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tokens: spectrum and 27 have multiple archival spectra. As we are refining our CLAGN candidates by selecting candidates where the archival spectra already show some signs of change, there is the potential to miss CLAGNs where the spectra have changed after the last archival spectra was taken and this will decrease our completeness. Of the AGNs that were not identified by our CLAGN candidate selection methods and have multiple archival spectra, we identified AGNs that appeared to have some small variations in the spectra, however, these variations were not significant enough to require further investigation (i.e. changes in spectral class were 0.1 or less). Thus, while our three candidate selection criteria select many AGNs that are not CLAGNs, our selection criteria are not missing a large number of nearby CLAGNs. 3 SPECTROSCOPIC FOLLOW-UP Once candidates were identified using the colour and flux criteria discussed in Sections 2.2– 2.4 , we inspected the archival spectra of these objects in order to identify potential CLAGNs without obtaining new spectra. It should be noted that we did not follow up candidates where archival spectra from the past two decades showed no variability (irrespective of the selection criteria). We used the Wide Field Spectrograph (WiFeS, Dopita et al. 2010 ) integral field unit (IFU) on the Australian National University’s 2.3-m telescope at Siding Spring to obtain new spectra of our candidates to confirm that they are indeed CLAGN. WiFeS has a field of view of 25 × 38 arcsec 2 , divided into 950 spaxels. The advantage of using an IFU for follow-up observations of candidates is that extraction aperture size can be matched to previous observations (e.g. the 7-arcsec fibre of 6dF, Jones et al. 2009 ). The wavelength coverage is 3800–9200 Å, which spans the H α , H β , and O iii lines at z 0.04, and we expect H α to show the most clear signs of change in CLAGNs. We observed in nod-and-shuffle mode taking at least three frames with 60s on object, 60s on sky, and 10 cycles per frame. This results in 40 min on object, 40 min on sky, and ∼15 min on overheads including telescope nod time, guide star re-acquisition and CCD readout. In total we allow ∼100 min per galaxy. Our observations were taken between 2018 July and 2019 March. We reduced our data with PyWiFeS, Python-based pipeline (Childress et al. 2014 ). We observed 15 CLAGN candidates over multiple observing sessions, the AGNs are presented in Table 4 . Table 4. CLAGN candidates that were observed with WiFeS between 2018 July and 2019 March. a New CLAGN that we have identified. b Known CLAGN. 4 SPECTRAL VARIABILITY AND NEW CLAGNS We next present the spectra of the new CLAGNs that we have identified using the selection criteria mentioned in Sections 2.2 – 2.4 , where we compare archival spectra of the galaxies with spectra taken using WiFeS. We plot archival spectra, where available, with the spectra taken using WiFeS to display the change. Multiplicative scaling has