# Internal Consistency of Each Parameter in SSPP – SSPP

There are about 43,000 stars which have more than one spectroscopic observation over the entire SDSS and SEGUE-1 and -2 surveys. From these, we select ~9000 stars for which the S/N value between two spectra (both should have S/N ≥ 10) is closer than +/-10, SSPP flag sets to ‘nnnnn’, correlation coefficient between model and observed spectrum is larger than zero, there is no any bad pixel in flux, and valid stellar parameters are available. Comparison of the parameter estimates for these duplicate observations provides an excellent basis for a new estimate of the internal uncertainties of the SSPP. We look at the residual distribution between two measurements of each parameter from two different observations as a function of signal-to-noise ratio (S/N) in four different regions of g-r and two metallicity ranges (metal-poor for [Fe/H] < -1.5 and metal-rich for [Fe/H] > -1.5).

Three figures below show the residual distribution of the effective temperature, surface gravity, and metallicity. Each panel in each figure lists the color and metallicity ranges and the Gaussian mean (μ) and scatter (σ) is calculated for the stars in each color and metallicity bin. In this analysis, when we compute the Gaussian sigma, we do not attempt to clip the outliers as we already imposed various restrictions on each object to obtain parameters as reliable as possible. The dashed line indicates the Gaussian sigma listed in each panel, while the red-dashed line denotes one Gaussian sigma as computed for bins of 200 stars ordered in S/N. Each bin overlaps by 100 stars with the neighboring bins.

Inspection of each figure tells that internal error of `T`_{eff} is ~50 K for a typical G-type dwarf or redder stars in the color range of 0.4 < g-r < 1.3 with S/N = 30. This error increases to ~80 K for stars with -0.3 < g-r < 0.2, [Fe/H] < -1.5, and S/N < 15. Similarly for the surface gravity and metallicity, the middle and right figures indicate that we can achieve the internal errors of log *g* and [Fe/H] to ~0.12 dex and ~0.10 dex, respectively, for a typical G-type dwarf or redder stars in the color range of 0.4 < g-r < 1.3 with S/N = 30. These errors increase to ~0.30 dex for log *g* and 0.25 dex for [Fe/H] for stars with -0.3 < g-r < 0.2, [Fe/H] < -2.0, and S/N < 15.