  The transmission spectrum of the ultrahot Jupiter KELT-9b ($T_{eq}$ $\sim$
4000 K) exhibits absorption by several metal species. We searched for atomic
and molecular lines in its emission spectrum by observing partial phase curves
with the CARMENES spectrograph ($R$ $\sim$ 80,000 $-$ 95,000). We find evidence
for emission by Si I in the atmosphere of KELT-9b for the first time.
Additionally we find evidence for emission by Mg I and Ca II, which were
previously detected in transmission, and confirmed earlier detections of Fe I
emission. Conversely, we find no evidence for dayside emission from Al I, Ca I,
Cr I, FeH, Fe II, K I, Li I, Mg II, Na I, OH, Ti I, TiO, V I, V II, VO, and Y
I. By employing likelihood mapping, we find indications of there being little
variation in emission line contrast between the day- and nightsides
$-$suggesting that KELT-9b may harbor iron emission on its nightside. Our
results demonstrate that high-resolution ground-based emission spectroscopy can
provide valuable insights into exoplanet atmospheres.
