In this tutorial,
- The energy band structure of CsPbI3 is computed in both an ideal cubic structure, and also a pseudocubic structure, using the LDA code lmf.
- Corresponding calculations are carried out using the ASA code lm, and results compared.
- A QSGW calculation is carried out, which modifies the band structure and widens the bandgap.
This tutorial is self-contained. It is required to prepare necessary inputs to the Levenberg-Marquardt tutorial which makes small adjustments to the ASA potential parameters to fit the ASA bands to QSGW bands.
You may wish to go through the introductory tutorial for the ASA, if you haven’t already done so.
** Cubic structure **
** Pseudocubic structure **
** QSGW **
** Levenberg-Marquardt **
CsPbI3 is a close cousin of NH3CH3PbI3 (usually called MAPI). They are in the family of perovskites that have attracted a great deal of attention recently because of their considerable potential as efficient, low-cost solar cells.
CsPbI3 has, on average, a cubic structure. However, the PbI3 cage flexes rather dramatically in time, roughly on the scale of a phonon period, distorting the underlying cubic structure and changing the instantaneous band structure. MAPI flexes in a similar way, but CsPbI3 is simpler so this tutorial is written for it. The effect of distortions on the band structure is significant, and it is the subject of this tutorial. It is based on a paper analyzing the effects of nuclear motion in CHNHPbI and CsPbI.
This tutorial develops the energy bands for CsPbI3 in its ideal cubic structure, and a pseudocubic structure which approximates the flexing of the system at room temperature.
Copy the following box to file site0.cspbi
% site-data vn=3.0 xpos fast io=15 nbas=5 alat=11.82540057 plat= 1.0 0.0 0.0 0.0 1.0 0.0 0.0 0.0 1.0 # pos Pb 0.0000000 0.0000000 0.0000000 Cs 0.5000000 0.5000000 0.5000000 I 0.5000000 0.0000000 0.0000000 I 0.0000000 0.5000000 0.0000000 I 0.0000000 0.0000000 0.5000000
and the box below to site0.dcspbi.
% site-data vn=3.0 xpos fast io=15 nbas=5 alat=1.88972688 plat= 6.2887979 0.0 0.0 0.0015427 6.2287686 0.0 0.1397332 -0.0003656 6.3725603 # pos Pb 0.4448840 -0.5000200 -0.0223770 Cs 0.0094815 0.0000333 -0.4695814 I 0.4094870 -0.5000180 0.4751450 I 0.3992710 -0.0000420 0.0236640 I -0.0676570 0.4999950 -0.0775210
and the box below to syml.cspbi.
#Template file generated by Syml_template.py 31 0.500000 0.500000 0.000000 0.500000 0.500000 0.500000 M to R 41 0.500000 0.500000 0.500000 0.000000 0.000000 0.000000 R to G
LDA energy bands, calculated with lmf
Use site0.cspbi to create the input file
blm --pr55 --nfile --rdsite=site0 --nosort --shorten=no --nk=4 --gw --wsitex@fn=site1 --gmax=8 cspbi cp actrl.cspbi ctrl.fp cp site1.cspbi site.fp
Command line switches to blm are explained here.
Make the system self-consistent and draw energy bands
lmfa ctrl.fp cp basp0.fp basp.fp lmfa ctrl.fp lmf ctrl.fp >out.fp cp syml.cspbi syml.fp lmf ctrl.fp --band~mq~fn=syml
LDA-ASA energy bands, calculated with lm
The ASA doesn’t have a Mattheis construction to supply a reasonable starting guess the charge density, as lmf does. On the other hand, because it is the ASA, it is able to store information about the density in a highly compact way1.
- Extract l resolved sphere charges generated by lmf
- The ASA contracts all the information about the density into energy moments of the sphere charges 1, for each l. This step is not necessary, but it makes use of moments generated by lmf as input to the ASA. Thus it supplies a reasonable starting guess for the density.
blm --pr55 --nfile --rdsite=site0 --nosort --shorten=no --nk=4 --asa~pfree~rmaxs=10 --wsitex@fn=site cspbi cp actrl.cspbi ctrl.asa cp site.cspbi site.asa lmf ctrl.fp --asars2 cp rsta.fp rsta.asa lm ctrl.asa -vnit=0 --rs=1
Note that there is missing charge. From the end of the output of the last step you should see
Sum Q=-6.262774 Emad=-0.724614(-3.110233) Vmtz=-0.279207
We will address the deviation from charge neutrality by adding empty spheres, and adding charges to them to satisfy charge neutrality.
