HILIB Stellar Library Input Source Summary
   Spectral  Lumin.   Navail/  Lambda Range     R    A/  xBin  Usage                         Ref
      Types  Class     Nused                        pix   {a}  
SVID{b} O--M  I--V     98/98   1200--- 10500   50    50     -  SED, uv for late types           1
IUE     O--G  I--V    229/173  1153---  3201  500     2     2  uv for early types               2
GS      O--M  I--V    175/170  3160--- 10620  250 10/20     -  3200-3500A, 9000---10620A        3
KIEHL   F--M  I--V     60/59   3200---  8800  500    10     -  where available                  4
JHC     O--M  I--V    161/157  3510---  7427 1200   1.4     3  where available                  5
SC      O--M  I--V     72/52   3510---  8930  500     5     -  some doubtful types excluded     6
PIC     O--M  I--V     48/34   3600--- 10000  500     3     2  3900-10000A                      7 
N6522   K     III      16/15   3800---  6800  400     6     -  where available                  8 
SRBJ    GKM   I/III    21/19   4800---  8920 6000  0.43    10  where available                  9 
SRBJ    GKM   I/III     7/7    5000---  9783 1000   3.3     2  where available                  9 
DD      O-M   I--V    130/121  5804--- 10200  800     4     -  contin. fitted to SVID or GS    10 
LRV     O--M  I--V     84/83  14300--- 25000  500    ~7     -  where available                 11 
DBJ     O--M  I,III,V  40/36  15700---165000 2000   3/6   2/1  where available                 12 
KH      F--M  I--V     26/24  20100--- 24100 3000    ~2     4  contin. fitted to LRV or COHEN  13 
COHEN   AGKM  III,V    14/8   10000---350000  100   100     -  where available                 14 
FLUKS   M     III      11/11    995---125000 5000     1     8  Synthetic MIII spectra          15

Notes
{a}Binning of data prior to combination; the IUE, JHC and higher resolution SRBJ data were also 
slightly gauss filtered to match other data sets and conform to the chosen output resolution.
{b}SVID spectra were used to define the Spectral Energy Distribution (SED) for most types and to 
check other input spectra flux calibrations. They were included in the final combination when no 
other spectra were available; the uv of some late types, and a few other gaps.}
References
(1) Sviderskiene 1988; (2) Heck et al. 1984; (3) Gunn and Stryker 1983;
(4) Kiehling 1987; (5) Jacoby, Hunter and Christian 1984; (6) Silva and Cornell 1992;
(7) Pickles 1985; (8) Pickles and van der Kruit 1990; (9) Serote Roos, Boisson and Joly 1996;
(10) Danks and Dennefeld 1994; (11) Lancon and Rocca-Volmerange 1992;
(12) Dallier, Boisson and Joly 1996; (13) Kleinmann and Hall 1986; 
(14) Cohen et al. 1995, 1996a 1996b; 
(15) Fluks et al. 1994