Large NLO corrections in tt¯W±\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}{W}^{\pm } $$\end{document} and tt¯tt¯\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}t\overline{t} $$\end{document} hadroproduction from supposedly subleading EW contributions

We calculate the complete-NLO predictions for tt¯W±\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}{W}^{\pm } $$\end{document} and tt¯tt¯\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}t\overline{t} $$\end{document} production in proton-proton collisions at 13 and 100 TeV. All the non-vanishing contributions of Oαsiαj\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s^i{\alpha}^j\right) $$\end{document} with i + j = 3, 4 for tt¯W±\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}{W}^{\pm } $$\end{document} and i + j = 4, 5 for tt¯tt¯\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}t\overline{t} $$\end{document} are evaluated without any approximation. For tt¯W±\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}{W}^{\pm } $$\end{document} we find that, due to the presence of tW → tW scattering, at 13(100) TeV the Oαsα3\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s{\alpha}^3\right) $$\end{document} contribution is about 12(70)% of the LO, i.e., it is larger than the so-called NLO EW corrections (the Oαs2α2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s^2{\alpha}^2\right) $$\end{document} terms) and has opposite sign. In the case of tt¯tt¯\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ t\overline{t}t\overline{t} $$\end{document} production, large contributions from electroweak tt → tt scattering are already present at LO in the Oαs3α\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s^3\alpha \right) $$\end{document} and Oαs2α2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s^2{\alpha}^2\right) $$\end{document} terms. For the same reason we find that both NLO terms of Oαs4α\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s^4\alpha \right) $$\end{document}, i.e., the NLO EW corrections, and Oαs3α2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s^3{\alpha}^2\right) $$\end{document} are large (±15% of the LO) and their relative contributions strongly depend on the values of the renormalisation and factorisation scales. However, large accidental cancellations are present (away from the threshold region) between these two contributions. Moreover, the NLO corrections strongly depend on the kinematics and are particularly large at the threshold, where even the relative contribution from Oαs2α3\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{O}\left({\alpha}_s^2{\alpha}^3\right) $$\end{document} terms amounts to tens of percents.


JHEP02(2018)031
to different kinds of effects such as weak Sudakov enhancements or collinear photon finalstate-radiation (FSR) in sufficiently exclusive observables. Thus, they have to be taken into account for a reliable comparison to data. For many production processes at the LHC, also next-to-NLO (NNLO) QCD corrections, the O(α i+2 s α j ) contributions, are essential and indeed many calculations have appeared in the recent years (see, e.g., ref. [22] and references therein). Even the next-to-NNLO (N 3 LO) QCD calculation for the Higgs production cross section is now available [23,24].
From a technical point of view, NLO QCD and EW corrections are simpler than NNLO corrections; they involve at most one loop or one additional radiated parton more than the LO calculation. However, they are not the only perturbative orders sharing this feature. Already starting from 2 → 2 processes with coloured and EW-charged initialand final-state particles, such as dijet or top-quark pair hadroproduction, additional NLO terms appears. For these two processes, one-loop and real-emission corrections in the SM involve also O(α s α 2 ) and O(α 3 ) terms, which are neither part of the NLO QCD corrections nor of the NLO EW ones. Moreover, Born diagrams originate also O(α s α) and O(α 2 ) contributions, which are typically not included in LO predictions. The sum of all these contributions yields the prediction at "complete-NLO" accuracy.
The complete-NLO results for dijet production at the LHC have been calculated in ref. [19] and for top-quark pair production in ref. [25], the latter also combined with NNLO QCD corrections. Although one-loop contributions that are not part of NLO QCD and NLO EW corrections are present for many production processes at the LHC, calculations at this level of accuracy are rare, and those performed for dijet and top-quark pair production represent an exception. The reason is twofold. First, being higher-order effects and α/α s ∼ 0.1 these corrections are expected to be smaller than standard NLO EW ones, and indeed they are for the case of dijet and top-quark pair production. Second, only with the recent automation of the calculation of EW corrections the necessary effort for calculating these additional orders has been reduced and therefore justified given their expected smallness. Besides these reasons, in the subleading orders there can be new production mechanisms and care has to be taken to avoid process overlap. For example, the O(α 2 ) contribution to dijet production contains hadronically decaying heavy vector bosons.
To our knowledge, the only other calculation where all the NLO effects beyond the NLO QCD and NLO EW accuracy have been considered is the case of vector-boson-scattering (VBS) for two positively charged W bosons at the LHC including leptonic decays, namely the pp → µ + ν µ e + ν e jj process [26]. This complete-NLO prediction includes all the terms of O(α i s α j ) with i + j = 6, 7 and j ≥ 4, featuring both QCD-induced W + W + jj production and electroweak W + W + scattering. Remarkably, at variance with dijet and top-quark pair production, the expected hierarchy of the different perturbative orders is not respected. Indeed, with proper VBS cuts the O(α 7 ) is by far the largest of the NLO contributions and moreover O(α 7 ) > O(α 6 α s ) > O(α 5 α 2 s ) ∼ O(α 4 α 3 s ). In this article we want to give evidence that what has been found in ref. [26], i.e., large contributions from supposedly subleading corrections, is not an exception due to the particularities of this process [27] and standard VBS selection cuts, which reduce the "QCD backgrounds". It is rather a feature that may appear whenever the process considered -2 -

JHEP02(2018)031
involves the scattering of heavy particles in the SM, namely the W , Z and Higgs bosons, but also top quarks. Indeed, although it is customary to expand in powers of α, for these kind of processes O(α) corrections actually involve enhancements already at the coupling level, e.g., in the interactions among the top-quark, the Higgs boson and the longitudinal polarisations of the W and Z bosons. Thus, the O(α) ∼ 0.01 assumption is in general not valid and the expected hierarchy among perturbative orders may be not respected even at the inclusive level.
Here we focus on the case of the top quark and we explicitly show two different cases in which the expected hierarchy is not respected: the ttW ± and tttt production processes, which are already part of the current physics program at the LHC [28][29][30]. To this purpose we perform the calculation of the complete-NLO predictions of these two processes at 13 and 100 TeV in proton-proton collisions. All the seven O(α i s α j ) contributions with i + j = 3, 4 and j ≥ 1 for ttW ± production and all the eleven O(α i s α j ) contributions with i + j = 4, 5 are calculated exactly without any approximation. For both processes the calculation has been performed in a completely automated way via an extension of the code MadGraph5 aMC@NLO [11]. This extension has already been validated for the NLO EW case in refs. [18,31] and in refs. [19,25] for the calculation of the complete-NLO corrections. The code will soon be released and further documented in a detailed dedicated paper [32].
Complete-NLO corrections involve large contributions for both the ttW ± and tttt production processes, but very different structures underlie the two calculations. Indeed, while large EW effects in ttW ± production originate from the tW → tW scattering, which appears only via NLO corrections, in tttt production large EW effects are already present at LO, due to the electroweak tt → tt scattering.
It has been noted in ref. [33] that EW pp → ttW ± j production involves tW → tW scattering via the gq → ttW ± q channel. Even though ref. [33] focusses on BSM physics in tW → tW scattering, this contribution is sizeable already in the SM and is part of the NLO contributions of O(α s α 3 ) to the inclusive ttW ± production. It is not part of the NLO EW corrections, which are of O(α 2 s α 2 ) and have already been calculated in ref. [18]. However, while in the case of pp → ttW ± j production the final-state jet must be reconstructed, this is not necessary for the inclusive pp → ttW ± process. In fact, we will argue that the tW → tW scattering component can be enhanced over the irreducible background from inclusive ttW ± production by applying a central jet veto.
Recently it was suggested that tttt production can be used as a probe of the top-quark Yukawa coupling (y t ), as discussed in the tree-level analysis presented in ref. [34]. Performing an expansion in power of y t one finds that O(y 2 t ) and O(y 4 t ) contributions to tttt production are not much smaller than purely-QCD induced terms (and in general non-Yukawa induced contributions) and therefore tttt production is quite sensitive to the value of the top Yukawa coupling. Expanding the LO prediction in powers of α, the O(y 2 t ) and O(y 4 t ) terms are fully included in the O(α 3 s α) and O(α 2 s α 2 ) terms. These perturbative orders are even larger than their Yukawa-induced components, and they also feature large cancellations at the inclusive level. It is therefore interesting to compute NLO corrections to all these terms, since we expect them to be large as well. Indeed, we find that they are much larger than the values expected from a naive α s and α power counting. On the other hand, even larger cancellations are present among NLO terms, although not over the whole phase space.

