Sensitivity of Neutron-Rich Nuclear Isomer Behavior to Uncertainties in Direct Transitions ^†

Abstract

Nuclear isomers are populated in the rapid neutron capture process (r process) of nucleosynthesis. The r process may cover a wide range of temperatures, potentially starting from several tens of GK (several MeV) and then cooling as material is ejected from the event. As the r-process environment cools, isomers can freeze out of thermal equilibrium or be directly populated as astrophysically metastable isomers (astromers). Astromers can undergo reactions and decays at rates very different from the ground state, so they may need to be treated independently in nucleosythesis simulations. Two key behaviors of astromers—ground state ↔ isomer transition rates and thermalization temperatures—are determined by direct transition rates between pairs of nuclear states. We perform a sensitivity study to constrain the effects of unknown transitions on astromer behavior. Detailed balance ensures that ground → isomer and isomer → ground transitions are symmetric, so unknown transitions are equally impactful in both directions. We also introduce a categorization of astromers that describes their potential effects in hot environments. We provide a table of neutron-rich isomers that includes the astromer type, thermalization temperature, and key unmeasured transition rates.

1. Introduction

Nuclear isomers are excited states of atomic nuclei with half-lives longer than the typical half-lives of picoseconds or femtoseconds [1]. These metastable states exhibit inhibited transitions to lower-lying levels due to structural dissimilarities between them; large differences in nuclear deformation, spin, and the projection of spin along the symmetry axis can each be responsible for nuclear isomerism [2,3,4].

Hahn [5] was the first to experimentally verify isomers in a 1921 study of uranium. Since then, hundreds of isomeric states have been identified in nuclei across the chart of nuclides from mass number $A=12$ (the 2.251 MeV state in ${}^{12}$Be) up to mass number $A=277$ (the uncertain state of ${}^{277}$Hs) as of the time of writing (From ENSDF database as of 29 June 2020. Version available at http://www.nndc.bnl.gov/ensarchivals/ accessed on 17 September 2020) [6]. Measurements of isomers and their properties continue to be a point of experimental interest for a variety of reasons, including not only as astrophysical model inputs, but also for applications in industry, medicine, and tests of fundamental nuclear physics [7,8,9,10,11,12,13,14,15,16,17]. For a recent review, see [18].

Astrophysical nucleosynthesis simulations usually take one of two approaches to the distribution of nuclear states: either they assume a thermal equilibrium distribution, or they use only the ground state (GS) properties. The pioneering work of Ward and Fowler [19] demonstrated that the presence of an isomer complicates calculations because it can render invalid both of these assumptions. Inhibited communication between the GS and isomer can hinder thermal equilibration, as well as trap the nucleus in an excited state that might behave radically different from the GS. Although many nuclei possess isomeric states, not all isomers are of astrophysical interest. They may readily reach thermal equilibrium, or they may decay at a rate similar to the GS. Those isomers that lead to other-than-thermal behavior in an astrophysical environment are known as “astromers” [20].

The 228 keV state in ${}^{26}$Al is the best-known astromer. The ${}^{26}$Al GS has a $\beta$-decay half-life of ∼700 kyr, while its isomer decays with a half-life of ∼6 s. This nuclide—the first radioisotope to be observed in the heavens—is an important tracer of star formation [21,22,23]. The isomer decays faster than it can be thermally repopulated from the GS when the ambient temperature is below about 35 keV; the implication is that it becomes depopulated relative to a thermal distribution. Furthermore, at those low temperatures, ${}^{26}$Al that is produced in the isomeric state will $\beta$ decay before it can be thermally driven to the GS. Therefore, neither the GS-only assumption nor the thermal-equilibrium assumption holds [24,25,26,27,28]. Consequently, the study of element formation via nucleosynthesis must treat certain nuclei with isomers explicitly as two distinct species: A ground-state species, and a separate astromer species, such as in [29].

There is also the interesting ${}^{180}$Ta. The metastable state of this isotope (77.2 keV) has a half-life greater than ${10}^{15}$ yr, while the ground state decays in 8 h. In fact, the isomer saves ${}^{180}$Ta from decaying rapidly away after its astrophysical synthesis—the site of which is as yet unclear—and allows it to survive to be the rarest primordial isotope on Earth. Belic et al. [30], Belic et al. [31] demonstrated that there exist intermediate states that connect the GS and isomer at least down to ∼1 MeV excitation. However, there are many measured levels below this energy, and Mohr et al. [32] showed that, under reasonable assumptions, they can enhance the thermal transition rates by as much as 10 orders of magnitude. Central to one of the thrusts of this work, Hayakawa et al. [33] went on to point out that the details of the transition rates between low-lying intermediate states matter, as they not only set the freeze-out temperature, but they also determine how the GS/isomer ratio evolves in the intermediate temperatures between completely frozen out and completely thermalized.

Other well-known nuclei with astromers include ${}^{34}$Cl (possibly visible in nova bursts, isomer at 146 keV [24,34]) and ${}^{85}$Kr (in the slow neutron capture (s) process a branch point, in the r process a $\beta$-decay accelerant and possible electromagnetic source; isomer at 305 keV [35,36]). Isomers, including the 130 keV isomer in ${}^{38}$K, may play a role in the rapid proton capture process ($rp$ process) [37,38,39,40]. ${}^{176}$Lu can be an s-process thermometer [41], and geochemists use it as a chronometer [42,43,44,45], both of which are influenced by its isomer at 123 keV.

Despite being known in the contexts discussed above, isomers have only recently been included in larger networks, such as those that describe the r process that is believed to occur in explosive environments [46]. Fujimoto and Hashimoto [47] included the direct population of nuclear isomers in the r process by replacing GS properties with isomer properties. In their study, several hand-picked isomers in the second r-process peak were shown to impact the radioactive heating of a kilonova. Misch et al. [36] recently studied the dynamic population, de-population, and decay of nuclear isomers in the r process by including in a radioactive-decay network all isomers in the ENSDF database with a half-life greater than 100 $\mathsf{\mu }$s. As the temperature of an r-process event drops below each isomer’s thermalization temperature (temperature below which the nuclide cannot reach thermal equilibrium), the isomer will begin to freeze out as an astromer and affect the subsequent heating and evolution of isotopic abundances.

With respect to calculating nucleosynthetic yields for astrophysical r-process events [48,49,50,51,52,53] (as could be used in, e.g., galactic chemical evolution or population synthesis studies [54]), we note that isomers considered in this work lie on isobaric $\beta$-decay series that are generally populated well after nuclear reactions have subsided in response to cooling temperatures and falling free neutron densities in these environments [55]. The most conspicuous effects of these isomers in the r process would involve the delaying or acceleration of the radioactive decay of nuclei with respect to baseline calculations that omit isomers altogether [36].

Because the temperature rapidly drops in the r process, those isotopes near stability will be populated and destroyed predominantly by reactions and decays, rather than primarily through thermal effects. On the other hand, some of the neutron-rich isomers nearest stability may play a role in the neutron burst in supernovas [56], which can reach temperatures of T∼1 GK (∼100 keV).

In this paper, we treat nuclear isomers as in [20,36,55] and extend the results of those works. In particular, we examine the impact of the unknown properties of the intermediate states that facilitate GS ↔ isomer transitions in neutron-rich r-process nuclei. The GS ↔ isomer transition rates set the thermalization temperature $T_{\mathrm{therm}}^{}$, which, in turn, governs astromer freeze-out. We show that the missing data have a large effect on our computed rates and thermalization temperatures. We use the pathfinding technique of Misch et al. [20] to identify key nuclear states and transitions for experimental campaigns to target. Misch et al. [20] showed that the GS → isomer transition paths are the reverse of the isomer → GS paths. This symmetry implies that key states and transitions affect both directions equally.

2. Methods

In cold environments (e.g., terrestrial), nuclear isomers—by definition—do not readily transition to lower-lying states. However, in a hot environment (e.g., stellar interiors, explosive astrophysical events, etc.), the ground state and isomer can more readily communicate by transitions through other intermediate excited nuclear states. We use the terms “direct transition” or “state-to-state transition” (interchangeably) to refer to transitions directly from one nuclear state to another. “Effective transitions” between long-lived states (GS and isomers) include direct GS ↔ isomer transitions, as well as chains of thermally mediated direct transitions through intermediate states.

We employ the formalism of Misch et al. [20] to compute the effective transition rates between long-lived nuclear states via intermediate states. This method takes as inputs temperature and spontaneous nuclear transition rates, uses them to compute thermally enhanced direct transition rates (both exothermic “down” transitions and endothermic “up” transitions), and uses the results to derive effective transition rates. We restrict our rate enhancements to transitions driven by a thermal photon bath and do not include, e.g., electron collisions. The thermal direct transition rates between a higher-energy state h and a lower-energy state l are then given by

$$\begin{array}{cc}\hfill {\lambda }_{hl}& ={\lambda }_{hl}^s(1+u),\hfill \end{array}$$

(1)

$$\begin{array}{cc}\hfill {\lambda }_{lh}& =\frac{2J_h+1}{2J_l+1}{\lambda }_{hl}^{s}u,\hfill \end{array}$$

(2)

$$\begin{array}{cc}\hfill u& =\frac{1}{e^{(E_h-E_l)/T}-1}.\hfill \end{array}$$

(3)

In these equations, E and J are the energy and spin of the indicated nuclear level, T is the temperature, and ${\lambda }_{hl}^s$ is the spontaneous transition rate.

With the direct rates in hand, the next step is to compute the probability $b_{st}$ that nuclear state s goes to state t when it transitions. This is the fraction of the total transition rate out of s that is to t and is subject to the constraint ${\displaystyle \sum _t}{b}_{st}=1$.

$$\begin{array}{c}\hfill b_{st}=\frac{{\lambda }_{st}}{{\displaystyle \sum _f}{\lambda }_{sf}}\end{array}$$

(4)

We now use the b’s to calculate the probability $P_{iB}$ that a nucleus in an intermediate state i follows a chain of transitions that takes it to long-lived state B without passing through long-lived state A. This quantity can be computed from a recursive relationship that forms a system of coupled linear equations.

$$\begin{array}{c}\hfill P_{iB}=b_{iB}+\sum _j{b}_{ij}{P}_{jB}\end{array}$$

(5)

Finally, we have all of the ingredients to compute the effective transition rate ${\Lambda }_{AB}$ from long-lived state A to long-lived state B:

$$\begin{array}{cc}\hfill {\Lambda }_{AB}& ={\lambda }_{AB}+\sum _i{\lambda }_{Ai}{P}_{iB}.\hfill \end{array}$$

(6)

This expression for ${\Lambda }_{AB}$ includes explicitly the direct transition rate ${\lambda }_{AB}$ and implicitly the rates to follow all possible chains of transitions through intermediate states (“paths”).

Naturally, this method is powered by nuclear data, which we take from ENSDF [57]; we use the evaluated nuclear level energies, spins, parities, half-lives, and $\gamma$ intensities (ENSDF database as of 29 June 2020. Version available at http://www.nndc.bnl.gov/ensarchivals/ accessed on 17 September 2020). We convert half-lives and intensities into state-to-state transition rates (“measured” rates); if either the initial state half-life or $\gamma$ intensity for a transition is not reported, the rate is unmeasured irrespective of whether the $\gamma$ ray has been observed. We estimate unmeasured rates with the Weisskopf approximation [58]. In turn, the Weisskopf approximation requires the level spins and parities as inputs. Where the spins and parities are uncertain, we average together the Weisskopf rates for all possible combinations of initial- and final-state spins and parities within the uncertainties. We exclude states with completely unknown half-lives, spins, and parities.

These treatments of transition rates include the effects of internal conversion (electron ejection from the atom via nuclear de-excitation, abbreviated IC) for measured rates and exclude it for the Weisskopf estimates. In hot or dense environments, the inclusion of IC is a complicated problem and outside the scope of this study. Our main goal is to quantify the effects of the uncertainties in unmeasured transitions, and since the atoms will be fully ionized over the vast majority of the temperature range we explore, it is appropriate to neglect IC for those transitions.

Apart from the excluded information-deficient states, the uncertainties in our calculations of effective GS ↔ isomer transition rates lie principally in the unmeasured Weisskopf rates: most measured rates have a relative uncertainty of less than 50%, while the Weisskopf approximation often disagrees with experiment by one or two orders of magnitude. Therefore, in this sensitivity study, we fixed the measured rates and varied the Weisskopf rates up and down by factors of 10 and 100. In these variations, we shifted all of the Weisskopf rates together rather than independently. This approach constrains the likely bounds of effective GS ↔ isomer transition rates.

The constraints on the GS ↔ isomer transition rates also bound the thermalization temperatures for astromers. Astromers thermalize and behave like non-isomeric states when the transition rates dominate other reaction rates, that is, when their communication is sufficiently unhindered, such that they can reach a thermal-equilibrium population. We define the thermalization temperature, $T_{\mathrm{therm}}^{}$, as the lowest temperature such that the transition rate out of each nuclear state is equal to or greater than its destruction rate.

$$\begin{array}{c}\hfill T_{\mathrm{therm}}\equiv \underset{T}{min}:\left\{\begin{array}{c}{\Lambda }_{gm}\left(T\right) \ge {\Lambda }_{g\beta }\left(T\right)\&\hfill \\ {\Lambda }_{mg}\left(T\right) \ge {\Lambda }_{m\beta }\left(T\right)\hfill \end{array}\right.\end{array}$$

(7)

The temperature T is as in Equation (3). The indices g and m denote the ground and isomeric states, respectively, and ${\Lambda }_{A\beta }$ indicates the $\beta$-decay rate for a thermal ensemble associated with state A; see Gupta and Meyer [25]. Above the thermalization temperature, transitions dominate decays, so thermal equilibrium between the nuclear levels is restored by transitions more rapidly than decays can push them out. Below $T_{\mathrm{therm}}^{}$, decays dominate transitions in at least one of the long-lived states; in most cases, this can result in a failure to achieve thermal equilibrium.

The thermalization temperature is a key component to understanding the behavior and influence of astromers: isomers freeze out of thermal equilibrium as astromers at their thermalization temperatures. This freeze-out should not be understood as sudden, but rather a situation where the isotope no longer thermally equilibrates. We computed the range of $T_{\mathrm{therm}}^{}$ under the influence of our Weisskopf variations for each isotope in our study. The thermalization temperature depends on which destruction channels are in play in a given environment, and our intent is to highlight the effects of nuclear uncertainties without the distractions of astrophysical uncertainties. Therefore, we considered only $\beta$ decay because it is utterly essential astrophysically, straightforward to compute, and relatively insensitive to anything but temperature and electron density. We did not include any reaction rates, and all subsequent instances of $T_{\mathrm{therm}}^{}$ should be considered to be a thermalization temperature with respect to $\beta$ decay only ($T_{\mathrm{therm}}^{\beta }$).

Because we varied all Weisskopf rates together, our variations alone do not reveal which individual unmeasured transitions are most influential. We addressed this by using the pathfinding method of Misch et al. [20] to isolate which individual state-to-state transitions contribute most to the total effective GS ↔ isomer transition rate. For unstable nuclei, we identified all unmeasured (Weisskopf) transitions which lie along paths that contribute at least 1% of the effective transition rate at temperatures below $T_{\mathrm{therm}}^{}$. For stable nuclei, we performed the same analysis with a fixed cut-off temperature of 30 keV.

Example: ${}^{129}$Sn

Here we will walk through a detailed result for ${}^{129}$Sn to help build intuition for our results in the next section. Misch et al. [20] identified this as a potentially influential astromer that is populated on the ∼1 s timescale in the r process. It can extend the half-life of the isotope from 2.23 min to 6.9 min, and because it is highly populated (near the A∼130 peak), this has implications for heating early in the decay back to stability.

Figure 1 shows the essential behavior of the isotope as a function of temperature. The ground state is labeled 1, and the isomer is labeled 2. Solid lines show our computed transition rates between these two long-lived states; we have included uncertainty bands from the Weisskopf approximation. The dashed lines show the $\beta$-decay rates of each long-lived state.

The next line to examine should be the thermal $\beta$-decay rate, the blue dotted X’s. This would be the steady-state decay rate of the species if the states had a thermal equilibrium population distribution. Because the isomer has the longer half-life, any population of the isotope in the isomer effectively decreases the overall decay rate. Beginning at T∼8 keV, the isomer becomes sufficiently populated to affect the rate, and indeed, the thermal decay rate continues to decrease at higher temperatures where the isomer would be increasingly populated.

However, because internal transitions are inhibited, the true steady-state decay rate (given by the black dotted plus-sign line) may not agree with the thermal rate. In this isotope, beginning at high temperature in the figure and moving to lower temperature, the steady-state and thermal rates begin to diverge at T∼31 keV. By about T∼25 keV, the steady-state rate is simply the isomer’s decay rate. This occurs because there is essentially zero transition between the long-lived states. Eventually, any material in the GS decays away, and only the isomer population remains.

