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While monitoring a sample of apparently slowly rotating superficially normalearly A stars, we have discovered that HR 8844 (A0 V), is actually a newChemically Peculiar star. We have first compared the high resolution spectrumof HR 8844 to that of four slow rotators near A0V ($\nu$ Cap, $\nu$ Cnc ,Sirius A and HD 72660) to highlight similarities and differences. The lines ofTi II, Cr II, Sr II and Ba II are conspicuous features in the high resolutionhigh signal-to-noise SOPHIE spectra of HR 8844 and much stronger than in thespectra of the normal star $\nu$ Cap. The Hg II line at 3983.93 \AA\ is alsopresent in a 3.5 \% blend. Selected unblended lines of 31 chemical elementsfrom He up to Hg have been synthesized using model atmospheres computed withATLAS9 and the spectrum synthesis code SYNSPEC48 including hyperfine structureof various isotopes when relevant. These synthetic spectra have been adjustedto the mean SOPHIE spectrum of HR 8844, and high resolution spectra of thecomparison stars. Chisquares were minimized in order to derive abundances orupper limits to the abundances of these elements for HR 8844 and the comparisonstars. HR 8844 is found to have underabundances of He, C, O, Mg, Ca and Sc,mild enhancements of Ti, V, Cr, Mn and distinct enhancements of the heavyelements Sr, Y, Zr, Ba, La, Pr, Sm, Eu and Hg, the overabundances increasingsteadily with atomic number. This chemical pattern suggests that HR 8844 mayactually be a new transition object between the coolest HgMn stars and the Amstars.

HR 8844: a new transition object between the Am stars and the HgMn stars ?