The slow-roll trajectory is given by the integral

$$N_{\text{end}} - N = \int_{x_{\text{end}}}^{x} \frac{y + \alpha y \ln(y) + \beta y \ln^2(y)}{p + \alpha + (p\alpha + 2\beta) \ln(y) + p\beta \ln^2(y)} dy. \qquad (7.193)$$

It can be determined analytically after expanding the denominator, which is proportional to $V'(y)$, over its roots. Defining the, possibly complex, numbers

$$z_{\pm} \equiv \frac{-(p\alpha + 2\beta) \pm \sqrt{\Delta}}{2p\beta}, \qquad (7.194)$$

one has for $\Delta \neq 0$

$$N_{\text{end}} - N = \frac{1}{\sqrt{\Delta}} \int_{x_{\text{end}}}^{x} \frac{y + \alpha y \ln(y) + \beta y \ln^2(y)}{\ln(y) - z_{+}} dy - \frac{1}{\sqrt{\Delta}} \int_{x_{\text{end}}}^{x} \frac{y + \alpha y \ln(y) + \beta y \ln^2(y)}{\ln(y) - z_{-}} dy. \qquad (7.195)$$

Let us notice that, for $\Delta > 0$, one has $x_{V'=0}^{\pm} = \exp(z_{\pm})$. All the terms obtained by expanding the numerators of Eq. (7.195) can be expressed as exponential integrals, and, after some algebra, one gets

$$N_{\text{end}} - N = \frac{x^2 - x_{\text{end}}^2}{2p} + \frac{e^{2z_+} (1 + \alpha z_+ + \beta z_+^2)}{\sqrt{\Delta}} \{ \text{Ei} [2 \ln(x) - 2z_+] - \text{Ei} [2 \ln(x_{\text{end}}) - 2z_+] \} \\ - \frac{e^{2z_-} (1 + \alpha z_- + \beta z_-^2)}{\sqrt{\Delta}} \{ \text{Ei} [2 \ln(x) - 2z_-] - \text{Ei} [2 \ln(x_{\text{end}}) - 2z_-] \}. \qquad (7.196)$$

Let us notice that, for RCIPI1, when $x \to x_{V'=0}^{-}$ the argument of the exponential integral becomes very small, and negative. In this limit, one has $Ei(x) \to \gamma + \ln(-x)$ and the logarithmic divergence implies that an arbitrarily large number of e-folds can be realized at the top of the local maximum. However, the argument of the exponential integral being a logarithm of the field value, it is very slowly divergent, not faster than $\Delta N \propto -\ln[-2 \ln(x/x_{V'=0}^{-})]$. In other words, to obtain 60 e-folds of inflation at the top of the local maximum, one should fine tune the initial field values as $x/x_{V'=0}^{-} < \exp[-e^{-60}] \approx 1 - e^{-60}$.

The case of a flat inflection point for $\alpha = \pm \alpha_0$ implies that $\Delta = 0$ and requires special treatment. Denoting

$$z_0 \equiv \ln(x_0) = -\frac{p\alpha + 2\beta}{2p\beta}, \qquad (7.197)$$

one can replace the denominator of Eq. (7.193) by

$$p + \alpha + (p\alpha + 2\beta) \ln(y) + p\beta \ln^2(y) = p\beta [\ln(y) - z_0]^2. \qquad (7.198)$$

After expressing all terms of Eq. (7.193) as exponential integrals, one gets for $\Delta = 0$

$$N_{\text{end}} - N = e^{2z_0} [2 + \alpha + 2(\alpha + \beta)z_0 + 2\beta z_0^2] \{ \text{Ei} [2 \ln(x) - 2z_0] - \text{Ei} [2 \ln(x_{\text{end}}) - 2z_0] \} \\ + \frac{x^2 [2 + (2\alpha + \beta)z_0 + 2\beta z_0^2 - \beta \ln(x)]}{2z_0 - 2 \ln(x)} \\ - \frac{x_{\text{end}}^2 [2 + (2\alpha + \beta)z_0 + 2\beta z_0^2 - \beta \ln(x_{\text{end}})]}{2z_0 - 2 \ln(x_{\text{end}})} . \qquad (7.199)$$

This time, for RCIPI1 and $x \to x_{V'=0}^{-}$, we see that $\Delta N$ is divergent as $1/\ln(x_0/x)$ and getting enough e-folds of inflation close to the inflection point requires only $x/x_0 < e^{-1/\Delta N} \approx 1 - 1/\Delta N$.

From the numerical solution $x_{\text{end}}$, the analytical trajectories of Eqs. (7.196) and (7.199), and the reheating equation (3.48), one can determine $x_*$, the field value at which the pivot mode crosses the Hubble radius during inflation. It fixes the normalization of the potential $M^4$ from the amplitude of the CMB anisotropies and one has

$$\left(\frac{M}{M_{\text{Pl}}}\right)^4 = 720\pi^2 \frac{[p + \alpha + (p\alpha + 2\beta)\ln(x_*) + p\beta\ln^2(x_*)]^2}{x_*^{p+2} [1 + \alpha \ln(x_*) + \beta \ln^2(x_*)]^3} \frac{Q_{\text{rms-PS}}^2}{T^2}. \qquad (7.200)$$

The reheating-consistent slow-roll predictions for RCIPI1 are represented in Fig. 488 to 502 and for RCIPI2 in Fig. 503 to 513. As already noticed, successful inflation near the detuned inflection point requires quite some fine-tuning and the presence of a tachyonic mass induces a strong sensitivity of the observables with respect to the model parameters. For both RCIPI1 and RCIPI2, small values of $\beta$ allow for just enough inflation to make observable the “distorted parts of the potential. Due to the potentially large values of $\epsilon_2$ and $\epsilon_3$, the model predictions explore a large part of the space $(n_s, r)$ even for small changes in the parameter $\alpha$ and $\beta$.

## 8. Conclusions

Let us very briefly recap our main findings and present some directions for future works.

In this article, we have discussed the question of how the inflationary theory can be constrained given that we now have at our disposal high-accuracy cosmological data. We have argued that this can be done by means of the slow-roll power spectrum which has the advantage of being relatively model independent. Concretely, it leads to the Hubble flow posterior distributions $P(\epsilon_n | C_{\epsilon}^{\text{meas}})$. This is interesting since it gives a general constraint on the derivatives of the inflaton potential. But, at the same time, this does not answer some legitimate fundamental questions one might have about the plethora of inflationary scenarios studied so far. For instance, it does not tell us rigorously which constraints exist on the parameters of a given model. Indeed, suppose that we are interested in LFI, $V(\phi) \propto \phi^p$. It is obvious that we would like to know which values of $p$ are favored by the data for this class of models.
<figure><img src="image_126.png" /><figcaption>Fig. 123. Upper panel: various ASPIC scenarios in the $(n_s, r)$ plane using the Schwarz–Terrero–Escalante classification [710] and compared to the Planck 2018 + Bicep-Keck data (yellow contours) and the Planck 2013 data [95,99,100,185,186,209] (light gray shading). Bottom panel: same plot in logarithmic scale for another sample of models.</figcaption></figure>

<figure><img src="image_127.png" /><figcaption>Fig. 124. Observable predictions in the $(n_s, r)$ plane for various models belonging to region 1 of the Schwarz–Terrero–Escalante classification (see Fig. 123). Despite the fact that they are in the same broad class, the accuracy of the CMB data allows us to discriminate among them thereby justifying a detailed navigation within the inflationary landscape.</figcaption></figure>
In order to complement the slow-roll approximated power spectra and to address the above mentioned issues, we have argued that it is interesting to scan the inflationary landscape model by model and have provided the public code ASPIC to do so. Such a strategy has to be done for all the inflationary scenarios since it would be arbitrary to consider only a restricted class while ignoring the others. In fact, this question deserves to be discussed in more detail. One could indeed imagine that it is not necessary to consider all the models one by one and that considering a representative for each class is sufficient. Indeed, before this work, it was common to distinguish three broad types of scenarios: large field models (LFI), small field models (SFI) and Hybrid models (VHI). Such a classification is not very precise and biased because it pushes to the front line these three models. It could be reasonably argued that a better classification is the one of Schwarz and Terrero-Escalante introduced in Ref. [710]. For a scalar field, the ratio of the kinetic energy to the total energy density is given by $\epsilon_1/3 = \dot{\phi}^2/(2\rho)$. Because $\epsilon_2$ is, by definition, the logarithmic derivative of $\epsilon_1$ with respect to the e-fold number, the kinetic contribution to the total energy density increases if $\epsilon_2 > 0$ and decreases if $\epsilon_2 < 0$. On the other hand, we also have

$$ \frac{d(\phi^2/2)}{dt} = H \frac{\dot{\phi}^2}{2} (\epsilon_2 - 2\epsilon_1), \qquad (8.1) $$

and, therefore, the absolute value of the kinetic energy increases if $\epsilon_2 > 2\epsilon_1$ whereas it decreases if $\epsilon_2 < 2\epsilon_1$. This allows us to identify three different regions: $\epsilon_2 > 0$ and $2\epsilon_1 < \epsilon_2 < \epsilon_1$ (region 1), $\epsilon_2 < 2\epsilon_1$ (region 2), $\epsilon_2 < 0 < 2\epsilon_1$ (region 3).

These three regions are identified in Fig. 123, together with the Planck 2013 and the Planck 2018 + Bicep-Keck bounds.<fnref n="14" /> If we use the first-order slow-roll expressions, the condition $\epsilon_2 > 0$ is equivalent to $r < 8(1 - n_s)$ while $\epsilon_2 > 2\epsilon_1$ amounts to $r < 4(1 - n_s)$. These two lines are also represented in Fig. 123 (solid black lines). These three regions encompass the large field, small field and hybrid cases previously mentioned. However, the correspondence is not perfect and we notice, for instance, that LFI for $p = 1$ belongs to region 1 whereas for $p > 2$ it belongs to region 2.

Having identified three broad classes of scenarios, the next question is whether testing only a representative model for each class could be sufficient. For instance, the confidence regions of Fig. 123 show that, over a decade of CMB measurements, the cosmological data have essentially excluded region 2 and region 3 and one may be tempted to summarize region 1 to one of its prototypical representative: Starobinsky Inflation (SI). In Fig. 124, we have considered the predictions of seven other different models that all belong to region 1. This plot clearly shows that these models make predictions spanning different domains that are separated enough to be distinguishable within current or future data. Given the quality of the current data, working only with broad classes of models seems to be no longer justified. Therefore, if one really wants to scan the inflationary landscape, the approach advocated in this paper is well-suited.

With ASPIC, we have provided a new tool to treat any model of inflation and this has led us to derive observational predictions for 118 models. ASPIC is an evolutive project and therefore the next steps will be to complete and upgrade it with new models. Finally, the ultimate goal is to identify which ASPIC models are performing the best at explaining cosmological data. In order to carry out this task, an appropriate method is to use Bayesian evidence and model comparison. Then, we should be able to identify, in a statistically well-defined manner, and for any data sets, what might be called “the best model of inflation” [711–715].

### CRediT authorship contribution statement

**Jérôme Martin:** Writing – review & editing, Writing – original draft, Visualization, Validation, Resources, Methodology, Investigation, Formal analysis, Conceptualization. **Christophe Ringeval:** Writing – review & editing, Writing – original draft, Visualization, Validation, Software, Resources, Methodology, Investigation, Funding acquisition, Formal analysis, Data curation, Conceptualization. **Vincent Vennin:** Writing – review & editing, Writing – original draft, Visualization, Validation, Software, Resources, Methodology, Investigation, Formal analysis, Data curation, Conceptualization.

### Declaration of competing interest

The authors declare that they have no known competing financial interests or personal relationships that could have appeared to influence the work reported in this paper.

### Data availability

Source files are GPLv3 and available in the repositories described in the manuscript.

### Acknowledgments

We would like to thank the ten referees who have accepted to review this work over the past decade. Their insightful comments and careful checking of some calculations have been much appreciated. This work is partially supported by the ESA Belgian Federal PRODEX Grant No. 4000103071 and the Wallonia-Brussels Federation grant ARC No. 11/15-049. The “Opiparous Edition” has benefited from support by the ESA Belgian Federal PRODEX Grant No. 4000143201, the “Fonds de la Recherche Scientifique - FNRS” under Grant N°T.0198.19 as well as by the Wallonia-Brussels Federation Grant ARC N°19/24-103. We would like to thank EvaluatorIAP for his everyday and decade-long encouragements.

<footnote n="14">¹⁴ The slight shift visible on the one- and two-sigma contours between the two plots come from the different priors used, either flat on $\epsilon_1$ or flat on $\log \epsilon_1$ (Jeffreys’ prior).</footnote>
# Appendix. Reheating consistent slow-roll predictions

## A.1. Starobinsky and Higgs Inflation (SI /HI)

See Fig. 125.