We might conclude that the steady-state rate is adequate, but there are two facts which rule this out. First, the populations may take a long time to reach steady state [59]. Second, and relatedly, the true steady-state decay rate can be a function of which energy level is populated in the production of the isotope. We illustrate this by the dotted lines marked with triangles, which show the steady state rate when there is constant production in the GS (${\Lambda }_{\beta SS}^{P1}$ in the figure) or the isomer (${\Lambda }_{\beta SS}^{P2}$). Below T∼25 keV, the limited communication between the long-lived states results in a steady-state decay rate equal to that of whichever level is produced.

Now, we may compare the four collective rates (thermal and three steady-state) as a function of temperature. Near T∼27 keV, they begin to draw together, and by T∼33 keV, they have all converged to the thermal rate. This is entirely due to the growing internal transition rates. Once the transitions dominate the decays, the nuclear levels at last reach a thermal equilibrium distribution; this gives rise to the notion of $T_{\mathrm{therm}}^{}$ in Equation (7).

The need to account for distinct GS and isomer behaviors at different temperatures is particularly well illustrated by ${}^{129}$Sn. It is populated in the r process at ∼1 s when the temperature can be around T∼45 keV. However, of course, it decays on the timescale of 2–7 m, when the temperature may range from ∼0.5 to ∼2 keV. That means that a thermal equilibrium distribution freezes out at $T_{\mathrm{therm}}^{}$∼31 keV to a situation where the long-lived states must evolve separately.

3. Results

We included in our study those nuclei with isomers in the neutron-rich r-process region between mass numbers $A=69$ and $A=209$ with half-lives $T_{1/2}>100$ $\mathsf{\mu }$s. We highlight the specific astromers of likely import in the r process listed in Table I of Misch et al. [36]. In identifying those astromers, that work held the Weisskopf rates fixed and used a single temperature-density trajectory [60,61] in the Jade network of Sprouse et al. [55]. The fixed Weisskopf rates may inadvertently over- or under-emphasize some astromers, but we nevertheless have an adequate starting set to examine. The r process is subject to astrophysical variations in environmental conditions [62,63] and we plan to address this point in follow up work. Here, we focus our attention on the nuclear uncertainties that arise from unknown transitions. This approach allows us not only to zoom in on potential key astromers, but also to disentangle the nuclear physics uncertainty effects on their behavior from the astrophysics. An influential astromer with large uncertainties is then a priority for experimental or deeper theoretical inquiry.

We use a system of types to categorize each astromer according to the role it could play in the r-process decay back to stability.

Type A (“accelerant”) astromers have a $\beta$-decay rate greater than the ground state and can accelerate abundance evolution and energy release. Even if the isotope is thermalized, the greater decay rate of the thermally populated excited state will accelerate the overall $\beta$-decay rate.

Type B (“battery”) astromers decay (via all channels, including de-excitation) slower than the ground state, storing energy and releasing it later. Type B astromers have an associated temperature above which they are not batteries; it is the temperature above which the total destruction rate of the isomer via all channels is greater than or equal to the GS $\beta$-decay rate. Above this temperature, the isomer is clearly not a battery, because it is not in fact storing energy for longer than the GS.

Type N (“neutral”) astromers do not fall into either of these categories and will not have a large direct impact on decay or heating under the conditions of this study. However, type N astromers may decay to feed another more interesting astromer, and particularly long-lived type N astromers may produce an electromagnetic signal; some type N astromers in stable isotopes can play the latter role.

We assign the type of the isomer using the following procedure. If the isotope is stable, the isomer is type N. For unstable isotopes, we compare the total decay rates of the GS and isomer at low temperature; if the rates are not different by a threshold factor (we used a factor of 2), the isomer is type N. If the isomer’s $\beta$-decay rate is greater than the ground state rate by the threshold factor, it is a type A astromer. If the total decay rate of the isomer is slower than the $\beta$-decay rate of the GS by the threshold factor, it is a type B astromer. For type B astromers, we also identify the temperature above which they are not batteries, that is, the temperature above which the decay rate is no longer dissimilar from the GS rate by the threshold factor.

In what follows, we present detailed results for the nuclei appearing in Table I of Misch et al. [36]. For each detailed isotope, we show a figure indicating the uncertainty bands for the effective transition rates in each of these nuclei. The figures also show the $\beta$-decay rates and a vertical line indicating the approximate thermalization temperature; if no $T_{\mathrm{therm}}^{}$ line is shown, there is insufficient data to calculate a thermalization temperature. In the discussion accompanying each figure, we indicate the number of measured levels appearing in ENSDF and the number of those used in our calculations; for convenience, we also include all of the information from

Table A1. Results for each isomer studied in this work. We provide the range of thermalization temperatures in the “T${}_{\mathrm{therm}}$” column. We give the energy of each long-lived state (“E”, in keV) along with its half-life (“T${}_{1/2}$”, in seconds). The “B${}_{\beta }$” column gives the isomer low-temperature $\beta$-decay branching percentage (approximately the terrestrial branching ratio). The “Type” column indicates whether each isomer is a decay accelerant (A), a decay battery (B), or neutral with respect to decay rate (N); type B isomers show in parentheses the maximum temperature (in keV) at which they behave as batteries. We list in the “Unmeasured Transitions” column which unmeasured individual transitions appear along pathways that contribute at least 1% to the effective transition rate. We only consider paths at temperatures below the greatest value in the ${\mathrm{T}}_{\mathrm{therm}}$ column, and stable isotopes use an artificial ${\mathrm{T}}_{\mathrm{therm}}$ of 30 keV.

