Atomic energy level diagrams

Palladium energy level diagram

Energy levels and transitions of neutral palladium (Pd I): the 46 strongest classified lines below 2 µm from the NIST Atomic Spectra Database and the 25 levels they connect, each line with its vacuum wavelength, frequency and, for 46 of them, the reduced dipole matrix element derived from the NIST transition rate. Measured lifetimes, transition rates, hyperfine constants and isotope shifts from the literature are included, each with its citation.

Hover a line or a level to isolate it, click to keep it selected. Scroll to zoom, drag to move.

Palladium energy level diagram with transition wavelengths and dipole matrix elements

Download: diagram (PDF) diagram (SVG) transitions (CSV) levels (CSV) source code

Key transitions of palladium

Transitionλ vac (nm)λ air (nm)ν (THz)|⟨J‖er‖J′⟩| (ea₀)A (s⁻¹)Γ/2π up. (MHz)branch (%)Use
1S0 – 2[1/2]°1244.8647244.79061224.31861.1646.233e+0733.1628.6ground-state resonance line 244.9 nm
1S0 – 2[3/2]°1247.7161247.64131210.22611.0925.300e+0731.8326.5ground-state resonance line 247.7 nm
1S0 – 2[3/2]°1276.3906276.30901084.66940.5681.033e+0720.947.9ground-state resonance
2[5/2]3 – 2[7/2]°4340.5554340.4577880.30464.8691.351e+0821.51100closed J=3 -> J=4 cycling transition from the metastable…
2[3/2]1 – 2[1/2]°0357.2169357.1149839.24501.6361.190e+0818.95100357.2 nm line used for collinear laser spectroscopy tests
2[5/2]2 – 2[7/2]°3361.0575360.9546830.31773.6528.200e+0719.4167.2361.1 nm
2[5/2]3 – 2[3/2]°2363.5725363.4689824.57403.673*1.137e+0817.88100363.5 nm line from metastable 3D3: main line for collinea…
2[3/2]2 – 2[5/2]°2369.1387369.0337812.14041.803*2.618e+0719.8920.9369.1 nm line used for collinear laser spectroscopy tests

λ, ν from NIST level energies unless a measured frequency for this isotope is available. A: measured value or NIST. Γ/2π: natural linewidth of the upper level, 1/(2πτ).

105Pd hyperfine structure (I = 5/2)

LevelA (MHz)B (MHz)Shift of each F level from the centre of gravity (MHz)
2[5/2]3-391.1790(10)-652.906(15)F=1/2: +3520.05 F=3/2: +3109.56 F=5/2: +2360.13 F=7/2: +1173.82 F=9/2: -586.49 F=11/2: -3097.07
2[5/2]266.3590(10)-398.192(10)F=1/2: -743.25 F=3/2: -464.52 F=5/2: -99.53 F=7/2: +202.41 F=9/2: +232.25
2[3/2]°2-83.5(3)-304(3)F=1/2: +371.63 F=3/2: +383.23 F=5/2: +326.52 F=7/2: +87.49 F=9/2: -493.52
2[7/2]°3-115.3(3)-497(4)F=1/2: +854.80 F=3/2: +816.04 F=5/2: +701.74 F=7/2: +437.35 F=9/2: -81.50 F=11/2: -989.00
2[7/2]°4-79.7(3)-469.9(18)F=3/2: +765.50 F=5/2: +704.70 F=7/2: +566.72 F=9/2: +298.69 F=11/2: -167.35 F=13/2: -914.48
2[3/2]°1-126.2(6)6.0(20)F=3/2: +445.90 F=5/2: +121.40 F=7/2: -314.00

Measured A, B constants; sources in the data file.

Isotope shifts

Transitionλ vac (nm)IsotopesShift (MHz)
1S0 – 2[3/2]°1276.391105-10877(3)
2[5/2]3 – 2[7/2]°4340.555104-106468.6(27)
2[5/2]3 – 2[7/2]°4340.555105-106347(3)
2[5/2]3 – 2[7/2]°4340.555108-106-505(4)
2[5/2]3 – 2[7/2]°4340.555110-106-947(5)
2[5/2]3 – 2[7/2]°4340.555102-106938(18)
2[3/2]1 – 2[1/2]°0357.217102-1081446(4)
2[3/2]1 – 2[1/2]°0357.217104-108958(3)
2[3/2]1 – 2[1/2]°0357.217105-108842.0(20)
2[3/2]1 – 2[1/2]°0357.217106-108490.0(20)
2[3/2]1 – 2[1/2]°0357.217110-108-443(5)
2[5/2]2 – 2[7/2]°3361.058102-1081413.6(14)
2[5/2]2 – 2[7/2]°3361.058104-108948.4(11)
2[5/2]2 – 2[7/2]°3361.058105-108844.7(9)
2[5/2]2 – 2[7/2]°3361.058106-108486.2(11)
2[5/2]2 – 2[7/2]°3361.058110-108-429.4(15)
2[5/2]3 – 2[3/2]°2363.572104-106467.1(14)
2[5/2]3 – 2[3/2]°2363.572105-106348.4(16)
2[5/2]3 – 2[3/2]°2363.572108-106-497.2(15)
2[5/2]3 – 2[3/2]°2363.572110-106-939.2(27)
2[3/2]2 – 2[5/2]°2369.139102-1081337(4)
2[3/2]2 – 2[5/2]°2369.139104-108889(4)