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The structure of the paper is the following. In section 2 we describe the calculations and we introduce a more suitable notation for referring to the various O(α i s α j ) contributions. In section 3 we provide numerical results at the inclusive and differential levels for complete-NLO predictions for proton-proton collisions at 13 and 100 TeV. We discuss in detail the impact of the individual O(α i s α j ) contributions. The common input parameters are described in section 3.1, while pp → ttW ± and pp → tttt results are described in sections 3.2 and 3.3, respectively. Conclusions are given in section 4.
2 Calculation framework for ttW ± and tttt production at complete-NLO Performing an expansion in powers of α s and α, a generic observable for the processes pp → ttW ± (+X) and pp → tttt(+X) can be expressed as respectively, where m and n are positive integer numbers and we have used the notation introduced in refs. [11,17]. For ttW ± production, LO contributions consist of Σ ttW ± m+n+1,n terms with m + n = 2 and are induced by tree-level diagrams only. NLO corrections are given by the terms with m + n = 3 and are induced by the interference of diagrams from the all the possible Born-level and one-loop amplitudes as well all the possible interferences among tree-level diagrams involving one additional quark, gluon or photon emission. Analogously, for tttt production, LO contributions consist of Σ tttt m+n,n terms with m + n = 4 and NLO corrections are given by the terms with m + n = 5. In this work we calculate all the perturbative orders entering at the complete-NLO accuracy, i.e., m + n = 2, 3 for Σ ttW ± (α s , α) and m + n = 4, 5 for Σ tttt (α s , α).
Similarly to ref. [19], we introduce a more user-friendly notation for referring to the different Σ ttW ± m+n+1,n and Σ tttt m+n,n quantities. At LO accuracy, we can denote the ttW ± and tttt observables as Σ ttW ± LO and Σ tttt LO and further redefine the perturbative orders entering these two quantities as In a similar fashion the NLO corrections and their single perturbative orders can be defined as Figure 2. Representative diagrams for theqg → ttW ±q real-emission amplitudes. The left diagram is of O(α 3/2 s α 1/2 ) and leads to log 2 (p 2 T (tt)/m 2 W ) terms in the NLO 1 contribution. The right one is of O(α 1/2 s α 3/2 ), involves the tW → tW scattering and contributes to the NLO 3 .
In the following we will use the symbols Σ (N)LO i or interchangeably their shortened aliases (N)LO i for referring to the different perturbative orders. Clearly the Σ (N)LO i terms in ttW ± production, eqs. (2.3) and (2.5), and in tttt production, eqs. (2.4) and (2.6), are different quantities. One should bear in mind that, usually, with the term "LO" one refers only to LO 1 , which here we will also denote as LO QCD , while an observable at NLO QCD accuracy is Σ LO 1 + Σ NLO 1 , which we will also denote as LO QCD + NLO QCD . The so-called NLO EW corrections which are of O(α) w.r.t. the LO 1 , are the Σ NLO 2 terms, so we will also denote it as NLO EW . Since in this article we will use the (N)LO i notation, the term "LO" will refer to the sum of all the LO i contributions rather than LO 1 alone. The prediction at complete-NLO accuracy, which is the sum of all the LO i and NLO i terms, will be also denoted as "LO + NLO".
We now turn to the description of the structures underlying the calculation of ttW ± and tttt predictions at complete-NLO accuracy. We start with ttW ± production, which is in turn composed by ttW + and ttW − production, and then we move to tttt production.
In ttW + (ttW − )production, tree-level diagrams originate only from ud(ūd) initial states (u and d denote generic up-and down-type quarks), where a W + (W − ) is radiated from the u(d) quark and the tt pair is produced either via a gluon or a photon/Z boson (see figure 1). The former class of diagrams leads to the LO 1 via squared amplitude, the latter to LO 3 . The interference between these two classes of diagrams is absent due to colour, thus LO 2 is analytically zero. Conversely, all the NLO i contributions are non-vanishing. The NLO 1 is in general large, it has been calculated in refs. [10,[35][36][37] and studied in detail in ref. [38], where giant K-factors for the p T (tt) distribution have been found. Large QCD corrections are induced also by the opening of the gq → ttW ± q channels, which depend on the gluon luminosity and are therefore enhanced for high-energy proton-proton collisions. Moreover, the p T (tt) distribution receives an additional log 2 (p 2 T (tt)/m 2 W ) enhancement in the qg initial-state subprocess (see left diagram in figure 2 and ref. [38] for a detailed discussion). Also, the impact of soft-gluon emissions is non-negligible and their resummed contribution has been calculated in refs. [39][40][41] up to next-to-next-to-leading-logarithmic accuracy. The NLO 2 has been calculated for the first time in ref. [18] and further phenomenological studies have been provided in ref. [42]. In a boosted regime, due to Sudakov logarithms, the NLO 2 contribution can be as large as the NLO QCD scale uncertainty.
The NLO 3 and NLO 4 contributions are calculated for the first time here. In particular, the NLO 3 contribution is expected to be sizeable since it contains gq → ttW ± q realemission channels that involve EW tW → tW scattering (see right diagram in figure 2), which as pointed out in ref. [33] can be quite large. Moreover, as in the case of NLO 1 , due to the initial-state gluon this channel becomes even larger by increasing the energy of proton-proton collisions. 1 The tW → tW scattering is present also in the NLO 4 via the γq → ttW ± q , however in this case its contribution is suppressed by a factor α/α s and especially by the smaller luminosity of the photon. In addition to the real radiation of quarks, also the qq → ttW ± g and qq → ttW ± γ processes contribute to the NLO 3 and NLO 4 , respectively. Concerning virtual corrections, the NLO 4 receives contributions only from one-loop amplitudes of O(α 5/2 ), interfering with O(α 3/2 ) Born diagrams. Instead, the NLO 3 receives contributions both from O(α 5/2 ) and O(α s α 3/2 ) one-loop amplitudes interfering with O(α s α 1/2 ) and O(α 3/2 ) Born diagrams, respectively. Clearly, due to the different charges, NLO i terms are different for the ttW + and ttW − case, however, since we did not find large qualitative differences at the numerical level, we provide only inclusive results for ttW ± production. 1 In ttZ(ttH) production the NLO3 contributions feature tH → tH(tZ → tZ) scattering in gq → ttZq(gq → ttHq) real-emission channels. However, at variance with ttW ± production, the gg initial state is available at LOQCD. Thus, the qg luminosity is not giving an enhancement and the relative impact from NLO3 is smaller than in ttW ± production. We now turn to the case of tttt production, whose calculation involves a much higher level of complexity. While the NLO 1 contribution have already been calculated in refs. [11,43] and studied in detail in ref. [38], all the other (N)LO i contributions are calculated for the first time here.
The gg → tttt Born amplitude contains only O(α 2 s ) and O(α s α) diagrams, while the qq → tttt Born amplitude contains also O(α 2 ) diagrams. Thus the gg initial state contributes to LO i with i ≤ 3 and the qq initial states contribute to all the LO i . Also the γg and γγ initial states are available at the Born level; they contributes to LO i with respectively i ≥ 2 and i ≥ 3. However, their contributions are suppressed by the size of the photon parton distribution function (PDF). Representative gg → tttt Born diagrams are shown in figure 3. As already mentioned in the introduction, LO 2 and LO 3 are larger than the values naively expected from α s and α power counting, i.e., LO 2 (α/α s ) × LO QCD and LO 3 (α/α s ) 2 × LO QCD . Thus, NLO 2 , NLO 3 and also NLO 4 are expected to be nonnegligible, especially NLO 2 , NLO 3 because they involve "QCD corrections" 2 to LO 2 and LO 3 contributions, respectively. As discussed in ref. [38], the tttt production cross-section is mainly given by the gg initial state, for this reason we expect LO 4 , (N)LO 5 and NLO 6 to be negligible. Representative gg → tttt one-loop diagrams are shown in figure 4. Although suppressed by the photon luminosity, also the γg and γγ initial states contribute to NLO i with i ≥ 2 and i ≥ 3 respectively, Note that, for both the pp → ttW ± and pp → tttt processes, we do not include the (finite) contributions from the real-emission of heavy particles (W ± , Z and H bosons and top quarks), sometimes called the "heavy-boson-radiation (HBR) contributions". Although they can be formally considered as part of the inclusive predictions at complete-NLO accuracy, these finite contributions are typically small and generally lead to very different collider signatures. 3 Eqs. (2.5) and (2.6) define the NLO corrections in an additive approach. Another possibility would be applying the corrections multiplicatively, which is not uncommon 2 As discussed in ref. [17], this classification of terms entering at a given order is not well defined; some diagrams can be viewed both as a "QCD correction" and an "EW correction" to different tree-level diagrams. Nevertheless, this intuitive classification is useful for understanding the underlying structure of such calculations. For this reason we use these expressions within quotation marks. 3 HBR contributions to NLO2 in ttW ± production have been provided in ref. [18]. when combining NLO QCD and NLO EW corrections. The difference between the two approaches only enters at the NNLO-level and is formally beyond the accuracy of our calculations. The typical example where the multiplicative approach is well-motivated is when the NLO 1 corrections are dominated by soft-QCD physics, and the NLO 2 corrections by large EW Sudakov logarithms. Since these two corrections almost completely factorise, it can be expected that the mixed NNLO O(α s α) corrections to LO 1 are dominated by the product of the O(α s ) and O(α) corrections, i.e., the NLO 1 and NLO 2 contributions. Hence, in this case, the dominant contribution to the mixed NNLO corrections can be taken into account by simply combining NLO corrections in the multiplicative approach. However, for ttW ± production, the NLO 1 terms are dominated by hard radiation, as we argued above. Therefore, even though the NLO 2 is dominated by large Sudakov logarithms, the multiplicative approach leads to uncontrolled NNLO terms. Moreover, due to the opening of the tW → tW scattering, the same would apply also for a multiplicative combination with the NLO 3 . A similar argument is present for tttt production: for i ≤ 3, the NLO i terms are dominated by "QCD corrections" on top of the LO i terms. Since the various LO i have clearly different underlying structures due to the possibility of EW tt → tt scattering, also in this case there is no reason for believing that their NLO corrections factorise at NNLO and therefore that mixed NNLO corrections are dominated by products of NLO i corrections. Hence, for both the pp → ttW ± and pp → tttt processes, not only the multiplicative approach is not leading to improved predictions, but there are clear indications to the fact that this approximation introduces uncontrolled terms. Thus, we use only the additive one. Before discussing the numerical results of the complete-NLO predictions in the next section, we would like to mention that the calculation for tttt production shows a remarkably rich structure for the NLO 3 and NLO 4 contributions. As already said, the qq → tttt Born amplitude contains O(α 2 s ), O(α s α) and O(α 2 ) diagrams, and for this reason, the qq → tttt process contributes to LO 3 via both the square of its O(α s α) Born amplitude and the interference of its O(α 2 s ) and O(α 2 ) Born amplitudes. In order to have such a double structure at the leading order, it is necessary to have at least six external particles that are all coloured and EW interacting at the same time. Since each NLO i is given by "QCD corrections" on top of the LO i and by "EW corrections" on top of the LO i−1 , the NLO 3 and NLO 4 virtual corrections to qq → tttt extend this double structure to three different interference (or squared) terms: two originating from LO 3 and one from either LO 2 (in the case of NLO 3 ) or LO 4 (in the case of NLO 4 ). This is the first time that a calculation with such a triple structure for the virtual corrections has been performed.

