SIMBAD references

S. Mazuk, D. K. Lynch, R. J. Rudy, R. W. Russell, R. L. Pearson, The Aerospace Corporation; C. E. Woodward, University of Minnesota; R. C. Puetter, Center for Astrophysics and Space Science, University of California at San Diego; and R. B. Perry, Langley Research Center, NASA, report 0.4- to 2.5-micron spectroscopy of this nova (cf. IAUC 8821) using the Lick 3-m telescope (+ VNIRIS) on May 7 UT, as well as 0.8- to 5.5-micron spectroscopy using the Infrared Telescope Facility 3-m telescope (+ SpeX) on May 31. The spectrum increased in excitation between the two epochs, displaying coronal lines of [Si VI], [Si VII], [Ca VIII], [S VIII], and [S IX] at the later date. All coronal lines had complex profiles. He II emission was also present, in addition to the unidentified novae lines (Rudy et al. 2002, Ap.J. 573, 794) at 1.11, 1.19, 1.55, and 2.10 microns. Despite the presence of these high-excitation features, emission from C I, N I, and O I persisted. There was no evidence of dust formation. The interstellar reddening derived from the O I lines was E(B-V) = 1.5.