<figure><img src="image_128.png" /><figcaption>**Fig. 125.** Reheating consistent slow-roll predictions for the Starobinsky and the Higgs model in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
## A.2. Radiatively Corrected Higgs Inflation (RCHI)

See Fig. 126.

<figure><img src="image_129.png" /><figcaption>**Fig. 126.** Reheating consistent slow-roll predictions for the radiatively corrected Higgs model in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
### A.3. Large Field Inflation (LFI)

See Fig. 127.

<figure><img src="image_130.png" /><figcaption>**Fig. 127.** Reheating consistent slow-roll predictions for the large field models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.4. Mixed Large Field Inflation (MLFI)

See Fig. 128.

<figure><img src="image_131.png" /><figcaption>**Fig. 128.** Reheating consistent slow-roll predictions for the mixed large field models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Predictions are within the one of the quadratic LFI ($p = 2$) and quartic LFI ($p = 4$) models.</figcaption></figure>
A.5. Radiatively Corrected Massive Inflation (RCMI)

See Fig. 129.

<figure><img src="image_132.png" /><figcaption>**Fig. 129.** Reheating consistent slow-roll predictions for the radiatively corrected massive models in the plane $(n_s, r)$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\alpha \to 0$, the predictions match the ones of the LFI quadratic model ($p = 2$).</figcaption></figure>
A.6. Radiatively Corrected Quartic Inflation (RCQI)

See Figs. 130 and 131.

<figure><img src="image_133.png" /><figcaption>**Fig. 130.** Reheating consistent slow-roll predictions for the radiatively corrected quartic models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with $\bar{w}_{\text{reh}} = 0$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_134.png" /><figcaption>**Fig. 131.** Reheating consistent slow-roll predictions for the radiatively corrected quartic models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with $\bar{w}_{\text{reh}} = \frac{1}{3}$. This value of $\bar{w}_{\text{reh}}$ may be more physically justified if the reheating phase takes place at the bottom of the potential, which is quartic in a good approximation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.7. Natural Inflation (NI)

See Fig. 132.

<figure><img src="image_135.png" /><figcaption>Fig. 132. Reheating consistent slow-roll predictions for the natural inflation models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.8. Exponential SUSY Inflation (ESI)

See Figs. 133 and 134.

<figure><img src="image_136.png" /><figcaption>Fig. 133. Reheating consistent slow-roll predictions for the exponential Susy models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_137.png" /><figcaption>Fig. 134. Reheating consistent slow-roll predictions for the exponential Susy models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with $\bar{w}_{\text{reh}} = -1/3$. This value of $\bar{w}_{\text{reh}}$ may be more physically justified (although rather extreme) if a parametric reheating feels the bottom of the potential, which is linear in a good approximation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.9. Power Law Inflation (PLI)

See Fig. 135.

<figure><img src="image_138.png" /><figcaption>Fig. 135. Reheating consistent slow-roll predictions for the power law models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.10. Kähler Moduli Inflation I (KMII)

See Fig. 136.

<figure><img src="image_139.png" /><figcaption>**Fig. 136.** Reheating consistent slow-roll predictions for the Kähler Moduli I models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Predictions remain mostly insensitive to the value of $\alpha$..</figcaption></figure>
A.11. Horizon Flow Inflation at first order (HF11)

See Fig. 137.

<figure><img src="image_140.png" /><figcaption>Fig. 137. Reheating consistent (exact) predictions for the horizon flow inflation at first order models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours trace the two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Notice that, up to the amplitude of the CMB anisotropies, the predictions do not depend much on $A_1$ as they are all superimposed..</figcaption></figure>
A.12. Colemann–Weinberg Inflation (CWI)

See Figs. 138 and 139.

<figure><img src="image_141.png" /><figcaption>**Fig. 138.** Reheating consistent slow-roll predictions for the Colemann–Weinberg models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), in the physical domain $Q/M_n \in [10^{-5}, 10^{-3}]$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The typical amount of gravitational waves is extremely small and dominated by second order effects (not accounted for in the figures)..</figcaption></figure>
<figure><img src="image_142.png" /><figcaption>**Fig. 139.** Reheating consistent slow-roll predictions for the Coleman–Weinberg models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), in the domain $Q/M_n \in [1, 100]$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $Q/M_n \gg 1$, the model is similar to a quadratic potential close to its minimum, and the predictions match the LFI $\epsilon_1 = \epsilon_2/2$ relation (see Section 5.2).</figcaption></figure>
A.13. Loop Inflation (LI)

See Figs. 140 and 141.

<figure><img src="image_143.png" /><figcaption>**Fig. 140.** Reheating consistent slow-roll predictions for the loop inflation models for $\alpha > 0$, in the plane $(n_s, r)$ (top panel), and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll)..</figcaption></figure>
<figure><img src="image_144.png" /><figcaption>Fig. 141. Reheating consistent slow-roll predictions for the loop inflation models for $\alpha < 0$, in the plane $(n_s, r)$ (top panel), and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll)..</figcaption></figure>
A.14. R + R$^{2p}$ Inflation (RpI)

See Figs. 142–146.

<figure><img src="image_145.png" /><figcaption>Fig. 142. Reheating consistent slow-roll predictions for the R + R$^{2p}$ inflation models in the RpI1 regime, in the plane $(n_s, r)$ (top panel), and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $p \to 0$, one recovers Starobinski Inflation..</figcaption></figure>
<figure><img src="image_146.png" /><figcaption>**Fig. 143.** Reheating consistent slow-roll predictions for the $R + R^{2p}$ inflation models in the Rpl2 regime and for $p-1 = 10^{-2}$, in the plane $(n_s, r)$ (top panel), and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $y_{\text{end}} \gg 1$, one has $\epsilon_2 \to 0$.</figcaption></figure>
<figure><img src="image_147.png" /><figcaption>**Fig. 144.** Reheating consistent slow-roll predictions for the $R + R^{2p}$ inflation models in the Rpl2 regime and for $p-1 = 0.03$, in the plane $(n_s, r)$ (top panel), and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). As for Fig. 143, the limit $y_{\text{end}} \gg 1$ corresponds to $\epsilon_2 \to 0$..</figcaption></figure>
<figure><img src="image_148.png" /><figcaption>**Fig. 145.** Reheating consistent slow-roll predictions for the $R + R^{2p}$ inflation models in the Rpl2 regime and for $p-1 = 0.06$, in the plane $(n_s, r)$ (top panel), and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Increasing the values of $p-1$ within the Rpl2 models boosts the production of primordial gravitational waves..</figcaption></figure>
<figure><img src="image_149.png" /><figcaption>**Fig. 146.** Reheating consistent slow-roll predictions for the $R + R^{2p}$ inflation models in the Rpl3 regime, in the plane $(n_s, r)$ (top panel), and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.15. Double Well Inflation (DWI)

See Fig. 147.

<figure><img src="image_150.png" /><figcaption>**Fig. 147.** Reheating consistent slow-roll predictions for the double well models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The shape of the zone covered by the models predictions is similar to the one for Small Field Inflation (SFI, see Fig. 169), except in the domain $\phi_0 \gg M_{\text{pl}}$, which is the one favored by the observations..</figcaption></figure>
A.16. Mutated Hilltop Inflation (MHI)

See Fig. 148.

<figure><img src="image_151.png" /><figcaption>**Fig. 148.** Reheating consistent slow-roll predictions for the mutated hilltop models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For small values of $\mu/M_{\phi}$, this model predicts a very small amount of primordial gravitational waves..</figcaption></figure>
A.17. Radion Gauge Inflation (RGI)

See Fig. 149.

<figure><img src="image_152.png" /><figcaption>**Fig. 149.** Reheating consistent slow-roll predictions for the radion gauge models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). At large values of $\alpha$, the predictions are the same as the large field model with $p=2$ (see Fig. 127) for which $\epsilon_2 = 2\epsilon_1$..</figcaption></figure>
A.18. MSSM Inflation (MSSMI)

See Fig. 150.

<figure><img src="image_153.png" /><figcaption>**Fig. 150.** Reheating consistent slow-roll predictions for the MSSMI models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For large values of $\phi_0 M_{\text{Pl}}$, the model predictions approach $r = 4(1 - n_s)$, i.e., $\epsilon_2 = 2\epsilon_1$.</figcaption></figure>
A.19. Renormalizable Inflection Point Inflation (RIPI)

See Fig. 151.

<figure><img src="image_154.png" /><figcaption>**Fig. 151.** Reheating consistent slow-roll predictions for the renormalizable inflection point models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.20. Arctan Inflation (AI)

See Fig. 152.

<figure><img src="image_155.png" /><figcaption>**Fig. 152.** Reheating consistent slow-roll predictions for the ArcTan models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.21. Constant $n_s$ A Inflation (CNAI)

See Fig. 153.

<figure><img src="image_156.png" /><figcaption>Fig. 153. Reheating consistent slow-roll predictions for the constant $n_s$ A models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.22. Constant $n_s$ B Inflation (CNBI)

See Fig. 154.

<figure><img src="image_157.png" /><figcaption>Fig. 154. Reheating consistent slow-roll predictions for the constant $n_s$ B models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.23. Open String Tachyonic Inflation (OSTI)

See Fig. 155.

<figure><img src="image_158.png" /><figcaption>**Fig. 155.** Reheating consistent slow-roll predictions for the open string tachyonic models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\phi_0/M_{\text{Pl}} \gg 1$, the model predictions approach $r = 4(1-n_s)$, i.e. $\epsilon_2 = 2\epsilon_1$..</figcaption></figure>
A.24. Witten–O’Raifeartaigh Inflation (WRI)

See Fig. 156.

<figure><img src="image_159.png" /><figcaption>**Fig. 156.** Reheating consistent slow-roll predictions for the Witten–O’Raifeartaigh models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). At large field values $\phi_q/M_n \gg 1$, the model predictions approach $r = 4(1-n_s)$, i.e. $\epsilon_2 = 2\epsilon_1$..</figcaption></figure>
A.25. Dual Inflation (DI)

See Fig. 157.

<figure><img src="image_160.png" /><figcaption>Fig. 157. Reheating consistent slow-roll predictions for the dual inflation in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.26. Cubically Corrected Starobinsky Inflation (CCSI)

See Figs. 158–162.

<figure><img src="image_161.png" /><figcaption>Fig. 158. Reheating consistent slow-roll predictions for cubically corrected Starobinsky inflation with $\alpha > 0$ and at small field values (CSSI1), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_162.png" /><figcaption>**Fig. 159.** Reheating consistent slow-roll predictions for cubically corrected Starobinsky inflation with $\alpha = 10^{-5}$ and at large field values (CSSI2), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The dimensionless field values at which inflation ends, $y_{\text{end}}$, varies between the minimal possible value to obtain 120 e-folds of inflation up to five times this number.</figcaption></figure>
<figure><img src="image_163.png" /><figcaption>**Fig. 160.** Reheating consistent slow-roll predictions for cubically corrected Starobinsky inflation with $\alpha = 10^{-4}$ and at large field values (CSSI2), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The dimensionless field values at which inflation ends, $y_{\text{end}}$, varies between the minimal possible value to obtain 120 e-folds of inflation up to five times this number.</figcaption></figure>
<figure><img src="image_164.png" /><figcaption>**Fig. 161.** Reheating consistent slow-roll predictions for cubically corrected Starobinsky inflation with $\alpha = 10^{-3}$ and at large field values (CSSI2), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The dimensionless field values at which inflation ends, $y_{\text{end}}$, varies between the minimal possible value to obtain 120 e-folds of inflation up to five times this number.</figcaption></figure>
<figure><img src="image_165.png" /><figcaption>**Fig. 162.** Reheating consistent slow-roll predictions for cubically corrected Starobinsky inflation with $\alpha < 0$ and at small field values (CSSI3), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.27. Symmetry Breaking Kähler Inflation (SBKI)

See Fig. 163.

<figure><img src="image_166.png" /><figcaption>**Fig. 163.** Reheating consistent slow-roll predictions for the Symmetry Breaking Kähler Inflation models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.28. Axion Hilltop Inflation (AHI)

See Fig. 164.

<figure><img src="image_167.png" /><figcaption>**Fig. 164.** Reheating consistent slow-roll predictions for the axion hilltop inflation model as a function of $f/M_n$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.29. Pure Arctan Inflation (PAI)

See Fig. 165.

<figure><img src="image_168.png" /><figcaption>**Fig. 165.** Reheating consistent slow-roll predictions for the pure arctan inflation model as a function of $\mu/M_{\pi}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.30. Superconformal $\alpha$-Attractor A Inflation (SAAI)

See Fig. 166.

<figure><img src="image_169.png" /><figcaption>Fig. 166. Reheating consistent slow-roll predictions for the superconformal $\alpha$-attractor A inflation model as a function of $\alpha$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.31. T-Model Inflation (TMI)

See Fig. 167.

