We have studied the spectral energy distribution of the quasar LBQS 0102-2713 .
The available multiwavelength data in the observers frame are one optical spectrum between 3200 and 7400 Ã Â ( Morris et al .
1991 ) , 7 HST FOS spectra between 1700 and 2300Â Ã Â ( York et al .
1990 ) , one GALEX NUV flux density and a K _ { S } magnitude obtained from NED , and 3 public ROSAT PSPC pointed observations in the 0.1 - 2.4 keV energy band .
The \alpha _ { ox } values obtained from the HST FOS- , the optical spectrum , and the ROSAT observations are -2.3 and -2.2 , respectively , comparable to BAL quasars ( e.g .
Gallagher et al .
2006 ) .
The 2500Â Ã Â luminosity density is about a factor of 10 higher compared to the mean of the most luminous SDSS quasars ( Richards et al .
2006 , their Fig .
11 ) .
The 2 keV \nu L _ { \nu } value is lower by about a factor of 10 compared to the radio loud quasars shown in Fig .
10 of Richards et al .
( 2006 ) .
LBQS 0102-2713 exhibits one of the steepest soft X-ray photon indices obtained so far .
For a simple power law fit with leaving the N _ { H } free in the fit we obtain a photon index of \Gamma = 6.0 \pm 1.3 .
Fixing the N _ { H } value to the Galactic value the photon index still remains steep with a value of about 3.5 .
We argue that LBQS 0102-2713 is similar to BAL quasars with respect to their UV brightness and 2 keV X-ray weakness .
However , the absorption by neutral matter is significantly lower compared to BAL quasars .
The X-ray weakness is most probably not due intrinsically X-ray weakness based on the UV line strenghts which are comparable to the line strength values reported in quasar composites ( e.g .
Brotherthon et al .
2001 , Vanden Berk et al .
2001 , or Zheng et al .
1997 ) .
If the X-ray weakness will be confirmed in future observations , LBQS 0102-2713 might be indicative for a new class of quasars with an unusual combination in their UV- , X-ray , and N _ { H } properties .