Nucleus	T${}_{\mathbf{therm}}^{\mathit{\beta }}$ (keV)	E (keV)	T${}_{1/2}$ (s)	B${}_{\mathit{\beta }}$ %	Type (keV)	Unmeasured Transitions
${}^{69}$Zn	24–36	0.0 438.6	$3.38\times {10}^3$ $4.95\times {10}^4$	0.0	B (5.0)	($531.3\to 0.0$), ($531.3\to 438.636$), ($872.0\to 438.636$), ($872.0\to 531.3$)
${}^{71}$Zn	12–17	0.0 157.7	$1.47\times {10}^2$ $1.43\times {10}^4$	100.0	B (6.0)	($157.7\to 0.0$), ($286.3\to 0.0$), ($286.3\to 157.7$), ($465.0\to 157.7$), ($465.0\to 286.3$), ($489.8\to 0.0$), ($489.8\to 286.3$)
${}^{73}$Zn	9–12	0.0 195.5	$2.45\times {10}^1$ $1.30\times {10}^{-2}$	0.0	N	($307.2\to 0.0$), ($307.2\to 195.5$)
${}^{77}$Zn	34–45	0.0 772.4	$2.08\times {10}^0$ $1.05\times {10}^0$	65.9	N	($1130.5\to 772.44$), ($1130.5\to 801.89$), ($114.721\to 0.0$), ($1235.1\to 772.44$), ($1235.1\to 801.89$), ($1277.69\to 0.0$), ($1277.69\to 772.44$), ($1277.69\to 801.89$), ($772.44\to 114.721$), ($801.89\to 114.721$), ($801.89\to 772.44$)
${}^{79}$Zn	41–57	0.0 1100.0	$7.46\times {10}^{-1}$ $2.00\times {10}^{-1}$	0.0	N	($1100.0\to 0.0$), ($1100.0\to 983.0$), ($1336.0\to 0.0$), ($1336.0\to 1100.0$), ($1336.0\to 983.0$), ($1424.0\to 1100.0$), ($1424.0\to 983.0$), ($2312.0\to 0.0$), ($2312.0\to 1100.0$), ($2521.0\to 0.0$), ($2521.0\to 1100.0$), ($3195.0\to 0.0$), ($3195.0\to 1100.0$), ($983.0\to 0.0$)
${}^{72}$Ga	4–5	0.0 119.7	$5.08\times {10}^4$ $3.97\times {10}^{-2}$	0.0	N	($128.79\to 0.0$), ($128.79\to 119.66$), ($128.79\to 16.44$)
${}^{73}$Ga	1	0.0 0.3	$1.75\times {10}^4$ $2.00\times {10}^{-1}$	0.0	N	($0.3\to 0.0$)
${}^{74}$Ga	4–5	0.0 59.6	$4.87\times {10}^2$ $9.50\times {10}^0$	24.2	A	($108.654\to 56.55$), ($108.654\to 59.571$), ($141.334\to 0.0$), ($141.334\to 56.55$), ($141.334\to 59.571$)
${}^{80}$Ga	6–13	0.0 22.4	$1.90\times {10}^0$ $1.30\times {10}^0$	100.0	N	($22.4\to 0.0$), ($97.2\to 0.0$), ($97.2\to 22.4$)
${}^{73}$Ge	N/A	0.0 66.7	stable $4.99\times {10}^{-1}$	0.0	N	($353.7\to 13.2845$), ($353.7\to 68.752$), ($364.03\to 13.2845$), ($364.03\to 66.725$), ($392.47\to 13.2845$), ($392.47\to 66.725$), ($68.752\to 13.2845$)
${}^{75}$Ge	8–9	0.0 139.7	$4.97\times {10}^3$ $4.77\times {10}^1$	0.0	N	($192.19\to 0.0$), ($253.15\to 0.0$), ($253.15\to 192.19$), ($316.81\to 139.69$), ($316.81\to 192.19$)
${}^{77}$Ge	14–18	0.0 159.7	$4.04\times {10}^4$ $5.37\times {10}^1$	81.2	A	($421.39\to 0.0$), ($421.39\to 159.71$), ($492.05\to 0.0$), ($492.05\to 159.71$), ($504.76\to 0.0$), ($618.86\to 159.71$), ($618.86\to 421.39$), ($618.86\to 492.05$), ($629.68\to 159.71$), ($629.68\to 421.39$), ($629.68\to 504.76$)
${}^{79}$Ge	14–19	0.0 185.9	$1.90\times {10}^1$ $3.90\times {10}^1$	96.3	N	($464.73\to 0.0$), ($464.73\to 185.95$), ($516.41\to 0.0$), ($516.41\to 185.95$)
${}^{81}$Ge	34–44	0.0 679.1	$7.60\times {10}^0$ $7.60\times {10}^0$	67.6	N	($1241.44\to 679.14$), ($1241.44\to 711.207$), ($1241.44\to 895.63$), ($1286.466\to 0.0$), ($1286.466\to 711.207$), ($1303.23\to 0.0$), ($1303.23\to 711.207$), ($679.14\to 0.0$), ($711.207\to 679.14$)
${}^{75}$As	N/A	0.0 303.9	stable $1.76\times {10}^{-2}$	0.0	N	($400.6583\to 198.6063$), ($572.41\to 400.6583$), ($617.68\to 0.0$), ($617.68\to 400.6583$), ($821.62\to 303.9243$), ($821.62\to 400.6583$)
${}^{82}$As	9–15	0.0 131.6	$1.91\times {10}^1$ $1.36\times {10}^1$	94.8	N	($131.6\to 0.0$), ($224.2\to 0.0$), ($224.2\to 131.6$)
${}^{77}$Se	N/A	0.0 161.9	stable $1.74\times {10}^1$	0.0	N	($249.7885\to 238.9988$), ($301.1496\to 161.9223$), ($301.1496\to 238.9988$), ($301.1496\to 249.7885$), ($439.4517\to 301.1496$)
${}^{79}$Se	4–5	0.0 95.8	$1.03\times {10}^{13}$ $2.35\times {10}^2$	0.1	A	($128.0\to 0.0$), ($128.0\to 95.77$)
${}^{81}$Se	15–20	0.0 103.0	$1.11\times {10}^3$ $3.44\times {10}^3$	0.1	B (13.0)	($467.74\to 0.0$), ($467.74\to 103.0$), ($491.06\to 0.0$), ($491.06\to 103.0$), ($491.06\to 467.74$), ($624.11\to 103.0$), ($624.11\to 467.74$)
${}^{83}$Se	14–20	0.0 228.9	$1.34\times {10}^3$ $7.01\times {10}^1$	100.0	A	($228.92\to 0.0$), ($430.0\to 0.0$), ($430.0\to 228.92$), ($582.22\to 430.0$)
${}^{79}$Br	N/A	0.0 207.6	stable $4.85\times {10}^0$	0.0	N	($217.1\to 207.61$), ($306.51\to 217.1$), ($306.51\to 261.33$), ($381.5\to 217.1$), ($381.5\to 261.33$), ($381.5\to 306.51$), ($906.45\to 207.61$), ($906.45\to 381.5$)
${}^{82}$Br	9	0.0 45.9	$1.27\times {10}^5$ $3.68\times {10}^2$	2.5	A	($290.7807\to 0.0$), ($290.7807\to 45.9492$)
${}^{84}$Br	83–100	0.0 320.0	$1.91\times {10}^3$ $3.60\times {10}^2$	96.7	A	($320.0\to 0.0$)
${}^{83}$Kr	N/A	0.0 41.6	stable $6.59\times {10}^3$	0.0	N	($571.1538\to 561.9585$), ($571.1538\to 9.4057$), ($799.48\to 561.9585$), ($799.48\to 571.1538$)
${}^{85}$Kr	26–29	0.0 304.9	$3.39\times {10}^8$ $1.61\times {10}^4$	77.5	A	($1107.32\to 304.871$), ($1140.73\to 1107.32$), ($1166.69\to 1140.73$), ($1166.69\to 304.871$), ($1223.98\to 1140.73$), ($1223.98\to 1166.69$), ($1416.57\to 1107.32$)
${}^{90}$Rb	7–9	0.0 106.9	$1.58\times {10}^2$ $2.58\times {10}^2$	97.4	N	($121.79\to 0.0$), ($121.79\to 106.9$), ($227.83\to 106.9$), ($227.83\to 121.79$)
${}^{98}$Rb	8–11	0.0 270.0	$1.15\times {10}^{-1}$ $9.60\times {10}^{-2}$	0.0	N	($123.8\to 0.0$), ($123.8\to 113.8$), ($270.0\to 113.8$), ($270.0\to 123.8$)
${}^{89}$Y	N/A	0.0 909.0	stable $1.57\times {10}^1$	0.0	N	($1507.41\to 908.97$), ($1744.74\to 1507.41$), ($1744.74\to 908.97$), ($2566.55\to 0.0$), ($2622.1\to 0.0$), ($2892.98\to 0.0$), ($3343.44\to 0.0$), ($3621.1\to 0.0$), ($3621.1\to 908.97$), ($3630.3\to 0.0$), ($3630.3\to 908.97$)
${}^{90}$Y	29–38	0.0 682.0	$2.31\times {10}^5$ $1.15\times {10}^4$	0.0	N	($1047.22\to 202.496$), ($1047.22\to 682.01$), ($1298.0\to 1047.22$), ($1298.0\to 682.01$), ($1561.9\to 1047.22$), ($1561.9\to 776.593$), ($1561.9\to 953.512$), ($776.593\to 0.0$), ($776.593\to 202.496$), ($953.512\to 0.0$)
${}^{91}$Y	25–30	0.0 555.6	$5.06\times {10}^6$ $2.98\times {10}^3$	1.5	A	($1186.88\to 555.58$), ($1186.88\to 925.74$), ($1305.39\to 1186.88$), ($1305.39\to 653.02$), ($1305.39\to 925.74$), ($653.02\to 0.0$), ($653.02\to 555.58$), ($925.74\to 0.0$), ($925.74\to 555.58$), ($925.74\to 653.02$)
${}^{93}$Y	33–41	0.0 758.7	$3.66\times {10}^4$ $8.20\times {10}^{-1}$	0.0	N	($1135.97\to 0.0$), ($1135.97\to 590.22$), ($1135.97\to 758.719$), ($1135.97\to 875.88$), ($1300.522\to 0.0$), ($1647.04\to 0.0$), ($1647.04\to 1135.97$), ($1647.04\to 1300.522$), ($1647.04\to 590.22$), ($1647.04\to 758.719$), ($1647.04\to 875.88$), ($758.719\to 0.0$), ($875.88\to 0.0$), ($875.88\to 590.22$), ($875.88\to 758.719$)
${}^{96}$Y	?	0.0 1140.0	$5.34\times {10}^0$ $9.60\times {10}^0$	100.0	N	($1140.0\to 122.297$), ($1140.0\to 652.29$), ($1140.0\to 718.7$), ($1287.89\to 0.0$), ($1287.89\to 1140.0$), ($1287.89\to 122.297$), ($1287.89\to 652.29$), ($1287.89\to 718.7$), ($1287.89\to 931.7$), ($718.7\to 0.0$), ($718.7\to 122.297$), ($718.7\to 652.29$)
${}^{97}$Y	?	0.0 667.5 3522.6	$3.75\times {10}^0$ $1.17\times {10}^0$ $1.42\times {10}^{-1}$	99.4 6.1	A N	($1319.54\to 0.0$), ($1613.8\to 0.0$), ($1613.8\to 1319.54$), ($1613.8\to 1428.11$), ($1613.8\to 697.32$), ($1738.8\to 0.0$), ($1738.8\to 1319.54$), ($1799.6\to 0.0$), ($1799.6\to 1319.54$), ($1799.6\to 697.32$), ($953.82\to 667.52$), ($953.82\to 697.32$)
${}^{98}$Y	18–25	0.0 465.7	$5.48\times {10}^{-1}$ $2.32\times {10}^0$	0.0	N	($358.13\to 0.0$), ($358.13\to 119.353$), ($358.13\to 170.78$), ($446.07\to 358.13$), ($465.7\to 374.97$), ($564.0+X\to 374.97$), ($564.0+X\to 446.07$), ($596.73\to 374.97$), ($596.73\to 465.7$), ($603.57\to 374.97$), ($603.57\to 465.7$), ($615.17\to 170.78$), ($615.17\to 358.13$), ($615.17\to 374.97$), ($615.17\to 496.1$)
${}^{100}$Y	5–7	0.0 145.0	$7.35\times {10}^{-1}$ $9.40\times {10}^{-1}$	0.0	N	($10.7\to 0.0$), ($145.0\to 0.0$), ($145.0\to 76.15$), ($145.0\to 99.16$), ($76.15\to 0.0$), ($99.16\to 0.0$), ($99.16\to 10.7$)
${}^{90}$Zr	N/A	0.0 2319.0	stable $8.09\times {10}^{-1}$	0.0	N	($1760.74\to 0.0$), ($2319.0\to 1760.74$), ($2739.29\to 0.0$), ($2739.29\to 2186.273$), ($2739.29\to 2319.0$), ($2747.875\to 1760.74$), ($2747.875\to 2739.29$), ($3076.925\to 2319.0$), ($3076.925\to 2739.29$), ($3076.925\to 2747.875$), ($3448.23\to 0.0$), ($3589.418\to 0.0$), ($4058.07\to 0.0$), ($4058.07\to 2319.0$), ($4232.22\to 0.0$), ($4331.93\to 0.0$), ($4331.93\to 2739.29$)
${}^{93}$Nb	N/A	0.0 30.8	stable $5.09\times {10}^8$	0.0	N	($1127.09\to 0.0$), ($1127.09\to 30.77$), ($808.82\to 686.79$), ($810.32\to 743.95$)
${}^{95}$Nb	18–22	0.0 235.7	$3.02\times {10}^6$ $3.12\times {10}^5$	5.4	N	($730.0\to 0.0$), ($756.728\to 730.0$), ($799.0\to 235.69$), ($799.0\to 730.0$), ($805.0\to 0.0$), ($805.0\to 730.0$), ($877.0\to 0.0$), ($877.0\to 799.0$)
${}^{97}$Nb	34–44	0.0 743.4	$4.33\times {10}^3$ $5.87\times {10}^1$	0.0	N	($1160.0\to 0.0$), ($1160.0\to 1147.96$), ($1251.01\to 0.0$), ($1251.01\to 743.35$), ($1276.09\to 0.0$), ($1276.09\to 1147.96$), ($1276.09\to 1251.01$), ($1433.92\to 1147.96$), ($1433.92\to 1251.01$), ($1433.92\to 1276.09$), ($1548.36\to 0.0$), ($1548.36\to 1147.96$), ($1548.36\to 1276.09$), ($1548.36\to 743.35$), ($1750.43\to 1251.01$), ($2357.0\to 0.0$), ($2357.0\to 743.35$)
${}^{98}$Nb	25–37	0.0 84.0	$2.86\times {10}^0$ $3.07\times {10}^3$	100.0	B (26.0)	($226.0\to 0.0$), ($226.0\to 84.0$), ($737.0\to 0.0$), ($737.0\to 226.0$), ($84.0\to 0.0$)
${}^{99}$Nb	21–27	0.0 365.3	$1.50\times {10}^1$ $1.50\times {10}^2$	96.3	B (7.0)	($469.139\to 365.27$), ($630.7\to 387.38$), ($630.7\to 469.139$), ($630.7\to 544.23$), ($765.05\to 365.27$), ($765.05\to 544.23$), ($765.05\to 630.7$), ($816.73\to 544.23$), ($816.73\to 630.7$)
${}^{100}$Nb	15–19	0.0 314.0	$1.50\times {10}^0$ $2.99\times {10}^0$	-0.0	N	($0+X\to 0.0$), ($207.4+X\to 0+X$), ($34.3+X\to 0+X$), ($34.3+X\to 0.0$), ($34.3+X\to 314.0$), ($34.3+X\to 498.1$), ($498.1\to 0.0$)
${}^{104}$Nb	?	0.0 215.0	$4.90\times {10}^0$ $9.40\times {10}^{-1}$	100.0	A	($109.6\to 0.0$), ($215.0\to 0.0$), ($215.0\to 109.6$), ($215.0\to 37.5$), ($215.0\to 8.7$), ($250.6\to 0.0$), ($250.6\to 215.0$), ($311.8\to 0.0$), ($311.8\to 215.0$), ($37.5\to 0.0$), ($37.5\to 8.7$), ($8.7\to 0.0$)
${}^{99}$Tc	5–7	0.0 142.7	$6.66\times {10}^{12}$ $2.16\times {10}^4$	0.0	A	($181.09423\to 142.6836$)
${}^{103}$Ru	10	0.0 238.2	$3.39\times {10}^6$ $1.69\times {10}^{-3}$	0.0	N	($136.079\to 0.0$), ($136.079\to 2.81$), ($2.81\to 0.0$), ($238.2\to 2.81$), ($297.48\to 136.079$), ($297.48\to 2.81$), ($297.48\to 213.56$), ($297.48\to 238.2$)
${}^{103}$Rh	N/A	0.0 39.8	stable $3.37\times {10}^3$	0.0	N	($294.965\to 39.753$), ($357.396\to 93.036$), ($536.84\to 357.396$), ($607.409\to 294.965$), ($607.409\to 357.396$), ($607.409\to 39.753$), ($607.409\to 93.036$), ($650.064\to 294.965$), ($651.716\to 0.0$), ($651.716\to 294.965$), ($651.716\to 357.396$)
${}^{105}$Rh	12–14	0.0 129.7	$1.27\times {10}^5$ $4.28\times {10}^1$	0.0	N	($392.526\to 0.0$), ($392.526\to 129.742$), ($455.871\to 0.0$), ($455.871\to 392.526$), ($469.369\to 392.526$), ($469.369\to 455.871$), ($499.236\to 0.0$), ($499.236\to 392.526$), ($499.236\to 455.871$)
${}^{106}$Rh	?	0.0 137.0	$3.01\times {10}^1$ $7.86\times {10}^3$	100.0	B (?)	($137.0\to 0.0$), ($247.7\to 0.0$), ($247.7\to 137.0$)
${}^{116}$Rh	?	0.0 150.0	$6.80\times {10}^{-1}$ $5.70\times {10}^{-1}$	100.0	N	($150.0\to 0.0$)
${}^{107}$Pd	6	0.0 214.6	$2.05\times {10}^{14}$ $2.13\times {10}^1$	0.0	N	($312.2\to 0.0$), ($312.2\to 214.6$)
${}^{109}$Pd	8–10	0.0 189.0	$4.89\times {10}^4$ $2.82\times {10}^2$	0.0	N	($248.01\to 0.0$), ($248.01\to 188.9903$), ($248.01\to 245.0807$), ($276.289\to 245.0807$), ($276.289\to 248.01$), ($287.25\to 245.0807$), ($287.25\to 248.01$), ($287.25\to 276.289$)
${}^{111}$Pd	7–9	0.0 172.2	$1.40\times {10}^3$ $1.98\times {10}^4$	29.0	B (1.0)	($230.8\to 0.0$), ($230.8\to 172.18$)
${}^{113}$Pd	6–8	0.0 81.1	$9.30\times {10}^1$ $3.00\times {10}^{-1}$	0.0	N	($189.61\to 0.0$), ($189.61\to 81.1$)
${}^{115}$Pd	8–11	0.0 89.2	$2.50\times {10}^1$ $5.00\times {10}^1$	92.0	N	($127.84\to 0.0$), ($127.84\to 89.21$), ($253.62\to 127.84$), ($253.62\to 89.21$)
${}^{117}$Pd	22–32	0.0 203.3	$4.30\times {10}^0$ $1.91\times {10}^{-2}$	0.0	N	($131.76\to 0.0$), ($131.76\to 34.64$), ($203.3\to 0.0$), ($34.64\to 0.0$)
${}^{126}$Pd	?	0.0 2406.4	$4.86\times {10}^{-2}$ $2.30\times {10}^{-2}$	72.0	A	($1481.0\to 0.0$), ($1481.0\to 693.3$), ($2023.5\to 0.0$), ($2109.7\to 1481.0$), ($2109.7\to 693.3$), ($2406.4\to 2023.5$), ($693.3\to 0.0$)
${}^{107}$Ag	N/A	0.0 93.1	stable $4.43\times {10}^1$	0.0	N	($324.81\to 93.125$), ($423.15\to 125.59$), ($922.06\to 423.15$)
${}^{109}$Ag	N/A	0.0 88.0	stable $3.98\times {10}^1$	0.0	N	($311.378\to 88.0337$), ($420.0\to 132.762$), ($420.0\to 415.193$), ($420.0\to 88.0337$), ($706.971\to 0.0$), ($706.971\to 311.378$), ($706.971\to 415.193$), ($706.971\to 420.0$), ($706.971\to 88.0337$), ($735.32\to 311.378$), ($735.32\to 415.193$), ($735.32\to 88.0337$)
${}^{113}$Ag	7	0.0 43.5	$1.93\times {10}^4$ $6.87\times {10}^1$	23.6	A	($222.08\to 43.5$), ($270.82\to 0.0$), ($270.82\to 222.08$)
${}^{114}$Ag	?	0.0 199.0	$4.60\times {10}^0$ $1.50\times {10}^{-3}$	0.0	B (?)	($126.7\to 0.0$), ($136.7\to 0.0$), ($136.7\to 126.7$), ($199.0\to 0.0$), ($199.0\to 126.7$), ($199.0\to 136.7$), ($358.5\to 0.0$), ($358.5\to 126.7$)
${}^{115}$Ag	9–12	0.0 41.2	$1.20\times {10}^3$ $1.80\times {10}^1$	79.0	A	($255.48\to 0.0$), ($342.62\to 0.0$), ($342.62\to 255.48$), ($342.62\to 303.84$), ($342.62\to 41.16$)
${}^{116}$Ag	?	0.0 47.9 129.8	$2.30\times {10}^2$ $2.00\times {10}^1$ $9.30\times {10}^0$	98.1 86.1	A A	($114.73\to 0.0$), ($114.73\to 47.9$), ($114.73\to 91.06$), ($215.82\to 114.73$), ($215.82\to 47.9$), ($215.82\to 91.06$), ($393.42\to 0.0$), ($393.42\to 215.82$), ($393.42\to 91.06$), ($47.9\to 0.0$), ($91.06\to 0.0$), ($91.06\to 47.9$)
${}^{117}$Ag	10–15	0.0 28.6	$7.28\times {10}^1$ $5.34\times {10}^0$	94.6	A	($247.5\to 0.0$), ($247.5\to 28.6$), ($323.9\to 0.0$), ($323.9\to 247.5$), ($323.9\to 28.6$)
${}^{118}$Ag	10–16	0.0 127.6	$3.76\times {10}^0$ $2.00\times {10}^0$	0.0	N	($125.43\to 0.0$), ($125.43\to 45.79$), ($127.63\to 45.79$), ($127.63\to 95.61$), ($279.37\to 0.0$), ($279.37\to 125.43$), ($279.37\to 45.79$), ($279.37\to 95.61$), ($95.61\to 0.0$), ($95.61\to 45.79$)
${}^{122}$Ag	?	0.0 0.0 + X 80.0	$5.29\times {10}^{-1}$ $5.50\times {10}^{-1}$ $2.00\times {10}^{-1}$	0.0 0.0	B (?) B (?)	($0.0+X\to 0.0$)
${}^{111}$Cd	N/A	0.0 396.2	stable $2.91\times {10}^3$	0.0	N	($416.72\to 396.214$), ($680.48\to 396.214$), ($680.48\to 416.72$), ($700.0\to 245.39$), ($700.0\to 396.214$), ($700.0\to 416.72$), ($704.93\to 245.39$), ($736.0\to 0.0$), ($736.0\to 245.39$), ($752.81\to 245.39$), ($752.81\to 342.135$), ($754.9\to 0.0$), ($754.9\to 245.39$), ($831.26\to 245.39$)
${}^{113}$Cd	6–7	0.0 263.5	$2.54\times {10}^{23}$ $4.45\times {10}^8$	99.8	A	($316.206\to 263.54$), ($458.633\to 263.54$), ($458.633\to 316.206$), ($522.259\to 458.633$), ($530.0\to 263.54$), ($530.0\to 316.206$), ($530.0\to 458.633$)
${}^{115}$Cd	10–12	0.0 181.0	$1.92\times {10}^5$ $3.85\times {10}^6$	100.0	B (6.0)	($181.0\to 0.0$), ($229.1\to 0.0$), ($360.5\to 229.1$), ($389.0\to 181.0$), ($389.0\to 360.5$), ($393.9\to 360.5$), ($393.9\to 389.0$), ($417.2\to 181.0$), ($417.2\to 393.9$)
${}^{117}$Cd	10–13	0.0 136.4	$8.96\times {10}^3$ $1.21\times {10}^4$	100.0	N	($136.4\to 0.0$), ($278.4\to 136.4$), ($292.0\to 0.0$), ($292.0\to 135.4$), ($293.5\to 278.4$), ($293.5\to 292.0$), ($442.6\to 0.0$), ($442.6\to 135.4$), ($442.6\to 292.0$), ($442.6\to 293.5$)
${}^{119}$Cd	10–14	0.0 146.5	$1.61\times {10}^2$ $1.32\times {10}^2$	100.0	N	($146.54\to 27.0$), ($213.91\to 27.0$), ($228.27\to 27.0$), ($399.17\to 0.0$), ($399.17\to 228.27$), ($399.17\to 27.0$)
${}^{121}$Cd	14–16	0.0 214.9	$1.35\times {10}^1$ $8.30\times {10}^0$	100.0	N	($214.86\to 0.0$), ($314.5\to 7.52$), ($329.92\to 314.5$), ($353.48\to 0.0$), ($353.48\to 314.5$), ($353.48\to 329.92$), ($369.35\to 0.0$), ($369.35\to 314.5$), ($7.52\to 0.0$)
