Quantifying the (X/Peanut)-Shaped Structure in Edge-on Disc Galaxies:
  Length, Strength, and Nested Peanuts
  X-shaped or peanut-shaped (X/P) bulges are observed in more than 40% of
(nearly) edge-on disc galaxies, though to date a robust method to quantify them
is lacking. Using Fourier harmonics to describe the deviation of galaxy
isophotes from ellipses, we demonstrate with a sample of 11 such galaxies
(including NGC 128) that the sixth Fourier component ($B_6$) carries physical
meaning by tracing this X/P structure. We introduce five quantitative
diagnostics based on the radial $B_6$ profile, namely: its `peak' amplitude
($\Pi_{\rm max}$); the (projected major-axis) `length' where this peak occurs
($R_{\Pi,max}$); its vertical `height' above the disc plane ($z_{\Pi,max}$);
the $B_6$ profile's integrated `strength' ($S_{\Pi}$); and the $B_6$ peak
`width' ($W_{\Pi}$). We also introduce different `classes' of $B_6$ profile
shape. Furthermore, we convincingly detect and measure the properties of
multiple (nested) X/P structures in individual galaxies which additionally
display the signatures of multiple bars in their surface brightness profiles,
thus consolidating further the scenario in which peanuts are associated with
bars. We reveal that the peanut parameter space (`length', `strength' and
`height') for real galaxies is not randomly populated, but the 3 metrics are
inter-correlated (both in kpc and disc scale-length $h$). Additionally, the X/P
`length' and `strength' appear to correlate with $v_{rot}/\sigma_*$, lending
further support to the notion that peanuts `know' about the galactic disc in
which they reside. Such constraints are important for simulations, as they
provide a direct link between peanuts and their host disc. Our diagnostics
reveal a spectrum of X/P properties and could provide a means of distinguishing
between different peanut formation scenarios. Moreover, nested peanuts, as
remnants of bar buckling events, can provide insights into the disc and bar
instability history.