Shift = ν(first isotope) − ν(second isotope).

Closed and nearly closed transitions of palladium

Transitionλ vacuum (nm)Lower levelA (s⁻¹)Leak per scattered photonPhotons before a leakWhere the leak goes
2[3/2]1 → 2[1/2]°0357.2169metastable1.190e+08 measured1.03 × 10−8 from semi-empirical calc.9.71 × 1073P1 ≈ 1.03 × 10−8
2[5/2]3 → 2[7/2]°4340.5554metastable1.351e+08 measured6.24 × 10−4 from semi-empirical calc.1,6003F4 ≈ 6.1 × 10−4 (long-lived); 3F3 ≈ 1.45 × 10−5 (long-lived)
2[5/2]3 → 2[3/2]°2363.5725metastable1.137e+08 theory4.41 % from semi-empirical calc.232[5/2]2 4.13 %* (long-lived); 2[3/2]2 0.32 %* (long-lived); 2[3/2]1 0.16 %* (long-lived); 2 weaker lines

A transition is closed when its upper level can decay only to the level it was excited from, so the atom keeps scattering photons. “closed”: among the levels NIST lists, no other level below the upper level has the opposite parity and |ΔJ| ≤ 1, so no other electric-dipole decay exists. Otherwise the leak is the sum of the branching ratios of the other decay lines of the upper level (or 1 − branching ratio where that of the line itself has been measured), and the number of photons is 1 / leak. “≥” and “≤”: at least one possible decay path has no listed rate, so the leak is a lower limit. These numbers are derived from the branching ratios, lifetimes and rates of this page, not measured as such; the tag names the weakest of the inputs, * marks theory and ≈ a model or semi-empirical calculation. Listed: lines that start on the ground level or on a metastable level and leak at most 10 %, unless more than three possible decay paths have no listed rate. Fine-structure levels only: hyperfine and Zeeman dark states and forbidden decays without a listed rate are not considered. Select a line in the diagram for the full list of its leak channels.

