roughly equally strong H$\alpha$, H$\beta$, and/or \[OIII\] emission lines along with several additional lines such as HeI at 5876Å, 6680Å and 7065Å, HeII at 4686Å, \[ArIII\] at 7136Å, \[NII\] at 6548Å and 6584Å, \[SII\] 6716Å and 6731Å, and/or \[ArIV\] at 4711Å and 4740Å (see, e.g., @1991ApJS...75..407M). Of the 17 we classified as PNe based on our spectra, 7 were classified as such in SIMBAD and 5 were classified as YSOs.

[*Young stellar objects.*]{} We classified sources as candidate YSOs if they had significantly weaker \[OIII\] and H$\beta$ lines relative to H$\alpha$ combined with relatively strong \[SII\] emission lines at 6716Å and 6731Å, \[OI\] at 6300Å, and/or \[NII\] at 6548Å and 6584Å (see, e.g., @1998AJ....115.2491K). Of the 115 objects we classified as YSOs, 18 were classified as such by SIMBAD and 1 was classified as a PN, leaving 96 new candidate YSOs. There were also four additional sources we identify as YSO/PN where we were uncertain as to the correct classification. SIMBAD has two of these four classified as YSOs.

[*Be and blue stars*]{}. Blue stars had blue spectra with strong hydrogen Balmer series absorption. They were then further classed as Be stars if they had strong hydrogen H$\alpha$ (H$\beta$) emission 