<figure><img src="image_170.png" /><figcaption>**Fig. 167.** Reheating consistent slow-roll predictions for T-Model Inflation. Predictions are represented as a function of $n$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.32. Small Field Inflation (SFI)

See Figs. 168–170.

<figure><img src="image_171.png" /><figcaption>Fig. 168. Reheating consistent slow-roll predictions for the small field models with $p = 1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions are insensitive to the value of $\mu$ and verify $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$..</figcaption></figure>
<figure><img src="image_172.png" /><figcaption>**Fig. 169.** Reheating consistent slow-roll predictions for the small field models with $p = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Clearly, if $\mu/M_{\text{pl}}$ is not too high these values are limited from below to stay inside the two-sigma contours, and $\mu/M_{\text{pl}} < 10$ is disfavored by the data. For $\mu/M_{\text{pl}} \gg 1$, the model predictions approach $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$..</figcaption></figure>
<figure><img src="image_173.png" /><figcaption>**Fig. 170.** Reheating consistent slow-roll predictions for the small field models with $p = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Clearly, if $\mu/M_{\pi}$ is not too high these values are limited from below to stay inside the two-sigma contours. For $\mu/M_{\pi} \gg 1$, the model predictions approach $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$..</figcaption></figure>
### A.33. Intermediate Inflation (11)

See Figs. 171–174.

<figure><img src="image_174.png" /><figcaption>Fig. 171. Reheating consistent slow-roll predictions for the intermediate inflation models with $\beta = 1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions for $x_{\text{end}} \gg 1$ correspond to the points such that $\epsilon_1 = -(\beta/4)\epsilon_2$. Let us notice that the energy scale at which reheating ends is degenerated with $x_{\text{end}}$..</figcaption></figure>
<figure><img src="image_175.png" /><figcaption>**Fig. 172.** Reheating consistent slow-roll predictions for the intermediate inflation models with $\bar{\beta} = 4.1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_176.png" /><figcaption>Fig. 173. Reheating consistent slow-roll predictions for the intermediate inflation models with $\beta = 17$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_177.png" /><figcaption>Fig. 174. Reheating consistent slow-roll predictions for the intermediate inflation models with $\bar{\beta} = 70$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For large values of $\bar{\beta}$, the spectral index is red ($n_s < 1$) but the at the expense of producing a significant amount of primordial gravitational waves..</figcaption></figure>
A.34. Kähler Moduli Inflation II (KMIII)

See Fig. 175.

<figure><img src="image_178.png" /><figcaption>**Fig. 175.** Reheating consistent slow-roll predictions for the Kähler moduli III models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), for $10^5 < \mathcal{V} < 10^7$, $\alpha = \mathcal{V}^{5/3}$ and $\beta = \mathcal{V}^{2/3}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.35. Log-mediated Inflation (LMI)

See Figs. 176–187.

<figure><img src="image_179.png" /><figcaption>**Fig. 176.** Reheating consistent slow-roll predictions for the Log-mediated Inflation 1 models with $\beta = 10^{-3}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). Inflation proceeds at decreasing field values $x < x_{\text{in}}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\beta \ll 1$, the exponential term in the potential Eq. (6.68) is almost constant so that the model is close to large field inflation (LFI, see Section 5.2). In that limit, one has $\epsilon_1 = (1 - \gamma)\epsilon_2$.</figcaption></figure>
<figure><img src="image_180.png" /><figcaption>Fig. 177. Reheating consistent slow-roll predictions for the Logamediate Inflation 1 models with $\beta = 1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). Inflation proceeds as in Fig. 176, at decreasing field values and with $x < x_{\text{max}}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_181.png" /><figcaption>**Fig. 178.** Reheating consistent slow-roll predictions for the Logamediate Inflation 1 models ($x < x_{\text{max}}$) with $\bar{\beta} = 50$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For such high values of $\bar{\beta}$, only small values of $\gamma$ are in agreement with observations.</figcaption></figure>
<figure><img src="image_182.png" /><figcaption>Fig. 179. Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models with $\beta = 0.1$ and $\gamma = 0.95$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). Inflation proceeds at increasing field values and with $x > x_{\text{max}}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_183.png" /><figcaption>**Fig. 180.** Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models with $\beta = 0.1$ and $\gamma$ slightly increased to $\gamma = 0.97$ with respect to the previous Fig. 179. Inflation proceeds at increasing field values and with $x > x_{\gamma\text{min}}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_184.png" /><figcaption>Fig. 181. Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models with $\beta = 0.1$ and another slightly larger value of $\gamma = 0.99$ with respect to the two previous Figs. 179 and 180. Inflation proceeds at increasing field values and with $x > x_{\gamma \text{max}}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_185.png" /><figcaption>**Fig. 182.** Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models ($x > x_{\text{end}}$) with $\beta = 1$ and $\gamma = 0.6$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $x_{\text{end}}$ becomes large and lies in the fine-tuned region of LMI2, i.e. $x_{\text{end}} < x < x_{\text{end-1}}$, the predictions approach the pure de Sitter case.</figcaption></figure>
<figure><img src="image_186.png" /><figcaption>**Fig. 183.** Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models ($x > x_{\text{y,max}}$) with $\beta = 1$ and a small increase of $\gamma$ to $\gamma = 0.63$ compared to Fig. 182. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $x_{\text{end}}$ becomes large and lies in the fine-tuned region of LMI2, i.e. $x_{\text{y,max}} < x_{\text{end}} < x_{\text{end, pure}}$, the predictions approach the pure de Sitter case.</figcaption></figure>
<figure><img src="image_187.png" /><figcaption>**Fig. 184.** Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models ($x > x_{\text{max}}$) with $\beta = 1$ and another increase of $\gamma$ to $\gamma = 0.66$ compared to Figs. 182 and 183. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_188.png" /><figcaption>**Fig. 185.** Reheating consistent slow-roll predictions for the Log-mediated Inflation 2 models ($x > x_{\text{max}}$) with $\beta = 10$ and $\gamma = 0.22$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $x_{\text{end}}$ becomes large and lies in the fine-tuned region of LMI2, i.e. $x_{\text{max}} < x_{\text{end}} < x_{\text{end,1}}$, the predictions approach the pure de Sitter case.</figcaption></figure>
<figure><img src="image_189.png" /><figcaption>**Fig. 186.** Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models ($x > x_{\text{in}}$) with $\beta = 10$ and a slightly increased value of $\gamma = 0.23$ (compared to Fig. 185), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_190.png" /><figcaption>Fig. 187. Reheating consistent slow-roll predictions for the Logamediate Inflation 2 models ($x > x_{\text{max}}$) with $\beta = 10$ and $\gamma$ increased $\gamma = 0.24$ with respect to Figs. 185 and 186, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.36. Twisted Inflation (TWI)

See Figs. 188–190.

<figure><img src="image_191.png" /><figcaption>**Fig. 188.** Reheating consistent slow-roll predictions for the twisted models having $\phi_0/M_{Pl} = 10^{-2}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_192.png" /><figcaption>**Fig. 189.** Reheating consistent slow-roll predictions for the twisted models having $\phi_0/M_{Pl} = 10^{-1}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_193.png" /><figcaption>**Fig. 190.** Reheating consistent slow-roll predictions for the twisted models having $\phi = M_p$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.37. GMSSM Inflation (GMSSMI)

See Figs. 191–194.

<figure><img src="image_194.png" /><figcaption>**Fig. 191.** Reheating consistent slow-roll predictions for the GMSSMI models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with $\phi_v = M_p$ and for $1 < \alpha < 1 + \phi_v^4/M_p^4\pi^2/900/(N_{\text{end}} - N_{\text{im}})^2$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $\alpha \to 1$, one recovers the standard MSSM predictions, see Fig. 150.</figcaption></figure>
<figure><img src="image_195.png" /><figcaption>**Fig. 192.** Reheating consistent slow-roll predictions for the GMSSMI models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with sub-Planckian $\phi/M_{\text{pl}} = 0.32$ and for $1 < \alpha < 1 + \phi^4/M^4\pi^2/900/(N_{\text{end}} - N_{\text{min}})^2$. Compared to Fig. 191, the amount of primordial gravitational waves produced is much reduced. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_196.png" /><figcaption>**Fig. 193.** Reheating consistent slow-roll predictions for the GMSSMI models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with $\phi_0 = M_{\nu}$ and for $1 - \phi^4/M^4\pi^2/900/(N_{\text{end}} - N_{\text{in}})^2 < \alpha < 1$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $\alpha \to 1$, one recovers the standard MSSM predictions, see Fig. 150. Notice the rather strong fine-tuning on $\alpha$ for the model predictions to be compatible with observations.</figcaption></figure>
<figure><img src="image_197.png" /><figcaption>**Fig. 194.** Reheating consistent slow-roll predictions for the GMSSMI models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with sub-Planckian $\phi_0/M_{\text{Pl}} - 0.32$ and for $1 - \phi_0^2/M_{\text{Pl}}^2\pi^2/900/(N_{\text{end}} - N_{\text{ini}})^2 < \alpha < 1$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $\alpha \to 1$, Compared to Fig. 193, the amount of primordial gravitational waves is reduced.</figcaption></figure>
A.38. Generalized Renormalizable Inflection Point Inflation (GRIPI)

See Figs. 195–198.

<figure><img src="image_198.png" /><figcaption>**Fig. 195.** Reheating consistent slow-roll predictions for the generalized renormalizable inflection point models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with $\phi_0 = M_{\nabla}$ and for $1 < \alpha < 1 + \phi_0^4/M_{\nabla}^4\pi^2/576/(N_{\text{end}} - N_{\text{ini}} = 60)^2$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). When $\alpha \to 1$, one recovers the standard RIPI predictions, see Fig. 151.</figcaption></figure>
<figure><img src="image_199.png" /><figcaption>**Fig. 196.** Reheating consistent slow-roll predictions for the generalized renormalizable inflection point models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with sub-Planckian $\phi_\phi = 0.32 M_\phi$ and for $1 < \alpha < 1 + \phi_0^4 / M_p^4 \pi^2 / 576 / (N_{\text{end}} - N_{\text{ini}} = 60)^2$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Reducing $\phi_\phi$ strongly lowers the amount of primordial gravitational wave produced, see Fig. 195.</figcaption></figure>
<figure><img src="image_200.png" /><figcaption>**Fig. 197.** Reheating consistent slow-roll predictions for the generalized renormalizable inflection point models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with $\phi_0 = M_{\tilde{\nu}}$ and for $1 - \phi_0^4/M_{\tilde{\nu}}^4\pi^2/576/(N_{\text{end}} - N_{\text{ini}} = 60)^2 < \alpha < 1$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Notice the strong fine-tuning required on $\alpha$ for the model to be compatible with the observations.</figcaption></figure>
<figure><img src="image_201.png" /><figcaption>**Fig. 198.** Reheating consistent slow-roll predictions for the generalized renormalizable inflection point models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), with sub-Planckian $\phi = 0.32 M_{\text{pl}}$ and for $1 - \phi^4 / M_{\text{pl}}^4 \pi^2 / 576 / (N_{\text{end}} - N_{\text{ini}} = 60)^2 < \alpha < 1$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Compared to Fig. 197, the amount of primordial gravitational waves is reduced.</figcaption></figure>
A.39. Brane SUSY Breaking Inflation (BSUSYBI)

See Figs. 199 and 200.

<figure><img src="image_202.png" /><figcaption>**Fig. 199.** Reheating consistent slow-roll predictions for the BSUSYBI models with $\gamma = 10^{-2}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $x_{\text{end}}$ varies between $2x_{\text{end}}^{\text{max}} < x_{\text{end}} < x_{\text{end}}^{\text{max}}$ ($x_{\text{end}}^{\text{max}} < 0$), under which the predictions of the model coincide with the line $\epsilon_2 = 0$ (black solid), i.e. PLI (see Section 5.8).</figcaption></figure>
<figure><img src="image_203.png" /><figcaption>**Fig. 200.** Reheating consistent slow-roll predictions for the BSUSYBI models with $\gamma = 0.029$, slightly increased compared to Fig. 199, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\gamma$ should be $\lesssim 5 \times 10^{-2}$ to predict a reasonable amount of primordial gravitational waves.</figcaption></figure>
A.40. Tip Inflation (TI)

See Figs. 201–207.

