Part 2:Validation for line lists generated for nitric acid (H14N16O3) for the ν1 band and its first two associated hot bands (ν1+ν9-ν9, ν1+ν7-ν7) in the 2.8 μm region, the ν1-ν9, ν1+ν9 and ν1+ν7 bands at 3.2 μm, 2.5 μm and 2.4 μm, respectively

Fits to a solar occultation spectrum measured at 21.7 km tangent altitude from balloon above Esrange, Sweden in Dec. 1999 (Black points). The residual trace represents the difference of the measured and calculated transmittances. Colored lines represent the contributions of individual gases (Red: HNO 3 ; Yellow: CO 2 ; Green: H 2 O; Blue: Other). The HITRAN 2020 line list was used to represent the non-HNO 3 absorptions -- mainly CO 2 and H 2 O. For the HNO 3 line list we used: (a) HITRAN (i.e., none), (b) ExoMol computed for 220K, (c) the JPL empirical pseudo-line-list, and (d) the HNO 3 line list from this work. Each panel shows improved spectral fits compared with the previous panel, from 8.84% RMS in panel (a) to 1.77% RMS in panel (d). [Display omitted] • Validation of the linelist generated for HNO 3 at 2.8 μm (ν 1 cold band at 3551.7 cm−1 and the hot band) and at 3.2 μm (ν 1 -ν 9), 2.5 μm (ν 1 + ν 9) and 2.4 μm (ν 1 + ν 7); Comparison with the Pacific National Northwest Laboratory cross sections for HNO 3 ; Comparison with high resolution spectra recorded in laboratory conditions (SOLEIL synchrotron); Comparison with high resolution stratospheric solar occultation spectra recorded by the MkIV balloon-borne instrument of the Jet Propulsion Laboratory (JPL); Similar inter-comparisons performed using the pseudo-line list generated by the JPL laboratory and the ab initio ExoMol list calculated by the University College of London. This is the second of two back-to-back works, whose goal is to generate line lists for the ν 1 band (3551.766 cm−1) and for the ν 1 +ν 9 -ν 9 and ν 1 +ν 7 -ν 7 hot bands for HNO 3 in the 2.8 μm region. Also, we computed line lists for the weaker ν 1 -ν 9 , ν 1 +ν 9 , and ν 1 +ν 7 bands, centered at 3093.53 cm−1, 4006.97 cm−1 and 4127.78 cm−1, respectively. While the first paper (Ref. [1] , the preceding article in this issue), here labeled as "Part-1", was devoted to the description of the determination of the needed spectroscopic parameters in term of line positions and intensities, this paper describes the resulting line lists and the validation process. For this task, we use laboratory spectra recorded at high resolution and described in Part-1, together with the cross-sections established by the Pacific Northwest Laboratory at low resolution. Also, we use high resolution stratospheric solar occultation spectra recorded by the MkIV balloon-borne instrument of the NASA Jet Propulsion Laboratory (JPL). Similar inter-comparisons with laboratory or atmospheric spectra are also performed using the pseudo-line-list generated at JPL in 2005 and with the ab initio ExoMol list calculated by the University College of London. It proves that the line list generated during this work provides significant better agreements between observed and computed spectra. [ABSTRACT FROM AUTHOR]