- Autogenerate empty spheres
- Use blm to remake the ctrl.asa, but this time locating empty spheres.
blm --pr55 --nfile --rdsite=site0 --nosort --shorten=no --nk=4 --asa~pfree~rmaxs=10 --wsitex@fn=site cspbi --findes~rmin=1.5~omax=0~sclwsr=20~nspmx=3
Note the --asa switch.
- pfree inserts a line into ctrl.cspbi to keep the continuous principal quantum number Pl from falling too low
- rmaxs=10 sets the range of the tight binding structure constants. The entire family of command line switches is explained here.
Compare site.cspbi and site.asa. They should be the same except for the addition of empty spheres.
Use the –zerq command-line switch to tell lm to add charges to empty spheres in a manner that charge neutrality is satisfied.
cp site.cspbi site.asa cp actrl.cspbi ctrl.asa lm ctrl.asa -vnit=0 --zerq~es~add~qin
You should see these lines near the beginning of stdout
asazerq : system charge is now -6.262774 adding charge 0.956974 to s channel, class 1 adding charge 0.423982 to s channel, class 2
lm added electrons to the s channel in the empty spheres, in proportion to their volumes, so that the total extra charge makes the system neutral. You should see this table at the end of stdout
Class Qtot Qbak Vmad Vh(Rmax) V(Rmax) Pb -1.324686 0.000000 0.516047 -0.286793 -0.807596 Cs -1.361714 0.000000 0.991409 0.166127 -0.285513 I -1.192124 0.000000 0.697869 -0.024630 -0.551172 E 0.956974 0.000000 -0.421284 0.176218 -0.299758 E1 0.423982 0.000000 -0.312501 0.034746 -0.434927 Sum Q=0.000000 Emad=0.432771(-3.399443) Vmtz=-0.453235
The E sphere has twice the volume of the E1 sphere, so it gets twice the charge.
We now have a good starting point for a self-consistent ASA calculation.
- Self-consistent ASA, first attempt
- Drive the density to self-consistency, and make the energy bands.
lmstr ctrl.asa rm -f mixm.asa sv.asa log.asa lm ctrl.asa -vnit=100 > out.asa
The density converged smoothly, as can be seen by inspecting the first column of sv.asa.
See this page for a description of the program flow in lm, how it manages the charge density and iterates towards self-consistency.
Create the energy bands:
cp syml.cspbi syml.asa lm ctrl.asa -vnit=100 --band~mq~col=1:9~col2=10:18~col3=19:45~fn=syml
LDA (blue) and first attempt at LDA-ASA energy bands of CsPbI3. Note the spurious band at 3 eV in the ASA.
The energy bands compare favorably to the full LDA calculation, except for a spurious flat state near 3 eV.
This is a Pb 6d state. You can establish this out by using using color weights to distinguish the Cs, Pb, and I characters. Invoke
lm ctrl.asa --pr55 --quit=ham
The table tells you to choose color weights 1:9 for Pb, 10:18 for Cs and 19:45 for I.
lm ctrl.asa --band~mq~col=1:9~col2=10:18~col3=19:45~fn=syml echo -8,6,5,10 | plbnds -fplot~sh -ef=0 -scl=13.6 -lt=1,col=0,0,0,colw=1,0,0,colw2=0,1,0,colw3=0,0,1 -lbl=M,R,G bnds.asa
The flat state at 3 eV is bright red, showing that is of Pb character. You can make further use of the color weights to establish that it is a Pb d state (we won’t do that here).
- Self-consistent ASA
The spurious state or “ghost band,” 2 must be removed before proceeding. In this particular instance the problem can be fixed simply by reducing the overlap between the Pb and empty spheres. But this is a special case. For pedagogical reasons, we point out three other ways to solve the problem.
- Option 1 : Downfold the Pb 6d.
- Set IDXDN to 2 in the Pb d channel and iterate to self-consistency
cat actrl.cspbi | sed 's/\(ATOM=Pb.*IDXDN=0,0\),0/\1,2/' > ctrl.asa rm -f mixm.asa sv.asa log.asa lm ctrl.asa -vnit=100 > out
Draw the energy bands of the downfolded hamiltonian
lm ctrl.asa -vnit=100 --band~mq~col=1:4~col2=5:13~col3=14:40~fn=syml echo -8,6,5,10 | plbnds -fplot~sh -ef=0 -scl=13.6 -lt=1,col=0,0,0,colw=1,0,0,colw2=0,1,0,colw3=0,0,1 -lbl=M,R,G bnds.asa
The spurious state is gone; now the bands compare favorably with the full LDA result.
Note: this method has one drawback: namely that the layer Green’s function code lmpg does not have downfolding capability.