${}^{123}$Cd	15–20	0.0 316.5	$2.10\times {10}^0$ $1.82\times {10}^0$	0.3	N	($116.4\to 0.0$), ($263.867\to 116.4$), ($316.53\to 263.867$), ($409.76\to 0.0$), ($409.76\to 263.867$), ($440.1\to 263.867$), ($440.1\to 316.53$)
${}^{129}$Cd	?	0.0 0+X 1940.0	$1.54\times {10}^{-1}$ $1.46\times {10}^{-1}$ $3.60\times {10}^{-3}$	100.0 0.0	N N	($0+X\to 0.0$)
${}^{115}$In	9	0.0 336.2	$1.39\times {10}^{22}$ $1.61\times {10}^4$	4.4	A	($597.144\to 0.0$)
${}^{116}$In	18–25	0.0 127.3 289.7	$1.41\times {10}^1$ $3.26\times {10}^3$ $2.18\times {10}^0$	100.0 0.0	B (9.0) N	($127.267\to 0.0$), ($223.33\to 0.0$), ($272.966\to 223.33$), ($373.373\to 127.267$), ($373.373\to 313.476$), ($448.032\to 0.0$), ($448.032\to 223.33$), ($448.032\to 272.966$), ($448.032\to 313.476$), ($458.942\to 127.267$), ($458.942\to 223.33$), ($458.942\to 313.476$)
${}^{117}$In	24–30	0.0 315.3	$2.59\times {10}^3$ $6.97\times {10}^3$	37.4	B (13.0)	($1028.04\to 659.765$), ($1028.04\to 748.07$), ($1028.04\to 880.72$), ($588.653\to 0.0$), ($748.07\to 0.0$), ($880.72\to 0.0$), ($880.72\to 588.653$), ($880.72\to 659.765$), ($880.72\to 748.07$)
${}^{118}$In	?	0.0 60.0 200.0	$5.00\times {10}^0$ $2.67\times {10}^2$ $8.50\times {10}^0$	100.0 1.4	B (?) N	($60.0\to 0.0$)
${}^{119}$In	26–33	0.0 311.4	$1.44\times {10}^2$ $1.08\times {10}^3$	95.7	B (17.0)	($1044.44\to 654.27$), ($1044.44\to 720.6$), ($1044.44\to 788.26$), ($604.18\to 0.0$), ($720.6\to 0.0$), ($720.6\to 654.27$), ($941.43\to 0.0$), ($941.43\to 604.18$), ($941.43\to 654.27$), ($941.43\to 720.6$)
${}^{120}$In	?	0.0 0.0 + X 70.0	$3.08\times {10}^0$ $4.73\times {10}^1$ $4.62\times {10}^1$	0.1 100.0	N B (39.0)	($70.0\to 0.0$), ($70.0\to 0.0+X$)
${}^{121}$In	33–45	0.0 313.7	$2.31\times {10}^1$ $2.33\times {10}^2$	98.8	B (21.0)	($1040.33\to 0.0$), ($1040.33\to 637.9$), ($637.9\to 0.0$), ($637.9\to 313.68$)
${}^{122}$In	?	0.0 40.0 290.0	$1.50\times {10}^0$ $1.03\times {10}^1$ $1.08\times {10}^1$	100.0 0.2	B (42.0) N	($40.0\to 0.0$)
${}^{123}$In	34–48	0.0 327.2	$6.17\times {10}^0$ $4.74\times {10}^1$	100.0	B (24.0)	($1052.29\to 0.0$), ($1052.29\to 698.55$), ($327.21\to 0.0$), ($698.55\to 0.0$), ($698.55\to 327.21$)
${}^{124}$In	?	0.0 50.0	$3.12\times {10}^0$ $3.70\times {10}^0$	100.0	N	($122.0\to 0.0$), ($122.0\to 36.53$), ($122.0\to 50.0$), ($179.88\to 0.0$), ($179.88\to 122.0$), ($179.88\to 36.53$), ($36.53\to 0.0$), ($50.0\to 0.0$), ($50.0\to 36.53$)
${}^{125}$In	?	0.0 360.1 2161.2	$2.36\times {10}^0$ $1.22\times {10}^1$ $5.00\times {10}^{-3}$	100.0 0.0	B (25.0) N	($1099.48\to 0.0$), ($1099.48\to 796.44$), ($1219.8\to 360.12$), ($1219.8\to 796.44$), ($360.12\to 0.0$), ($796.44\to 0.0$), ($796.44\to 360.12$)
${}^{126}$In	?	0.0 102.0	$1.53\times {10}^0$ $1.64\times {10}^0$	100.0	N	($102.0\to 0.0$), ($260.09\to 0.0$), ($260.09\to 102.0$), ($308.1\to 0.0$), ($308.1\to 102.0$), ($308.1\to 260.09$)
${}^{127}$In	?	0.0 408.9 1863.0	$1.09\times {10}^0$ $3.67\times {10}^0$ $1.04\times {10}^0$	100.0 100.0	B (20.0) N	($1066.26\to 0.0$), ($1066.26\to 932.5$), ($1202.3\to 0.0$), ($1202.3\to 932.5$), ($1235.16\to 0.0$), ($1235.16\to 932.5$), ($408.9\to 0.0$), ($932.5\to 408.9$)
${}^{128}$In	?	0.0 340.0	$8.40\times {10}^{-1}$ $7.20\times {10}^{-1}$	100.0	N	($340.0\to 0.0$)
${}^{129}$In	?	0.0 459.0 1630.0 1911.0	$6.11\times {10}^{-1}$ $1.23\times {10}^0$ $6.70\times {10}^{-1}$ $1.10\times {10}^{-1}$	100.0 100.0 0.0	B (17.0) N N	($1020.5\to 0.0$), ($1020.5\to 858.8$), ($1091.0\to 459.0$), ($1091.0\to 858.8$), ($1422.8\to 1091.0$), ($1422.8\to 858.8$), ($459.0\to 0.0$), ($858.8\to 0.0$), ($858.8\to 459.0$)
${}^{130}$In	?	0.0 50.0 400.0	$2.90\times {10}^{-1}$ $5.40\times {10}^{-1}$ $5.40\times {10}^{-1}$	100.0 10.5	B (?) N	($1170.3\to 0.0$), ($1170.3\to 388.3$), ($1170.3\to 400.0$), ($400.0\to 388.3$), ($400.0\to 50.0$), ($50.0\to 0.0$)
${}^{131}$In	?	0.0 302.0 3764.0	$2.80\times {10}^{-1}$ $3.50\times {10}^{-1}$ $3.20\times {10}^{-1}$	100.0 89.0	N B (?)	($1650.0\to 0.0$), ($1650.0\to 302.0$), ($2750.0\to 0.0$), ($2750.0\to 1650.0$), ($302.0\to 0.0$)
${}^{133}$In	?	0.0 330.0	$1.65\times {10}^{-1}$ $1.80\times {10}^{-1}$	0.0	B (?)	($330.0\to 0.0$)
${}^{117}$Sn	N/A	0.0 314.6	stable $1.21\times {10}^6$	0.0	N	($1019.92\to 711.54$), ($1304.3\to 711.54$)
${}^{119}$Sn	N/A	0.0 89.5	stable $2.53\times {10}^7$	0.0	N	($1062.4\to 787.01$), ($1062.4\to 89.531$), ($1062.4\to 921.39$), ($921.39\to 787.01$)
${}^{121}$Sn	19–24	0.0 6.3	$9.73\times {10}^4$ $1.39\times {10}^9$	21.6	B (20.0)	($663.63\to 0.0$), ($663.63\to 6.31$), ($869.25\to 0.0$), ($869.25\to 663.63$), ($908.8\to 0.0$), ($908.8\to 663.63$)
${}^{123}$Sn	24–31	0.0 24.6	$1.12\times {10}^7$ $2.40\times {10}^3$	100.0	A	($1044.3\to 931.4$), ($1136.3\to 150.4$), ($1136.3\to 24.6$), ($1136.3\to 618.81$), ($150.4\to 24.6$), ($24.6\to 0.0$), ($618.81\to 0.0$), ($618.81\to 24.6$), ($870.2\to 150.4$), ($870.2\to 24.6$), ($931.4\to 0.0$), ($931.4\to 618.81$), ($931.4\to 870.2$)
${}^{125}$Sn	24–32	0.0 27.5	$8.33\times {10}^5$ $5.71\times {10}^2$	100.0	A	($27.5\to 0.0$), ($617.89\to 0.0$), ($617.89\to 27.5$), ($854.69\to 27.5$), ($854.69\to 617.89$)
${}^{127}$Sn	25–33	0.0 5.1	$7.56\times {10}^3$ $2.48\times {10}^2$	100.0	A	($1053.62\to 646.31$), ($1053.62\to 809.94$), ($1053.62\to 963.61$), ($257.76\to 0.0$), ($257.76\to 5.07$), ($5.07\to 0.0$), ($646.31\to 0.0$), ($646.31\to 5.07$), ($809.94\to 5.07$), ($963.61\to 0.0$), ($963.61\to 646.31$), ($963.61\to 809.94$)
${}^{128}$Sn	69–91	0.0 2091.5	$3.54\times {10}^3$ $6.50\times {10}^0$	0.0	N	($2000.37\to 1168.82$), ($2091.5\to 0.0$), ($2091.5\to 1168.82$), ($2104.07\to 1168.82$), ($2120.91\to 1168.82$), ($2120.91\to 2091.5$), ($2120.91\to 2104.07$), ($2274.06\to 1168.82$), ($2274.06\to 2000.37$), ($2274.06\to 2120.91$), ($2378.08\to 0.0$), ($2378.08\to 2091.5$), ($2378.08\to 2120.91$), ($2412.71\to 0.0$), ($2412.71\to 2378.08$), ($2491.89\to 0.0$), ($2547.1\to 2091.5$), ($2547.1\to 2120.91$), ($2547.1\to 2412.71$), ($2633.09\to 1168.82$), ($2633.09\to 2120.91$), ($2642.27\to 1168.82$), ($2642.27\to 2120.91$), ($3175.78\to 0.0$), ($3175.78\to 2412.71$), ($3383.14\to 0.0$), ($3383.14\to 2412.71$), ($3553.8\to 0.0$), ($3553.8\to 2491.89$)
${}^{129}$Sn	27–36	0.0 35.1	$1.34\times {10}^2$ $4.14\times {10}^2$	100.0	B (29.0)	($1043.66\to 35.15$), ($1043.66\to 763.7$), ($1043.66\to 769.07$), ($1047.35\to 0.0$), ($1047.35\to 763.7$), ($1047.35\to 769.07$), ($1054.21\to 763.7$), ($1054.21\to 769.07$), ($35.15\to 0.0$), ($763.7\to 0.0$), ($763.7\to 35.15$), ($769.07\to 0.0$), ($769.07\to 35.15$)
${}^{130}$Sn	56–70	0.0 1946.9	$2.23\times {10}^2$ $1.02\times {10}^2$	100.0	A	($1221.26\to 0.0$), ($1946.88\to 0.0$), ($1946.88\to 1221.26$), ($1995.62\to 1221.26$), ($1995.62\to 1946.88$), ($2028.31\to 1221.26$), ($2028.31\to 1995.62$), ($2084.84\to 1221.26$), ($2214.64\to 1221.26$), ($2256.96\to 0.0$), ($2256.96\to 1946.88$), ($2256.96\to 2084.84$), ($2338.26\to 0.0$), ($2338.26\to 2256.96$), ($2434.79\to 0.0$), ($2434.79\to 1946.88$), ($2490.86\to 1221.26$), ($2490.86\to 1995.62$), ($2490.86\to 2084.84$), ($2490.86\to 2214.64$), ($2492.99\to 1995.62$), ($2492.99\to 2084.84$), ($2492.99\to 2214.64$), ($2492.99\to 2256.96$), ($4205.73\to 0.0$), ($4205.73\to 2338.26$)
${}^{128}$Sb	?	0.0 0.0 + X	$3.26\times {10}^4$ $6.25\times {10}^2$	99.9	A	($0.0+X\to 0.0$)
${}^{129}$Sb	49–61	0.0 1851.3	$1.57\times {10}^4$ $1.06\times {10}^3$	0.0	A	($1128.63\to 0.0$), ($1128.63\to 645.14$), ($1161.39\to 0.0$), ($1161.39\to 1128.63$), ($1161.39\to 645.14$), ($1252.25\to 0.0$), ($1252.25\to 645.14$), ($1252.25\to 913.58$), ($1851.31\to 1161.39$), ($1851.31\to 1252.25$), ($1861.06\to 0.0$), ($1861.06\to 1252.25$), ($1911.21\to 1128.63$), ($1911.21\to 1861.06$), ($1928.63\to 1851.31$), ($1928.63\to 1861.06$), ($1940.37\to 1851.31$), ($1940.37\to 1861.06$), ($1972.75\to 1128.63$), ($1972.75\to 1861.06$), ($1991.95\to 1128.63$), ($1991.95\to 1861.06$), ($2040.81\to 1851.31$), ($2040.81\to 1928.63$), ($2040.81\to 1940.37$), ($2148.46\to 0.0$), ($2148.46\to 1128.63$), ($2148.46\to 1861.06$), ($2148.46\to 1940.37$), ($2221.32\to 0.0$), ($2221.32\to 1940.37$), ($2232.16\to 0.0$), ($2232.16\to 1128.63$), ($2232.16\to 1940.37$), ($645.14\to 0.0$), ($913.58\to 645.14$)
${}^{130}$Sb	3–4	0.0 4.8	$2.37\times {10}^3$ $3.78\times {10}^2$	100.0	A	($4.8\to 0.0$), ($84.67\to 0.0$), ($84.67\to 4.8$)
${}^{134}$Sb	19–26	0.0 279.0	$7.80\times {10}^{-1}$ $1.01\times {10}^1$	100.0	B (10.0)	($13.0\to 0.0$), ($279.0\to 13.0$), ($384.0\to 13.0$), ($384.0\to 331.1$), ($441.0\to 279.0$), ($441.0\to 384.0$), ($555.0\to 384.0$), ($555.0\to 441.0$), ($617.0\to 279.0$), ($617.0\to 441.0$)
${}^{125}$Te	N/A	0.0 144.8	stable $4.96\times {10}^6$	0.0	N	($321.09\to 35.4925$), ($402.09\to 321.09$), ($402.09\to 35.4925$), ($463.3668\to 402.09$), ($525.228\to 402.09$), ($652.9\to 35.4925$), ($652.9\to 402.09$), ($671.4448\to 525.228$)
${}^{127}$Te	15–19	0.0 88.2	$3.37\times {10}^4$ $9.17\times {10}^6$	2.3	B (13.0)	($340.87\to 0.0$), ($473.26\to 0.0$), ($631.4\to 340.87$), ($631.4\to 473.26$), ($685.09\to 340.87$), ($685.09\to 473.26$), ($685.09\to 631.4$)
${}^{129}$Te	13–17	0.0 105.5	$4.18\times {10}^3$ $2.90\times {10}^6$	35.2	B (10.0)	($180.356\to 0.0$), ($360.0\to 0.0$), ($360.0\to 180.356$), ($455.0\to 0.0$), ($455.0\to 105.51$), ($455.0\to 360.0$)
${}^{131}$Te	?	0.0 182.3 1940.0	$1.50\times {10}^3$ $1.20\times {10}^5$ $9.30\times {10}^{-2}$	62.6 0.0	B (21.0) N	($1267.5\to 0.0$), ($1267.5\to 802.214$), ($1267.5\to 880.315$), ($642.331\to 0.0$), ($802.214\to 182.258$), ($880.315\to 182.258$), ($880.315\to 642.331$), ($880.315\to 802.214$), ($943.43\to 0.0$), ($943.43\to 642.331$), ($943.43\to 802.214$), ($943.43\to 880.315$)
${}^{133}$Te	35–45	0.0 334.3	$7.50\times {10}^2$ $3.32\times {10}^3$	81.0	B (29.0)	($1096.22\to 0.0$), ($1096.22\to 334.26$), ($1265.326\to 0.0$), ($1500.56\to 0.0$), ($1500.56\to 1096.22$), ($1500.56\to 334.26$), ($1639.5\to 1096.22$), ($1639.5\to 1265.326$), ($1639.5\to 334.26$)
${}^{132}$I	60	0.0 120.0	$8.26\times {10}^3$ $4.99\times {10}^3$	12.5	N	($22.0\to 0.0$)
${}^{133}$I	40–50	0.0 1634.1	$7.50\times {10}^4$ $9.00\times {10}^0$	0.0	N	($1560.103\to 912.671$), ($1560.103\to 914.811$), ($1634.148\to 912.671$), ($1634.148\to 914.811$), ($1729.137\to 912.671$), ($1776.619\to 1560.103$), ($1776.619\to 1729.137$), ($1776.619\to 912.671$), ($1776.619\to 914.811$), ($1798.549\to 1560.103$), ($1798.549\to 1634.148$), ($1798.549\to 1729.137$), ($1816.67\to 1560.103$), ($1942.615\to 1560.103$), ($1942.615\to 912.671$), ($312.075\to 0.0$), ($786.915\to 312.075$), ($912.671\to 0.0$), ($912.671\to 312.075$), ($912.671\to 786.915$), ($914.811\to 0.0$), ($914.811\to 312.075$), ($914.811\to 786.915$), ($914.811\to 912.671$)
${}^{134}$I	74	0.0 316.5	$3.15\times {10}^3$ $2.11\times {10}^2$	2.0	N	($210.457\to 44.39$), ($645.471\to 0.0$), ($645.471\to 210.457$), ($645.471\to 44.39$), ($645.471\to 79.461$)
${}^{136}$I	?	0.0 201.0	$8.34\times {10}^1$ $4.66\times {10}^1$	100.0	N	($201.0\to 86.73$), ($333.97\to 0.0$), ($333.97\to 86.73$), ($578.77\to 0.0$), ($578.77\to 201.0$), ($578.77\to 86.73$), ($738.21\to 0.0$), ($738.21\to 201.0$), ($738.21\to 333.97$), ($738.21\to 86.73$)
${}^{129}$Xe	N/A	0.0 236.1	stable $7.67\times {10}^5$	0.0	N	($274.29\to 236.14$), ($274.29\to 39.5774$), ($321.711\to 274.29$), ($321.711\to 318.1787$), ($442.2\to 318.1787$), ($442.2\to 321.711$), ($442.2\to 39.5774$), ($518.7\to 274.29$), ($518.7\to 321.711$), ($518.7\to 442.2$), ($525.26\to 321.711$), ($525.26\to 39.5774$)
${}^{131}$Xe	N/A	0.0 163.9	stable $1.02\times {10}^6$	0.0	N	($341.144\to 0.0$), ($636.99\to 163.93$), ($666.934\to 636.99$), ($722.909\to 666.934$), ($971.22\to 163.93$), ($971.22\to 341.144$), ($971.22\to 666.934$), ($973.11\to 341.144$), ($973.11\to 666.934$)
${}^{132}$Xe	N/A	0.0 2752.2	stable $8.39\times {10}^{-3}$	0.0	N	($1440.323\to 1297.912$), ($1803.714\to 1297.912$), ($1963.01\to 1297.912$), ($1963.01\to 1440.323$), ($1963.01\to 1803.714$), ($1963.01\to 667.715$), ($2040.31\to 1440.323$), ($2040.31\to 1963.01$), ($2111.88\to 1440.323$), ($2111.88\to 1963.01$), ($2111.88\to 2040.31$), ($2214.01\to 2111.88$), ($2303.42\to 2040.31$), ($2353.1\to 1440.323$), ($2353.1\to 1803.714$), ($2650.3\to 2111.88$), ($2650.3\to 2303.42$), ($2650.3\to 2353.1$), ($2752.21\to 2111.88$), ($2752.21\to 2650.3$), ($2828.0\to 2111.88$), ($2828.0\to 2214.01$), ($2828.0\to 2303.42$), ($2828.0\to 2353.1$), ($2828.0\to 2650.3$), ($2828.0\to 2752.21$), ($2960.3\to 2111.88$), ($2960.3\to 2214.01$), ($2960.3\to 2752.21$)
${}^{133}$Xe	19–24	0.0 233.2	$4.53\times {10}^5$ $1.90\times {10}^5$	0.0	N	($529.872\to 0.0$), ($529.872\to 233.221$), ($607.87\to 0.0$), ($607.87\to 233.221$), ($743.752\to 233.221$), ($875.328\to 0.0$), ($875.328\to 529.872$), ($875.328\to 607.87$), ($875.328\to 743.752$)
${}^{134}$Xe	N/A	0.0 1965.5	$1.83\times {10}^{30}$ $2.90\times {10}^{-1}$	0.0	N	($1613.77\to 847.041$), ($1731.17\to 1613.77$), ($1919.6\to 1731.17$), ($1919.6\to 847.041$), ($1965.5\to 0.0$), ($1965.5\to 1613.77$), ($1965.5\to 1919.6$), ($1965.5\to 847.041$), ($2082.0\to 1731.17$), ($2116.4\to 847.041$), ($2136.6\to 0.0$), ($2136.61\to 0.0$), ($2136.61\to 1731.17$), ($2136.61\to 1965.5$), ($2136.61\to 2136.6$), ($2272.01\to 1731.17$), ($2272.01\to 2082.0$), ($2272.01\to 2116.4$), ($2272.01\to 2136.61$), ($2408.5\to 1731.17$), ($2408.5\to 2116.4$), ($2408.5\to 2136.61$), ($2997.2\to 0.0$), ($2997.2\to 1965.5$), ($3025.2\to 0.0$), ($3025.2\to 1965.5$)
${}^{135}$Xe	34–44	0.0 526.6	$3.29\times {10}^4$ $9.17\times {10}^2$	0.7	N	($1131.512\to 0.0$), ($1131.512\to 526.551$), ($1260.416\to 0.0$), ($1260.416\to 1131.512$), ($1565.288\to 1131.512$), ($1565.288\to 526.551$), ($1894.45\to 1131.512$), ($1894.45\to 1260.416$), ($1894.45\to 526.551$)
${}^{135}$Cs	66	0.0 1632.9	$7.26\times {10}^{13}$ $3.18\times {10}^3$	0.0	N	($1062.385\to 408.026$), ($1062.385\to 608.153$), ($1133.0\to 608.153$), ($1632.9\to 1062.385$), ($1632.9\to 1133.0$), ($1632.9\to 249.767$), ($1632.9\to 408.026$), ($1632.9\to 608.153$), ($1632.9\to 981.396$), ($408.026\to 0.0$), ($408.026\to 249.767$), ($608.153\to 0.0$), ($608.153\to 249.767$), ($786.838\to 0.0$), ($786.838\to 249.767$), ($786.838\to 608.153$), ($981.396\to 408.026$), ($981.396\to 608.153$)
${}^{135}$Ba	N/A	0.0 268.2	stable $1.03\times {10}^5$	0.0	N	($480.532\to 268.218$), ($587.827\to 0.0$), ($587.827\to 220.968$), ($587.827\to 480.532$), ($714.2\to 268.218$), ($714.2\to 480.532$)
${}^{137}$Ba	N/A	0.0 661.7	stable $1.53\times {10}^2$	0.0	N	($1251.82\to 661.659$), ($1293.9\to 0.0$), ($1293.9\to 1251.82$)
${}^{144}$Pr	4	0.0 59.0	$1.04\times {10}^3$ $4.32\times {10}^2$	0.0	N	($80.12\to 59.03$), ($99.952\to 80.12$)
${}^{148}$Pr	4–6	0.0 76.8	$1.37\times {10}^2$ $1.21\times {10}^2$	15.7	N	($98.166\to 0.0$), ($98.166\to 76.8$)
${}^{153}$Sm	5–6	0.0 98.4	$1.67\times {10}^5$ $1.06\times {10}^{-2}$	0.0	N	($188.9\to 65.468$), ($188.9\to 98.37$), ($53.533\to 7.535$), ($65.468\to 53.533$), ($7.535\to 0.0$), ($98.37\to 53.533$)
${}^{155}$Gd	N/A	0.0 121.1	stable $3.20\times {10}^{-2}$	0.0	N	($107.5804\to 60.0106$), ($107.5804\to 86.5464$), ($117.9981\to 107.5804$), ($117.9981\to 60.0106$), ($117.9981\to 86.5464$), ($146.0696\to 107.5804$), ($146.0696\to 117.9981$), ($146.0696\to 121.1$), ($146.0696\to 86.5464$), ($230.1286\to 107.5804$), ($230.1286\to 121.1$), ($251.7056\to 107.5804$), ($251.7056\to 121.1$), ($251.7056\to 230.1286$), ($266.6474\to 0.0$), ($266.6474\to 146.0696$)
${}^{165}$Dy	6–7	0.0 108.2	$8.40\times {10}^3$ $7.54\times {10}^1$	2.2	A	($158.5885\to 0.0$), ($180.922\to 0.0$), ($180.922\to 158.5885$), ($184.2552\to 158.5885$)
${}^{166}$Ho	7–8	0.0 6.0 190.9	$9.66\times {10}^4$ $3.79\times {10}^{10}$ $1.85\times {10}^{-4}$	100.0 0.0	B (7.0) N	($171.0738\to 54.2391$), ($180.467\to 171.0738$), ($180.467\to 5.969$), ($180.467\to 54.2391$), ($260.6625\to 180.467$), ($263.7876\to 180.467$), ($296.8\to 0.0$), ($296.8\to 263.7876$), ($296.8\to 5.969$), ($296.8\to 54.2391$), ($296.8\to 82.4707$), ($54.2391\to 5.969$)
