============================================================================ COMPOSITE OF OBSERVED SPECTRUM OF MU URSAE MAJORIS Assembled 04-02-96 mu UMa photometry file: photometry actually used to construct the spectrum Name FWHM Mag.+/-Unc. Eff Wvl Eff Wvl Flambda Source (Vega) (star) W/cm2/um (um) (um) (um) Lp 0.1443 -0.99 0.03 3.761 3.744 1.31E-14 Sinton & Tittemore 1984 M 0.6677 -0.62 0.05 4.758 4.751 3.73E-15 Sinton & Tittemore 1984 M 0.6677 -0.69 0.03 4.758 4.751 3.97E-15 Hanner {\it et al.} 1984 [8.7] 1.1576 -0.85 0.01 8.753 8.720 4.26E-16 UKIRT Service Obs. [11.7] 1.2008 -1.00 0.01 11.650 11.623 1.59E-16 UKIRT Service Obs. These uncertainties in the photometry by Sinton & Tittemore (1984) and Hanner {\it et al.} (1984) incorporate uncertainties in our redefinition of their zero points as well as the quoted errors in photometry. UKIRT Service Observations were from Jan. 14, 1995 and photometry is reduced with respect to alp CMa, bet Gem, and alp Hya. Spectral fragments and portions of these actually used in observed spectrum (``used" may include combination with other data where overlaps occur) Fragment Reference Total range Start and stop Average resolving (um) wavelengths (um) power NIR 1a 3.37- 5.30 3.37- 5.30 50 NIR 1b 3.11- 5.40 3.11- 5.40 120 KAO 2a 4.79 -8.75 4.79- 8.75 50 KAO 2b 4.92 -9.38 4.92- 9.38 150 KAO 2c 4.94 -9.35 4.94- 9.35 150 8-13 3 7.59-13.37 7.59-13.37 55 LRS 4 7.67-22.74 7.67-14.90 30 VLONG 5 1.25-35.00 11.00-35.00 -- References: 1a. KAO flight of Jan. 18, 1991 [mu UMa/alp CMa] with the Ames SIRAS. 1b. HIFOGS data of May 4, 1995 KAO flight [mu UMa/alpha Boo]. 2a. KAO flight of Jan. 18, 1991 [mu UMa/alp CMa] with the Ames FOGS. 2b,c. HIFOGS data of May 4, 1995 KAO flight [mu UMa/alpha Boo]. 3. UKIRT CGS3 data of Feb. 9, 1993 [mu UMa/alpha CMa] (details in Paper V). 4. LRS raw data extracted from the NASA-Ames ``LRSVAX" database and recalibrated correctly (cf. Paper II). 5. Engelke Fn. used for T=3735K (no value specific to this star could be found so we adopted the generic M0III from the temperature scale by Di Benedetto & Rabbia 1987), and our initial guess of 8.57 mas; we rescaled this to 8.32 mas. This Engelke Function was locked to the photometrically scaled combination of 8-13 and LRS spectra by splicing and used to replace the observations beyond 14.90 um. We applied an estimated uncertainty in EFn. of 2.9%, allowing for the change in shape of the EFn. for a temperature uncertainty of 100K at this effective temperature. INFORMATION ON SPLICES AND BIASES INCURRED Process Factor determined Bias (%) NIR cf. photometry 0.915 2.06 813 cf. photometry 1.068 0.71 LRS blue/red bias -- 0.72 LRS splice to 813 0.955 0.22 KAO joint splice to NIR and merged 813/LRS 1.033 0.85 Engelke Fn. splice to combined 813/LRS 0.943 0.34 ============================================================================ Notes: 1. Composite spectra are NOT tabulated at equal intervals of the wavelength, but rather at the wavelengths of the original model. 2. In most cases "total uncertainty" is the error term most appropriate to use. It is the standard deviation of the spectral irradiance and includes the local and global biases. Local and global biases are given as a percent of the irradiance. The global bias does not contribute error to flux ratios or color measurements, and may, in those cases, be removed (in the RSS sense) from the total error. ============================================================================