Instruct: Identify the main and secondary category of Arxiv papers based on the titles and abstracts
Query: Parity-violating CMB correlators with non-decaying statistical
  anisotropy   We examine the cosmological correlators induced by the simultaneous breaking
of parity and of statistical isotropy, e.g., in presence of the coupling ${\cal
L} = f(\phi) ( - \frac{1}{4} F^2 + \frac{\gamma}{4} F \tilde{F} )$ between the
inflaton $\phi$ and a vector field with vacuum expectation value ${\bf A}$. For
a suitably chosen function $f$, the energy in the vector field $\rho_{\rm A}$
does not decay during inflation. This results in nearly scale-invariant
signatures of broken statistical isotropy and parity. Specifically, we find
that the scalar-scalar correlator of primordial curvature perturbations
includes a quadrupolar anisotropy, $P_\zeta ( {\bf k}) = P(k)[ 1 + g_* (
\hat{\bf k} \cdot \hat{\bf A})^2]$, and a (angle-averaged) scalar bispectrum
that is a linear combination of the first $3$ Legendre polynomials,
$B_\zeta(k_1, k_2, k_3) = \sum_L c_L P_L (\hat{\bf k}_1 \cdot \hat{\bf k}_2)
P(k_1) P(k_2) + 2~{\rm perms} $, with $c_0 : c_1 : c_2 = 2 : -3 : 1$ ($c_1 \neq
0$ is a consequence of parity violation, corresponding to the constant $\gamma
\neq 0$). The latter is one of the main results of this paper, which provides
for the first time a clear example of an inflationary model where a
non-negligible $c_1$ contribution to the bispectrum is generated. The
scalar-tensor and tensor-tensor correlators induce characteristic signatures in
the Cosmic Microwave Background temperature anisotropies (T) and polarization
(E/B modes); namely, non-diagonal contributions to $\langle a_{\ell_1 m_1}
a_{\ell_2 m_2}^* \rangle$, with $|\ell_1 - \ell_2| = 1$ in TT, TE, EE and BB,
and $|\ell_1 - \ell_2| = 2$ in TB and EB. The latest CMB bounds on the scalar
observables ($g_*$, $c_0$, $c_1$ and $c_2$), translate into the upper limit
$\rho_{\rm A} / \rho_\phi \lesssim 10^{-9}$ at $\gamma=0$. We find that the
upper limit on the vector energy density becomes much more stringent as
$\gamma$ grows.

11
The categories of this paper are: hep-lat
3
The categories of this paper are: physics
28
The categories of this paper are: alg-geom
35
The categories of this paper are: mtrl-th
8
The categories of this paper are: hep-ex
26
The categories of this paper are: bayes-an
9
The categories of this paper are: nlin
25
The categories of this paper are: patt-sol
14
The categories of this paper are: math-ph
36
The categories of this paper are: cmp-lg
12
The categories of this paper are: nucl-th
10
The categories of this paper are: q-bio
2
The categories of this paper are: math
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The categories of this paper are: adap-org
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The categories of this paper are: stat
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The categories of this paper are: acc-phys