- Option 2. Freeze the Pb 6d Pnu at a higher linearization energy
- Set IDMOD to 1 in the Pb d channel; replace P the Pb d (now at about 6.15) with 6.2, and iterate to self-consistency
sed -i 's/\(2 6.[0-9]*\) / 2 6.2 /' pb.asa cat actrl.cspbi | sed 's/\(ATOM=Pb.*\)/\1 IDMOD=0,0,1/' > ctrl.asa rm -f mixm.asa sv.asa log.asa lm ctrl.asa -vnit=100 > out lm ctrl.asa -vnit=100 --band~mq~col=1:9~col2=10:18~col3=19:27~fn=syml echo -8,6,5,10 | plbnds -fplot~sh -ef=0 -scl=13.6 -lt=1,col=0,0,0,colw=1,0,0,colw2=0,1,0,colw3=0,0,1 -lbl=M,R,G bnds.asa
These bands are practically indistinguishable from Option 1.
- Option 3 : Replace the Pb 6d with Pb 5d.
- Replace P on the Pb with 5d. So far we have treated the Pb 5d as a core state. This will improve the treateent of the the Pb 5d, but in the region of the Fermi level, Pb has more 6d than 5d character near the Fermi level, so we might expect this method to be a little less accurate.
In setting up the starting conditions the Pb moments are now completely out of whack, since Pb 6d and Pb 5d are very different. Rather than try to guess Pb moments, instead we can remove the Pb atom file, let lm choose some moments taken from the free atom, and scale the charge on that atom to enforce charge neutrality.
cat actrl.cspbi | sed 's/\(ATOM=Pb.*\)/\1 P=0,0,5.93/' > ctrl.asa rm pb.asa lm ctrl.asa -vnit=0 --zerq~qin~ic=1 rm -f mixm.asa sv.asa log.asa lm ctrl.asa -vnit=100 > out lm ctrl.asa -vnit=100 --band~mq~col=1:9~col2=10:18~col3=19:45~fn=syml
Agreement now is bit worse, as the Figure shows. Pb d partial waves do have some effect near the Fermi level.
Here we adopt option 1, and also adjust the ES positions to reduce overlaps. This is automatically done with the lmchk utility.
cp site.asa site1.asa lmchk -vfile=1 ctrl.asa --mino~z --wsite@short@fn=site cat actrl.cspbi | sed 's/\(ATOM=Pb.*IDXDN=0,0\),0/\1,2/' > ctrl.asa
The largest atom-ES overlap, initially 16%, drops to 12.8%. Make the system self-consistent and draw the energy bands.
rm -f mixm.asa sv.asa log.asa lmstr ctrl.asa lm ctrl.asa -vnit=100 lm ctrl.asa -vnit=100 --band~mq~col=1:4~col2=5:13~col3=14:40~fn=syml echo -8,6,5,10 | plbnds -fplot~sh -ef=0 -scl=13.6 -lt=1,col=0,0,0,colw=1,0,0,colw2=0,1,0,colw3=0,0,1 -lbl=M,R,G bnds.asa
LDA (blue) and LDA-ASA energy bands of CsPbI3, with the Pb 6d folded down.
Bands no longer have a spurious state at 3 eV, and they are in reasonable agreement with the full LDA result.
Compare site0.dcspbi and site0.cspbi. They are basically the same structure, with relatively modest distortions, but:
- alat and plat are distributed differently: plat(i,i) is about 6.2, corresponding to the (slightly distorted) cube edge in Angstroms. This data was extracted from a VASP POSCAR file.
- Some sites are translated by approximate integer multiples of lattice vectors (approximate because of distortions)
- The order of the Iodine sites is permuted.
It is convenient to render the site file of the distorted lattice as near as possible to the undistorted one. Then comparisons are simpler to make. A combination of switches in the blm and lmscell make this easy work.
LDA energy bands, pseudocubic structure
blm can eliminate difference (1) with the --scala switch, and most of the differences in lattice translations elminated with the --xshft switch.
blm --pr55 --scala=6.25772999 --nfile --rdsite=site0 --nk=4 --gw --wsitex@fn=site1 --gmax=8 dcspbi --xshftx=-.5,.5,0 cp actrl.dcspbi ctrl.dfp cp site1.dcspbi site1.dfp
site1.dfp and site.fp are much closer to each other. The superlattice editor lmscell --stack can undo the permutation of Iodine sites with the ~sort option, and it can clean the up the one remaining difference in the translation vector (Cs) with the ~addpos option.
lmscell -vfile=1 ctrl.dfp --stack~sort@targ=1,2,5,4,3~addpos@dp=0,1,1@targ=2~wsitex@short@fn=site
site.dfp and site.fp are as similar as they can be: the remaining differences are all connected with distortions, which is the property of interest.