${}^{170}$Ho	?	0.0 120.0	$1.66\times {10}^2$ $4.30\times {10}^1$	100.0	A	($120.0\to 0.0$)
${}^{167}$Er	N/A	0.0 207.8	stable $2.27\times {10}^0$	0.0	N	($281.574\to 0.0$), ($281.574\to 207.801$), ($281.574\to 264.874$), ($346.554\to 264.874$), ($346.554\to 281.574$), ($413.272\to 0.0$), ($531.54\to 346.554$), ($573.76\to 264.874$), ($573.76\to 281.574$), ($573.76\to 346.554$), ($573.76\to 413.272$)
${}^{171}$Yb	N/A	0.0 95.3	stable $5.25\times {10}^{-3}$	0.0	N	($167.662\to 95.282$), ($208.019\to 122.416$), ($208.019\to 167.662$), ($208.019\to 66.732$), ($208.019\to 75.882$), ($208.019\to 95.282$), ($230.631\to 167.662$), ($230.631\to 95.282$), ($246.617\to 167.662$), ($246.617\to 95.282$), ($95.282\to 66.732$)
${}^{175}$Yb	15–19	0.0 514.9	$3.62\times {10}^5$ $6.82\times {10}^{-2}$	0.0	N	($104.5263\to 0.0$), ($514.866\to 104.5263$), ($556.084\to 0.0$), ($556.084\to 514.866$), ($602.836\to 0.0$), ($602.836\to 556.084$), ($639.256\to 0.0$), ($639.256\to 556.084$)
${}^{176}$Yb	N/A	0.0 1049.8	stable $1.14\times {10}^1$	0.0	N	($1049.8\to 564.5$), ($271.85\to 0.0$), ($564.5\to 82.135$), ($953.9\to 271.85$)
${}^{177}$Yb	12–17	0.0 331.5	$6.88\times {10}^3$ $6.41\times {10}^0$	0.0	N	($121.7\to 0.0$), ($220.6\to 0.0$), ($220.6\to 104.51$), ($220.6\to 121.7$), ($375.3\to 104.51$), ($375.3\to 331.5$), ($423.4\to 104.51$), ($423.4\to 375.3$)
${}^{177}$Lu	33–45	0.0 569.7 970.2	$5.74\times {10}^5$ $1.55\times {10}^{-4}$ $1.39\times {10}^7$	0.0 9.6	N B (3.0)	($573.6203\to 0.0$), ($573.6203\to 569.6721$), ($709.4074\to 0.0$), ($709.4074\to 573.6203$), ($761.863\to 457.9568$), ($761.863\to 569.6721$), ($761.863\to 573.6203$), ($795.218\to 569.6721$), ($795.218\to 573.6203$), ($956.411\to 457.9568$), ($956.411\to 569.6721$), ($956.411\to 573.6203$), ($956.411\to 709.4074$)
${}^{178}$Lu	12–19	0.0 123.8	$1.70\times {10}^3$ $1.39\times {10}^3$	100.0	N	($133.0\to 123.8$), ($133.0\to 42.4$), ($133.0\to 96.0$), ($187.0\to 123.8$), ($187.0\to 133.0$), ($300.0\to 133.0$), ($300.0\to 96.0$), ($42.4\to 0.0$), ($96.0\to 42.4$)
${}^{179}$Lu	21–26	0.0 592.4	$1.65\times {10}^4$ $3.10\times {10}^{-3}$	0.0	N	($35.0\to 0.0$), ($593.0\to 0.0$), ($593.0\to 592.4$), ($653.4\to 0.0$), ($653.4\to 592.4$), ($653.4\to 593.0$), ($735.0\to 35.0$), ($916.7\to 0.0$), ($916.7\to 592.4$), ($916.7\to 593.0$), ($916.7\to 653.4$), ($916.7\to 735.0$)
${}^{180}$Lu	24–37	0.0 624.0	$3.42\times {10}^2$ $1.00\times {10}^{-3}$	0.0	N	($141.0\to 0.0$), ($306.0\to 141.0$), ($496.0\to 306.0$), ($624.0\to 306.0$)
${}^{177}$Hf	N/A	0.0 1315.5 2740.0	stable $1.09\times {10}^0$ $3.08\times {10}^3$	0.0 0.0	N N	($1017.7911\to 882.8611$), ($1086.9662\to 794.4394$), ($1301.4004\to 1017.7911$), ($1315.4502\to 1017.7911$), ($1520.6\to 1301.4004$), ($1520.6\to 1315.4502$), ($1583.0\to 1086.9662$), ($1583.0\to 1315.4502$), ($409.4085\to 249.6744$), ($555.1779\to 249.6744$), ($555.1779\to 409.4085$), ($591.3179\to 409.4085$), ($591.3179\to 555.1779$), ($708.4622\to 409.4085$), ($708.4622\to 591.3179$), ($794.4394\to 708.4622$), ($882.8611\to 591.3179$)
${}^{178}$Hf	N/A	0.0 1147.4 2446.1	stable $4.00\times {10}^0$ $9.78\times {10}^8$	0.0 0.0	N N	($1147.416\to 632.178$), ($1364.078\to 1058.55$), ($1364.078\to 1147.416$), ($1479.025\to 1058.55$), ($1479.025\to 1147.416$), ($306.6182\to 0.0$), ($306.6182\to 93.1803$), ($632.178\to 93.1803$)
${}^{179}$Hf	N/A	0.0 375.0 1105.7	stable $1.87\times {10}^1$ $2.16\times {10}^6$	0.0 0.0	N N	($337.7178\to 0.0$), ($337.7178\to 122.7904$), ($337.7178\to 214.3395$), ($420.8943\to 214.3395$), ($420.8943\to 375.0352$), ($476.3341\to 214.3395$), ($476.3341\to 420.8943$), ($679.516\to 375.0352$), ($679.516\to 476.3341$), ($701.0552\to 214.3395$), ($701.0552\to 420.8943$)
${}^{180}$Hf	2	0.0 1141.6	stable $1.99\times {10}^4$	0.0	A	($1141.552\to 308.576$), ($308.576\to 0.0$), ($640.849\to 93.324$)
${}^{181}$Hf	44–74	0.0 1043.5 1741.9	$3.66\times {10}^6$ $1.00\times {10}^{-4}$ $1.50\times {10}^{-3}$	0.0 0.0	N N	($1009.07\to 465.93$), ($1009.07\to 835.0$), ($1043.5\to 835.0$), ($203.992\to 98.603$), ($251.991\to 0.0$), ($251.991\to 45.763$), ($251.991\to 98.603$), ($303.88\to 203.992$), ($303.88\to 98.603$), ($440.68\to 98.603$), ($45.763\to 0.0$), ($465.93\to 303.88$), ($595.27\to 203.992$), ($595.27\to 303.88$), ($595.27\to 440.68$), ($595.27\to 465.93$), ($617.2\to 303.88$), ($617.2\to 465.93$), ($619.9\to 465.93$), ($758.63\to 465.93$), ($758.63\to 617.2$), ($758.63\to 619.9$), ($835.0\to 619.9$), ($835.0\to 758.63$), ($98.603\to 45.763$)
${}^{182}$Hf	21–24	0.0 1172.9	$2.81\times {10}^{14}$ $3.69\times {10}^3$	0.3	A	($1122.07\to 666.27$), ($1172.87\to 322.17$), ($1419.5\to 1122.07$), ($1419.5\to 1172.87$), ($322.17\to 0.0$), ($322.17\to 97.79$), ($666.27\to 322.17$), ($666.27\to 97.79$), ($97.79\to 0.0$)
${}^{184}$Hf	82–100	0.0 1272.2	$1.48\times {10}^4$ $4.80\times {10}^1$	0.0	N	($107.1\to 0.0$), ($1199.5\to 717.2$), ($1272.2\to 349.6$), ($349.6\to 0.0$), ($349.6\to 107.1$), ($717.2\to 107.1$), ($717.2\to 349.6$)
${}^{182}$Ta	47–68	0.0 16.3 519.6	$9.91\times {10}^6$ $2.83\times {10}^{-1}$ $9.50\times {10}^2$	0.0 0.0	N N	($114.3126\to 0.0$), ($114.3126\to 16.273$), ($150.15\to 0.0$), ($150.15\to 114.3126$), ($150.15\to 16.273$), ($150.15\to 97.8304$), ($237.286\to 150.15$), ($237.286\to 16.273$), ($249.982\to 0.0$), ($249.982\to 114.3126$), ($249.982\to 97.8304$), ($292.9352\to 150.15$), ($292.9352\to 16.273$), ($364.359\to 0.0$), ($364.359\to 114.3126$), ($97.8304\to 0.0$), ($97.8304\to 16.273$)
${}^{188}$Ta	?	0.0 99.0	$1.96\times {10}^1$ $1.96\times {10}^1$	0.0	B (?)	($99.0\to 0.0$)
${}^{183}$W	N/A	0.0 309.5	$2.11\times {10}^{28}$ $5.30\times {10}^0$	0.0	N	($207.0114\to 99.0791$), ($308.9466\to 207.0114$), ($309.492\to 308.9466$), ($475.05\to 308.9466$), ($475.05\to 309.492$), ($551.24\to 207.0114$), ($551.24\to 309.492$), ($557.5\to 0.0$), ($557.5\to 99.0791$), ($622.6\to 207.0114$), ($622.6\to 475.05$)
${}^{185}$W	7–9	0.0 197.4	$6.49\times {10}^6$ $1.00\times {10}^2$	0.0	N	($187.878\to 0.0$), ($187.878\to 173.702$), ($187.878\to 65.854$), ($187.878\to 93.295$), ($23.547\to 0.0$), ($243.62\to 187.878$), ($243.62\to 197.383$), ($302.0\to 173.702$), ($302.0\to 197.383$), ($302.0\to 243.62$), ($65.854\to 0.0$), ($93.295\to 0.0$), ($93.295\to 23.547$)
${}^{186}$W	N/A	0.0 3542.8	stable $3.00\times {10}^{-3}$	0.0	N	($1517.2\to 1349.2$), ($1517.2\to 809.25$), ($2117.8\to 1349.2$), ($2117.8\to 2002.4$), ($2285.8\to 2002.4$), ($2522.8\to 2002.4$), ($2672.8\to 2002.4$), ($2672.8\to 2285.8$), ($2672.8\to 2522.8$), ($2750.9\to 2522.8$), ($2837.8\to 2522.8$), ($2837.8\to 2672.8$), ($2837.8\to 2750.9$), ($3143.8\to 2837.8$), ($3362.8\to 3143.8$), ($3542.8\to 3362.8$)
${}^{190}$W	69–93	0.0 2381.0	$1.80\times {10}^3$ $3.10\times {10}^{-3}$	0.0	N	($1049.0\to 207.0$), ($1049.0\to 564.0$), ($1640.0\to 1049.0$), ($1640.0\to 564.0$), ($207.0\to 0.0$), ($2335.0\to 1640.0$), ($2381.0\to 1049.0$), ($2381.0\to 1640.0$), ($564.0\to 0.0$), ($564.0\to 207.0$)
${}^{188}$Re	9–11	0.0 172.1	$6.12\times {10}^4$ $1.12\times {10}^3$	0.0	N	($156.0558\to 63.5959$), ($169.449\to 63.5959$), ($182.7594\to 156.0558$), ($182.7594\to 169.449$), ($182.7594\to 172.0848$), ($230.9213\to 182.7594$), ($230.9213\to 205.3539$), ($339.956\to 172.0848$), ($339.956\to 182.7594$)
${}^{190}$Re	49–100	0.0 210.0	$1.86\times {10}^2$ $1.15\times {10}^4$	5.3	B (87.0)	($119.12\to 0.0$), ($210.0\to 0.0$), ($210.0\to 119.12$)
${}^{194}$Re	?	0.0 285.0 833.0	$5.00\times {10}^0$ $2.50\times {10}^1$ $1.00\times {10}^2$	100.0 100.0	B (?) B (?)	($X\to 0.0$), ($X\to 285.0$)
${}^{189}$Os	N/A	0.0 30.8	stable $2.09\times {10}^4$	0.0	N	($350.0\to 216.67$), ($350.0\to 219.39$), ($350.0\to 97.35$), ($365.78\to 30.82$), ($365.78\to 69.54$), ($427.93\to 69.54$), ($427.93\to 95.27$), ($438.73\to 0.0$), ($438.73\to 69.54$), ($444.23\to 216.67$), ($444.23\to 219.39$), ($444.23\to 233.58$), ($444.23\to 30.82$), ($444.23\to 69.54$), ($69.54\to 30.82$), ($97.35\to 30.82$)
${}^{190}$Os	N/A	0.0 1705.4	stable $5.94\times {10}^2$	0.0	N	($1203.86\to 1050.38$), ($1203.86\to 547.854$), ($1474.2\to 1203.86$), ($1666.47\to 1474.2$), ($1705.4\to 1050.38$), ($1705.4\to 1203.86$), ($1705.4\to 1474.2$), ($756.022\to 186.718$), ($756.022\to 547.854$)
${}^{191}$Os	4–6	0.0 74.4	$1.33\times {10}^6$ $4.72\times {10}^4$	0.0	N	($131.941\to 0.0$), ($131.941\to 74.382$)
${}^{192}$Os	3	0.0 2015.4	stable $5.90\times {10}^0$	7.6	A	($1089.23\to 909.592$), ($1143.519\to 580.28$), ($1143.519\to 909.592$), ($1465.34\to 1143.519$), ($1712.91\to 1089.23$), ($1712.91\to 1465.34$), ($2015.4\to 1089.23$), ($2015.4\to 1465.34$)
${}^{195}$Os	1	0.0 454.0	$3.90\times {10}^2$ $5.40\times {10}^2$	0.0	N	($438.6\to 0.0$), ($454.0\to 0.0$), ($454.0\to 438.6$)
${}^{191}$Ir	N/A	0.0 171.3	stable $4.90\times {10}^0$	0.0	N	($343.23\to 171.29$), ($390.94\to 129.413$), ($390.94\to 343.23$), ($502.61\to 171.29$), ($502.61\to 390.94$)
${}^{192}$Ir	32–100	0.0 56.7 168.1	$6.38\times {10}^6$ $8.70\times {10}^1$ $7.61\times {10}^9$	0.0 0.0	A B (?)	($115.564\to 104.776$), ($115.564\to 56.72$), ($115.564\to 84.275$), ($139.942\to 0.0$), ($139.942\to 66.83$), ($144.904\to 0.0$), ($144.904\to 66.83$), ($192.935\to 104.776$), ($192.935\to 115.564$), ($192.935\to 118.7824$), ($192.935\to 56.72$), ($192.935\to 84.275$), ($212.808\to 56.72$), ($212.808\to 84.275$), ($216.905\to 0.0$), ($216.905\to 118.7824$), ($216.905\to 66.83$), ($216.905\to 84.275$), ($225.918\to 56.72$), ($225.918\to 84.275$), ($240.902\to 56.72$), ($240.902\to 84.275$), ($256.8\to 0.0$), ($256.8\to 139.942$), ($256.8\to 144.904$), ($256.8\to 216.905$), ($84.275\to 56.72$), ($84.275\to 66.83$)
${}^{193}$Ir	N/A	0.0 80.2 2278.9	stable $9.10\times {10}^5$ $1.25\times {10}^{-4}$	0.0 0.0	N N	($138.941\to 80.238$), ($299.396\to 138.941$), ($521.926\to 299.396$), ($521.926\to 80.238$)
${}^{194}$Ir	?	0.0 147.1 190.0 + X	$6.94\times {10}^4$ $3.19\times {10}^{-2}$ $1.48\times {10}^7$	0.0 100.0	N B (?)	($112.232\to 0.0$), ($138.688\to 0.0$), ($148.934\to 0.0$), ($148.934\to 112.232$), ($148.934\to 147.072$), ($148.934\to 82.336$), ($148.934\to 84.285$), ($160.998\to 0.0$), ($184.688\to 112.232$), ($184.688\to 147.072$), ($184.688\to 148.934$), ($184.688\to 84.285$), ($195.527\to 0.0$), ($245.11\to 112.232$), ($245.11\to 147.072$), ($245.11\to 84.285$), ($254.161\to 0.0$), ($270.917\to 112.232$), ($270.917\to 148.934$), ($270.917\to 184.688$), ($270.917\to 84.285$), ($278.505\to 0.0$), ($390.963\to 0.0$), ($390.963\to 138.688$), ($390.963\to 147.072$), ($390.963\to 160.998$), ($407.018\to 112.232$), ($407.018\to 184.688$), ($407.018\to 195.527$), ($407.018\to 245.11$), ($407.018\to 254.161$), ($407.018\to 278.505$), ($82.336\to 0.0$), ($84.285\to 0.0$)
${}^{195}$Ir	14–20	0.0 100.0	$8.24\times {10}^3$ $1.32\times {10}^4$	100.0	N	($100.0\to 0.0$), ($175.221\to 0.0$), ($175.221\to 100.0$), ($394.0\to 100.0$), ($394.0\to 175.221$)
${}^{196}$Ir	?	0.0 410.0	$5.20\times {10}^1$ $5.04\times {10}^3$	100.0	B (?)	($126.2\to 0.0$), ($207.04\to 0.0$), ($207.04\to 126.2$), ($407.88\to 0.0$), ($407.88\to 126.2$), ($407.88\to 207.04$), ($410.0\to 126.2$), ($522.37\to 0.0$), ($522.37\to 126.2$)
${}^{197}$Ir	26–48	0.0 115.0	$3.48\times {10}^2$ $5.34\times {10}^2$	100.0	N	($115.0\to 0.0$), ($460.0\to 0.0$), ($460.0\to 115.0$), ($606.0\to 0.0$), ($606.0\to 115.0$), ($761.0\to 0.0$), ($761.0\to 115.0$)
${}^{195}$Pt	N/A	0.0 259.1	stable $3.46\times {10}^5$	0.0	N	($199.532\to 129.772$), ($211.406\to 129.772$), ($211.406\to 98.88$), ($222.23\to 0.0$), ($222.23\to 98.88$), ($239.264\to 129.772$), ($431.98\to 259.077$), ($449.65\to 129.772$), ($449.65\to 239.264$), ($449.65\to 431.98$), ($507.917\to 199.532$), ($507.917\to 239.264$), ($507.917\to 431.98$), ($547.16\to 259.077$), ($547.16\to 431.98$), ($562.8\to 431.98$), ($667.0\to 431.98$), ($667.0\to 547.16$)
${}^{197}$Pt	16–23	0.0 399.6	$7.16\times {10}^4$ $5.72\times {10}^3$	0.0	N	($273.0\to 53.088$), ($273.0\to 71.6$), ($371.0\to 273.0$), ($371.0\to 53.088$), ($399.59\to 371.0$), ($520.0\to 273.0$), ($520.0\to 399.59$), ($520.0\to 53.088$), ($612.0\to 371.0$), ($612.0\to 399.59$), ($71.6\to 0.0$), ($71.6\to 53.088$), ($98.6\to 0.0$), ($98.6\to 53.088$)
${}^{199}$Pt	17–25	0.0 424.0	$1.85\times {10}^3$ $1.36\times {10}^1$	0.0	N	($32.0\to 0.0$), ($35.9\to 0.0$), ($351.0\to 0.0$), ($351.0\to 32.0$), ($351.0\to 35.9$), ($351.0\to 42.0$), ($351.0\to 87.4$), ($42.0\to 0.0$), ($424.0\to 351.0$), ($495.0\to 32.0$), ($495.0\to 424.0$), ($87.4\to 0.0$)
${}^{197}$Au	N/A	0.0 409.1	stable $7.73\times {10}^0$	0.0	N	($279.0\to 268.788$), ($502.5\to 268.788$), ($502.5\to 279.0$), ($547.5\to 409.15$), ($547.5\to 502.5$), ($736.7\to 502.5$), ($736.7\to 547.5$), ($855.5\to 409.15$), ($855.5\to 736.7$)
${}^{200}$Au	?	0.0 962.0	$2.90\times {10}^3$ $6.73\times {10}^4$	100.0	B (?)	($103.65\to 0.0$), ($103.65\to 59.98$), ($166.0\to 0.0$), ($292.71\to 0.0$), ($292.71\to 59.98$), ($303.69\to 0.0$), ($303.69\to 59.98$), ($390.22\to 0.0$), ($59.98\to 0.0$), ($76.22\to 0.0$), ($76.22\to 59.98$), ($962.0\to 103.65$), ($962.0\to 166.0$), ($962.0\to 292.71$), ($962.0\to 303.69$), ($962.0\to 390.22$), ($962.0\to 59.98$), ($962.0\to 76.22$)
${}^{199}$Hg	N/A	0.0 532.5	stable $2.56\times {10}^3$	0.0	N	($455.462\to 0.0$), ($455.462\to 158.37859$), ($492.297\to 0.0$), ($492.297\to 158.37859$), ($667.0\to 158.37859$), ($667.0\to 208.20494$), ($667.0\to 532.48$), ($699.0\to 158.37859$), ($699.0\to 208.20494$), ($699.0\to 532.48$)
${}^{205}$Hg	50–65	0.0 1556.4	$3.08\times {10}^2$ $1.09\times {10}^{-3}$	0.0	N	($1280.73\to 379.47$), ($1325.24\to 1280.73$), ($1346.12\to 1325.24$), ($1346.12\to 379.47$), ($1346.12\to 467.52$), ($1395.05\to 1346.12$), ($1395.05\to 379.47$), ($1447.5\to 1395.05$), ($1556.4\to 1447.5$), ($1556.4\to 379.47$), ($1818.18\to 1447.5$), ($1847.23\to 1346.12$), ($1847.23\to 1395.05$), ($1847.23\to 1556.4$), ($2011.41\to 1346.12$), ($2011.41\to 1395.05$), ($2011.41\to 1556.4$), ($379.47\to 0.0$), ($467.52\to 0.0$), ($467.52\to 379.47$)
${}^{206}$Tl	?	0.0 2643.1	$2.52\times {10}^2$ $2.24\times {10}^2$	0.0	N	($1079.6\to 265.832$), ($1079.6\to 304.896$), ($1079.6\to 635.02$), ($1079.6\to 649.42$), ($1079.6\to 801.36$), ($1405.47\to 998.17$), ($1621.7\to 952.17$), ($1710.53\to 1405.47$), ($1710.53\to 1621.7$), ($1710.53\to 952.17$), ($1800.0\to 265.832$), ($1800.0\to 635.02$), ($1800.0\to 952.17$), ($2078.9\to 1621.7$), ($2126.0\to 1621.7$), ($2126.0\to 952.17$), ($2217.0\to 1079.6$), ($2217.0\to 1405.47$), ($2243.0\to 1621.7$), ($2243.0\to 952.17$), ($2264.0\to 1621.7$), ($2264.0\to 952.17$), ($2326.16\to 1621.7$), ($2326.16\to 2078.9$), ($304.896\to 265.832$), ($649.42\to 0.0$), ($649.42\to 265.832$), ($649.42\to 304.896$), ($801.36\to 635.02$), ($952.17\to 801.36$), ($998.17\to 265.832$), ($998.17\to 304.896$), ($998.17\to 635.02$)
${}^{207}$Tl	62–77	0.0 1348.2	$2.86\times {10}^2$ $1.33\times {10}^0$	0.0	N	($1682.58\to 0.0$), ($1682.58\to 1348.18$), ($1682.58\to 351.06$), ($2911.83\to 1348.18$), ($2911.83\to 1682.58$), ($3143.1\to 1348.18$), ($3143.1\to 1682.58$), ($3272.56\to 1348.18$), ($3272.56\to 1682.58$), ($3295.5\to 1348.18$), ($3295.5\to 1682.58$)
${}^{207}$Pb	N/A	0.0 1633.4	stable $8.06\times {10}^{-1}$	0.0	N	($1633.356\to 897.698$), ($2339.921\to 1633.356$), ($2339.921\to 897.698$), ($2623.871\to 1633.356$), ($2623.871\to 2339.921$)
${}^{210}$Bi	17	0.0 271.3	$4.33\times {10}^5$ $9.59\times {10}^{13}$	0.0	B (8.0)	($271.31\to 0.0$), ($319.73\to 46.539$), ($347.95\to 0.0$), ($347.95\to 319.73$), ($439.24\to 433.48$), ($582.54\to 271.31$), ($582.54\to 433.48$)
${}^{212}$Bi	?	0.0 250.0 1910.0	$3.63\times {10}^3$ $1.50\times {10}^3$ $4.20\times {10}^2$	100.0 100.0	N A	($196.0\to 0.0$), ($196.0\to 115.183$), ($213.1\to 115.183$), ($213.1\to 196.0$), ($238.632\to 196.0$), ($250.0\to 196.0$), ($250.7\to 196.0$), ($250.7\to 213.1$), ($338.0\to 250.0$), ($338.0\to 250.7$)

