============================================================================ COMPOSITE OF OBSERVED SPECTRA OF GAMMA DRA Assembled 12-22-95. Gam Dra photometry file: photometry actually used to construct the spectrum. Name FWHM Mag. +/-Unc. Eff Wvl Eff Wvl F-lam Reference (Vega) (star) W/cm2/um (um) (um) (um) Kn 0.0488 -1.37 0.01 2.208 2.205 1.40E-13 Selby/Hammersley Ln 0.1443 -1.49 0.02 3.782 3.765 2.06E-13 Selby/Hammersley TCS-H 0.2600 -1.15 0.01 1.636 1.645 3.27E-13 Alonso et al. 1994 TCS-K 0.3941 -1.31 0.01 2.160 2.158 1.40E-13 Alonso et al. 1994 TCS-L' 0.5725 -1.46 0.02 3.649 3.651 2.22E-14 Alonso et al. 1994 UKIRT87 0.8611 -1.38 0.01 8.770 8.780 6.86E-16 UKIRT Service data UKIRT98 0.9455 -1.46 0.01 9.843 9.913 4.70E-16 UKIRT Service data UKIRT12 1.1782 -1.48 0.01 12.432 12.414 1.90E-16 UKIRT Service data --------------------------------------------------------------------------- The "TCS" passbands are used at the Telescopio Carlos Sanchez of the Instituto de Astrofisica de Canarias: see Alonso et al. 1994, A&A, 282, 684. Selby et al. (1988) and independent higher precision measurements by Hammersley (1995) are available. Likewise, these TCS mags. represent an independent reduction by Hammersley of all the Tenerife broadband data on this star, originally made by Alonso et al. (1994). UKIRT filter set represents a series of narrowband 10 um passbands provided in common to UKIRT, Univ. Minnesota, and IRTF for "silicate" work. The "12" filter is centered near 12.5 um. Spectral fragments and portions of these actually used in observed spectrum ("used" may include combination with other data where overlaps occur). *** N.B. because of the complete absence of, and the impossibility of securing from the Kuiper Airborne Observatory, a complete 1.2-5.5 um spectrum of gam Dra, portions of the complete SEW shape of alp Tau's spectrum were inserted between our newly measured short wave segments. Both alp Tau and gam Dra have spectral type K5III, and the shapes of the new short wavelength fragments of gam Dra closely match the shape of the SEW alp Tau spectrum wherever they overlap. Portions substituted were confined to two regions opaque from the ground and shortward of our new KAO observations, namely from 1.76--2.02 um and from 2.43--2.92 um. *** Fragment Reference Total range Start and stop Average resolving (um) wavelengths (um) power NIR 1 1.24- 5.50 1.24- 5.50 50 NIR 1a 1.46- 2.43 1.46- 2.43 100 KAO 1b 2.92- 5.38 2.92- 5.38 160 KAO 2 4.74- 9.37 4.92- 8.99 180 8-13 3a 7.34-13.18 7.83-13.18 55 8-13 3b 7.87-13.14 7.83-13.14 55 LRS 4 7.67-22.74 7.67-18.44 30 LONG 5 1.22-35.00 18.50-35.00 -- References: 1. Strecker, Erickson, and Witteborn 1979, Ap.J. Suppl., 41, 501, for alp Tau, rescaled by 0.234 and inserted between fragments NIR-1a and NIR-1b below. 1a. Measurements with a CVF on the 1.5m TCS by Hammersley Dec. 3, 1994, from [gam Dra/alp Lyr]. 1b. HIFOGS data of May 5, 1995 KAO flight for [gam Dra/alp Boo]. 2. HIFOGS data of April 14 and May 5, 1995 KAO flights [gam Dra/alp Boo and [gam Dra/alp Lyr]. 3a. CGS3 UKIRT Service data of August 26, 1994 [gam Dra/alp Lyr]. 3a. CGS3 UKIRT Service data of August 31, 1994 [gam Dra/alp Lyr]. 4. LRSVAX version of Groningen database at NASA-Ames; spliced and recalibrated; also directly from the new complete Groningen LRS archive, calibrated with LRSCAL in GIPSY. 5. Engelke Fn. used for T=3986K and an angular diameter of 9.997 milliarcsec [mas] (Blackwell, Lynas-Gray & Petford 1991); we found the best fitting ang. diam. to be 10.17 mas. This Engelke Function was locked to the photometrically scaled combination of 8-13 and the LRS, by "splicing" longward of the SiO fundamental and used to replace the observations beyond 18.65 um, with an estimated uncertainty in EFn. of 2.6%, allowing for the change in shape of the EFn. for a temperature uncertainty of 100K. INFORMATION ON SPLICES AND BIASES INCURRED Process Factor determined +/-Bias% NIR cf. photometry 0.999 0.59 813 cf. photometry 1.100 0.56 LRS blue/red bias ..... 0.06 LRS splice to 813 1.010 0.05 KAO joint splice to NIR and merged 813/LRS 0.940 0.19 Engelke Fn. splice to combined 813/LRS 1.035 0.54 ============================================================================ 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. ============================================================================