Use lmf to make self-consistent and draw the energy bands. Here we can re-use the basis set from the undistorted lattice.
cp basp.fp basp.dfp lmfa ctrl.dfp lmf ctrl.dfp >out.dfp cp syml.cspbi syml.dfp lmf ctrl.dfp --band~mq~fn=syml
Notice that the gap in the pseudocubic structure is 1.58 eV, almost 0.3 eV larger than the gap of the cubic structure. This change is important for the hybrid perovskite devices.
To find the gap, do
grep gap out.fp out.dfp
LDA-ASA energy bands, pseudocubic structure
The procedure follows that of the cubic structure, but we can reuse site and ctrl files from prior calculations.
- Extract l resolved sphere charges from the lmf calcualtion
cp ctrl.asa ctrl.dasa cp site.dfp site.dasa lmf ctrl.dfp --asars2 cp rsta.dfp rsta.dasa lm ctrl.dasa -vnit=0 --rs=1
- Add empty spheres
- Take the empty spheres from the cubic lattice, and use the overlap minimizer to optimize their positions:
cp ctrl.asa ctrl.dasa cp site.dfp site1.dasa tail -11 site.asa >> site1.dasa sed -i 's/nbas=5/nbas=16/' site1.dasa lmchk -vfile=1 ctrl.dasa --mino~z --wsite@short@fn=site
This creates a working site file. The volume of the pseudocubic lattice is slightly larger than the cubic one. So sphere volumes no long quite fill the cell volumes, a requirement for the ASA.
This is remedied with sphere resizer, invoked by the command-line argument --sfill
lmchk dasa --sfill~sclwsr=11~lock=1,1,1~omax=.18,.26,.26~wsrmx=3.3 --pr20
You should see this table
spec name old rmax new rmax ratio 1 Pb 3.300000 3.300000 1.000000 2 Cs 3.300000 3.300000 1.000000 3 I 3.300000 3.300000 1.000000 4 E 3.203246 3.239422 1.011294 5 E1 2.441964 2.469543 1.011294
Use your text editor to cut and paste the modified E and E1 sphere radii into ctrl.dasa. Alternatively do it with sed:
sed -i 's/\(ATOM=E .*R= *\)\([.0-9]*\)/\13.239422/' ctrl.dasa sed -i 's/\(ATOM=E1 .*R= *\)\([.0-9]*\)/\12.469543/' ctrl.dasa
- Self-consistent ASA
- Drive the density to self-consistency, and make the energy bands.
lm ctrl.dasa -vnit=0 --zerq~qin~ic=1 lmstr ctrl.dasa rm -f mixm.dasa sv.dasa log.dasa lm ctrl.dasa -vscr=0 -vnit=100 --pr31,20 > out.dasa cp syml.cspbi syml.dasa lm ctrl.dasa -vnit=100 --band~mq~col=1:4~col2=5:13~col3=14:40~fn=syml
LDA (blue) and LDA-ASA energy bands of CsPbI3, with the Pb 6d folded down. Left: cubic structure. Right: pseudocubic structure.
Distortions widen the gap. The figure shows that the ASA tracks shifts in the bands with displacement fairly well.
Footnotes and references
1 The ASA does not keep the density itself, but contracts all the information about the density into energy moments of the sphere charges, , , and , of the density of states for each , and the continuous principal quantum number. . It can do this because of the special structure of the ASA. When the density is needed to make the potential, it is constructed from the and the .
If no data is available for a particular atom, the ASA codes lm, lmgf, and lmpg select from charges in the atom, and sets to zero. It reads preset values for the and from a lookup table. This is will make a crude estimate of the density, but it is usually sufficient to make a starting guess, which can be iterated to the self-consistent values.
Another alternative is to extract the moments from the same species of a different self-consistent calculation, as a starting guess for the self-consistent moments.
A third alternative is to extract the moments , and boundary conditions , from a full-potential calculation run by lmf. The present tutorial follows this strategy.
2 Normally the continuous principal quantum numbers. are allowed to float to band center of gravity (the at which vanishes), but when the partial wave is far removed from the Fermi level, this can cause “ghost bands” to appear. One guard against this is to restrict the , and not let it fall below the free-electron value. Tag HAM_PMIN is designed for this purpose. Another guard is to freeze the to a fixed value, using SPEC_ATOM_IDMOD. Another way is to downfold the . You can tell the ASA codes to downfold a particular state with SPEC_ATOM_IDXDN.