. We follow this information with some brief comments about each isotope. Type B astromers have the associated temperature listed along with the type.

Important note: Because we do not speculate about any uncertainties other than the Weisskopf approximation, the bands here should be considered lower bounds on the effective transition rate uncertainties. Other, as yet unmeasured, nuclear properties could have a dramatic effect on the rates. There may be substantial uncertainty in a critical experimental rate, or key intermediate states may be missing or lack adequate information for a Weisskopf calculation. A striking example of the latter situation is ${}^{126}$Sb, shown below in Section 3.8. The dominant pathways consist almost entirely of measured transitions, so the bands are extremely narrow. However, this isotope only has six measured levels, the highest of which is at 127.9 keV. More levels would open more paths, and the effective transition rates would certainly change.

Our full sensitivity study results are provided in Table A1 of the Appendix A. The table includes the thermalization temperature range, type, and key unmeasured transitions for each potential astromer.

3.1. Zn ($Z=30$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 2.

${}^{69}$Zn: First r-process peak (A∼80) nuclide. In total, 73 measured levels, 30 in this calculation. Isomer at 438.636 keV (type B, 5 keV). Known uncertainties dominated by unmeasured ($531.3\to 0.0$), ($531.3\to 438.636$), ($872.0\to 438.636$), and ($872.0\to 531.3$) transition rates. The isomer greatly delays $\beta$ decay, which may influence late time nucleosynthesis and result in a $\gamma$-ray signal shortly after an r-process event.

${}^{71}$Zn: First r-process peak (A∼80) nuclide. In total, 158 measured levels, 30 in this calculation. Isomer at 157.7 keV (type B, 6 keV). Known uncertainties dominated by unmeasured ($157.7\to 0.0$), ($286.3\to 0.0$), ($286.3\to 157.7$), ($465.0\to 157.7$), ($465.0\to 286.3$), ($489.8\to 0.0$), ($489.8\to 286.3$) transition rates. The isomer somewhat delays $\beta$ decay, which may influence late time nucleosynthesis and result in a $\gamma$-ray signal shortly after an r-process event.

3.2. Se ($Z=34$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 3.

${}^{79}$Se: First r-process peak (A∼80) nuclide. In total, 116 measured levels, 30 in this calculation. Isomer at 95.77 keV (type A). Known uncertainties dominated by unmeasured ($128.0\to 0.0$), ($128.0\to 95.77$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{81}$Se: First r-process peak (A∼80) nuclide. In total, 77 measured levels, 30 in this calculation. Isomer at 103.0 keV (type B, 13 keV). Known uncertainties dominated by unmeasured ($467.74\to 0.0$), ($467.74\to 103.0$), ($491.06\to 0.0$), ($491.06\to 103.0$), ($491.06\to 467.74$), ($624.11\to 103.0$), ($624.11\to 467.74$) transition rates. The isomer significantly delays $\beta$ decay, which may influence late-time r-process nucleosynthesis and heating.

3.3. Kr ($Z=36$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 4.

${}^{83}$Kr: First r-process peak (A∼80) nuclide. In total, 74 measured levels, 30 in this calculation. Isomer at 41.5575 keV (type N). Known uncertainties dominated by unmeasured ($571.1538\to 561.9585$), ($571.1538\to 9.4057$), ($799.48\to 561.9585$), ($799.48\to 571.1538$) transition rates. No expected new effect on the r process due to its short half-life and lack of $\beta$ decay.

${}^{85}$Kr: First r-process peak (A∼80) nuclide. In total, 222 measured levels, 30 in this calculation. Isomer at 304.871 keV (type A). Known uncertainties dominated by unmeasured ($1107.32\to 304.871$), ($1140.73\to 1107.32$), ($1166.69\to 1140.73$), ($1166.69\to 304.871$), ($1223.98\to 1140.73$), ($1223.98\to 1166.69$), ($1416.57\to 1107.32$) transition rates. The isomer greatly accelerates $\beta$ decay, which may result in a $\gamma$-ray signal shortly after an r-process event.