Listed Pd transitions below 2 µm

Lower levelUpper levelλ vacuum (nm)λ air (nm)ν (THz)Type|⟨J‖er‖J′⟩| (ea₀)A (s⁻¹)Branching (%)Source of matrix element / A
1S02[1/2]°1244.8647244.79061224.3186E11.164 measured6.233e+07 measured28.6Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
1S02[3/2]°1247.7161247.64131210.2261E11.092 measured5.300e+07 measured26.5Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
1S02[3/2]°1276.3906276.30901084.6694E10.568 measured1.033e+07 measured7.9Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]32[3/2]°2292.3347292.24921025.5109E10.400 measured2.600e+06 measured2Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]32[5/2]°3300.3525300.2650998.1354E10.594 theory3.771e+06 theory2.94Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
3F43F°4301.0651300.9774995.7729E10.373 semi-empirical1.150e+06 semi-empirical–Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
2[5/2]22[3/2]°2302.8790302.7908989.8093E10.959 measured1.340e+07 measured10.2Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]22[3/2]°1306.6189306.5298977.7363E10.843 measured1.667e+07 measured8.3Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]22[5/2]°3311.4941311.4038962.4338E11.224 theory1.434e+07 theory11.2Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[5/2]22[5/2]°2321.9899321.8970931.0616E10.230 theory6.400e+05 theory0.512Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[5/2]32[5/2]°3324.3635324.2699924.2486E13.547 measured1.067e+08 measured76.8Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[3/2]12[1/2]°1325.2574325.1636921.7084E11.520 measured4.533e+07 measured20.9Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[3/2]12[3/2]°2325.9716325.8776919.6889E11.685 measured3.320e+07 measured25.2Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]32[5/2]°2328.8195328.7248911.7236E10.603 theory4.140e+06 theory3.4Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]12[3/2]°1330.3077330.2126907.6158E12.175 measured8.867e+07 measured44.4Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]22[5/2]°3337.3963337.2994888.5470E11.747 measured2.300e+07 measured16.6Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]32[7/2]°4340.5554340.4577880.3046E14.869 measured1.351e+08 measured100Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]22[5/2]°2342.2202342.1221876.0220E13.483 theory1.226e+08 theory100Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]22[1/2]°1343.4412343.3428872.9076E12.565 measured1.097e+08 measured50.5Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[3/2]22[3/2]°2344.2376344.1390870.8881E12.877 measured8.220e+07 measured62.4Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]32[7/2]°3346.1729346.0738866.0193E12.074 NIST3.000e+07 NIST24.6NIST ASD (accuracy n/a)
2[3/2]12[5/2]°2348.2148348.1152860.9411E13.290 theory1.039e+08 theory83.1Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]22[3/2]°1349.0769348.9770858.8151E11.620 measured4.167e+07 measured20.8Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]22[3/2]°1351.7949351.6943852.1796E12.679 measured1.113e+08 measured84.5Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[3/2]22[5/2]°3355.4096355.3081843.5126E14.237 theory1.157e+08 theory90.3Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]12[1/2]°0357.2169357.1149839.2450E11.636 measured1.190e+08 measured100Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[5/2]22[7/2]°3361.0575360.9546830.3177E13.652 NIST8.200e+07 NIST67.2NIST ASD (accuracy n/a)
2[5/2]32[3/2]°2363.5725363.4689824.5740E13.673 theory1.137e+08 theory100Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]22[5/2]°2369.1387369.0337812.1404E11.803 theory2.618e+07 theory20.9Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]12[5/2]°2371.9964371.8906805.9015E10.741 theory4.320e+06 theory3.54Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[5/2]22[3/2]°2380.0265379.9187788.8724E10.793 theory4.640e+06 theory4.13Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]12[3/2]°1383.3373383.2286782.0591E10.800 measured7.667e+06 measured5.9Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[3/2]22[5/2]°3389.5302389.4198769.6258E11.345 measured8.857e+06 measured6.4Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[3/2]22[5/2]°2395.9743395.8623757.1008E10.970 theory6.140e+06 theory5.04Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]22[3/2]°1408.8497408.7343733.2584E10.461 measured2.100e+06 measured1.6Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table 2
2[3/2]12[3/2]°2417.1014416.9839718.7520E10.179 theory1.800e+05 theory0.16Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]22[7/2]°3421.4140421.2953711.3965E11.060 theory4.343e+06 theory3.56Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[3/2]22[3/2]°2447.4840447.3585669.9512E10.282 theory3.600e+05 theory0.32Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …
2[5/2]°22[7/2]3511.8433511.7007585.7114E16.506 semi-empirical9.136e+07 semi-empirical–Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
2[7/2]°32[9/2]4516.5279516.3840580.3994E17.565 semi-empirical9.348e+07 semi-empirical–Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
2[7/2]°42[9/2]5529.7100529.5626565.9558E18.645 semi-empirical9.261e+07 semi-empirical–Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
2[5/2]°32[7/2]4567.1644567.0070528.5813E16.716 semi-empirical5.565e+07 semi-empirical–Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
3F42[5/2]°3677.6387677.4517442.4075E10.342 semi-empirical1.087e+05 semi-empirical0.0848Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
2[7/2]°32[5/2]2737.0125736.8096406.7671E14.920 semi-empirical2.450e+07 semi-empirical–Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
2[7/2]°42[5/2]3776.6107776.3970386.0267E16.307 semi-empirical2.458e+07 semi-empirical–Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…
3F42[5/2]°3813.5024813.2788368.5207E10.759 semi-empirical3.100e+05 semi-empirical0.223Kurucz, R. L., Can. J. Phys. 89, 417 (2011); semi-empirical line list gf4600.pos of 2017-…

Reduced dipole matrix elements follow the convention A = ω³|d|²/(3πε₀ħc³(2J′+1)), with J′ the upper level. Tags show where a number comes from: measured, NIST compilation, high-accuracy theory, a semi-empirical calculation (Kurucz line list, used only where no measurement or NIST value exists; typically within a factor 2), or a model calculation.

