We have observed the region of the hard X-ray transient EXS 1737.9 - 2952 near the Galactic Centre using the Narrow Field Instruments ( NFI ) of the BeppoSAX X-ray satellite .
In this second part of our investigation we report on our spectrum analysis and time variability study of the field .
The main results are the MECS spectra of each of the 10 identified sources in the interval 1.65 - 10 keV and spectral fits of the source data .
The fluxes obtained with the spectral fits are 1.7 - 4.8 \cdot 10 ^ { -12 } \mbox { erg } \mbox { cm } ^ { -2 } \mbox { s } ^ { -1 } .
The absorption for the sources with powerlaw and Raymond-Smith thermal plasma models is in the range N _ { H } = 0.5 - 6.7 \cdot 10 ^ { 22 } \mbox { cm } ^ { -2 } .
The low number of counts and lack of source identifications in the simultaneous 0.1 - 2 keV LECS data of the same field supports high absorption .
This indicates that these sources are at least at the distance of the Galactic Centre .
From the distance estimate a lower limit for the X-ray luminosity L _ { x } \approx 2 - 5 \cdot 10 ^ { 34 } erg/s ( 2 - 10 keV ) is obtained .
A powerlaw with a photon index in the range \alpha = 1.1 - 1.8 generally gives a fair fit to the data , but strong line contribution ( iron line at 6 - 7 keV ) is evident for 5 sources and exists at lower confidence also in the other 5 sources .
The fits indicate differences in line position in the range 6.1 - 7.0 keV suggesting that the ionisation state and/or emission mechanism may not be the same in all sources .
The Raymond-Smith model for the 5 sources with reasonable spectral fit yields \mathrm { k } T \approx 8 - 10 keV .
Due to the low S/N of the data , other line parameters are not used in our analysis .
A \chi ^ { 2 } -analysis of the time-binned data indicates that two of the sources are variable on a time scale of hours at very high confidence ( > 99.99 % ) , and one source with lower confidence ( 99.67 % ) .
The scale ( \sim hours ) of the time variability indicates that these sources could be low-mass X-ray binaries .
The other sources are most probably high or low mass X-ray binaries or supernova remnants .
We also extracted and analysed spectra from larger subfields in the observed MECS region .
A subfield including 8 of the new sources and a major contribution of diffuse emission between them yielded a fairly good fit to a power-law spectrum with photon index \alpha = 1.3 and a strong iron line at 6.8 keV , but a poor fit to a Raymond-Smith and bremsstrahlung model for a single source .
A spectral fit to another field with only residual emission and no point sources yielded spectral parameters close to the diffuse emission near GC observed by other investigators , except for the high interstellar absorption ( N _ { H } \approx 2.0 \cdot 10 ^ { 22 } \mbox { cm } ^ { -2 } ) .
The PDS spectrum at harder X-rays centred on the same position was also observed .
Due to lack of spatial resolution , and a FOV larger than that of MECS , this spectrum was more difficult to interpret .
The largest contribution of the spectrum is probably by 1E1740.7 - 2942 .
It is reasonably close to the centre of PDS collimator field , and also the observed flux matches the prediction .
The source for the hard X-ray transient EXS 17137.9 - 2952 can not be identified from the present observations .