3.4. Nb ($Z=41$) and Tc ($Z=43$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 5.

${}^{93}$Nb: Transition region nuclide. In total, 128 measured levels, 30 in this calculation. Isomer at 30.77 keV (type N). Known uncertainties dominated by unmeasured ($1127.09\to 0.0$), ($1127.09\to 30.77$), ($808.82\to 686.79$), ($810.32\to 743.95$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{95}$Nb: Transition region nuclide. In total, 119 measured levels, 30 in this calculation. Isomer at 235.69 keV (type N). Known uncertainties dominated by unmeasured ($730.0\to 0.0$), ($756.728\to 730.0$), ($799.0\to 235.69$), ($799.0\to 730.0$), ($805.0\to 0.0$), ($805.0\to 730.0$), ($877.0\to 0.0$), ($877.0\to 799.0$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{97}$Nb: Transition region nuclide. In total, 62 measured levels, 30 in this calculation. Isomer at 743.35 keV (type N). Known uncertainties dominated by unmeasured ($1160.0\to 0.0$), ($1160.0\to 1147.96$), ($1251.01\to 0.0$), ($1251.01\to 743.35$), ($1276.09\to 0.0$), ($1276.09\to 1147.96$), ($1276.09\to 1251.01$), ($1433.92\to 1147.96$), ($1433.92\to 1251.01$), ($1433.92\to 1276.09$), ($1548.36\to 0.0$), ($1548.36\to 1147.96$), ($1548.36\to 1276.09$), ($1548.36\to 743.35$), ($1750.43\to 1251.01$), ($2357.0\to 0.0$), ($2357.0\to 743.35$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{99}$Tc: Transition region nuclide. In total, 144 measured levels, 30 in this calculation. Isomer at 142.6836 keV (type A). Known uncertainties dominated by unmeasured ($181.09423\to 142.6836$) transition rate. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

3.5. Cd ($Z=48$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 6.

${}^{113}$Cd: Transition region nuclide. In total, 215 measured levels, 30 in this calculation. Isomer at 263.54 keV (type A). Known uncertainties dominated by unmeasured ($316.206\to 263.54$), ($458.633\to 263.54$), ($458.633\to 316.206$), ($522.259\to 458.633$), ($530.0\to 263.54$), ($530.0\to 316.206$), ($530.0\to 458.633$) transition rates. Isomer greatly accelerates $\beta$ decay, but likely unobservable because the half-life is still quite long (14 y) and the isomer population is relatively low.

${}^{115}$Cd: Transition region nuclide. IN total, 70 measured levels, 30 in this calculation. Isomer at 181.0 keV (type B, 6 keV). Known uncertainties dominated by unmeasured ($181.0\to 0.0$), ($229.1\to 0.0$), ($360.5\to 229.1$), ($389.0\to 181.0$), ($389.0\to 360.5$), ($393.9\to 360.5$), ($393.9\to 389.0$), ($417.2\to 181.0$), ($417.2\to 393.9$) transition rates. Isomer significantly slows $\beta$ decay with possible consequences for r-process heating curves.

3.6. In ($Z=49$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 7.

${}^{115}$In: Transition region nuclide. In total, 92 measured levels, 30 in this calculation. Isomer at 336.244 keV (type A). Known uncertainties dominated by unmeasured ($597.144\to 0.0$) transition rate. Isomer could boost ${}^{115}$Sn production and may generate a $\gamma$-ray signal shortly after an r-process event.

${}^{117}$In: Transition region nuclide. In total, 79 measured levels, 30 in this calculation. Isomer at 315.303 keV (type B, 13 keV). Known uncertainties dominated by unmeasured ($1028.04\to 659.765$), ($1028.04\to 748.07$), ($1028.04\to 880.72$), ($588.653\to 0.0$), ($748.07\to 0.0$), ($880.72\to 0.0$), ($880.72\to 588.653$), ($880.72\to 659.765$), ($880.72\to 748.07$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{119}$In: Second r-process peak (A∼130) nuclide. In total, 74 measured levels, 30 in this calculation. Isomer at 311.37 keV (type B, 17 keV). Known uncertainties dominated by unmeasured ($1044.44\to 654.27$), ($1044.44\to 720.6$), ($1044.44\to 788.26$), ($604.18\to 0.0$), ($720.6\to 0.0$), ($720.6\to 654.27$), ($941.43\to 0.0$), ($941.43\to 604.18$), ($941.43\to 654.27$), ($941.43\to 720.6$) transition rates. The isomer significantly slows $\beta$ decay with possible consequences for r-process heating curves.

${}^{121}$In: Second r-process peak (A∼130) nuclide. In total, 64 measured levels, 30 in this calculation. Isomer at 313.68 keV (type B, 21 keV). Known uncertainties dominated by unmeasured ($1040.33\to 0.0$), ($1040.33\to 637.9$), ($637.9\to 0.0$), ($637.9\to 313.68$) transition rates. The isomer somewhat slows $\beta$ decay, but it is primarily interesting because it feeds the ${}^{121}$Sn isomer.

3.7. Sn ($Z=50$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 8.

${}^{119}$Sn: Second r-process peak (A∼130) nuclide. In total, 157 measured levels, 30 in this calculation. Isomer at 89.531 keV (type N). Known uncertainties dominated by unmeasured ($1062.4\to 787.01$), ($1062.4\to 89.531$), ($1062.4\to 921.39$), ($921.39\to 787.01$) transition rates. The relatively long half-life of ∼300 days may imply an X- or $\gamma$-ray signal from an r-process event.

${}^{121}$Sn: Second r-process peak (A∼130) nuclide. In total, 143 measured levels, 30 in this calculation. Isomer at 6.31 keV (type B, 20 keV). Known uncertainties dominated by unmeasured ($663.63\to 0.0$), ($663.63\to 6.31$), ($869.25\to 0.0$), ($869.25\to 663.63$), ($908.8\to 0.0$), ($908.8\to 663.63$) transition rates. The isomer dramatically slows $\beta$ decay, which contributes to heating and a possible electromagnetic signal on the timescale of years after an r-process event.

${}^{129}$Sn: Second r-process peak (A∼130) nuclide. In total, 34 measured levels, 30 in this calculation. Isomer at 35.15 keV (type B, 29 keV). Known uncertainties dominated by unmeasured ($1043.66\to 35.15$), ($1043.66\to 763.7$), ($1043.66\to 769.07$), ($1047.35\to 0.0$), ($1047.35\to 763.7$), ($1047.35\to 769.07$), ($1054.21\to 763.7$), ($1054.21\to 769.07$), ($35.15\to 0.0$), ($763.7\to 0.0$), ($763.7\to 35.15$), ($769.07\to 0.0$), ($769.07\to 35.15$) transition rates. The isomer somewhat slows $\beta$ decay early in the r process decay back to stability, possibly affecting the heating curve.

3.8. Sb ($Z=51$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 9.

${}^{126}$Sb: Second r-process peak (A∼130) nuclide. In total, 6 measured levels, 6 in this calculation. Isomers at 17.7 keV (type A) and 40.4 keV (type N). The effective transition rates are dominated at all temperatures by experimental state-to-state transition rates. However, the small number of measured states suggests that there are almost certainly many missing intermediate states that could dramatically change the effective rates. Nevertheless, we do not expect new effects on the r process due to the half-lives being much shorter than that of the $\beta$-decay parent.

${}^{128}$Sb: Second r-process peak (A∼130) nuclide. In total, 9 measured levels, 9 in this calculation. Isomer at unknown energy, likely <20 keV (type A). There are no measured transitions to ground and no measured intermediate state half-lives. The isomer is potentially highly influential in the decay back to stability in the r process as it seems to be heavily populated by the $\beta$-decay parent and it has a far shorter half-life than the ground state.

${}^{130}$Sb: Second r-process peak (A∼130) nuclide. 61 measured levels, 30 in this calculation. Isomer at 4.8 keV (type A). Known uncertainties dominated by unmeasured ($4.8\to 0.0$), ($84.67\to 0.0$), ($84.67\to 4.8$) transition rates. The isomer significantly accelerates $\beta$ decay early in the r process decay back to stability, possibly affecting the heating curve.

3.9. Te ($Z=52$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 10.

${}^{125}$Te: Second r-process peak (A∼130) nuclide. In total, 309 measured levels, 30 in this calculation. Isomer at 144.775 keV (type N). Known uncertainties dominated by unmeasured ($321.09\to 35.4925$), ($402.09\to 321.09$), ($402.09\to 35.4925$), ($463.3668\to 402.09$), ($525.228\to 402.09$), ($652.9\to 35.4925$), ($652.9\to 402.09$), ($671.4448\to 525.228$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{127}$Te: Second r-process peak (A∼130) nuclide. In total, 283 measured levels, 30 in this calculation. Isomer at 88.23 keV (type B, 13 keV). Known uncertainties dominated by unmeasured ($340.87\to 0.0$), ($473.26\to 0.0$), ($631.4\to 340.87$), ($631.4\to 473.26$), ($685.09\to 340.87$), ($685.09\to 473.26$), ($685.09\to 631.4$) transition rates. The isomer dramatically slows $\beta$ decay, which could influence the heating curve and possibly produce an X-ray signal weeks or months after an r-process event.

${}^{129}$Te: Second r-process peak (A∼130) nuclide. In total, 407 measured levels, 30 in this calculation. Isomer at 105.51 keV (type B, 10 keV). Known uncertainties dominated by unmeasured ($180.356\to 0.0$), ($360.0\to 0.0$), ($360.0\to 180.356$), ($455.0\to 0.0$), ($455.0\to 105.51$), ($455.0\to 360.0$) transition rates. The isomer dramatically slows $\beta$ decay, which could influence the heating curve and possibly produce an X- or $\gamma$-ray signal weeks or months after an r-process event.

${}^{131}$Te: Second r-process peak (A∼130) nuclide. In total, 319 measured levels, 44 in this calculation. Isomers at 182.258 keV (type B, 21 keV) and 1940.0 keV (type N). Known uncertainties dominated by unmeasured ($1267.5\to 0.0$), ($1267.5\to 802.214$), ($1267.5\to 880.315$), ($642.331\to 0.0$), ($802.214\to 182.258$), ($880.315\to 182.258$), ($880.315\to 642.331$), ($880.315\to 802.214$), ($943.43\to 0.0$), ($943.43\to 642.331$), ($943.43\to 802.214$), ($943.43\to 880.315$) transition rates. The 1940 keV isomer decays to lower energies very quickly and likely has no effect, but the 182.258 keV isomer substantially slows $\beta$ decay, which could influence the heating curve and possibly produce an X- or $\gamma$-ray signal days after an r-process event.

${}^{133}$Te: Second r-process peak (A∼130) nuclide. 37 measured levels, 30 in this calculation. Isomer at 334.26 keV (type B, 29 keV). Known uncertainties dominated by unmeasured ($1096.22\to 0.0$), ($1096.22\to 334.26$), ($1265.326\to 0.0$), ($1500.56\to 0.0$), ($1500.56\to 1096.22$), ($1500.56\to 334.26$), ($1639.5\to 1096.22$), ($1639.5\to 1265.326$), ($1639.5\to 334.26$) transition rates. The isomer somewhat slows $\beta$ decay in the first hours after an r-process event, possibly affecting the heating curve.

3.10. Xe ($Z=54$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 11.

${}^{131}$Xe: Second r-process peak (A∼130) nuclide. In total, 58 measured levels, 30 in this calculation. Isomer at 163.93 keV (type N). Known uncertainties dominated by unmeasured ($341.144\to 0.0$), ($636.99\to 163.93$), ($666.934\to 636.99$), ($722.909\to 666.934$), ($971.22\to 163.93$), ($971.22\to 341.144$), ($971.22\to 666.934$), ($973.11\to 341.144$), ($973.11\to 666.934$) transition rates. The isomer half-life of ∼12 days is a bit longer than that of its $\beta$-decay parent, and its de-excitation may produce an X-ray signal.

${}^{133}$Xe: Second r-process peak (A∼130) nuclide. In total, 29 measured levels, 29 in this calculation. Isomer at 233.221 keV (type N). Known uncertainties dominated by unmeasured ($529.872\to 0.0$), ($529.872\to 233.221$), ($607.87\to 0.0$), ($607.87\to 233.221$), ($743.752\to 233.221$), ($875.328\to 0.0$), ($875.328\to 529.872$), ($875.328\to 607.87$), ($875.328\to 743.752$) transition rates. The isomer de-excitation may produce an X-ray signal a few days after an r-process event.

3.11. Ba ($Z=56$), Pr ($Z=59$), and Ho ($Z=67$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 12.

${}^{137}$Ba: Second r-process peak (A∼130) nuclide. In total, 96 measured levels, 30 in this calculation. Isomer at 661.659 keV (type N). Known uncertainties dominated by unmeasured ($1251.82\to 661.659$), ($1293.9\to 0.0$), ($1293.9\to 1251.82$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{144}$Pr: Rare earth nuclide. In total, 5 measured levels, 5 in this calculation. Isomer at 59.03 keV (type N). Known uncertainties dominated by unmeasured ($80.12\to 59.03$), ($99.952\to 80.12$) transition rates. However, the small number of measured states suggests that there are almost certainly many missing intermediate states that could dramatically change the effective rates. Nevertheless, we do not expect new effects on the r process due to the half-lives being much shorter than that of the $\beta$-decay parent.

${}^{166}$Ho: Rare earth nuclide. In total, 356 measured levels, 30 in this calculation. Isomers at 5.969 keV (type B, 6 keV) and 190.9021 keV (type N). Known uncertainties dominated by unmeasured ($171.0738\to 54.2391$), ($180.467\to 171.0738$), ($180.467\to 5.969$), ($180.467\to 54.2391$), ($260.6625\to 180.467$), ($263.7876\to 180.467$), ($296.8\to 0.0$), ($296.8\to 263.7876$), ($296.8\to 5.969$), ($296.8\to 54.2391$), ($296.8\to 82.4707$), ($54.2391\to 5.969$) transition rates. The 191 keV isomer decays to lower energies very quickly and likely has no effect, but the 6 keV isomer dramatically slows $\beta$ decay, which could influence the heating curve. It also has strong $\gamma$ and X-ray lines, and the 1200 yr half-life make it a compelling candidate for observing old r-process remnants.

3.12. Os ($Z=76$), Ir ($Z=77$), and Pt ($Z=78$) Isotopes

Results for the isotopes in the following discussion are shown in Figure 13.

${}^{189}$Os: Third r-process peak (A∼195) nuclide. IN total, 96 measured levels, 30 in this calculation. Isomer at 30.82 keV (type N). Known uncertainties dominated by unmeasured ($350.0\to 216.67$), ($350.0\to 219.39$), ($350.0\to 97.35$), ($365.78\to 30.82$), ($365.78\to 69.54$), ($427.93\to 69.54$), ($427.93\to 95.27$), ($438.73\to 0.0$), ($438.73\to 69.54$), ($444.23\to 216.67$), ($444.23\to 219.39$), ($444.23\to 233.58$), ($444.23\to 30.82$), ($444.23\to 69.54$), ($69.54\to 30.82$), ($97.35\to 30.82$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{191}$Ir: Third r-process peak (A∼195) nuclide. In total, 74 measured levels, 30 in this calculation. Isomer at 171.29 keV (type N). Known uncertainties dominated by unmeasured ($343.23\to 171.29$), ($390.94\to 129.413$), ($390.94\to 343.23$), ($502.61\to 171.29$), ($502.61\to 390.94$) transition rates. No expected new effect on the r process due to its half-life being much shorter than that of its $\beta$-decay parent.

${}^{195}$Ir: Third r-process peak (A∼195) nuclide. In total, 44 measured levels, 30 in this calculation. Isomer at 100.0 keV (type N). Known uncertainties dominated by unmeasured ($100.0\to 0.0$), ($175.221\to 0.0$), ($175.221\to 100.0$), ($394.0\to 100.0$), ($394.0\to 175.221$) transition rates. The isomer somewhat slows $\beta$ decay and could affect the heating curve, but it is primarily interesting because it feeds the ${}^{195}$Pt isomer.

${}^{195}$Pt: Third r-process peak (A∼195) nuclide. In total, 92 measured levels, 30 in this calculation. Isomer at 259.077 keV (type N). Known uncertainties dominated by unmeasured ($199.532\to 129.772$), ($211.406\to 129.772$), ($211.406\to 98.88$), ($222.23\to 0.0$), ($222.23\to 98.88$), ($239.264\to 129.772$), ($431.98\to 259.077$), ($449.65\to 129.772$), ($449.65\to 239.264$), ($449.65\to 431.98$), ($507.917\to 199.532$), ($507.917\to 239.264$), ($507.917\to 431.98$), ($547.16\to 259.077$), ($547.16\to 431.98$), ($562.8\to 431.98$), ($667.0\to 431.98$), ($667.0\to 547.16$) transition rates. Due to the high abundance of this isotope, its isomer could a strong X-ray source in the early days after an r-process event.