Numerical results
In this section, we present numerical results for the complete-NLO predictions for the ttW ± and tttt production processes. As mentioned in the introduction, we used an extension of the MadGraph5 aMC@NLO framework for all our numerical studies. This extension has already been used for the calculation of complete-NLO corrections as already mentioned in the introduction. In MadGraph5 aMC@NLO, infra-red singularities are dealt with via the FKS method [44,45] (automated in the module MadFKS [46,47]). One-loop amplitudes -8 -

Input parameters
In the following we specify the common set of input parameters that are used in the pp → ttW ± and pp → tttt calculations. The masses of the heavy SM particles are set to m t = 173.34 GeV , m H = 125 GeV , m W = 80.385 GeV , m Z = 91.1876 GeV , (3.1) while all the other masses are set equal to zero. We employ the on-shell renormalisation for all the masses and set all the decay widths equal to zero. The renormalisation of α s is performed in the MS-scheme with five active flavours, 4 while the EW input parameters and the associated condition for the renormalisation of α are in the G µ -scheme, with The CKM matrix is set equal to the 3 × 3 unity matrix. We employ dynamical definitions for the renormalisation (µ r ) and factorisation (µ f ) scales. In particular, their common central value µ c is defined as where and m T,i ≡ m 2 i + p 2 T (i) are the transverse masses of the N (+1) final-state particles. Our scale choice for tttt production is motivated by the study in ref. [38]. Theoretical uncertainties due to the scale definition are estimated via the independent variation of µ r and µ f in the interval {µ c /2, 2µ c }. In order to show the scale dependence of (N)LO i /LO QCD relative corrections we will also consider the diagonal variation µ r = µ f , simultaneously in the numerator and the denominator. This scale dependence does not directly indicate scale uncertainties, but it will be very useful in our discussion.
Concerning the PDFs, we use the LUXqed plus PDF4LHC15 nnlo 100 set [57,58], which is in turn based on the PDF4LHC set [59][60][61][62]. This PDF set includes NLO QED effects in the DGLAP evolution and especially the most precise determination of the photon density. Table 1. Cross sections for ttW ± production at 13 TeV in various approximations. The numbers in parentheses are obtained with the jet veto of eq. (3.6) applied.