<figure><img src="image_204.png" /><figcaption>**Fig. 201.** Reheating consistent slow-roll predictions for the tip inflation models with $\alpha < 1/2$, and for $\mu/M_{\text{Pl}} = 10^{-2}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_205.png" /><figcaption>**Fig. 202.** Reheating consistent slow-roll predictions for the tip inflation models with $\alpha < 1/2$, and for $\mu/M_{Pl} = 10^{-1}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Fig. 201.</figcaption></figure>
<figure><img src="image_206.png" /><figcaption>**Fig. 203.** Reheating consistent slow-roll predictions for the tip inflation models with $\alpha < 1/2$, and for $\mu/M_{\phi} = 0.5$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). To be compared to smaller values of $\mu/M_{\phi}$ in Figs. 201 and 202.</figcaption></figure>
<figure><img src="image_207.png" /><figcaption>**Fig. 204.** Reheating consistent slow-roll predictions for the tip inflation models with $\alpha > 1/2$, and for $\mu/M_{\text{pl}} = 10^{-2}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_208.png" /><figcaption>**Fig. 205.** Reheating consistent slow-roll predictions for the tip inflation models with $\alpha > 1/2$, and for $\mu/M_{Pl} = 10^{-1}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_209.png" /><figcaption>**Fig. 206.** Reheating consistent slow-roll predictions for the tip inflation models with $\alpha > 1/2$, and for $\mu/M_{\phi} = 0.5$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). To be compared to smaller values of $\mu/M_{\phi}$ in Figs. 204 and 205.</figcaption></figure>
<figure><img src="image_210.png" /><figcaption>Fig. 207. Reheating consistent slow-roll predictions for the tip inflation models with $\alpha = 1/2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.41. $\beta$ Exponential Inflation (BEI)

See Figs. 208 and 209.

<figure><img src="image_211.png" /><figcaption>Fig. 208. Reheating consistent slow-roll predictions for the $\beta$ Exponential Inflation models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The parameter $\lambda$ has been fixed to $10^{-3}$ for this plot but the predictions almost do not depend on it (see Fig. 209). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_212.png" /><figcaption>**Fig. 209.** Reheating consistent slow-roll predictions for the $\beta$ Exponential Inflation models with a large value of $\lambda = 10^3$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The predictions are undistinguishable from the ones having $\lambda = 10^{-3}$, see Fig. 208. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.42. Pseudo Natural Inflation (PSNI)

See Figs. 210–212.

<figure><img src="image_213.png" /><figcaption>**Fig. 210.** Reheating consistent slow-roll predictions for the pseudo natural inflation models with $f/M_n = 10$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_214.png" /><figcaption>**Fig. 211.** Reheating consistent slow-roll predictions for the pseudo natural inflation models with sub-Planckian $f/M_p = 0.1$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Compared to super-Planckian values of $f$, the amount of primordial gravitational waves is reduced, see Fig. 210.</figcaption></figure>
<figure><img src="image_215.png" /><figcaption>**Fig. 212.** Reheating consistent slow-roll predictions for the pseudo natural inflation models with a small $f/M_n = 10^{-2}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Predictions for larger values of $f$ are plotted in Figs. 210 and 211.</figcaption></figure>
A.43. Non Canonical Kähler Inflation (NCKI)

See Figs. 213–220.

<figure><img src="image_216.png" /><figcaption>Fig. 213. Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with positive $\beta = 10^{-4}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_217.png" /><figcaption>Fig. 214. Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with positive $\beta = 3.2 \times 10^{-3}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_218.png" /><figcaption>Fig. 215. Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with positive $\beta = 6.3 \times 10^{-3}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_219.png" /><figcaption>**Fig. 216.** Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with positive $\beta = 3.2 \times 10^{-2}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For larger values of $\beta \gtrsim 1$, the predictions are almost identical to those displayed here. See Figs. 213 to 215 for smaller values of $\beta$.</figcaption></figure>
<figure><img src="image_220.png" /><figcaption>Fig. 217. Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with negative $\beta = -10^{-4}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_221.png" /><figcaption>**Fig. 218.** Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with negative $\beta = -3.2 \times 10^{-3}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_222.png" /><figcaption>**Fig. 219.** Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with negative $\beta = -7.9 \times 10^{-3}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_223.png" /><figcaption>**Fig. 220.** Reheating consistent slow-roll predictions for the non canonical Kähler inflation models with negative $\rho = -0.5$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For smaller values of $\rho \lesssim -1$, the predictions are almost identical to those displayed here. See Figs. 217 to 219 for smaller values of $|\rho|$.</figcaption></figure>
A.44. Constant Spectrum Inflation (CSI)

See Figs. 221 and 222.

<figure><img src="image_224.png" /><figcaption>Fig. 221. Reheating consistent slow-roll predictions for the Constant Spectrum models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), for $\alpha = 10^{-3}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Model predictions verify $n_s = 1$.</figcaption></figure>
<figure><img src="image_225.png" /><figcaption>Fig. 222. Reheating consistent slow-roll predictions for the Constant Spectrum models in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel), for $\alpha = 1$. The two solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Independently of $\alpha$, one still has the predictions lying along $n_s = 1$, see also Fig. 221.</figcaption></figure>
A.45. Orientifold Inflation (OI)

See Figs. 223 and 224.

<figure><img src="image_226.png" /><figcaption>Fig. 223. Reheating consistent slow-roll predictions for the orientifold inflation models for $\phi_0/M_{Pl} = 10^{-4}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The predictions of the model almost do not depend on its parameters, they are all superimposed and one cannot distinguish the different values of $\alpha$, and of $\phi_0$ (see Fig. 224).</figcaption></figure>
<figure><img src="image_227.png" /><figcaption>**Fig. 224.** Reheating consistent slow-roll predictions for the orientifold inflation models for $\phi_s/M_{Pl} = 10^{-1}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The prediction of the model is the same as for $\phi_s/M_{Pl} = 10^{-4}$ (see Fig. 223) and almost do not depend on $\alpha$.</figcaption></figure>
A.46. Constant $n_s$ C Inflation (CNCI)

See Figs. 225–227.

<figure><img src="image_228.png" /><figcaption>Fig. 225. Reheating consistent slow-roll predictions for the constant $n_s$ C inflation models for $\alpha = 10^{-3}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For all values of $x_{\text{end}}$, the predictions are very close to the constant value $n_s = 1$.</figcaption></figure>
<figure><img src="image_229.png" /><figcaption>**Fig. 226.** Reheating consistent slow-roll predictions for the constant $n_s$ C inflation models for $\alpha = 0.1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Compared the smaller values of $\alpha$ (see Fig. 225), at intermediate values of $x_{\text{end}}$, the model predictions deviate from $n_s = 1$ while they approach $n_s = 1 - 2\alpha^2$ for small values of $x_{\text{end}}$.</figcaption></figure>
<figure><img src="image_230.png" /><figcaption>Fig. 227. Reheating consistent slow-roll predictions for the constant $n_s$ C inflation models for $\alpha = 0.2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Compared to smaller values of $\alpha$ (see Figs. 225 and 226), for most of the $x_{\text{end}}$ values, the model predictions are not with a constant spectral index. Only for very large $x_{\text{end}} \to x_{\text{end}}^{\text{max}}$ they are along $n_s = 1$ while the limit $n_s = 1 - 2\alpha^2$ is reached for $x_{\text{end}} \ll x_{\text{end}}^{\text{max}}$, with, however, an unreasonable amount of primordial gravitational waves.</figcaption></figure>
A.47. Supergravity Brane Inflation (SBI)

See Figs. 228–230.

<figure><img src="image_231.png" /><figcaption>**Fig. 228.** Reheating consistent slow-roll predictions for the supergravity brane inflation models for $\beta = 5 \times 10^{-5}$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_232.png" /><figcaption>**Fig. 229.** Reheating consistent slow-roll predictions for the supergravity brane inflation models for $\beta = 10^{-3}$ in the plane $(n_1, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_233.png" /><figcaption>**Fig. 230.** Reheating consistent slow-roll predictions for the supergravity brane inflation models for $\alpha = \alpha_{\min}(\beta)$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.48. Spontaneous Symmetry Breaking Inflation 1 (SSBI1)

See Figs. 231–233.

<figure><img src="image_234.png" /><figcaption>Fig. 231. Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 1 inflation ($\alpha > 0, \beta > 0$) models with $\beta = 10^{-3}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $\alpha_{\min}(\beta) < \alpha < 10^6 \alpha_{\min}(\beta)$.</figcaption></figure>
<figure><img src="image_235.png" /><figcaption>**Fig. 232.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 1 inflation ($\alpha > 0, \beta > 0$) models with $\beta = 10^{-1}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $\alpha_{\min}(\beta) < \alpha < 10^6 \alpha_{\min}(\beta)$.</figcaption></figure>
<figure><img src="image_236.png" /><figcaption>**Fig. 233.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 1 inflation ($\alpha > 0, \beta > 0$) models with $\beta = 10$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $\alpha_{\min}(\beta) < \alpha < 10^6 \alpha_{\min}(\beta)$ but model predictions are weakly sensitive to its value.</figcaption></figure>
A.49. Spontaneous Symmetry Breaking Inflation 2 (SSBI2)

See Figs. 234–237.

<figure><img src="image_237.png" /><figcaption>**Fig. 234.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 2 inflation ($\alpha < 0, \beta < 0$) models with $\beta = -10^{-10}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See Figs. 235 to 237 for larger values of $|\beta|$.</figcaption></figure>
<figure><img src="image_238.png" /><figcaption>**Fig. 235.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 2 inflation ($\alpha < 0, \beta < 0$) models with $\beta = -10^{-4}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_239.png" /><figcaption>**Fig. 236.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 2 inflation ($\alpha < 0, \beta < 0$) models with $\beta = -10^{-3}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_240.png" /><figcaption>Fig. 237. Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 2 inflation ($\alpha < 0, \beta < 0$) models with $\beta = -10^{-2}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.50. Spontaneous Symmetry Breaking Inflation 3 (SSBI3)

See Figs. 238–240.

<figure><img src="image_241.png" /><figcaption>Fig. 238. Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 3 inflation [$\alpha > 0, \beta < 0, x^2 < -\alpha/(2\beta)$] models for $\bar{\beta} = -10^{-3}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $\alpha_{\min}(\bar{\beta}) \approx 2 < \alpha < 10^3 \alpha_{\min}(\bar{\beta})$.</figcaption></figure>
<figure><img src="image_242.png" /><figcaption>**Fig. 239.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 3 inflation [$\alpha > 0$, $\beta < 0$, $x^2 < -\alpha / (2\beta)$] models for $\beta = -5 \times 10^{-3}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $\alpha_{\min}(\beta) \approx 2 < \alpha < 10^3 \alpha_{\min}(\beta)$.</figcaption></figure>
<figure><img src="image_243.png" /><figcaption>**Fig. 240.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 3 inflation [$\alpha > 0, \beta < 0, x^2 < -\alpha/(2\beta)$] models for $\beta = -10^{-2}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $\alpha_{\min}(\beta) \approx 2 < \alpha < 10^3 \alpha_{\min}(\beta)$.</figcaption></figure>
A.51. Spontaneous Symmetry Breaking Inflation 4 (SSB14)

See Figs. 241–243.

<figure><img src="image_244.png" /><figcaption>Fig. 241. Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 4 inflation [$\alpha > 0, \beta < 0, x^2 > -\alpha/(2\bar{\beta})$] models for $\bar{\beta} = -10^{-5}$, in the plane $(\epsilon_1, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_245.png" /><figcaption>**Fig. 242.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 4 inflation [$\alpha > 0, \beta < 0, x^2 > -\alpha/(2\beta)$] models for $\bar{\beta} = -10^{-4}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_246.png" /><figcaption>Fig. 243. Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 4 inflation [$\alpha > 0, \beta < 0, x^2 > -\alpha/(2\beta)$] models for $\bar{\beta} = -10^{-3}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.52. Spontaneous Symmetry Breaking Inflation 5 (SSBI5)

See Figs. 244–246.

<figure><img src="image_247.png" /><figcaption>**Fig. 244.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 5 inflation [$\alpha < 0$, $\beta > 0$, $x^2 < -\alpha/(2\beta)$] models for $\beta = 10^{-6}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $|\alpha_{\min}(\beta)| < |\alpha| < 10|\alpha_{\min}(\beta)|$.</figcaption></figure>
<figure><img src="image_248.png" /><figcaption>**Fig. 245.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 5 inflation $|α| < 0, β > 0, x^2 < -α/(2β)$] models for $β = 10^{-5}$, in the plane $(n_s, r)$ (top panel) and the plane $(ε_1, ε_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $α$ is varied between $|α_{min}(β)| < |α| < 10|α_{min}(β)|$.</figcaption></figure>
<figure><img src="image_249.png" /><figcaption>**Fig. 246.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 5 inflation $|α| < 0, β > 0, x^2 < -α/(2β)$ models for $β = 10^{-4}$, in the plane $(n_s, r)$ (top panel) and the plane $(ε_1, ε_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $α$ is varied between $|α_{min}(β)| < |α| < 10|α_{min}(β)|$.</figcaption></figure>
A.53. Spontaneous Symmetry Breaking Inflation 6 (SSBI6)

See Figs. 247–249.