4. Discussion and Conclusions

4.1. Comments on Selected Isomers and Mass Regions

Many isomers are interesting not only for their qualities as astromers, but also for terrestrial applications and the insights they can give into nuclear structure. We comment here on some selected isotopes covered in Section 3; we also briefly discuss the rare-earth region, which currently suffers from a dearth of experimental data.

${}^{93}$Nb: The spin-parity of the 1/2${}^{-}$ isomer at 30.77 keV differs very much from the 9/2${}^{+}$ ground state, and, therefore, this should be a good isomer terrestrially. A recent experiment at the National Superconducting Cyclotron Laboratory (NSCL) using a ${}^{93}$Nb(t, ${}^3$He) charge-exchange reaction has successfully established electron-capture rates of the ${}^{93}$Nb ground state [64]. However, capture rates of the 1/2${}^{-}$ isomer are completely unknown and must be calculated from theory [65].

${}^{99}$Tc: The excited state ${}^{99m}$Tc, produced from ${}^{99}$Mo, is an isomer used in nuclear medicine [66]. It decays with a half-life of about 6 h by emitting a 142 keV $\gamma$ ray, which is close to the energy of medical diagnostic X-rays.

Near ${}^{132}$Sn: Around the double-magic nucleus ${}^{132}$Sn (Z = 50, N = 82), isotopes discussed in the present paper with Z < 50 (In, Cd, Ag, Pd) and Z > 50 (Sb, Te, I, Cs) (Elements mentioned here which do not appear in Section 3 have isomers listed in the Appendix A) have been a focus for exploration in nuclear structure physics. Generally, the structure of near-double-magic nuclei is recognized in their level spectra, which consist of two types of excitations: excitations of valence single particles and excited states formed by couplings of the valence nucleons to core excitations. Isomeric states can be found in both types of states. However, lack of some basic experimental information has hindered understanding of both types of excitation. The experimental single particle states are at present incomplete for this neutron-rich mass region (in particular, there is no information at all to the south-east of ${}^{132}$Sn on the chart of nuclides); these are required inputs for reliable shell model calculations [67]. Moreover, there is only limited experimental information on the sizes of the shell gaps, which are also important ingredients for understanding r-process nucleosynthesis [68]; the lack of knowledge on shell gaps has hindered shell-model studies on core-excited states. Recently, progress has been made on large-scale shell model calculations, and a new type of shell model has appeared that unifies the discussion of the two aspects in a shell-model diagonalization calculation [69,70]; these theoretical advances make experimental results all the more needed.

Rare-earth nuclei: The structure of many neutron-rich rare-earth nuclei is relevant to the formation of the A∼160 abundance peak in r-process nucleosynthesis [71,72,73,74,75,76]. For most of the involved nuclei, experimental information is currently very limited, and understanding of the structure must rely on theories [77,78]. However, theoretical calculations for these exotic nuclei extrapolate existing models that have only been demonstrated to work well for near-stable regions. A recent work [79] found a serious problem in that for the rare-earth neutron-rich nuclei (Nd, Pm, Sm, Eu, and Gd), the well-established Woods–Saxon potential, the Nilsson modified oscillator potential with “universal” parameters, and the folded Yukawa potential all failed to describe the neutron single-particle states. A good understanding of the single-particle states is essential for the theoretical study of isomers, and these new results demand a careful reconsideration of mean-field models. In a first attempt [80], the traditional Nilsson model was extended in order to describe the deformed rare-earth nuclei in the very neutron-rich region.

4.2. Additional Modeling and Data Requirements

To reiterate, our study includes only $\beta$ decays and thermally mediated internal transitions, but other reaction and decay channels can populate and destroy isomers. We have also stressed the need for more nuclear data. Figure 14 emphasizes both of these points: further work is required to incorporate more channels, and (especially in the rare-earth region) we require many more isomer measurements.

The figure shows the decay flow (integrated over time) of an initial population of ${}^{170}$Ce that is allowed to undergo both $\beta$ decay and $\beta$-delayed neutron emission; species colored green have known isomers that we included in our network. As the decay chains progress, the abundances fan out like a river delta, feeding many isotopes from a single ancestor. The sparsity of known isomers in this delta is almost certainly due to insufficient data rather than an actual lack of isomers. Consequently, many of the isotopes fed in this decay chain likely have isomers that contribute to the chain’s dispersion, and we simply cannot adequately account for them until new measurements reveal their presence. Additional reaction channels not considered here, such as radiative capture and fission, may also contribute to isomer population and destruction during the later stages of the r process.

4.3. Experimental Prospects

Some experimental facilities for direct measurement of the nuclear properties needed to refine astromer predictions already exist, and the next decade will see a great expansion coming online. The basic properties needed are (1) level energies (below Q${}_{\beta }$ for most environments), (2) level spins and parities, (3) $\gamma$-ray transition strengths, particularly between ground and isomer bands, and (4) total $\beta$-decay branching ratios to the ground state and isomeric state.

Many of these isotopes are near stability and are already within reach of facilities, such as ISAC at TRIUMF, ISOLDE at CERN, and ATLAS at Argonne. With FRIB coming online, even more isotopes can be studied. In addition to beam availability, spectroscopic detector systems are also needed and are available or under construction. GAMMASPHERE has performed these types of studies for decades. AGATA in Europe and GRETA/GRETINA are designed to perform the necessary spectroscopy while taking full advantage of next-generation facilities. The N = 126 Factory under construction at Argonne will make available beams of isotopes in the Ir/Pt region that have long been difficult to obtain.

To give a concrete example of how these opportunities are becoming available, consider the case of ${}^{128}$Sb, as discussed in Section 3.8. The unmeasured isomer energy introduces significant uncertainties both in the transition rates between ground and isomeric states and in the thermal equilibrium populations. The estimated isomer energy of <20 keV precludes direct measurement of the $\gamma$-ray from the internal transition. However, recent advances in the phase-imaging ion cyclotron resonance (PI-ICR) technique have made a direct mass measurement of the ground and isomeric states sensitive enough to determine the isomer energy with sufficient precision [81]. The ISOLDE facility at CERN produces prolific beams of nearby Sb isotopes (>${10}^7$ for ${}^{114,131}$Sb, indicating that intensities would be adequate for a PI-ICR mass measurement of ${}^{128g,m}$Sb [82]. These types of advances in techniques and beams similarly open the possibility of many more measurements.

Finally, it is worth noting that some of the necessary data will likely be taken “for free” as part of a larger campaign that might be focused on another isotope; $\beta$-decay branching ratios are a particularly prominent example. As campaigns are developed for the FRIB decay station (FDS), for example, decays far off-stability could well decay back to stability through isotopes needed for isomer studies; simply by recognizing this additional interest, the planned experiment can have greater impact with no additional beamtime needed. This alone can improve $\beta$-decay branching ratio data for both Type A and Type B astromers.

4.4. Observational Prospects

The isomer properties can alter the expected emission from astrophysical sources for a broad set of observations. These properties may contribute to an explanation of some of the inconsistencies in our understanding of the emission from the neutron star merger event GW170817 [83]. For example, optical emission a few days after the kilonova outburst is brighter than expected from a standard grid of neutron star merger calculations (Ristic et al., in preparation). From

Table 1. Neutron-rich astromers most likely to have observable effects in the r process. We use g and m to indicate the ground state and isomer, respectively. The “${\mathrm{E}}_m$” column lists the isomer energy (keV), and the half-lives (“${\mathrm{T}}_{1/2}$”) of the ground state and isomer are given in their respective columns (s). The low-temperature $\beta$-decay branching percentage for the isomer is in the “${\mathrm{B}}_{\beta }^m$” column. The half-lives and branching percentages are as measured terrestrially. “${\mathrm{T}}_{pop}$” is the approximate timescale on which parent nuclei decay to populate the isotope. Finally, “Dominant Astromer Effects” details our interpretation of the most-likely observable consequences of the isomer as an astromer. T${}_{pop}$ and all timescales in the last column are estimated from half-lives and, therefore, should be interpreted as lower bounds on the relevant timescale.

Isotope	E${}_{\mathit{m}}$ (keV)	T${}_{1/2}^{\mathit{g}}$ (s)	T${}_{1/2}^{\mathit{m}}$ (s)	B${}_{\mathit{\beta }}^{\mathit{m}}$ (%)	T${}_{\mathit{p}\mathit{o}\mathit{p}}$	Dominant Astromer Effects
${}^{69}$Zn	438.636	$3.38\times {10}^3$	$4.95\times {10}^4$	0.033	3 min	Heating slowed from 1 h to 14 h 439 keV $\gamma$ ray at ∼14 h
${}^{71}$Zn	157.7	$1.47\times {10}^2$	$1.43\times {10}^4$	100	20 s	Heating slowed from 2 min to 4 h 386 keV $\gamma$ ray at ∼4 h
${}^{81}$Se	103.00	$1.11\times {10}^3$	$3.44\times {10}^3$	0.051	30 s	Heating slowed from 20 min to 1 h
${}^{83}$Kr	41.5575	stable	$6.59\times {10}^3$	0	2.5 h	9.4 keV $\gamma$ ray, 13 keV X-ray at ∼2 h Faint, but may be visible early
${}^{85}$Kr	304.871	$3.39\times {10}^8$	$1.61\times {10}^4$	78.8	3 min	Heating accelerated from 11 yr to 5 h 151 keV $\gamma$ ray at 5 h
${}^{113}$Cd	263.54	$2.54\times {10}^{23}$	$4.45\times {10}^8$	99.86	6 h	Weak 264 keV $\gamma$ ray at 14 yr Accelerates production of ${}^{113}$In
${}^{115}$Cd	181.0	$1.92\times {10}^5$	$3.85\times {10}^6$	100	20 min	Heating slowed from 54 h to 45 d Weak 934 $\gamma$ ray at 45 d
${}^{117}$Cd	136.4	$8.96\times {10}^3$	$1.21\times {10}^4$	100	70 s	Heating slowed from 2.5 h to 3.4 h 1997 keV $\gamma$ ray possibly observable early
${}^{115}$In	336.244	$1.39\times {10}^{22}$	$1.61\times {10}^4$	5.0	54 h	336 keV $\gamma$ ray at 4.5 h Accelerates production of ${}^{115}$Sn
${}^{119}$In	311.37	$1.44\times {10}^2$	$1.08\times {10}^3$	95.6	3 min	Heating slowed from 2.5 min to 18 min
${}^{119}$Sn	89.531	stable	$2.53\times {10}^7$	0	3–18 min	24 keV $\gamma$ ray, 25 keV X-ray at 293 d
${}^{121}$Sn	6.31	$9.73\times {10}^4$	$1.39\times {10}^9$	22.4	4 min	Decay/heating slowed from 27 h to 44 yr 26 keV X-ray, faint 3–4.5 keV X-ray
${}^{129}$Sn	35.15	$1.34\times {10}^2$	$4.14\times {10}^2$	100	1 s	Heating slowed from 2.2 to 7 min
${}^{128}$Sb	0.0 + X	$3.26\times {10}^4$	$6.25\times {10}^2$	96.4	1 h	Heating accelerated from 9 h to 10 min
${}^{130}$Sb	4.8	$2.37\times {10}^3$	$3.78\times {10}^2$	100	4 min	Heating accelerated from 40 min to 6.3 min
${}^{127}$Te	88.23	$3.37\times {10}^4$	$9.17\times {10}^6$	2.4	4 d	Heating/decay slowed from 9.4 h to 106 d 27 keV X-ray at 106 d
${}^{129}$Te	105.51	$4.18\times {10}^3$	$2.9\times {10}^6$	36	4.5 h	Heating/decay slowed from 70 min to 34 d 27 keV X-ray, faint 696 keV $\gamma$ ray at 34 d
${}^{131}$Te	182.258	$1.5\times {10}^3$	$1.2\times {10}^5$	74.1	23 min	Heating slowed from 25 min to 33 h 774 keV $\gamma$ ray, 29 keV X-ray at 33 h
${}^{133}$Te	334.26	$7.5\times {10}^2$	$3.32\times {10}^3$	83.5	2.5 min	Heating slowed from 12.5 min to 1 h
${}^{131}$Xe	163.930	stable	$1.02\times {10}^6$	0	8 d	30 keV X-ray at 12 d
${}^{133}$Xe	233.221	$4.53\times {10}^5$	$1.9\times {10}^5$	0	21 h	30 keV X-ray at 2 d
${}^{166}$Ho	5.969	$9.66\times {10}^4$	$3.79\times {10}^{10}$	100	82 h	Decay/heating slowed from 27 h to 1200 y 184, 280, 712, 810 keV $\gamma$ rays, 49 keV X-ray
${}^{195}$Ir	100	$8.24\times {10}^3$	$1.32\times {10}^4$	95	7 min	Feeds ${}^{195}$Pt isomer
${}^{195}$Pt	259.077	stable	$3.46\times {10}^5$	0	4 h	99 keV $\gamma$ ray, 8–14, ∼65, ∼75 keV X-ray at 4 d

, we note there are a few isomers whose half-life is either increased or decreased from the ground-state decay to a few to tens of hours: isomers of ${}^{69}$Zn, ${}^{71}$Zn, ${}^{85}$Kr, ${}^{115}$In, ${}^{131}$Te, ${}^{133}$Xe, and ${}^{195}$Pt. If these isomers are produced in sufficient abundance, they could increase the heating at these later times and, in the slow-moving ejecta, contribute enough heating to increase the optical emission at the few day timescale. Another key timescale in kilonova observations lies in understanding the observational features of kilonova remnants. Astromers with long-lived timescales (e.g., the 14 y half-life of the ${}^{113}$Cd isomer) could be observed in kilonova remnants in the Milky Way. For such observations, the most promising are isomers whose half-lives allow contributions to old remnants (ages in the 1000 to 100,000 y range) and with decay lines appropriate for X-ray missions (which are more sensitive than gamma-ray missions). ${}^{166}$Ho fits both these criteria with a decay half-life of 1200 y and decay lines in the gamma-rays and a 49 keV X-ray (Table 1). A much more thorough study of these isomers is essential to determine the role of isomers in neutron star merger observations.

4.5. Summary

We studied the sensitivity of effective thermal transition rates between nuclear isomers and ground states to unmeasured internal transitions. The most straightforward estimate of these unmeasured transitions is the Weisskopf approximation, which tends to be accurate within a factor of 100 relative to measured values. Therefore, we varied all Weisskopf rates in our calculations up and down by factors of 10 and 100 to assess the likely range of effective transition rates. We estimated the effect on thermalization temperatures and identified the likely most influential individual transitions. We categorized isomers as accelerants, batteries, or neutral according to the effects they could be expected to have in the r-process decay back to stability.

We found that unmeasured transitions can have a very large effect on the effective rates and thermalization temperatures. In isotopes where the effective rates are bottle-necked by the unmeasured rates, we see a strong sensitivity to our variations. Conversely, when effective transitions flow primarily through paths with measured individual transitions, we see much less sensitivity. Which type of transition (measured or unmeasured) limits the effective rates can vary sensitively with temperature, manifested by the variation with temperature in the widths of our uncertainty bands. Many nuclei in Section 3 exhibit this behavior, with measured rates dominating at low temperatures and giving way to unmeasured rates as temperature increases. The second isomer in ${}^{131}$Te exhibits the reverse effect: its de-excitation is controlled by unmeasured rates at low temperatures, but paths through measured transitions become accessible at higher temperatures.

Whether the measured or unmeasured individual rates throttle the effective rates can depend on whether the unmeasured rates are increased or decreased. At the beginning of the upturn of ${\Lambda }_{3,1}$ in ${}^{137}$Ba, the width of the uncertainty band arises almost entirely from turning the Weisskopf rates up. ${}^{119}$In shows a reverse effect, where the width at $T=45$ keV is due almost entirely to reductions in the Weisskopf rates. ${}^{189}$Os exhibits both behaviors: At low temperatures the width comes from turning the Weisskopf rates up, but at $T=30$ keV, the reverse is true.

The widths of the uncertainty bands can imply substantial variation in thermalization temperatures. In ${}^{121}$In, for example, the range of likely thermalization temperatures is about 12 keV wide. A few of the nuclei we studied are so inadequately measured that we cannot even calculate a thermalization temperature, including the likely influential ${}^{128}$Sb and ${}^{131}$Te (although in the latter case, we can compute a $T_{\mathrm{therm}}^{}$ between just the GS and the first isomer).

The results of this work illuminate the limitations of existing nuclear structure and transition data with respect to precisely understanding isomeric transitions in the r process, but these are not the only nuclear uncertainties in play. Another important quantity affected by these uncertainties is astromer $\beta$ feeding, that is, how much of a $\beta$-decay parent decays to the astromer versus the ground state. In addition to missing direct feeding data (information about which daughter states are directly populated in decay), the unmeasured transitions can affect the subsequent (thermally mediated) $\gamma$ cascades toward long-lived states. This, along with other reactions and decays, will be the focus of a future study. We also plan to combine the nuclear physics unknowns with astrophysical r-process uncertainties. These efforts will continue to shed light on the role of nuclear isomers in astrophysical environments and will motivate experiments to determine the key missing nuclear data quantities.