Results for pp → ttW ± production
We start by presenting predictions for pp → ttW ± total cross sections at 13 and 100 TeV proton-proton collisions with and without applying a jet veto and then we discuss results at the differential level. The total cross sections at 13 TeV for ttW ± production are shown in where also hard photons are considered as a jet. 5 The purpose of this jet veto will become clear in the discussion below. Further details about the size of the individual (N)LO i terms are provide in table 3 (13 TeV) and table 4 (100 TeV), where we show predictions for the quantities where Σ(µ) is simply the total cross section evaluated at the scale µ f = µ r = µ. In tables 3 and 4 we do not show the result for LO 1 ≡ LO QCD , since it is by definition always equal to one, regardless of the value of µ. We want to stress that results in tables 3 and 4 do not show directly scale uncertainties; the value of µ is varied simultaneously in the numerator and the denominator of δ. The purpose of studying δ as a function of µ will become clear below when we discuss the different dependence in δ NLO 1 versus δ NLO 2 and δ NLO 3 . From tables 1 and 2 it can be seen that the LO QCD predictions, both at 13 and 100 TeV, have a scale dependence that is larger than 20%. Including the LO i contributions with i > 1 changes the cross section by about 1% and leaves also the scale dependence almost unchanged. As discussed in section 2, the LO 2 is exactly zero due to colour, thus this small correction is entirely coming from the LO 3 contribution. In tables 3 and 4 it can be seen that NLO 3 11.9 (8.9) 12.2 (9.1) 12.5 (9.3) Table 3. σ (N)LO i /σ LOQCD ratios for ttW ± production at 13 TeV for various values of µ = µ r = µ f . the scale dependence of this LO 3 contribution is slightly different from the LO 1 . The factorisation scale dependence is almost identical for the LO 1 and LO 3 terms (both are qq initiated and have similar kinematic dependence), thus this difference is entirely due to the variation of the renormalisation scale, which, at leading order, only enters the running of α s . The LO 1 has two powers of α s while the LO 3 has none. The value of α s decreases with increasing scales, and therefore, it is no surprise that δ LO 3 increases with larger values for the scales.
As already known, in ttW ± production NLO QCD corrections are large and lead to a reduction of the scale uncertainty. Indeed, for the central scale choice, the total cross section at 13 TeV increases by 50% when including the NLO QCD contribution, and a massive 150% correction is present at 100 TeV. The reduction in the scale dependence is about a factor two for 13 TeV, resulting in an 11% uncertainty. On the other hand, given the large NLO QCD corrections, at 100 TeV the resulting scale dependence at LO QCD + NLO QCD is larger than at 13 TeV, remaining at about 16%. Comparing these pure-QCD predictions to the complete-NLO cross sections (LO + NLO) we see that the latter are about 6% larger at 13 TeV, while the relative scale dependencies are identical. At 100 TeV, even though the relative scale dependence at complete-NLO is 1-2 percentage points smaller than at LO QCD + NLO QCD , in absolute terms it is actually larger. This effect is due to the large increase of about 26% induced by (N)LO i terms with i > 1. Indeed, this increase is mostly coming from the contribution of the tW → tW scattering, which appears at NLO 3 via the quark real-emission and has a Born-like scale dependence. However, this dependence is relatively small since the NLO 3 involves only a single power of α s .
In tables 3 and 4 we can see that δ NLO 1 ≡ δ NLO QCD is strongly µ dependent, while this is not the case for δ NLO i with i > 1. In fact, this behaviour is quite generic and not restricted to ttW ± production; it can be observed for a wide class of processes. The µ dependence in δ NLO 1 leads to the reduction of the scale dependence of LO QCD +NLO QCD results w.r.t. the LO QCD ones. On the contrary, the δ NLO i quantities with i > 1 are typically quite independent of the value of µ. The reason is the following. The NLO i contributions are given by "QCD corrections" to LO i contributions as well "EW corrections" to the LO i−1 ones. The former involve explicit logarithms of µ due the renormalisation of both α s and PDFs, while the latter contain only explicit logarithms of µ due the O(α) PDFs counterterms. Indeed, in the G µ -scheme, or other schemes such as α(0) or α(m Z ), the numerical input for α does  Table 4. σ (N)LO i /σ LOQCD ratios for ttW ± production at 100 TeV for various values of µ = µ r = µ f . not depend on an external renormalisation scale. Moreover, the O(α) PDF counterterms induce a much smaller effect than those of QCD, since they are O(α/α s ) suppressed and do not directly involve the gluon PDF. Thus, for a generic process, since a LO i contribution is typically quite suppressed w.r.t. the LO i−1 one -or even absent, as e.g. for (multi) EW vector boson production -the scale dependence of δ NLO i with i > 1 is small. For this reason it is customary, and typically also reasonable, to quote NLO EW corrections independently from the scale definition. As can be seen in tables 3 and 4 this is also correct for ttW ± , but as we will see in the next section the situation is quite different for tttt production, where also the δ (N)LO i (µ) quantities with i > 1 strongly depend on the value of µ. By considering the µ dependence of the δ NLO 1 (µ) contributions in tables 3 and 4, we see a different behaviour in the two tables. At 13 TeV the scale dependence of δ NLO QCD (µ) increases with increasing scales. This is to be expected: the LO 1 contribution has a large renormalisation-scale dependence, resulting in a rapidly decreasing cross section with increasing scales. In order to counterbalance this, the scale dependence of the NLO 1 contribution must be opposite so that the scale dependence at NLO QCD accuracy is reduced. On the other hand, at 100 TeV, the scale dependence of the δ NLO 1 (µ) decreases with increasing scales, suggesting that the scale dependence at LO QCD + NLO QCD is actually larger than at LO QCD . As can be seen in table 2 this does not appear to be the case. The reason is that contrary to 13 TeV, at 100 TeV collision energy the LO QCD has not only a large renormalisation-scale dependence, but also the factorisation-scale one is sizeable. In fact, the scale dependence in table 2 is dominated by terms in which µ r and µ f are varied in opposite directions, i.e., {µ r , µ f } = {2µ c , µ c /2} and {2µ c , µ c /2}. However, in table 4 we only consider the simultaneous variation of µ r and µ f . If we had estimated the scale uncertainty in tables 1 and 2 by only varying µ = µ r = µ f , we would actually have seen an increment of the uncertainties in moving from LO QCD to LO QCD + NLO QCD .
The NLO EW corrections, the NLO 2 contribution, are negative and have a −4-6% impact w.r.t. the LO 1 cross section. This is well within the LO QCD +NLO QCD scale uncertainties. The opening of the tW → tW scattering enhances the NLO 3 contribution enormously. In fact, it is much larger than the NLO 2 terms, yielding a +12% effect at 13 TeV and almost a +70% increase of the cross section at 100 TeV, both w.r.t. LO QCD . While at 13 TeV this is still within the LO QCD + NLO QCD scale uncertainty band, this is not at all the case at -12 -

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100 TeV. Indeed, it is these NLO 3 contributions that are responsible for the enhancement in the cross sections at the complete-NLO level as compared to the LO QCD + NLO QCD ones, as presented in the last column of tables 1 and 2. Hence, they must be included for accurate predictions for pp → ttW ± cross sections. Conversely, the NLO 4 contributions are at the sub-percent level and can be neglected in all phenomenologically relevant studies.
Applying a jet veto, such as the one of eq. (3.6), impacts only the real-emission corrections for ttW ± production. All the LO i terms remain unaffected and, since the dominant NLO real-emission contributions for this process are positive, the NLO i cross sections decrease. This is also what one expects from a physical point of view: the jet veto cuts away part of the available phase space, resulting in a decrease in the number of expected events. Indeed, in tables 3 and 4 we can see that this is the case (for all values of µ). On the other hand, not all the NLO i are affected in the same way by the jet veto. The NLO QCD contribution is reduced by a large amount, about a factor two for the central value of the scales, while the reduction in the other NLO i cross sections is much smaller. The reason for this difference is the following: a large fraction of the NLO 1 contribution originates from hard radiation, mainly due to the opening of the quark-gluon luminosity and the double logarithmic enhancement due to the radiation of a relatively soft/collinear W boson from a hard quark jet, cf., the left diagram of figure 2. Instead, the NLO 2 ≡ NLO EW is dominated by "EW corrections" to LO 1 and, therefore, does not involve a large increase due to the opening of the qg initiated real-emission contributions. Hence, the effect from the jet veto is strongly reduced. On the other hand, the NLO 3 does contain the enhancement from the gluon luminosity and is completely dominated by the tW → tW scattering, which is part of the real-emission contributions, see the right diagram of figure 2 and the discussion in section 2. Even so, these contributions are not very strongly affected by the jet veto, since the jet in tW → tW scattering is going mostly in the forward directions, which are unaffected by the central jet veto of eq. (3.6). The jet veto may be customised in order to enhance or suppress the NLO i contributions, e.g., to study the impact of tW → tW scattering in more detail. However, it should be noted that a stronger jet veto would further suppress the NLO i contributions, but it may also lead to unreliable results at fixed-order, due to the presence of unresummed large and negative contributions from QCD Sudakov logarithms. We leave a detailed study of the effects of various jet vetoes for future work.
On the total cross sections, see tables 1 and 2, the effect of the jet veto is not only manifest in the reduction of the LO QCD + NLO QCD and LO + NLO cross sections, but also in their greatly-reduced scale uncertainties. The latter are almost halved for the 13 TeV cross sections and reduced to about 11% at 100 TeV. This is another confirmation that the NLO QCD is dominated by hard radiation due to the opening of additional production channels, which have a large tree-level induced scale dependence. This reduction of the uncertainties coming from scale variations means that the difference between the purely QCD calculation and complete-NLO predictions becomes of the same order as the scale uncertainties (at 13 TeV) or even considerably larger (at 100 TeV). Hence, with the jet veto applied, it becomes even more important to include the NLO 3 contribution for a reliable prediction of the cross section for ttW ± hadroproduction. We stress that the inclusion of only NLO EW corrections leads to a smaller shift and in the opposite direction.