<figure><img src="image_250.png" /><figcaption>**Fig. 247.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 6 inflation [$\alpha < 0, \beta > 0, \chi^2 > -a/(2\beta)$] models for $\beta = 10^{-5}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $|a_{\text{min}}(\beta)| < |\alpha| < 10^4|a_{\text{min}}(\beta)|$.</figcaption></figure>
<figure><img src="image_251.png" /><figcaption>**Fig. 248.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking 6 inflation [$\alpha < 0, \beta > 0, \chi^2 > -\alpha/(2\beta)$] models for $\beta = 10^{-1}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $|\alpha_{\min}(\beta)| < |\alpha| < 10^4|\alpha_{\min}(\beta)|$.</figcaption></figure>
<figure><img src="image_252.png" /><figcaption>**Fig. 249.** Reheating consistent slow-roll predictions for the spontaneous symmetry breaking of 6 inflation [$\alpha < 0, \beta > 0, \chi^2 > -\alpha/(2\bar{\beta})$] models for $\bar{\beta} = 1$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $\alpha$ is varied between $|\alpha_{\min}(\bar{\beta})| < |\alpha| < 10^4|\alpha_{\min}(\bar{\beta})|$ but the predictions are almost insensitive to its value.</figcaption></figure>
A.54. Inverse Monomial Inflation (IMI)

See Figs. 250–253.

<figure><img src="image_253.png" /><figcaption>Fig. 250. Reheating consistent slow-roll predictions for the IMI models with $p = 1$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $x_{\text{end}}$ varies above $x_{\text{end}}^{\min}$ ($\Delta N = 65$). The model predictions are along the curves $(1-2/p)r = 8(1-n_s)$, i.e. $\epsilon_1 = -(p/4)\epsilon_2$. For other values of $p$, see Figs. 251 to 253.</figcaption></figure>
<figure><img src="image_254.png" /><figcaption>**Fig. 251.** Reheating consistent slow-roll predictions for the IMI models with $p = 2$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $x_{\text{end}}$ varies above $x_{\text{end}}^{\text{min}}$ ($\Delta N = 65$). The model predictions verify $n_s = 1$.</figcaption></figure>
<figure><img src="image_255.png" /><figcaption>Fig. 252. Reheating consistent slow-roll predictions for the IMI models with $p = 3$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $x_{\text{end}}$ varies above $x_{\text{end}}^{\min}$ ($\Delta N = 65$). The model predictions are along the curves $(1-2/p)r = 8(1-n_s)$, i.e. $\epsilon_1 = -(p/4)\epsilon_2$.</figcaption></figure>
<figure><img src="image_256.png" /><figcaption>Fig. 253. Reheating consistent slow-roll predictions for the IMI models with $p = 4$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The parameter $x_{\text{end}}$ varies above $x_{\text{end}}^{\min}$ ($\Delta N = 65$). The model predictions are along the curves $(1-2/p)r = 8(1-n_s)$, i.e. $\epsilon_1 = -(p/4)\epsilon_2$.</figcaption></figure>
A.55. Brane Inflation (BI)

See Figs. 254–257.

<figure><img src="image_257.png" /><figcaption>Fig. 254. Reheating consistent slow-roll predictions for the brane inflation models with $p = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu \gg M_p$, the model predictions approach the curve $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$. See Figs. 255 and 256 for other values of $p$.</figcaption></figure>
<figure><img src="image_258.png" /><figcaption>Fig. 255. Reheating consistent slow-roll predictions for the brane inflation models with $p = 3$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu \gg M_p$, the model predictions approach the curve $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$.</figcaption></figure>
<figure><img src="image_259.png" /><figcaption>Fig. 256. Reheating consistent slow-roll predictions for the brane inflation models with $p = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu \gg M_p$, the model predictions approach the curve $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$.</figcaption></figure>
<figure><img src="image_260.png" /><figcaption>Fig. 257. Reheating consistent slow-roll predictions for the brane inflation models in the string framework ($p = 4, \mu \ll M_p, N = 5, v = 16/27, g_s = 5 \times 10^{-3}, \alpha' = 0.25$), in the plane ($n_s, r$) (top panel) and the plane ($\epsilon_1, \epsilon_2$) (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu/M_p > 0.02$, inflation ends by slow roll violation as opposed to tachyonic instability for lower values of $\mu/M_p$.</figcaption></figure>
A.56. KKLT Inflation (KKLTI)

See Figs. 258–261.

<figure><img src="image_261.png" /><figcaption>**Fig. 258.** Reheating consistent slow-roll predictions for the KKLT inflation models with $p = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu \gg M_{\text{Pl}}$, the model predictions deviate from the BI's ones, the latter lying along the locus $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$ (see Fig. 254).</figcaption></figure>
<figure><img src="image_262.png" /><figcaption>**Fig. 259.** Reheating consistent slow-roll predictions for the KKLT inflation models with $p = 3$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu \gg M_p$, the model predictions deviate from the BI's ones, the latter lying along the locus $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$ (see Fig. 255).</figcaption></figure>
<figure><img src="image_263.png" /><figcaption>**Fig. 260.** Reheating consistent slow-roll predictions for the KKLT inflation models with $p = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu \gg M_p$, the model predictions deviate from the BI's ones, the latter lying along the locus $r = (8/3)(1 - n_s)$, i.e. $\epsilon_2 = 4\epsilon_1$ (see Fig. 256).</figcaption></figure>
<figure><img src="image_264.png" /><figcaption>**Fig. 261.** Reheating consistent slow-roll predictions for the KKLT inflation models in the string framework ($p = 4$, $\mu \ll M_p$, $N = 5$, $v = 16/27$, $g_s = 0.005$, $\alpha' = 0.25$) for the, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $\mu/M_p > 0.02$, inflation ends by slow roll violation as opposed to tachyonic instability for lower values of $\mu$. Because $\mu \ll M_p$, the model predictions are undistinguishable from the BI's ones (see Fig. 257).</figcaption></figure>
A.57. String Axion Inflation I 1 (SAII1)

See Figs. 262–264.

<figure><img src="image_265.png" /><figcaption>**Fig. 262.** Reheating consistent slow-roll predictions for the SAI1 inflation models with $\alpha = -0.8$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions for larger values of $\alpha$ are represented in Figs. 263 to 264.</figcaption></figure>
<figure><img src="image_266.png" /><figcaption>**Fig. 263.** Reheating consistent slow-roll predictions for the SAI1 inflation models with $\alpha = -0.1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_267.png" /><figcaption>**Fig. 264.** Reheating consistent slow-roll predictions for the SAI1 inflation models with $\alpha = 0.6$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.58. String Axion Inflation I 2 (SAII2)

See Figs. 265–267.

<figure><img src="image_268.png" /><figcaption>Fig. 265. Reheating consistent slow-roll predictions for the SAII2 inflation models with $\alpha = -0.8$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions for larger values of $\alpha$ are represented in Figs. 266 to 267.</figcaption></figure>
<figure><img src="image_269.png" /><figcaption>**Fig. 266.** Reheating consistent slow-roll predictions for the SAI12 inflation models with $\alpha = -0.1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_270.png" /><figcaption>**Fig. 267.** Reheating consistent slow-roll predictions for the SAI2 inflation models with $\alpha = 0.6$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.59. Mukhanov Inflation (VFMI)

See Figs. 268–273.

<figure><img src="image_271.png" /><figcaption>Fig. 268. Reheating consistent slow-roll predictions for the Mukhanov inflationary models with $\alpha = 1/2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions for larger values of $\alpha$ are represented in Figs. 269 to 270.</figcaption></figure>
<figure><img src="image_272.png" /><figcaption>**Fig. 269.** Reheating consistent slow-roll predictions for the Mukhanov inflationary models with $\alpha = 1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_273.png" /><figcaption>**Fig. 270.** Reheating consistent slow-roll predictions for the Mukhanov inflationary models with $\alpha = 3/2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_274.png" /><figcaption>Fig. 271. Reheating consistent slow-roll predictions for the Mukhanov inflationary models with $\alpha = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_275.png" /><figcaption>**Fig. 272.** Reheating consistent slow-roll predictions for the Mukhanov inflationary models with $\alpha = 5/2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_276.png" /><figcaption>Fig. 273. Reheating consistent slow-roll predictions for the Mukhanov inflationary models with $\alpha = 3$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See Figs. 268 to 272 for smaller values of $a$.</figcaption></figure>
A.60. Fiber Inflation (FI)

See Figs. 274 and 275.

<figure><img src="image_277.png" /><figcaption>Fig. 274. Reheating consistent slow-roll predictions for the Fiber Inflation models with $n = 0$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_278.png" /><figcaption>Fig. 275. Reheating consistent slow-roll predictions for the Fiber Inflation models with $n = 1$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.61. Hyperbolic Inflation (HBI)

See Figs. 276–278.

<figure><img src="image_279.png" /><figcaption>Fig. 276. Reheating consistent slow-roll predictions for the Hyperbolic Inflation models with $n = 0.5$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See Figs. 277 and 278 for other values of $n$.</figcaption></figure>
<figure><img src="image_280.png" /><figcaption>Fig. 277. Reheating consistent slow-roll predictions for the Hyperbolic Inflation models with $n = 1$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_281.png" /><figcaption>Fig. 278. Reheating consistent slow-roll predictions for the Hyperbolic Inflation models with $n = 1.5$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.62. Smeared Higgs Inflation (SHI)

See Figs. 279–282.

<figure><img src="image_282.png" /><figcaption>Fig. 279. Reheating consistent slow-roll predictions for the Smeared Higgs Inflation models with $\phi_0 = 10M_p$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See Figs. 280, 281 and 282 for other values of $\phi_0$.</figcaption></figure>
<figure><img src="image_283.png" /><figcaption>**Fig. 280.** Reheating consistent slow-roll predictions for the Smeared Higgs Inflation models with $\phi_c = 15 M_P$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_284.png" /><figcaption>**Fig. 281.** Reheating consistent slow-roll predictions for the Smeared Higgs Inflation models with $\phi_0 = 20M_P$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_285.png" /><figcaption>**Fig. 282.** Reheating consistent slow-roll predictions for the Smeared Higgs Inflation models with $\phi_0 = 25M_p$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.63. Double Exponential Inflation (DEI)

See Figs. 283–286.

<figure><img src="image_286.png" /><figcaption>Fig. 283. Reheating consistent slow-roll predictions for the Double Exponential Inflation models with $\phi_0 = 10M_{\text{Pl}}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See Figs. 284, 285, and 286 for other values of $\phi_0$.</figcaption></figure>
<figure><img src="image_287.png" /><figcaption>**Fig. 284.** Reheating consistent slow-roll predictions for the Double Exponential Inflation models with $\phi_v = 20M_{pl}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_288.png" /><figcaption>**Fig. 285.** Reheating consistent slow-roll predictions for the Double Exponential Inflation models with $\phi_v = 50M_{pl}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_289.png" /><figcaption>**Fig. 286.** Reheating consistent slow-roll predictions for the Double Exponential Inflation models with $\phi_0 = 100M_P$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.64. S-Dual Inflation (SDI)

See Figs. 287–289.

<figure><img src="image_290.png" /><figcaption>Fig. 287. Reheating consistent slow-roll predictions for S-Dual Inflation and for $\mu = 6M_{\text{Pl}}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field value at which inflation ends $x_{\text{end}} = \phi_{\text{end}}/\mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 288 and 289 for other values of $\mu$.</figcaption></figure>
<figure><img src="image_291.png" /><figcaption>**Fig. 288.** Reheating consistent slow-roll predictions for S-Dual Inflation and for $\mu = 7 M_{\text{pl}}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field value at which inflation ends $x_{\text{end}} = \phi_{\text{end}}/\mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_292.png" /><figcaption>**Fig. 289.** Reheating consistent slow-roll predictions for S-Dual Inflation and for $\mu = 10M_p$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field value at which inflation ends $x_{\text{end}} = \phi_{\text{end}}/\mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.65. Generalized Double Well Inflation (GDWI)

See Figs. 290–292.

<figure><img src="image_293.png" /><figcaption>**Fig. 290.** Reheating consistent slow-roll predictions for the Generalized Double Well Inflation model with a power law index $p = 2$. Predictions are represented as a function of the vev $\phi/M_{\text{Pl}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 291 and 292 for other values of $p$.</figcaption></figure>
<figure><img src="image_294.png" /><figcaption>**Fig. 291.** Reheating consistent slow-roll predictions for the Generalized Double Well Inflation model with a power law index $p = 3$. Predictions are represented as a function of the vev $\phi_0/M_p$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_295.png" /><figcaption>Fig. 292. Reheating consistent slow-roll predictions for the Generalized Double Well Inflation model with a power law index $p = 4$. Predictions are represented as a function of the vev $\phi/M_{\phi}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.66. Non-Minimal Large Field Inflation 1 (NMLFI1)

See Figs. 293–298.

