SIMBAD references

I present data on the shell of classical Nova Persei (1901) obtained by the Advanced CCD Imaging Spectrometer S3 detector on board the Chandra X-Ray Observatory. The X-ray nebula is affected mostly by the complex interstellar medium around the nova and has not developed a regular shell. The X-ray nebula is lumpy and asymmetric, with the bulk of the emission coming from the southwestern quadrant. The brightest X-ray emission is detected as an arc that covers the region from the west to the south of the central source. Part of this feature, which is cospatial with the brightest nonthermal radio emission region, is found to be a source of nonthermal (synchrotron) X-ray emission with a power-law photon index of 2.3^+1.5_–0.9and α=0.68^+0.03_–0.15 at about a flux of 1.7x10^–13 ergs/cm2/s. This confirms that the shell is a site of particle acceleration, mainly in the reverse shock zone. There are strong indications for nonlinear diffusive shock acceleration occurring in the forward shock/transition zone with an upper limit on the nonthermal X-ray flux of 1.0x10^–14 ergs/cm2/s. The total X-ray spectrum of the nebula consists of two prominent components of emission (other than the resolved synchrotron X-ray emission). The component dominant below 2 keV is most likely a nonequilibrium ionization thermal plasma of kT_s=0.1-0.3 keV with an X-ray flux of 1.6x10^–11 ergs/cm2/s. There is also a higher temperature, kT_s=0.5-2.6 keV, embedded, N_H=(4.0-22.0)x10²²/cm2 emission component prominent above 2 keV. The unabsorbed X-ray flux from this component is 1.5x10^–10 ergs/cm2/s. The X-ray-emitting plasma is of solar composition except for enhancement in the elemental abundances (mean abundances over the remnant) of Ne/Ne_☉and N/N_☉in the ranges 13-21 and 1-5, respectively. A distinct emission line of neon, He-like Ne IX, is detected, which reveals a distribution of several emission knots/blobs and shows a conelike structure with wings extending toward the northwest and southeast at expansion velocities ∼2600 km/s in the X-ray wavelengths. The emission measures yield an average electron density in the range 0.6-11.2/cm3 for both of the components (fillingfactor=1). The electron density increases to higher values ∼300/cm3 if the filling factor is decreased substantially. The mass in the X-ray-emitting nebula is (2.1-38.5)x10^–4 M_☉. The X-ray luminosity of the forward shock ∼4.3x10³² ergs/s indicates that it is adiabatic. The shocked mass, the X-ray luminosity, and comparisons with other wavelengths suggest that the remnant has started cooling and most likely is in a Sedov phase.