Information about table 1:

2. Name: Name of the star

3. Sp T.: Spectral Type obtained using the method described in Hernández et al (2003).
   Link => Spectral Information about the object.
           Spectral Type and its error
           Numerical Results from each useful index.
           Emission lines measured on the spectrum     (Element    central wavelength    Equivalent Width)
           Abnormal features on the spectrum.          (Element    central wavelength    Equivalent Width)
           Previously published spectral types.

     The numerical scale applied  in the method is:    

 
     The indices used to obtain the spectral type are:

                                Index    Element         Central Wavelength (A)
                                1        CaII(K)         3933
                                2        HeI             4026
                                3        FeI+ScI         4047
                                4        Hdelta          4102
                                5        HeI+FeI         4144
                                6        CN+FeI          4175
                                7        CaI             4226
                                8        FeI             4271
                                9        CH (Gband)      4305
                                10       Hgamma          4349
                                11       HeI+FeI         4387
                                12       MnI+FeI         4458
                                13       HeI+FeI+MnII    4471
                                14       MnII            4481
                                15       FeI+MnII        4490
                                16       FeI             4532
                                17       HeII+OII+FeI    4669
                                18       FeI             4787
                                19       HeI+FeI         4922
                                20       HeI+FeI+TiI     5016
                                21       FeI+TiI+CrI     5079
                                22       FeII+MgI        5173
                                23       CaI+FeI         5270
                                24       FeI             5329
                                25       FeI             5404
                                26       CaI+TiO         5589
                                27       FeI+MgI         5711
                                28       HeI+NaI         5876
                                29       NaI+TiI         5890
                                30       MnI             6015
                                31       CaI             6162
                                32       HeI             6678
                                33       HeI             7066

4.    Err: Error of the calculated spectral type  ( in subclasses)

5.    Halpha: Equivalent Width of H alpha (A) :
      Link => Profile at the Balmer line H alpha (6463A - 6663A)
       The flux was normalized at the nearby continuum bands.

6.    Spectrum (View): Link => FAST spectrum of the object (To see)
       The flux was normalized at 5500 A.
       The detector response was taken out using spectrophotometric standard stars and the IRAF sensfunc task.
       Warning: This procedure is not a flux calibration of the spectrum.

7.    Spectrum (Load): Link => Spectrum of the object in FITS format (To load)

        Observations were done at the 1.5 meter telescope of the Whipple Observatory with the FAST Spectrograph, equipped with the Loral 512 x 2688 CCD (15 microns square pixels).  The spectrograph was set up in the standard configuration used for FAST COMBO projects: the 300 groove mm^{-1} grating and a 3''  wide slit. This combination offers 3400A of spectral coverage centered at 5500A, with a resolution ~ 6A.

8.    Image: Finding chart of the object.

       Link = >Image 0.2 x 0.2  degree from the Digital Sky Survey (Sky View).
       Object labeled are taken from Herbig and Bell catalog (1988).
       The object labeled number 1 is the selected star.

9.    SEDs: Link => Spectral energy distribution (U-L) of the star using optical and near infrared photometry (Table 2).

       We used the following filter wavelength (WL) and flux densities (fo) for the A0 (magnitude=0) star to
       transform magnitudes to fluxes.

       The magnitude (mo) corrected for absorption (mo=m-Am) was calculated using the relations from Cardelli et al (1989) and the Av
       derived from the color excess E(B-V) using different extinction law (Rv=3.1 and Rv=5.0)

       Av=Rv*E(B-V)

        Objects without spectral type in Hernández et al (2003) were plotted using an estimated type, taken from Table 10, column 6, in Hernández et al (2003), previously published spectral types were used for the continuum stars. The nominal error was set as one spectral type. These SED should de used with caution. See Hernández et al (2003) for details.

10.     LightCurv: number of V measurements for each object.

        Link => Light curve of V magnitude and the colors U-B, V-B and V-Rj (figure postscript)

       The line at the upper panel (V magnitude) show the median value of the data.
        The plot also show the information about the median values of colors U-B, B-Vand V-Rj.
        If are available, we give the median values of Rj-Ij, V-Rc, and  Rc-Ic  at the top of each figure.
       These data was obtained from Van Vleck Observatory database (Wesleyan University).
        Description of these data are at Herbst and Shevchenko (1999).

11.    REF(1960-2002): Link => References for the object until 2002 (SIMBAD)

12.    Comment: Comments about the object.