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Differential distributions. Results for three representative distributions, m(tt), p T (W ± ) and p T (tt), are shown for 13 TeV in figure 5 and for 100 TeV in figure 6. We consider the observables without (the plots on the left) and with (the plots on the right) the jet veto of eq. (3.6). Each plot has the following layout. The main panel shows distributions at NLO QCD (black) and complete-NLO (pink) accuracy, including scale variation uncertainties. For reference, we include also the LO QCD central value (µ = µ c ≡ H T /2) as a black-dashed line. 6 The lower insets show three different quantities, all normalised to the central value of the LO QCD +NLO QCD prediction. The grey band is the LO QCD +NLO QCD prediction including scale-uncertainties and the pink band is the one at complete-NLO accuracy, i.e., they are the same quantities in the main panel but normalised. The blue band is instead what is typically denoted as the result at "NLO QCD + EW" accuracy, namely, the LO QCD + NLO QCD + NLO EW prediction. Via the comparison of these three quantities one can see at the same time the difference between results at NLO QCD and complete-NLO accuracy but also their differences with NLO QCD + EW results, which have already been presented in refs. [18].
At 13 TeV and without the jet veto (left plots of figure 5), the predictions for the three observables at the various levels of accuracy presented, coincide within their respective scale uncertainties. For the m(tt) and, in particular the p T (W ± ), we see that the NLO EW corrections are negative and increase (in absolute value) towards the tails of the two distributions as expected from EW Sudakov logarithms coming from the virtual corrections. Only in the very tail of the distributions, close to m(tt) ∼ 2000 GeV and p T (W ± ) ∼ 2000 GeV the uncertainty bands of the NLO QCD and NLO QCD + EW predictions no longer overlap. As expected from the inclusive results, the complete-NLO results increase the NLO QCD + EW predictions such that they move again closer to the NLO QCD central value. Indeed, the NLO QCD and the complete-NLO bands do overlap for the complete phase-space range plotted. Moreover, the difference between the NLO QCD + EW predictions and the complete-NLO is close to a constant for these two observables. Conversely, applying the jet veto changes the picture. First, it is quite apparent that the relative impact of the NLO EW corrections is increased significantly, reaching up to −40% in the tail of the p T (W ± ) distribution, as compared to only −20% without the jet veto. The reason is obvious: the jet veto reduces the large contribution from the NLO QCD , hence, relatively speaking the NLO EW becomes more important. In other words, while the NLO QCD has a large contribution from the real-emission corrections, and are therefore greatly affected by the jet veto, in this region of phase space the NLO EW is dominated by the EW Sudakov logarithms, which are not influenced by the jet veto. The other important effect coming from the jet veto is the reduction of the scale uncertainties: as we have already seen at the inclusive level, this reduction is about a factor two for 13 TeV. For the m(tt) and p T (W ± ) this also appears to be the case over the complete kinematic ranges plotted for the NLO QCD predictions. At small and intermediate ranges, this is also the case for the NLO QCD + EW and the complete-NLO results. On the other hand,

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in the far tails, the uncertainty bands from the NLO QCD + EW and, to a slightly lesser extend, the complete-NLO are increased. Again, this is no surprise, since, as we have just concluded, these predictions contain a large contribution from EW Sudakov corrections in the NLO EW , which have the same large scale uncertainty as the LO 1 . Given that, relatively speaking, these NLO EW contributions become significantly more important with the jet veto, also the scale uncertainties become significantly larger.
For the third observable, p T (tt), the situation is extreme. This is mainly due to the fact that the NLO QCD corrections are not constant over the phase space as was the case for m(tt) and p T (W ± ). Rather, due to terms of order α s log 2 (p 2 T (tt)/m 2 W ) the NLO QCD greatly enhances the LO QCD predictions for moderate, and, in particular, large p T (tt). This enhancement originates from the real-emission ttW ± q final-states, where a soft and collinear W ± can be emitted from the final-state quark (see left diagram in figure 2). Thus, while at the Born level the tt pair is always recoiling against the W ± boson, at NLO QCD accuracy, for large p T (tt) values, it mainly recoils against a jet that is emitting the W ± boson. More details about this mechanism can be found in ref. [38]. For this reason, without a jet veto, at NLO QCD accuracy very large corrections and scale uncertainties are present for large p T (tt) values. Indeed, the dominant NLO QCD contribution, the soft and collinear emission of a W ± boson from a final-state quark, is very large and does not lead to a reduction of the scale dependence. 7 Moreover, since the NLO QCD are by far the dominant contributions, the effects from (N)LO i , with i > 1 are completely negligible at large transverse momenta. Only for intermediate transverse momenta, 80 GeV < p T (tt) < 400 GeV, we see a small effect in the comparison of NLO QCD and complete-NLO.
On the other hand, with a jet veto, the NLO QCD contribution (and therefore also the scale uncertainties) is strongly reduced. Indeed, when the jet veto is applied, hard-jets and the corresponding logarithmic enhancements are not present, and the tt pair is mostly recoiling directly against the W ± boson, making the predictions for p T (tt) and p T (W ± ) very similar. The only difference is in the comparison of the NLO QCD and the complete-NLO predictions. For the p T (W ± ) observable, this difference is basically a constant in the region 30 GeV < p T (W ± ) < 400 GeV. On the other hand, for p T (tt) we see that the NLO 3 contribution is not a constant: there is a reduction at small transverse momenta. Indeed, one would expect from tW → tW scattering that the transverse momenta of the top pair is typically larger than in the (N)LO 1 , due to the t-channel enhancement (between the tt and the W ± j pairs) at large transverse momenta. This is somewhat washed-out for the p T (W ± ) since it is the W boson together with the jet that receive this enhancement.
At 100 TeV, see figure 6, the differences between the various predictions are qualitatively different from 13 TeV. The reason is that the opening of the qg-induced contributions in NLO 1 and the tW → tW scattering contribution in NLO 3 are much more dramatic. The central value of the complete-NLO predictions is typically outside of the NLO QCD band even though the scale uncertainties are larger at 100 TeV than at 13 TeV. Moreover, with the jet veto, the bands generally do not even touch, apart from where they cross at large p T (W ± ) and p T (tt). 7 The size of the NLOQCD contribution is the difference between the dashed and the solid black line.

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Without a jet veto, on the basis of all the previous considerations, also NLO corrections on top of the ttW ± j final state may be relevant for ttW ± inclusive production. Indeed sizeable effects are expected from QCD and EW corrections on top of the dominant α s log 2 (p 2 T (tt)/m 2 W ) contribution and the large NLO 3 one, both arising from the qg initial state. The former would lead also to a reduction of the scale dependence in the tail of the p T (tt) distribution, which is dominated by the ttW ± j final state. However, these contributions are part of the NNLO corrections to the inclusive ttW ± production and therefore are not available and not included in our calculation. A possible way for estimating these effects is merging ttW ± and ttW ± j (and ttW ± γ) final states at NLO accuracy. In the case of NLO QCD corrections a study in this direction has been suggested for ttW ± production in ref. [38]. For NLO EW and subleading NLO i corrections a fully-consistent technology is not yet available to perform this kind of study.
Further details about individual NLO i contributions at the differential level are given in figure 7 (13 TeV) and figure 8 (100 TeV). In the plots we show all the δ NLO i (µ) for µ = µ c ≡ H T /2 (solid line), µ = µ c /2 (dashed line) and µ = 2µ c (dotted line). We show the same distributions (with and without veto) as in figures 5 and 6. We remark again that the δ NLO i (µ) do not show directly scale uncertainties since the value of µ is varied both in the numerator and the denominator of δ. On the other hand, we can directly see that also at the differential level the relative sizes of both NLO 2 and NLO 3 w.r.t. the LO QCD are almost insensitive to the value of the scale; the corresponding solid, dashed and dotted lines are almost indistinguishable. As expected, also at the differential level the impact of the NLO 4 is completely negligible for the whole range of the distributions considered.
As could already have been concluded by comparing the dashed and solid black lines in figures 5 and 6, the NLO QCD corrections are not at all a constant over phase space. The solid black lines in figures 7 and 8 make this very clear. In particular for the p T (tt) distributions without the jet veto (lower left plots), the NLO 1 ≡ NLO QCD contribution easily becomes as large as the LO 1 ≡ LO QCD and increases to more than an order of magnitude larger than LO 1 at large transverse momenta in 100 TeV collisions. But also for p T (W ± ) we see large NLO QCD corrections, in particular at 100 TeV. On the other hand, for m(tt) the NLO QCD corrections are mostly flat, in particular at 13 TeV. With the jet veto (plots on the right) the situation changes quite dramatically. The NLO QCD corrections are, in general, under much better control, even though one can see that the extreme tails in the p T (W ± ) and p T (tt) at 100 TeV the NLO QCD contributions decrease rapidly and are starting to be strongly influenced by logarithms related to the jet-veto scale. If one would look at even larger transverse momenta, or, equivalently, reduce the jet-veto scale, these logarithms will grow and eventually fixed-order perturbation theory would break down, showing the need for resummation of these jet-veto logarithms.
Since these plots are normalised w.r.t. the LO 1 (cf., the lower insets of figures 5 and 6 which are normalised to LO 1 +NLO 1 ), one can clearly see the effects of the NLO EW corrections, i.e., the NLO 2 , independently from the NLO QCD corrections. One sees the typical EW Sudakov logarithms: negligible effects at the percent level at small and moderate tt invariant masses and W ± and tt transverse momenta, but growing rapidly with increasing values of the observables, to about −20% at m(tt) 2000 GeV and −40% at p T (W ± ) -  Figure 5. Differential distributions for ttW ± production at 13 TeV. For the plots on the right, the jet veto of eq.   Figure 6. Same as figure 5 but for 100 TeV collisions.