<figure><img src="image_296.png" /><figcaption>Fig. 293. Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 1 model, for $p = 1$. Predictions are represented as a function of $\xi$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 294 to 295 for the other parameter values in the regime $p < 4$ where NMLFI1 is an hilltop-like model at small field values.</figcaption></figure>
<figure><img src="image_297.png" /><figcaption>**Fig. 294.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 1 model, for $p = 2$. Predictions are represented as a function of $\xi$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_298.png" /><figcaption>**Fig. 295.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 1 model, for $p = 3$. Predictions are represented as a function of $\xi$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_299.png" /><figcaption>**Fig. 296.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 1 model, in the plateau regime, for $p = 4$. Predictions are represented as a function of $\xi$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). For this value of $p = 4$, NMLF11 is the same model as Higgs Inflation (HI, with $v = 0$) whose reheating predictions are plotted in Fig. 125. Notice that, for NMLFI, $\xi$ remains a free parameter whereas it is fixed by the amplitude of the CMB anisotropies for HI. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_300.png" /><figcaption>Fig. 297. Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 1 model, for $p = 5$, in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). For $p > 4$, the potential of NMLFI is monotonously growing with $\chi$ and NMLFI1 is a large field model. See also Fig. 298.</figcaption></figure>
<figure><img src="image_301.png" /><figcaption>**Fig. 298.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 1 model, for $p = 8$. Predictions are represented as a function of $\xi < \xi_o(p)$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The condition $\xi < \xi_o(p)$ is necessary for $p > p_+ \approx 7.46$ to ensure that the potential is not too steep to support inflation.</figcaption></figure>
A.67. Non-Minimal Large Field Inflation 3 (NMLFI3)

See Figs. 299–316.

<figure><img src="image_302.png" /><figcaption>**Fig. 299.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.1$ and $\xi = 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 300 to 307 for the other “small” parameter values having $p < p_-$ and $\xi < \xi_0(p)$.</figcaption></figure>
<figure><img src="image_303.png" /><figcaption>**Fig. 300.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.1$ and $\xi = 2.5 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_304.png" /><figcaption>**Fig. 301.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.1$ and $\xi = 4 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_305.png" /><figcaption>**Fig. 302.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.25$ and $\xi = 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_306.png" /><figcaption>**Fig. 303.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.25$ and $\xi = 3 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_307.png" /><figcaption>**Fig. 304.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.25$ and $\xi = 4 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_308.png" /><figcaption>**Fig. 305.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.4$ and $\xi = 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_309.png" /><figcaption>**Fig. 306.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.4$ and $\bar{\xi} = 3 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_310.png" /><figcaption>**Fig. 307.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.4$ and $\xi = 4 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_311.png" /><figcaption>**Fig. 308.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.6$ and $\xi = 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 309 to 316 for the other “large” parameter values having $p > p_-$ (and $p < 4$).</figcaption></figure>
<figure><img src="image_312.png" /><figcaption>**Fig. 309.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.6$ and $\xi = 3 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_313.png" /><figcaption>Fig. 310. Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 0.6$ and $\xi = 4 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_314.png" /><figcaption>Fig. 311. Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 2$ and $\xi = 2 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_315.png" /><figcaption>Fig. 312. Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 2$ and $\xi = 4 \times 10^{-5}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_316.png" /><figcaption>**Fig. 313.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 2$ and $\xi = 5 \times 10^{-3}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_317.png" /><figcaption>Fig. 314. Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 3.5$ and $\xi = 10^{-2}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_318.png" /><figcaption>Fig. 315. Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 3.5$ and $\xi = 2 \times 10^{-2}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_319.png" /><figcaption>**Fig. 316.** Reheating consistent slow-roll predictions for the Non-Minimal Large Field Inflation 3 model, for $p = 3.5$ and $\xi = 3 \times 10^{-2}$. Predictions are represented as a function of $\chi_{\text{end}}$ in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.68. Superconformal $\alpha$-Attractor B Inflation (SABI)

See Figs. 317–319.

<figure><img src="image_320.png" /><figcaption>Fig. 317. Reheating consistent slow-roll predictions for the Superconformal $\alpha$-attractor B Inflation model for $n = 2$. Predictions are represented as a function of $\alpha$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 318 and 319 for other values of $n$.</figcaption></figure>
<figure><img src="image_321.png" /><figcaption>**Fig. 318.** Reheating consistent slow-roll predictions for the Superconformal $\alpha$-attractor B Inflation model for $n = 5$. Predictions are represented as a function of $\alpha$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_322.png" /><figcaption>**Fig. 319.** Reheating consistent slow-roll predictions for the Superconformal $\alpha$-attractor B Inflation model for $n = 20$. Predictions are represented as a function of $\alpha$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.69. Superconformal $\alpha$-Attractor T Inflation (SATI)

See Figs. 320–322.

<figure><img src="image_323.png" /><figcaption>Fig. 320. Reheating consistent slow-roll predictions for the Superconformal $\alpha$-attractor T Inflation model for $n = 1$. Predictions are represented as a function of $\alpha$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 321 and 322 for other values of $n$.</figcaption></figure>
<figure><img src="image_324.png" /><figcaption>**Fig. 321.** Reheating consistent slow-roll predictions for the Superconformal $\alpha$-attractor $T$ Inflation model for $n = 5$. Predictions are represented as a function of $\alpha$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_325.png" /><figcaption>**Fig. 322.** Reheating consistent slow-roll predictions for the Superconformal $\alpha$-attractor $T$ Inflation model for $n = 10$. Predictions are represented as a function of $\alpha$ in the plane $(n, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.70. Running Mass Inflation 1 (RMI1)

See Figs. 323–326.

<figure><img src="image_326.png" /><figcaption>Fig. 323. Reheating consistent slow-roll predictions for the running mass inflation 1 models ($c > 0, x < 1$) with $c = 0.02$ and $\phi_0/M_{\pi} = 2$ (which satisfies $\phi/M_{\pi} < 1/\sqrt{c}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{\text{end}} < 1$. See Figs. 324 to 326 for other values of $c$ and $\phi_0$.</figcaption></figure>
<figure><img src="image_327.png" /><figcaption>**Fig. 324.** Reheating consistent slow-roll predictions for the running mass inflation 1 models ($c > 0$, $x < 1$) with $c = 0.02$ and $\phi_0/M_{\text{Pl}} = 7$ (which satisfies $\phi/M_{\text{Pl}} < 1/\sqrt{c}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{\text{end}} < 1$.</figcaption></figure>
<figure><img src="image_328.png" /><figcaption>Fig. 325. Reheating consistent slow-roll predictions for the running mass inflation 1 models ($c > 0$, $x < 1$) with $c = 0.04$ and $\phi_0/M_{\text{Pl}} = 2$ (which satisfies $\phi/M_{\text{Pl}} < 1/\sqrt{c}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{\text{end}} < 1$.</figcaption></figure>
<figure><img src="image_329.png" /><figcaption>**Fig. 326.** Reheating consistent slow-roll predictions for the running mass inflation 1 models ($c > 0, x < 1$) with $c = 0.04$ and $\phi_c/M_{\text{Pl}} \to 5$ (which saturates $\phi/M_{\text{Pl}} < 1/\sqrt{c}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{\text{end}} < 1$.</figcaption></figure>
A.71. Running Mass Inflation 2 (RMI2)

See Figs. 327–330.

<figure><img src="image_330.png" /><figcaption>Fig. 327. Reheating consistent slow-roll predictions for the running mass inflation 2 models ($c > 0, x > 1$) with $c = 0.005$ and $\phi_0/M_n = 3$ (which satisfies $\phi_0/M_n < 1/\sqrt{c}$), in the plane $(n_s, r)$ (top panel) and the plane $(c_1, c_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < e$. See Figs. 328 to 330 for other values of $c$ and $\phi_0$.</figcaption></figure>
<figure><img src="image_331.png" /><figcaption>**Fig. 328.** Reheating consistent slow-roll predictions for the running mass inflation 2 models ($c > 0, x > 1$) with $c = 0.005$ and $\phi_>/M_{\text{Pl}} = 10$ (which satisfies $\phi_>/M_{\text{Pl}} < 1/\sqrt{c}$), in the plane $(n, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < e$.</figcaption></figure>
<figure><img src="image_332.png" /><figcaption>**Fig. 329.** Reheating consistent slow-roll predictions for the running mass inflation 2 models ($c > 0, x > 1$) with $c = 0.01$ and $\phi_*/M_{\text{Pl}} = 5$ (which satisfies $\phi_*/M_{\text{Pl}} < 1/\sqrt{c}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < e$.</figcaption></figure>
<figure><img src="image_333.png" /><figcaption>**Fig. 330.** Reheating consistent slow-roll predictions for the running mass inflation 2 models ($c > 0, x > 1$) with $c = 0.01$ and $\phi_0/M_{\text{pl}} \to 10$ (which saturates $\phi_0/M_{\text{pl}} < 1/\sqrt{c}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < e$.</figcaption></figure>
A.72. Running Mass Inflation 3 (RMI3)

See Figs. 331–334.

<figure><img src="image_334.png" /><figcaption>**Fig. 331.** Reheating consistent slow-roll predictions for the running mass inflation 3 models ($c < 0$, $x < 1$) with $c = -0.01$ and $\phi_e/M_{pl} = 8$ (which satisfies $\phi_e/M_{pl} < 1/\sqrt{-c}$) in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{end} < 1$. See Figs. 332 to 334 for other values of $c$ and $\phi_e$.</figcaption></figure>
<figure><img src="image_335.png" /><figcaption>**Fig. 332.** Reheating consistent slow-roll predictions for the running mass inflation 3 models ($c < 0, x < 1$) with $c = -0.01$ and $\phi_n/M_n \to 10$ (which saturates $\phi_s/M_s < 1/\sqrt{-c}$) in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{\text{end}} < 1$.</figcaption></figure>
<figure><img src="image_336.png" /><figcaption>Fig. 333. Reheating consistent slow-roll predictions for the running mass inflation 3 models ($c < 0$, $x < 1$) with $c = -0.02$ and $\phi_c/M_n = 5$ (which satisfies $\phi_c/M_n < 1/\sqrt{-c}$) in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{\text{end}} < 1$.</figcaption></figure>
<figure><img src="image_337.png" /><figcaption>**Fig. 334.** Reheating consistent slow-roll predictions for the running mass inflation 3 models ($c < 0$, $x < 1$) with $c = -0.02$ and $\phi_e/M_n = 7$ (which satisfies $\phi_e/M_n < 1/\sqrt{-c}$) in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1/e < x_{\text{end}} < 1$.</figcaption></figure>
A.73. Running Mass Inflation 4 (RMI4)

See Figs. 335–338.

<figure><img src="image_338.png" /><figcaption>Fig. 335. Reheating consistent slow-roll predictions for the running mass inflation 4 models ($c < 0, x > 1$) with $c = -0.01$ and $\phi_c/M_n = 2$ (which satisfies $\phi_c/M_n < 1/\sqrt{-c}$) in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < c$. See Figs. 336 to 338 for other values of $c$ and $\phi_u$.</figcaption></figure>
<figure><img src="image_339.png" /><figcaption>**Fig. 336.** Reheating consistent slow-roll predictions for the running mass inflation 4 models ($c < 0, x > 1$) with $c = -0.01$ and $\phi_a/M_{\pi} \to 10$ (which saturates $\phi_a/M_{\pi} < 1/\sqrt{-c}$) in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < e$.</figcaption></figure>
<figure><img src="image_340.png" /><figcaption>**Fig. 337.** Reheating consistent slow-roll predictions for the running mass inflation 4 models ($c < 0, x > 1$) with $c = -0.02$ and $\phi_e/M_p = 2$ (which satisfies $\phi_e/M_p < 1/\sqrt{-c}$) in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < e$.</figcaption></figure>
<figure><img src="image_341.png" /><figcaption>**Fig. 338.** Reheating consistent slow-roll predictions for the running mass inflation 4 models ($c < 0, x > 1$) with $c = -0.02$ and $\phi_c/M_{\text{pl}} = 7$ (which satisfies $\phi_c/M_{\text{pl}} < 1/\sqrt{-c}$) in the plane $(n_c, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied in the range $1 < x_{\text{end}} < e$.</figcaption></figure>
A.74. Valley Hybrid Inflation (VHI)

See Figs. 339–348.

