from the comparison of the sum of integrated BP and RP fluxes with respect to the flux in the G band. This measures the excess of flux in the BP and RP integrated photometry with respect to the G band.phot bp rp excess factor >1 :3 + 0 06( G BP RP)2. Finally, we selected the stars from the region in the colour{magnitude diagram that corresponds to red giants (see Figure1): G-band magnitude below 18, and BP RP:2 + 0 11(18 G). The nal sample contains ?0:5 106 stars, and is very clean { the fraction of foreground contaminants is less than 1%, as, gaia_ phot_bp_rp_excess_factor : Gaia BP/RP excess factor: REAL: htm9: HTM index (order 9 => ~10 arcmin size) INTEGER: lc_flux_ivar_w1_1: Inverse variance of LC_FLUX_W1: REAL: lc_flux_ivar_w1_10: Inverse variance of LC_FLUX_W1: REAL: lc_flux_ivar_w1_11: Inverse variance of LC_FLUX_W1: REAL: lc_flux_ivar_w1_2: Inverse variance of LC_FLUX_W1:.
Optional input parameters are Gaia photometric flags ( phot_bp_rp_excess_factor and phot_proc_mode) and uncertainties on the adopted photometry, surface gravity, metallicity, and reddening. If uncertainties are not provided, the routines will assume reasonable uncertainties when doing a MonteCarlo.
We make use of the parameter phot_bp_rp_excess_factor , which indicates the inconsistency between the sum of the fluxes in G BP and G RP with respect to the white light G broad-band. We limit our final catalogues to stars with phot_bp_rp_excess_factor < 1.5 and only consider those objects with at least five independent scans by Gaia ( visibility ...