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p T (tt) 2000 GeV. The fact that the NLO EW corrections are smaller for m(tt) in comparison to p T (W ± ) and p T (tt) is no surprise since the impact of the EW Sudakov logarithms is related to the number of invariants that are large for the observable considered. Typically, for large invariant masses, there need to be fewer large invariants than for producing large transverse momenta. The size of the NLO EW corrections relative to the LO 1 is quite similar for 13 TeV and 100 TeV collisions. Moreover, by comparing the distributions with and without the jet veto we also see that their sizes are hardly influenced by the jet veto. At variance with the NLO 2 term, at 13 TeV the NLO 3 contribution is much more constant w.r.t. the LO 1 over the whole phase space. Indeed, for the m(tt) the δ NLO 3 is effectively a constant, increasing the LO 1 cross section by about 12% (which is reduced by applying the jet veto to about 9%). Similarly, for the p T (W ± ) distribution, the NLO 3 correction is fairly flat. On the other hand, the p T (tt) does show some kinematic dependence in the δ NLO 3 ratio. It is small at small transverse momenta, increases at intermediate values and, in particular when the jet veto is applied, it decreases again at large values of p T (tt). This is consistent with what we found in the comparing the LO QCD + NLO QCD and NLO QCD + EW predictions in figure 5. At 100 TeV the NLO 3 contributions are large and the δ NLO 3 plots are not at all flat in the phase space. As at 13 TeV, the effects are most dramatic in the p T (tt) distributions, which show a large hump at around 500 GeV (1 TeV) with (without) the jet veto. However, as discussed before, without a jet veto, at large p T (tt) the NLO QCD corrections is giant and is even the dominant contribution among all the (N)LO i ones, including the LO 1 . For this reason, although δ NLO 2 and δ NLO 3 are large at high p T (tt), results at LO QCD + NLO QCD , LO QCD + NLO QCD + NLO EW , and LO + NLO accuracies are very close to each other; the three predictions are all dominated by NLO QCD , while δ NLO i are normalised to LO QCD .
The application of a jet veto as in eq. (3.6) may be exploited in BSM analyses such as the one described in ref. [33]; rather than requiring a forward jet it may be possible to observe enhancements in the tW ± → tW ± scattering directly in ttW ± production by vetoing hard central jets.

Results for pp → tttt production
Similarly to the previous section, we start by presenting predictions for tttt total cross sections at 13 and 100 TeV proton-proton collisions and then we discuss results at the differential level. Using a layout that is similar to As can be seen in tables 5 and 6, the scale dependence is very large at LO QCD and LO accuracy and it is strongly reduced both in the NLO QCD and complete-NLO predictions to about 20%. Nevertheless, it is still larger than the impact of the non-purely-QCD contributions, which is also reduced moving from LO to NLO accuracy, halved in the 100 TeV case. At the inclusive level, the difference between LO + NLO and LO QCD + NLO QCD predictions is well within their respective scale uncertainties, especially at 100 TeV where this difference is merely 5% of the LO QCD + NLO QCD result. However, the numbers in tables 5 and 6 hide the most important feature of the complete-NLO result, i.e., very large and scale-dependent cancellations among the (N)LO i terms with i ≥ 2. This will become clear from the discussion in the next paragraph.
As anticipated in section 2, in tttt production the LO 2 and LO 3 contributions are not so suppressed w.r.t. the LO QCD , at variance with ttW ± production (see tables 7 and 8, cf. tables 3 and 4). For tttt production, due to sizeable contributions from the EW tt → tt scattering, LO 2 and LO 3 can induce corrections of the order −30% and +40% on top of the LO 1 , respectively. 8 Therefore, also the NLO 2 and NLO 3 contributions are large, since they contain "QCD corrections" to LO 2 and LO 3 terms, respectively. The fact that a large fraction of NLO 2 and NLO 3 contributions is of QCD origin can be understood by the µ-dependencies of δ NLO 2 and δ NLO 3 ratios, which, as can be seen in tables 7 and 8, are very large. Indeed, NLO 2 and NLO 3 terms involve explicit logarithms of µ that compensate the PDF and α s scale dependence at LO 2 and LO 3 accuracy, respectively. Thus, in tttt 8 Similarly to the case of the LO3 in ttW ± production, the scale dependences of the LO2 and especially of the LO3 are much smaller than that of LO1, due to the different powers of αs associated to them. Hence, with larger(smaller) values of the scales and consequently smaller(larger) values of LO1, the δLO 2 and δLO 3 become larger(smaller) in absolute value.  production, at variance with most of the other production processes studied in the literature, quoting the relative size of NLO EW ≡ NLO 2 or NLO 3 corrections without specifying the QCD-renormalisation and factorisation scale is simply meaningless. Moreover, δ NLO 2 and δ NLO 3 corrections can separately be very large, easily reaching ±15% (depending on the value of µ). Surprisingly, for our central value of the renormalisation and factorisation scales, the δ NLO 2 and δ NLO 3 are almost zero, 9 particularly for 13 TeV. On the other hand, if we had taken H T /2 or even m tttt as our central scale choice, the NLO 2 and NLO 3 corrections relative to the LO 1 , δ NLO 2 and δ NLO 3 , would have been much larger. Still, even for the central value µ = H T /4, the corrections are much larger than foreseen, especially for δ NLO 3 which naively is expected to be of order α 3 s α 2 /α 4 s = α 2 /α s ∼ 0.1% level. On the other hand, the relative cancellation observed between NLO 2 and NLO 3 contributions is even larger than in the case of LO 2 and LO 3 . As can be seen in the last rows of tables 7 and 8, at the inclusive level the sum of the ratios δ NLO 2 + δ NLO 3 is not only small, but also stable under scale variation, 10 resulting in corrections of at most a few percents w.r.t. the LO QCD . Furthermore, particularly at 13 TeV, δ NLO 2 + δ NLO 3 receives also additional cancellations when summed to δ NLO 4 , which itself is much larger than the expected α 2 s α 3 /α 4 s = α 3 /α 2 s ∼ 0.01% level. To the best of our understanding, these cancellations are accidental.
These large and accidental cancellations among the (N)LO i terms with i > 1 are particularly relevant from a BSM perspective, since the level of these cancellations may be altered by new physics. As an example, we can refer to the case of an anomalous y t coupling, which, as we have already mentioned, has been considered in the tree-level analysis of ref. [34]. Terms proportional to y 2 t are present in all the (N)LO i with i ≥ 2 and terms 9 Our choice for the central value of the scales has not been tuned in order to reduce the effects from the NLO2 and NLO3. Rather, it is motivated by the study in ref. [38], which deals only with the LO1 and NLO1. 10 We verified this feature also with different functional forms for the scale µ.  proportional to y 4 t are present in all the (N)LO i with i ≥ 3, but also terms proportional to y 6 t are present for any i ≥ 3. Moreover, also contributions proportional to y t , y 3 t and y 5 t are possible. Similar considerations apply also to other new physics effects in tttt production (see, e.g., ref. [64] and references therein for scenarios already analysed in the literature).
In order to understand the hierarchy of the different (N)LO i contributions, it is important to note that at 13 TeV and especially at 100 TeV the total cross section is dominated by the gg initial state (see, e.g., ref. [38]). For this reason, the LO 4 , LO 5 , NLO 5 and NLO 6 contributions, which are vanishing for the gg initial state, are much smaller than the other contributions. The modest scale dependence of δ NLO 4 is also induced by this feature; the NLO 4 contribution mainly arises from "EW corrections" to gg-induced LO 3 contributions, which do not have any explicit dependence on µ; and therefore the scale dependence of the NLO 4 follows the scale dependence of the LO 3 to a large extent.
Differential distributions. We now move to the description of the results at the differential level, where we consider the following distributions: the invariant mass of the four (anti)top quarks m(tttt) (figure 9), the sum of the transverse masses of all the particles in the final state H T as defined in eq. (3.5) (figure 10), the transverse momenta of the hardest of the two top quarks p T (t 1 ) (figure 11), and the rapidity of the softest one y(t 2 ) (figure 12). At variance with the case of ttW ± production in section 3.2, we organise plots according to the observable considered. In the figures we display 13 TeV results on the left and 100 TeV results on the right. In the upper plots of each of these figures we provide predictions at different levels of accuracy, using a similar layout 11 as in figures 5 and 6, 11 At variance with ttW ± production, we do not show LOQCD + NLOQCD + NLOEW predictions. This level of accuracy is rather artificial, since the NLOEW ≡ NLO2 terms are dominated by "QCD corrections" to the LO2 ones. Hence, including NLO2 without LO2 would not be very consistent. Moreover, there are large cancellations between LO2 and LO3, so, including only the former and not the latter would not be -24 -