<figure><img src="image_342.png" /><figcaption>Fig. 339. Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 0.5$ and $\mu/M_{\phi} = 10^{-2}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See Figs. 340 to 348 for other values of $p$ and $\mu$.</figcaption></figure>
<figure><img src="image_343.png" /><figcaption>**Fig. 340.** Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 0.5$ and $\mu/M_{\pi} = 20$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_344.png" /><figcaption>**Fig. 341.** Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 1$ and $\mu/M_{\text{pl}} = 10^{-1}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions are degenerated along the curve $\epsilon_2 = 4\epsilon_1$, see also Fig. 342.</figcaption></figure>
<figure><img src="image_345.png" /><figcaption>**Fig. 342.** Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 1$ and $\mu/M_{\text{pl}} = 2$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions are degenerated along the curve $\epsilon_2 = 4\epsilon_1$, see also Fig. 341.</figcaption></figure>
<figure><img src="image_346.png" /><figcaption>Fig. 343. Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 1.5$ and $\mu = M_{\pi}$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_347.png" /><figcaption>Fig. 344. Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 1.5$ and $\mu/M_{\text{Pl}} = 5$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_348.png" /><figcaption>Fig. 345. Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 2$ and $\mu/M_{\text{pl}} = 0.8$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_349.png" /><figcaption>**Fig. 346.** Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 2$ and $\mu/M_{P_1} = 8$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_350.png" /><figcaption>Fig. 347. Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 3$ and $\mu/M_{P} = 5$, in the plane $(n_{s}, r)$ (top panel) and the plane $(\epsilon_{1}, \epsilon_{2})$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_351.png" /><figcaption>Fig. 348. Reheating consistent slow-roll predictions for the valley hybrid inflation models with $p = 3$ and $\mu/M_{Pl} = 10$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.75. Dynamical Supersymmetric Inflation (DSI)

See Figs. 349–354.

<figure><img src="image_352.png" /><figcaption>**Fig. 349.** Reheating consistent slow-roll predictions for the dynamical supersymmetric inflation models with $p = 2$ and $\mu/M_{pl} = 7 \times 10^{-8}$ (which satisfies $\mu < \mu_{max}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied within its maximal allowed range, i.e. with $\dot{x}_{end} \equiv (x_{end} - x_{end}^{\min})/(x_{end}^{\max} - x_{end}^{\min})$ in the domain $[0, 1]$. See Figs. 350 to 354 for other values of $p$ and $\mu$.</figcaption></figure>
<figure><img src="image_353.png" /><figcaption>**Fig. 350.** Reheating consistent slow-roll predictions for the dynamical supersymmetric inflation models with $p = 2$ and $\mu/M_{pl} = 3.5 \times 10^{-5}$ (which satisfies $\mu < \mu_{max}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied within its maximal allowed range, i.e. with $\tilde{x}_{\text{end}} \equiv (x_{\text{end}} - x_{\text{end}}^{\text{min}})/(x_{\text{end}}^{\text{max}} - x_{\text{end}}^{\text{min}})$ in the domain $[0, 1]$.</figcaption></figure>
<figure><img src="image_354.png" /><figcaption>**Fig. 351.** Reheating consistent slow-roll predictions for the dynamical supersymmetric inflation models with $p = 3$ and $\mu/M_{Pl} = 4.1 \times 10^{-7}$ (which satisfies $\mu < \mu_{max}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied within its maximal allowed range, i.e. with $\hat{x}_{end} \equiv (x_{end} - x_{end}^{\min})/(x_{end}^{\max} - x_{end}^{\min})$ in the domain $[0, 1]$.</figcaption></figure>
<figure><img src="image_355.png" /><figcaption>**Fig. 352.** Reheating consistent slow-roll predictions for the dynamical supersymmetric inflation models with $p = 3$ and $\mu/M_p = 2 \times 10^{-5}$ (which satisfies $\mu < \mu_{max}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied within its maximal allowed range, i.e. with $\hat{x}_{end} \equiv (x_{end} - x_{end}^{\min})/(x_{end}^{\max} - x_{end}^{\min})$ in the domain $[0, 1]$.</figcaption></figure>
<figure><img src="image_356.png" /><figcaption>Fig. 353. Reheating consistent slow-roll predictions for the dynamical supersymmetric inflation models with $p = 4$ and $\mu/M_{pl} = 10^{-6}$ (which satisfies $\mu < \mu_{max}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied within its maximal allowed range, i.e. with $\tilde{x}_{end} \equiv (x_{end} - x_{end}^{\min})/(x_{end}^{\max} - x_{end}^{\min})$ in the domain $[0, 1]$.</figcaption></figure>
<figure><img src="image_357.png" /><figcaption>**Fig. 354.** Reheating consistent slow-roll predictions for the dynamical supersymmetric inflation models with $p = 4$ and $\mu/M_{pl} = 10^{-6}$ (which satisfies $\mu < \mu_{max}$), in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The field value at which inflation ends is varied within its maximal allowed range, i.e. with $\tilde{x}_{\text{end}} \equiv (x_{\text{end}} - x_{\text{end}}^{\text{min}})/(x_{\text{end}}^{\text{max}} - x_{\text{end}}^{\text{min}})$ in the domain $[0, 1]$.</figcaption></figure>
A.76. Generalized Mixed Inflation (GMLFI)

See Figs. 355–357.

<figure><img src="image_358.png" /><figcaption>**Fig. 355.** Reheating consistent slow-roll predictions for the generalized mixed inflation models with $q = 1$ and $p = 2$, in the plane $(n_c, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_359.png" /><figcaption>Fig. 356. Reheating consistent slow-roll predictions for the generalized mixed inflation models with $q = 3$ and $p = 2$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_360.png" /><figcaption>Fig. 357. Reheating consistent slow-roll predictions for the generalized mixed inflation models with $q = 2$ and $p = 3$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.77. Logarithmic Potential Inflation 1 (LPI1)

See Figs. 358–360.

<figure><img src="image_361.png" /><figcaption>**Fig. 358.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 1 models for $q = 1$ and $p = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See Figs. 359 and 359 for other values of $q$.</figcaption></figure>
<figure><img src="image_362.png" /><figcaption>**Fig. 359.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 1 models for $q = 2$ and $p = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_363.png" /><figcaption>**Fig. 360.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 1 models for $q = 3$ and $p = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.78. Logarithmic Potential Inflation 2 (LPI2)

See Figs. 361–363.

<figure><img src="image_364.png" /><figcaption>Fig. 361. Reheating consistent slow-roll predictions for the logarithmic potential inflation 2 models for $p = 1$ and $q = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_365.png" /><figcaption>**Fig. 362.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 2 models for $p = 2$ and $q = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_366.png" /><figcaption>**Fig. 363.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 2 models for $p = 3$ and $q = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.79. Logarithmic Potential Inflation 3 (LPI3)

See Figs. 364–366.

<figure><img src="image_367.png" /><figcaption>**Fig. 364.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 3 models for $p = 1$ and $q = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_368.png" /><figcaption>**Fig. 365.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 3 models for $p = 2$ and $q = 2$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_369.png" /><figcaption>**Fig. 366.** Reheating consistent slow-roll predictions for the logarithmic potential inflation 3 models for $p = 3$ and $q = 4$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.80. Constant $n_s$ D Inflation (CNDI)

See Figs. 367–372.

<figure><img src="image_370.png" /><figcaption>Fig. 367. Reheating consistent slow-roll predictions for the constant $n_s$ D inflation models for $\alpha = 10^{-2}$ and $\beta = 5$, in the plane $(\epsilon_1, \epsilon_2)$ (top panel) and the plane $(\epsilon_1, r)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions match well the constant spectral index value $n_s = 1 + 4a^2\bar{\beta}/(\bar{\beta} + 1)$, see also Fig. 368.</figcaption></figure>
<figure><img src="image_371.png" /><figcaption>**Fig. 368.** Reheating consistent slow-roll predictions for the constant $n_s$ D inflation models for $\alpha = 10^{-1}$ and $\beta = 5$, in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). The model predictions match well the constant spectral index value $n_s = 1 + 4a^2\beta / (\beta + 1)$, see also Fig. 367.</figcaption></figure>
<figure><img src="image_372.png" /><figcaption>**Fig. 369.** Reheating consistent slow-roll predictions for the constant $n_s$ D inflation models for $\alpha = 0.25$ and $\beta = 0.1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). At large values of $x_{\text{end}}$, the model predictions deviate significantly from $n_s = 1 + 4\alpha^2\beta/(\beta+1)$. See Figs. 370 to 372 for other values of $\alpha$.</figcaption></figure>
<figure><img src="image_373.png" /><figcaption>**Fig. 370.** Reheating consistent slow-roll predictions for the constant $n_s$ D inflation models for $\alpha = 0.30$ and $\beta = 0.1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). At large values of $x_{\text{end}}$, the model predictions deviate significantly from $n_s = 1 + 4a^2\beta/(\beta + 1)$.</figcaption></figure>
<figure><img src="image_374.png" /><figcaption>**Fig. 371.** Reheating consistent slow-roll predictions for the constant $n_s$ D inflation models for $\alpha = 0.35$ and $\beta = 0.1$ in the plane $(n_s, r)$ (top panel) and the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). At large values of $x_{\text{end}}$, the model predictions deviate significantly from $n_s = 1 + 4\alpha^2\beta/(\beta+1)$.</figcaption></figure>
<figure><img src="image_375.png" /><figcaption>**Fig. 372.** Reheating consistent slow-roll predictions for the constant $n_s$ D inflation models for $\alpha = 0.40$ and $\beta = 0.1$ in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). At large values of $x_{\text{end}}$, the model predictions deviate significantly from $n_s = 1 + 4\alpha^2\beta/(\beta+1)$.</figcaption></figure>
A.81. String Axion Inflation II 1 (SAIII1)

See Figs. 373–384.

<figure><img src="image_376.png" /><figcaption>Fig. 373. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII1 regime and at a negative value of $\beta = -1.3$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 374.</figcaption></figure>
<figure><img src="image_377.png" /><figcaption>Fig. 374. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII1 regime and at a negative value of $\beta = -1.3$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_378.png" /><figcaption>Fig. 375. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII regime and at a negative value of $\beta = -0.68$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 376.</figcaption></figure>
<figure><img src="image_379.png" /><figcaption>Fig. 376. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII regime and at a negative value of $\beta = -0.68$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_380.png" /><figcaption>Fig. 377. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII regime and at a small negative value of $\beta = -0.05$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 378.</figcaption></figure>
<figure><img src="image_381.png" /><figcaption>Fig. 378. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII regime and at a small negative value of $\beta = -0.05$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_382.png" /><figcaption>Fig. 379. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII regime and at a small positive value of $\beta = 0.05$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 380.</figcaption></figure>
<figure><img src="image_383.png" /><figcaption>**Fig. 380.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII regime and at a small positive value of $\beta = 0.05$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_384.png" /><figcaption>Fig. 381. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIIII regime and at a positive value of $\beta = 0.68$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 382.</figcaption></figure>
<figure><img src="image_385.png" /><figcaption>Fig. 382. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIIII regime and at a positive value of $\beta = 0.68$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_386.png" /><figcaption>**Fig. 383.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII1 regime and at a positive value of $\beta = 1.3$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 384.</figcaption></figure>
<figure><img src="image_387.png" /><figcaption>Fig. 384. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII1 regime and at a positive value of $\beta = 1.3$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.82. String Axion Inflation II 2 (SAIII2)

See Figs. 385–396.

<figure><img src="image_388.png" /><figcaption>Fig. 385. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -0.23$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 386.</figcaption></figure>
<figure><img src="image_389.png" /><figcaption>Fig. 386. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -0.23$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_390.png" /><figcaption>Fig. 387. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -0.13$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 388.</figcaption></figure>
<figure><img src="image_391.png" /><figcaption>Fig. 388. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -0.13$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_392.png" /><figcaption>Fig. 389. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a small negative value of $\beta = -0.02$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 390.</figcaption></figure>
<figure><img src="image_393.png" /><figcaption>Fig. 390. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a small negative value of $\beta = -0.02$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_394.png" /><figcaption>**Fig. 391.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a small positive value of $\beta = 0.02$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 392.</figcaption></figure>
<figure><img src="image_395.png" /><figcaption>Fig. 392. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a small positive value of $\beta = 0.02$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_396.png" /><figcaption>Fig. 393. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a positive value of $\beta = 0.21$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 394.</figcaption></figure>
<figure><img src="image_397.png" /><figcaption>Fig. 394. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a positive value of $\beta = 0.21$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_398.png" /><figcaption>Fig. 395. Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a positive value of $\beta = 0.39$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 396.</figcaption></figure>
<figure><img src="image_399.png" /><figcaption>**Fig. 396.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a positive value of $\beta = 0.39$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.83. String Axion Inflation II 3 (SAIII3)

See Figs. 397–408.

