/asl/data/hitran/H2016/LineMix/LM_calc_CO2_2017_kcarta_5ptboxcar_newdir.for or earlier versions.

/home/sergio/KCARTA/WORK/RUN_TARA/GENERIC_RADSnJACS_MANYPROFILES... /JUNK_HITRAN_370ppmCO2_PERTURBS_forITOVS/compare_HT2016_GE2015.m **

Our CO₂ spectroscopy (line mixing + Birnbaum) was developed around 2000, and may be out of date. The Birnbaum and line-mixing parameters were fit to HITRAN 1998 CO₂. We are no longer pursuing this approach.

J.M. Hartmann made his line-mixing code available in 2008 or so. Our evaluation of it produced similar results to kCARTA, but the differences did not seem to warrant our adoption of it.

We now have LBLRTM versions 12.4 12.8 running at UMBC. More recently we started evaluating LBLRTM and decided to use it for CO₂ optical depths in our more recent version of SARTA. In addition, LBLRTM also implemented CH₄ line-mixing, which we have never worked on, so the more recent kCARTA CO₂ and CH4 database uses the LBLRTM CO₂ CH4 ods, and our run8 optical depths for every other gas (using the HITRAN 2016 database).

In 2016, the group working on the HITRAN database at the Harvard University Center For Astrophysics released a new LineMixing code, based on the latest coefficients by Niro and Lamoreaux. This webpage mainly details our ongoing comparisons to the latest version of this database, and the accompanying LM code.

As with all the monochromatic optical depths used by kCARTA, both the original HITRAN LM code, and my modifications to the code, have been run through the US Standard profile for 11 temperature offsets, and then compressed so they can be used with kCARTA.

A : Simple changes (should not significantly affect output ODs)

1. File access changed from /data_new to ../LineMix2/Updates_LMCO_{2}_HITRANonline2018/data_new
2. In parameters.inc updated the Qtips coeffs and the isotope masses
3. Now using QT_CO_{2}_sergio instead of QT_CO_{2}

B : Physics changes (could affect output ODs if not done correctly)

1. Changed code so it not only uses bands between SigMinR and SigMaxR but also uses sigMinR-xfar to SigmaxR+xfar, xfar=500.0 in run8, but I used 1250 here, maybe overkill?
2. Changed rdmult from 30 to 1000000 (distance in multiples of GamD after which you switch from voigt to lorentz). See /home/sergio/SPECTRA/doppler_widths_wavenumber.m (typical doppler widths ~ 1e-3) at 667 cm-1, typical width = 5e-4 ==> 5e-4 * 1e6 = 500 cm-1
3. The original LM code only used \(\nu \times (1-exp(-c_2 \nu/T))\) as an adjustment. I updated code so that every line in the CO2 database has the following radiation term

\begin{equation} \nu_i \times \frac{(1-e^{-c_2 \nu_i/T})} {(1-e^{-c_2 \nu_i/T_o})} \end{equation}

where \(T_o\) is 296 K.

The comparisons in Figure 1 below show comparisons between the original and modified HITRAN LM codes, compared to LBLRTM 12.8. The results are averaged over the UMBC 49 regression profiles

The upper panels of Figure 1 are comparisons using my modifications to the LM package, while the lower panels are comparison using the original LM package.

Note that while the original code looks better, it only used the bands that lay within the 25 cm-1 chunks I was building. The modified code looks far worse in the 8-10 um window region, but it used bands that also lay outside the 25 cm-1 chunks I was building (see change number 4), so that should technically be more correct. So it would appear that changes 5 or 6 are the likely cause of the increased OD in the 8-10 um region which cause a positive bias.

Figure 2 I is a slide from J.M. Hartmann's presentation at the HITRAN 2018 meeting (Cambridge, MA in Summer 2018) depicting the CO₂ collision-induced absorption that he and Ha Tran have been working on. See also /home/sergio/PAPERS/AIRS/airs_stm_oct18/SARTA/sergio_rta.pdf

For completeness, Figure 3 shows comparisons of LBLRTM 12.8 versus LBLRTM 12.4 and versus our older UMBC CO₂ line mixing. The UMBC CO₂ linemixing is what is in the current AIRS SARTA, while the LBLRTM 12.4 is in the most recent CrIS FSR SARTA.

Figure 4 shows the effects of the various CIA (from JM Hartmann and H.Tran) and are always (BT without- BT with CIA), for the 49 regression profiles. The baseline CO₂ ods were LBLRTM12.8 but since we are always adding on CIA, the plots should not depend on this.

The three graphs are presented in a slightly different way in Figure 5. Here the BT difference between (basic - cia) at 2400 cm-1 is shown as a function of column water amount for the 49 regression profiles, showing that indeed the Hartmann CIA lineshape(s) are dependent on water amount.

1. kcarta now has the JM Hartmann CIA (co2/n2 and co2/h2o) terms. They are independent of any compressed database and have to be tuned on. I plan to include them in comparisons soon (done 11/12/2018)
2. Collect actual "clear sky" observations, match to sondes (or NWP) and then compare to calculations made from the various CO₂ databases we have : UMBC 2000 linemixing, LBLRTM 12.4, LBLRTM 12.8 and HITRAN LM
3. In the meantime I can individually test some of my code changes to the LM code. The three main changes to test are points 4,5 and 6 in Section (4) above.

1. For now, continue use the CO₂ optical depths generated using LBLRTM 12.8
2. Continue testing the LM code and the CIA optical depths, against LBLRTM 12.8 as outlined above in Section 5.

1. Update 11/27/2018 : went back to the orig LM radiation term (Sect 4, point 6) and turned rdmult down to 1000.0; this had the effect of removing the bias at 8-10 um, as hoped/expected.

Notice the the difference between the radiance calcs using "original LM code" and this latest incarnation, look like a 2 ppm offset (see Figure 6). Indeed, in the /home/sergio/KCARTA/WORK/RUN_TARA/GENERIC_RADSnJACS_MANYPROFILES/template_Qrad.nml file I see a comment that I used a multiplier such that the CO2 was adjusted to 383 ppm instead of 385 ppm.

1. Have been using pretty old (about 2006) O2-O2 and N2-N2 continuum. Have now upgraded them to use

the MT-CKD3.2 continuums. The code has been incorporated as the default version of run8.m. Note I just wrote a matlab wrapper that shell escapes and calls the MT-CKD3.2 code, rather than copying the code and mexing it. Data is in /home/sergio/KCARTA/WORK/RUN_TARA/GENERIC_RADSnJACS_MANYPROFILES/JUNK_HITRAN_370ppmCO2_PERTURBS_forITOVS/N2_O2_MTCKD3.2. Figure 7 shows the difference between (new-old) N2 continuums, in delta BT at TOA space after averaging over the 49 regression profiles.

1. For tropical profile, ran off kcarta to see how CIA affects the TOA radiance, and also to see how large

the CIA ODs are. See code in /home/KCARTA/WORK/RUN_TARA/GENERIC_RADSnJACS_MANYPROFILES/JUNK_HITRAN_370ppmCO2_PERTURBS_forITOVS/N2_O2_MTCKD3.2/run_kc_n2_co2.m

Figure 8 shows the results. The left panel shows the Gnd2Space optical depth for N2, CO2/WV CIA and N2/WV CIA. Work by Ha tran focuses on the 2380 cm-1 bandhead, and there (in blue) is the CO2/WV CIA. The panel on the right shows how the TOA BT changes. Note for the "default" case we used CKD3.2 while for the CIA cases we used CKD 1.0