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which is described in detail in section 3.2. Also for tttt production, comparisons among the scale uncertainties of the LO QCD and LO QCD + NLO QCD result have been documented in detail in ref. [38] for 13 TeV, so they are not repeated here. Individual contributions from the different (N)LO i terms are instead displayed in the central and lower plots. In the central plots we show the δ (N)LO i (µ), see eq. (3.7), with µ = µ c ≡ H T /4, while the lower plots focus on NLO 2 and NLO 3 contributions and their sum featuring large cancellations. In particular, we show δ NLO 2 (µ), δ NLO 3 (µ) and their sum for µ = µ c (solid line), µ = µ c /2 (dashed line) and µ = 2µ c (dotted line). In practice, the dark-blue and red solid lines are the same quantities in the middle and lower plots. Once again, we remark that the δ NLO i (µ) ratio does not show directly the scale uncertainty since the value of µ is varied both in the numerator and the denominator of δ.
Away from the threshold region, i.e., m(tttt) > 900 GeV, the complete-NLO prediction for the four-top invariant-mass distribution is very close to the NLO QCD one, with an almost constant increase of about 10%, both at 13 and 100 TeV, see upper plots in figure 9. This increase is well within the uncertainty bands of either of the predictions. On the other hand, in the threshold region the enhancement of the cross section due to terms with (N)LO i , with i > 1, is much larger than for the inclusive results. In this region the central value of the complete-NLO predictions lies outside the LO 1 +NLO 1 uncertainty band. From the central plots of figure 9, it can be seen that the (N)LO 2 and (N)LO 3 contributions are individually sizeable w.r.t. LO QCD and their relative impact has a large dependence on kinematics, easily reaching several tens of percents in certain regions of phase space.
As anticipated from the inclusive results, there are large cancellations in the distributions among LO 2 and LO 3 contributions and especially among NLO 2 , NLO 3 ones; the latter are explicitly shown in the lower plots. In particular, although the corresponding δ (N)LO i terms individually depend on the value of m(tttt), they lead for m(tttt) > 900 GeV to the aforementioned constant increase of about 10% of the complete-NLO prediction w.r.t. the NLO QCD result. As can be seen in the central plots, the δ LO 2 is negative, it is about −10% at m(tttt) 4000 GeV and further decreases for smaller invariant masses, reaching about −40% at m(tttt) 900 GeV. On the other hand, the δ LO 3 is positive, and very close to the absolute value of δ LO 2 plus a constant 12 (at 13 TeV) or 16 (at 100 TeV) percentage points. Moreover, even though also the δ NLO 2 and δ NLO 3 are depending quite strongly on the value of m(tttt), they sum to almost a constant −1% (at 13 TeV) and −4% (at 100 TeV). Therefore, indeed, the entire sum LO 2 + LO 3 + NLO 2 + NLO 3 is almost a constant 10% correction to the LO 1 + NLO 1 -away from the threshold region.
In the threshold region, the situation is quite different. While the δ LO 3 keeps increasing closer and closer to threshold, the derivative of δ LO 2 reverses sign at m(tttt) 900 GeV. In other words, the δ LO 2 also starts to increase closer and closer to threshold. The same is true for the corrections induced by NLO 2 and NLO 3 contributions: the δ NLO 3 sharply increases close to threshold. Hence, the delicate cancellation among the LO 2 and LO 3 (and giving a correct picture. On top of this, from the inclusive results, we already know that there are also large cancellations between the NLO2 and NLO3 terms. Given the dominance of the gg-induced contributions,       Figure 10. The H T distribution in tttt production. See the caption of figure 9 for the description of the plots.  Figure 11. The p T (t 1 ) distribution in tttt production. See the caption of figure 9 for the description of the plots.   Figure 12. The y(t 2 ) distribution in tttt production. See the caption of figure 9 for the description of the plots.
-29 -JHEP02(2018)031 NLO 2 and NLO 3 ) contributions completely breaks down in this region of phase space. Moreover, also the NLO 4 reaches several tens of percent close to threshold and should not be neglected when studying this region of phase space. Conversely, also at the differential level, LO 4 , LO 5 , NLO 5 and NLO 6 contributions are negligible. There are two different physical effects at the origin of the large NLO corrections in the threshold region. First, also the LO 2 and LO 3 contributions are larger in this region and thus their "QCD corrections", which respectively enter the NLO 2 and NLO 3 contributions, preserve this increment w.r.t. the rest of the phase space. Second, the exchange of Z or Higgs bosons among top quarks, or in general among heavy particles, can lead to Sommerfeld enhancements when the top quarks are in a non-relativistic regime. This effect has already been documented in refs. [65,66] for the case of top-quark pair production and in refs. [67][68][69] for the exchange of a virtual Higgs boson between an onshell Higgs boson and another on-shell heavy particle. The threshold region forces each tt, tt ortt pair to potentially lead to this kind of effect. These large "EW corrections" on top of LO 1 and LO 2 terms lead to additional sizeable contributions to NLO 2 and NLO 3 , respectively. Moreover, since also LO 3 is large, via this kind of "EW corrections" even NLO 4 is very large and incredibly enhanced w.r.t. the result at the inclusive level.
The lower plots in figure 9 further confirm the QCD origin of the NLO 2 and NLO 3 contributions. In order to explain this, we remind the reader that the scale dependence of the LO 2 and LO 3 contributions is the typical one, i.e., LO 2 and LO 3 absolute values become smaller when the scales are increased. In the plots we see that for NLO 3 the (dark blue) dashed lines are larger than the solid lines, which are in turn larger than dotted lines, while in the case of NLO 2 the order is the reversed. Since the LO 2 is negative, the NLO 2 term reduces the µ dependence of the LO 2 one and, similarly, the NLO 3 term reduces the µ dependence of the LO 3 one. Moreover, these plots confirm that also at the differential level there are large cancellations among the NLO 2 and NLO 3 terms and that the δ NLO 2 + δ NLO 3 sum has a much smaller scale dependence than the two separate addends. In other words, the remarkable cancellations among the NLO 2 and NLO 3 corrections are not only present for the central value of µ, as already concluded from the middle plots in the discussion above, but also for their scale dependencies. Notably, these cancellations are present over a very large region of phase space. Also, if we had chosen, e.g., H T /2 as our central scale (dashed lines in the lower plot), the NLO 2 and NLO 3 curves in the middle plots would have been much further apart, leading to much larger cancellations, since their sum would hardly have changed at all.
Compared to the invariant-mass distribution of the four tops, the case of the H T distribution (figure 10) is similar in many respects. In particular, from the upper plots, we see that again only in the threshold region there is a sizeable difference between the NLO QCD predictions and the complete-NLO ones. It should be noted, though, that above the peak in the distribution, H T 1500 GeV, the difference between the two predictions is very small, their central values as well as the scale uncertainties are lying almost exactly on top of each other. Just as in the case of the m(tttt), the middle plots show that this is rather due to large and accidental cancellations among the various (N)LO i with i > 1 contributions, which can individually reach several tens of percent. dependence of δ NLO 2 does decrease with increasing transverse momenta, it remains anyway sizeable even in the far tail of the distribution. Therefore, a non-negligible part of NLO 2 is due to "QCD corrections" on top of the LO 2 also in the far tail. For these reasons, although in this phase-space region the individual and summed δ NLO i with i > 1 are not at all constant, the scale dependence of δ NLO 2 + δ NLO 3 remains very small. The non-constant part seems to be the "EW corrections" entering the NLO 2 , which are dominated by large and negative Sudakov logarithms and do not introduce a new scale dependence w.r.t. the LO 1 .
From the y(t 2 ) distribution ( figure 12) we can see that, besides the threshold region, a non-negligible difference between NLO QCD and complete-NLO predictions is present also at 13 TeV (not 100 TeV) in the peripheral region of the softest of the top quark quarks. The y(t 2 ) distribution is also the only one, among those considered, where the impact of the different (N)LO i terms is qualitatively different at 13 and 100 TeV. While the LO i corrections are rather flat at both 13 and 100 TeV, NLO i corrections are flat only at 100 TeV; the NLO i corrections for 13 TeV yield large effects in the peripheral region. The origin of this difference is the range of Bjorken-x probed in the PDFs, which is indeed very different at 13 and 100 TeV. While at 13 TeV the peripheral region is typically associated with tops that have large rapidities also in the tttt rest frame, at 100 TeV it is more likely that they originate from partonic initial states that are boosted w.r.t. the proton-proton reference frame. 13 For this reason the y(t 2 ) distribution is flatter at 100 TeV than at 13 TeV, where large rapidities are strongly suppressed in a Born-like kinematics and therefore they are also much more sensitive to effects due to real emission from NLO i contributions. However, as before, the NLO 2 and NLO 3 contributions almost cancel, resulting in at most ∼10% effects w.r.t. the LO 1 in the far forward and backward regions.
Given our findings, we suggest that the study of the µ-dependence of δ NLO i can be a very useful procedure for identifying the nature of NLO i corrections in numerical calculations. For higher values of i, the Σ NLO i (µ)/Σ LO i−1 (µ) may be even more appropriate given the different numerical sizes of the LO i terms and of their dependence on the running of α s . 14 For instance, we verified that in tttt production both Σ NLO 4 /Σ LO 3 and Σ NLO 6 /Σ LO 5 are very mildly scale-dependent at inclusive and differential level. Indeed, both can be considered almost purely "EW corrections"; the latter by construction and the former due to the dominance of the gg initial-state. Conversely, we do not find this feature in the Σ NLO 5 /Σ LO 4 ratio, since LO 4 and LO 5 contributions are both small but comparable in size and thus Σ NLO 5 receives large "QCD corrections" on top of LO 5 contributions.
In summary, at the inclusive and the differential levels complete-NLO results for tttt production are well within the NLO QCD uncertainties. For the observables presented here, there are no large qualitative differences between results at 13 and 100 TeV, except in the peripheral regions of the rapidity of the second hardest top quark. However, for all observables very large cancellations among the different perturbative orders are present both at the inclusive and differential level. Their individual sizes w.r.t. the LO QCD prediction 13 The maximum value for the rapidity of the tttt system in a Born-like configuration is log 13 TeV 4m t ∼ 3 at 13 TeV, while it is log 100 TeV 4m t ∼ 5 at 100 TeV. 14 Note that ΣNLO i /ΣLO i−1 = δNLO i /δLO i−1 , so at the inclusive level the necessary information can be obtained from tables 7 and 8. are also strongly dependent on the scale definition. All these arguments point to the fact that in any BSM analysis involving tttt production contributions from all NLO corrections can be relevant. Thus, they should be taken into account, at least in the estimate of the theory uncertainty.