<figure><img src="image_400.png" /><figcaption>Fig. 397: Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII3 regime and at a large negative value of $\beta = -2$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Notice the strong dependency of the predictions with respect to $\mu$. This is due to the modulations of the potential, a small change in the value of $x_{\text{end}}$ may produce drastic modifications of the observable model predictions. See also Fig. 398.</figcaption></figure>
<figure><img src="image_401.png" /><figcaption>**Fig. 398.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a large negative value of $\beta = -2$. Predictions are represented in the plane $(n_i, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_402.png" /><figcaption>**Fig. 399.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -1.5$. Predictions are represented in the plane $(n_i, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 400.</figcaption></figure>
<figure><img src="image_403.png" /><figcaption>**Fig. 400.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -1.5$. Predictions are represented in the plane $(n_i, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_404.png" /><figcaption>**Fig. 401.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -1$. Predictions are represented in the plane $(n_i, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 402.</figcaption></figure>
<figure><img src="image_405.png" /><figcaption>**Fig. 402.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII2 regime and at a negative value of $\beta = -1$. Predictions are represented in the plane $(n_i, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_406.png" /><figcaption>**Fig. 403.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII3 regime and at a positive value of $\beta = 1.6$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). Notice the strong dependency of the predictions with respect to $\mu$. This is due to the modulations of the potential, a small change in the value of $x_{\text{end}}$ may produce drastic modifications of the observable model predictions. See also Fig. 404.</figcaption></figure>
<figure><img src="image_407.png" /><figcaption>**Fig. 404.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII3 regime and at a positive value of $\beta = 1.6$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_408.png" /><figcaption>**Fig. 405.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII3 regime and at a positive value of $\beta = 4.7$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 406.</figcaption></figure>
<figure><img src="image_409.png" /><figcaption>**Fig. 406.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII3 regime and at a positive value of $\beta = 4.7$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_410.png" /><figcaption>**Fig. 407.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII3 regime and at a large positive value of $\beta = 7.8$. Predictions are represented in the plane $(n_i, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll), see also Fig. 408.</figcaption></figure>
<figure><img src="image_411.png" /><figcaption>**Fig. 408.** Reheating consistent slow-roll predictions for the String Axion Inflation II models, in the SAIII3 regime and at a large positive value of $\rho = 7.8$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.84. Radiatively Corrected Large Field Inflation 1 (RCLFI1)

See Figs. 409–420.

<figure><img src="image_412.png" /><figcaption>**Fig. 409.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p > 4$ and $\alpha < -[p(p-4)/4]\exp(2-p/4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 410 to 412 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_413.png" /><figcaption>**Fig. 410.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLF11 regime, for $p > 4$ and $\alpha < -[p(p-4)/4]\exp(2-p/4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_414.png" /><figcaption>**Fig. 411.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p > 4$ and $\alpha < -[p(p-4)/4]\exp(2-p/4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_415.png" /><figcaption>**Fig. 412.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p > 4$ and $\alpha < -[p(p-4)/4]\exp(2-p/4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_416.png" /><figcaption>Fig. 413. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\tilde{\psi}$ $\mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 414 to 416 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_417.png" /><figcaption>Fig. 414. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_418.png" /><figcaption>**Fig. 415.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_419.png" /><figcaption>Fig. 416. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_420.png" /><figcaption>**Fig. 417.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI1 regime, for $p < 4$ and $\alpha > -[p(p-4)/4]\exp(2-4/p) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 418 to 420 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_421.png" /><figcaption>**Fig. 418.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLF1 regime, for $p < 4$ and $\alpha > -[p(p-4)/4]\exp(2-4/p) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_422.png" /><figcaption>**Fig. 419.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLF1 regime, for $p < 4$ and $\alpha > -[p(p-4)/4]\exp(2-4/p) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_423.png" /><figcaption>**Fig. 420.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLF1 regime, for $p < 4$ and $\alpha > -[p(p-4)/4]\exp(2-4/p) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.85. Radiatively Corrected Large Field Inflation 2 (RCLFI2)

See Figs. 421–432.

<figure><img src="image_424.png" /><figcaption>Fig. 421. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 422 to 424 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_425.png" /><figcaption>**Fig. 422.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_426.png" /><figcaption>**Fig. 423.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_427.png" /><figcaption>**Fig. 424.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_428.png" /><figcaption>Fig. 425. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\tilde{\mu}$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 426 to 428 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_429.png" /><figcaption>**Fig. 426.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_430.png" /><figcaption>**Fig. 427.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_431.png" /><figcaption>**Fig. 428.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_432.png" /><figcaption>**Fig. 429.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 430 to 432 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_433.png" /><figcaption>**Fig. 430.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_434.png" /><figcaption>**Fig. 431.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_435.png" /><figcaption>**Fig. 432.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI2 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.86. Radiatively Corrected Large Field Inflation 3 (RCLFI3)

See Figs. 433–444.

<figure><img src="image_436.png" /><figcaption>**Fig. 433.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 434 to 436 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_437.png" /><figcaption>**Fig. 434.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_438.png" /><figcaption>Fig. 435. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_439.png" /><figcaption>**Fig. 436.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_440.png" /><figcaption>Fig. 437. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 438 to 440 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_441.png" /><figcaption>**Fig. 438.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_442.png" /><figcaption>**Fig. 439.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_443.png" /><figcaption>**Fig. 440.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p > 4$ and $\alpha < -e(p-4) < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_444.png" /><figcaption>Fig. 441. Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 442 to 444 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_445.png" /><figcaption>**Fig. 442.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_446.png" /><figcaption>**Fig. 443.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_447.png" /><figcaption>**Fig. 444.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI3 regime, for $p < 4$ and $\alpha > -e(p-4) > 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.87. Radiatively Corrected Large Field Inflation 4 (RCLFI4)

See Figs. 445–452.

<figure><img src="image_448.png" /><figcaption>**Fig. 445.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI4 regime, for $p > 4$ and $-[p(p-4)/4]\exp(2-p/4) < \alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{rev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 446 to 448 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_449.png" /><figcaption>**Fig. 446.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI4 regime, for $p > 4$ and $-[p(p-4)/4]\exp(2-p/4) < \alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_450.png" /><figcaption>**Fig. 447.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI4 regime, for $p > 4$ and $-[p(p-4)/4]\exp(2-p/4) < \alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_451.png" /><figcaption>**Fig. 448.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI4 regime, for $p > 4$ and $-[p(p-4)/4]\exp(2-p/4) < \alpha < 0$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_452.png" /><figcaption>**Fig. 449.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI4 regime, for $p < 4$ and $0 < \alpha < -[p(p-4)/4]\exp(2-p/4)$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } \mu$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 450 to 452 for other values of $p$ and $\alpha$.</figcaption></figure>
<figure><img src="image_453.png" /><figcaption>**Fig. 450.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLF14 regime, for $p < 4$ and $0 < \alpha < -[p(p-4)/4]\exp(2-p/4)$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_454.png" /><figcaption>**Fig. 451.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI4 regime, for $p < 4$ and $0 < \alpha < -[p(p-4)/4]\exp(2-p/4)$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_455.png" /><figcaption>**Fig. 452.** Reheating consistent slow-roll predictions for the Radiatively Corrected Large Field Inflation models, in the RCLFI4 regime, for $p < 4$ and $0 < \alpha < -[p(p-4)/4]\exp(2-p/4)$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.88. Non-Renormalizable Corrected Loop Inflation (NCLI)

See Figs. 453–456.

<figure><img src="image_456.png" /><figcaption>**Fig. 453.** Reheating consistent slow-roll predictions for the Non-Renormalizable Corrected Loop Inflation models, for $n = 2$ and $\alpha = 10^{-4}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 454 to 456 for other values of $\alpha$ and $n$.</figcaption></figure>
<figure><img src="image_457.png" /><figcaption>**Fig. 454.** Reheating consistent slow-roll predictions for the Non-Renormalizable Corrected Loop Inflation models, for $n = 2$ and $\alpha = 10^{-6}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_458.png" /><figcaption>**Fig. 455.** Reheating consistent slow-roll predictions for the Non-Renormalizable Corrected Loop Inflation models, for $n = 3$ and $\alpha = 10^{-4}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_459.png" /><figcaption>**Fig. 456.** Reheating consistent slow-roll predictions for the Non-Renormalizable Corrected Loop Inflation models, for $n = 3$ and $\alpha = 10^{-6}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel). The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.89. Hybrid Natural Inflation 1 (HNI1)

See Figs. 457–460.

<figure><img src="image_460.png" /><figcaption>**Fig. 457.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 1 and for $1 - \alpha = 9.6 \times 10^{-5}$ (inflation gracefully ends $\alpha > \alpha_1$). Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } f$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 458 to 460 for other values of $\alpha$.</figcaption></figure>
<figure><img src="image_461.png" /><figcaption>**Fig. 458.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 1 and for $1 - \alpha = 3.4 \times 10^{-3}$ (inflation gracefully ends $\alpha > \alpha_1$). Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } f$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 458 to 460 for other values of $\alpha$.</figcaption></figure>
<figure><img src="image_462.png" /><figcaption>**Fig. 459.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 1 and for $1 - \alpha = 6.7 \times 10^{-5}$ (inflation gracefully ends $\alpha > \alpha_1$). Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } f$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_463.png" /><figcaption>**Fig. 460.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 1 and for $1 - \alpha = 10^{-2}$ (inflation gracefully ends $\alpha > \alpha_1$). Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the field $\text{vev } f$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.90. Hybrid Natural Inflation 2 (HNI2)

See Figs. 461–468.

<figure><img src="image_464.png" /><figcaption>Fig. 461. Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.1$ and $f = 1.5M_p$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 462 to 468 for other values of $\alpha$ and $f$.</figcaption></figure>
<figure><img src="image_465.png" /><figcaption>**Fig. 462.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.1$ and $f = 4.3 M_p$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_466.png" /><figcaption>**Fig. 463.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.1$ and $f = 12M_p$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_467.png" /><figcaption>**Fig. 464.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.54$ and $f = 1.5 M_{\text{pl}}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_468.png" /><figcaption>**Fig. 465.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.54$ and $f = 4.3 M_\odot$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_469.png" /><figcaption>**Fig. 466.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.54$ and $f = 12M_{\text{Pl}}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_470.png" /><figcaption>**Fig. 467.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.97$ and $f = 4.3 M_{\text{Pl}}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_471.png" /><figcaption>**Fig. 468.** Reheating consistent slow-roll predictions for Hybrid Natural Inflation 2 and for $\alpha = 0.97$ and $f = 12M_{\text{pl}}$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various field values $x_{\text{end}}$ at which the instability ends inflation. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.91. N-Formalism Inflation 1 (NFI1)

See Figs. 469–471.

<figure><img src="image_472.png" /><figcaption>**Fig. 469.** Reheating consistent slow-roll predictions for N-Formalism Inflation 1 with $b = 3$ (inflation gracefully ends). Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the parameter $a$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 470 to 471 for other values of $b$.</figcaption></figure>
<figure><img src="image_473.png" /><figcaption>**Fig. 470.** Reheating consistent slow-roll predictions for N-Formalism Inflation 1 with $b = 3.5$ (inflation gracefully ends). Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the parameter $a$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
<figure><img src="image_474.png" /><figcaption>**Fig. 471.** Reheating consistent slow-roll predictions for N-Formalism Inflation 1 with $b = 4.5$ (inflation gracefully ends). Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the parameter $a$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>
A.92. N-Formalism Inflation 2 (NFI2)

See Figs. 472–475.

<figure><img src="image_475.png" /><figcaption>**Fig. 472.** Reheating consistent slow-roll predictions for N-Formalism Inflation 2 with $a = -0.2$ and $b = 2.5$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the normalized field values $\dot{x}_{\text{end}}$ at which inflation ends. This one is varied within its maximal allowed range, i.e. with $\dot{x}_{\text{end}} \equiv (x_{\text{end}} - x_{\text{end}}^{\text{min}})/(x_{\text{end}}^{\text{max}} - x_{\text{end}}^{\text{min}})$ in the domain $[0, 1]$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll). See also Figs. 473 to 475 for other values of $(a, b)$.</figcaption></figure>
<figure><img src="image_476.png" /><figcaption>**Fig. 473.** Reheating consistent slow-roll predictions for N-Formalism Inflation 2 with $a = -0.01$ and $b = 2.5$. Predictions are represented in the plane $(n_s, r)$ (top panel) and in the plane $(\epsilon_1, \epsilon_2)$ (bottom panel) for various values of the normalized field values $\tilde{x}_{\text{end}}$ at which inflation ends. This one is varied within its maximal allowed range, i.e. with $\tilde{x}_{\text{end}} \equiv (x_{\text{end}} - x_{\text{end}}^{\text{min}})/(x_{\text{end}}^{\text{max}} - x_{\text{end}}^{\text{min}})$ in the domain $[0, 1]$. The solid contours are the one and two-sigma Planck 2018 + Bicep-Keck confidence intervals (marginalized over second order slow-roll).</figcaption></figure>