"In response to the 18 April 2001 flare of SGR 1900+14 (GCN 1041) the Chandra X-ray Observatory has undertaken a sequence of two public 20-ksec observations of this source, on 22 and 30 April 2001.

The first observation began at 04:58 UT on 22 April and was taken in continuous-clocking mode (see also GCN 1046). Examination of the light curve reveals that at least one burst was observed, 9081 s after the start of the observation. Assuming the best-fit spectral parameters for the observation (see below), the peak 1-s flux of this burst was of order 5e-10 erg cm^-2 s^-1 (0.5-10 keV).

Spectral fits to the full background-subtracted data set allow for at least two emission models. A power-law plus absorption model has best-fit parameters of N_H = 3.18(2)e22 cm^-2, photon index alpha = 2.70(1), and unabsorbed 0.5-10 keV flux of 4.20(4)e-11 erg cm^-2 s^-1. A power-law plus blackbody and absorption model has best-fit parameters of N_H = 2.56(2)e22 cm^-2, photon index alpha = 1.88(1), blackbody temperature kT = 0.532(3) keV, unabsorbed 0.5-10 keV flux of 2.17(3)e-11 erg cm^-2 s^-1, and flux fraction for the blackbody component of 29% (0.5-10 keV). The addition of the blackbody component is not supported by an F-test (65% confidence level) but is consistent with models in the literature (Perna et al. 2001, astro-ph/0103273). Analysis of the RXTE PCA data may help to clarify the presence or absence of the blackbody component, as the PCA count rates inferred from the two models given above differ by 50%.

No narrow spectral features are apparent. The two-sigma upper limit to the flux of a persistent 0.2-keV FWHM emission line in the 5-7 keV range is 1e-5 photons cm^-2 s^-1.

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