Pd energy levels

LevelEnergy (cm⁻¹)JParityLifetimegJHyperfine A (MHz)Hyperfine B (MHz)Lifetime sourceHyperfine source
1S00.0000evenstable–––––
2[5/2]36564.1483even–1.333-391.179-652.906–Channappa, Pendlebury, Proc. Phys. Soc. 86, 1145 (1965) (atomic-beam magnetic resonance),…
2[5/2]27755.0252even–1.12866.359-398.192–Channappa, Pendlebury, Proc. Phys. Soc. 86, 1145 (1965) (atomic-beam magnetic resonance),…
2[3/2]110093.9921even–0.497––––
2[3/2]211721.8092even–1.04––––
3F425101.2354even––––––
2[3/2]°234068.9772odd8.9 ns measured1.482-83.5-304.1Biémont, Grevesse, Kwiatkowski, Zimmermann, Astron. Astrophys. 108, 127 (1982), Table 2 (…Sulai, Mueller, Phys. Rev. A 102, 042805 (2020) "Laser spectroscopy of metastable palladi…
2[7/2]°335451.4433odd8.2 ns measured1.063-115.3-497Biémont, Grevesse, Kwiatkowski, Zimmermann, Astron. Astrophys. 108, 127 (1982), Table 2 (…Geldhof, Campbell, Cheal, de Groote, Gins, Moore, Hyperfine Interact. 241, 41 (2020), Tab…
2[7/2]°435927.9484odd7.4 ns measured1.25-79.7-469.9Biémont, Grevesse, Kwiatkowski, Zimmermann, Astron. Astrophys. 108, 127 (1982), Table 2 (…Sulai, Mueller, Phys. Rev. A 102, 042805 (2020) "Laser spectroscopy of metastable palladi…
2[3/2]°136180.6771odd7.6 ns measured1.396-126.26Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …Geldhof, Campbell, Cheal, de Groote, Gins, Moore, Hyperfine Interact. 241, 41 (2020), Tab…
2[5/2]°236975.9732odd8.2 ns measured0.988––Biémont, Grevesse, Kwiatkowski, Zimmermann, Astron. Astrophys. 108, 127 (1982), Table 2 (…–
2[5/2]°337393.7623odd7.2 ns measured1.276––Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …–
2[1/2]°038088.1920odd8.4 ns measured–––Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …–
2[5/2]°238811.8962odd8 ns measured0.752––Biémont, Grevesse, Kwiatkowski, Zimmermann, Astron. Astrophys. 108, 127 (1982), Table 2 (…–
2[5/2]°339858.3613odd7.8 ns measured1.081––Biémont, Grevesse, Kwiatkowski, Zimmermann, Astron. Astrophys. 108, 127 (1982), Table 2 (…–
2[3/2]°140368.7961odd5 ns measured0.831––Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …–
2[3/2]°240771.5102odd7.2 ns measured1.114––Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …–
2[1/2]°140838.8741odd4.8 ns measured0.768––Xu, Sun, Dai, Jiang, Palmeri, Quinet, Biémont, Astron. Astrophys. 452, 357 (2006), Table …–
2[5/2]348804.4133even––––––
2[5/2]249019.7332even––––––
2[9/2]554806.2025even––––––
2[9/2]454811.4824even––––––
2[7/2]455025.3354even––––––
3F°458316.6454odd–1.25––––
2[7/2]358349.1253even––––––

Pd⁺ ionisation limit 67241.14 cm⁻¹ = 8.33684 eV (148.718 nm)

Sources

Isotope shifts are nu(first) - nu(second). Sulai & Mueller tabulate nu(A) - nu(106); Geldhof et al. tabulate delta nu(108,A) = nu(A) - nu(108); both kept as printed, so keys use 106 or 108 as the second isotope. For the Geldhof values "unc" is the statistical and "unc_syst" the systematic (acceleration/cooler voltage) uncertainty; the 105Pd values refer to the hyperfine centre of gravity. Level lifetimes: Xu et al. 2006 (time-resolved LIF, six levels) where available, otherwise Biémont et al. 1982 (time-resolved LIF on an atomic beam); other measurements and HFR theory under lifetime.alternatives. A_s for the 20 lines of Xu et al. Table 2 are experimental (A = BF/tau) and were converted from the printed g_k A_ki by dividing by 2J_upper+1; the 17 lines from their Table 3 are HFR theory (method "theory") and should only be used where nothing measured exists. NIST A values exist for only 8 Pd I lines (5 from Biémont et al. 1982, 3 from Morton 2000). Extra fields beyond SCHEMA.md: ionization_limit, lifetime.alternatives, hyperfine.<A>.alternatives, isotope_shift_other, linewidth_MHz, unc_syst, note. Hyperfine constants follow E = A K/2 + B [3K(K+1)/4 - I(I+1)J(J+1)] / [2I(2I-1)J(2J-1)]; 105Pd has I = 5/2 and negative magnetic moment (inverted structure for most levels). LS names in parentheses in the labels are those used by the cited papers (3D3, 3P2, 3F4, ...); NIST uses J1K notation.

Atoms with measured data

All elements: periodic table