Conclusions
In this paper we have presented the complete-NLO predictions for ttW ± and tttt production at 13 and 100 TeV in proton-proton collisions. All the seven O(α i s α j ) contributions with i + j = 3, 4 and j ≥ 1 for ttW ± production and all the eleven O(α i s α j ) contributions with i + j = 4, 5 have been calculated exactly without any approximation. We have shown that complete-NLO corrections involve large contributions beyond the NLO EW accuracy for both the ttW ± and tttt production processes In ttW ± production we find that the O(α s α 3 ) contributions, denoted as NLO 3 in this article, are larger than NLO EW corrections and have opposite sign. They are of the order 12(70)% of the LO at 13(100) TeV, with a strong dependence on particular kinematic variables such as p T (W ± ) and p T (tt), but not m(tt). Thus, they are several orders of magnitude larger than the values naively expected from their coupling orders, i.e., NLO 3 /LO α 2 /α s ∼ 0.1%. The main reason is the opening of the tW → tW scattering in the NLO 3 . Since the NLO QCD corrections are dominated by hard radiation, applying a jet veto suppresses the NLO QCD contributions considerably. Conversely, the NLO 3 (and the NLO EW corrections) are affected to a much lesser extent, resulting in large corrections on top of the NLO-QCD result. At 13 TeV, applying a 100 GeV central jet veto, the central value of the complete-NLO prediction is typically outside the NLO QCD scale-uncertainty band. At 100 TeV, the uncertainty bands of these two predictions do not even touch. Besides their relevance for the SM and reliable comparisons with current and future measurements, these results further support the proposal of the BSM analysis described in ref. [33], showing a possible sensitivity to higher-dimensional operators in tW → tW scattering directly in ttW ± production. Rather than requiring a jet and considering tW → tW scattering as a Born process, our results suggest that the sensitivity may be increased by directly considering ttW ± production and vetoing additional jets.
In tttt production, LO contributions of O(α 3 s α) are about −25-30% of the purely-QCD O(α 4 s ) ones, while O(α 2 s α 2 ) contributions are about +30-45%, depending on the scale choice. For this reason, we find that the O(α 4 s α) (the NLO EW corrections, or NLO 2 ) as well as the O(α 3 s α 2 ) (denoted as NLO 3 in this article) contributions are also large. Moreover, since they receive large contributions from "QCD corrections" (and thus α s and PDF renormalisation) on top of respectively O(α 3 s α) and O(α 2 s α 2 ) terms, they strongly depend on the scale definition. At 13 TeV, their relative impact w.r.t. purely-QCD O(α 4 s ) contribution varies in both cases between ±15%. On the other hand, their sum reduces to a rather small ±1-2%, and is almost independent from the QCD scale choice and kinematics. Qualitatively similar results are found also at 100 TeV. The size of the cancellations is quite remarkable, unexpected, and, to the best of our knowledge, accidental. Thus, a calculation of only part of the complete-NLO results would be missing important contributions. These large cancellations between the corrections and the reduced scale dependencies of their sum are not present very close to threshold. In this region of phase space, complete-NLO results are sizeably different from those at NLO QCD accuracy and even contributions of O(α 2 s α 3 ) (denoted as NLO 4 in this article) are found to be of the order of several tens of percents of the LO. Besides their relevance for the SM and reliable comparisons with current and future measurements, our calculations show that the possible impact of NLO corrections should be critically considered for studies such as ref. [34], where tttt production has been proposed as candidate, in conjunction with ttH production, for an independent determination of the Yukawa coupling of the top quark and the Higgs-boson total decay width. Similar considerations apply to other BSM studies involving tttt production: the various contributions from NLO corrections are large and the cancellations among them could be spoiled by BSM effects. This should be taken into account at least in the estimate of the theory uncertainties.
In this work we have also shown that the study of the µ-dependence of the quantity δ NLO i ≡ Σ NLO i (µ)/Σ LO 1 (µ) can be a very useful procedure for identifying the nature of NLO i corrections in numerical calculations. A large scale dependence is a signal of "QCD corrections" on top of the LO i contribution, while a scale independence for δ NLO i points to "EW corrections" on top of the LO i−1 contributions. For higher values of i, the Σ NLO i (µ)/Σ LO i−1 (µ) may be even more appropriate given the possible different numerical sizes of the LO i terms and of their dependence on the running of α s .
As a final remark, we want to remind the reader that the three known cases where NLO corrections from supposedly subleading EW contributions are large, pp → ttW ± , pp → tttt and pp → W + W + jj with leptonic W + decays [26], involve very different mechanisms. In ttW ± production it is the opening of tW → tW scattering via the real emission in the NLO 3 . In tttt production it is mainly the "QCD corrections" on top of EW tt → tt scattering, which gives large contributions already at the LO. In W + W + jj production it is instead the large EW Sudakov logarithmic corrections featured by the formally most subleading NLO contribution [27] together with the relatively large size (especially when standard VBS cuts are applied) of the purely EW W + W + scattering component.