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tokens: in any stripping of disk stars, as required in the harassment scenario. In addition, Aguerri ( 2016 ) concluded, based on his analysis of the – n diagram, that most dwarf ETGs in clusters are not transformed disk galaxies. In CG 611, minor mergers may have brought in some gas and stars in a clumpy manner, which is known to lead to the growth of disks, including counter-rotating cores and halos (Sancisi et al. 2008 ; González-Samaniego et al. 2014 ; Lane et al. 2015 ; Christensen et al. 2016 ). 25 25 https://www.youtube.com/watch?v=_Ssc1GsqHds As noted by Genel et al. ( 2010 ), minor mergers and smooth accretion, rather than major mergers, dominate galaxy growth (see also Murali et al. 2002 ; Semelin Combes 2005 ; Maller et al. 2006 ), and this supply channel also favors the formation of disks. Smooth gas flow onto a galaxy can occur via spherical accretion of ∼10 4 –10 5 K halo gas (e.g., White Frenk 1991 , see their Section 7; Birnboim Dekel 2003 ) or more directly from unshocked cold streams (e.g., Kereš et al. 2005 ; Dekel Birnboim 2006 ; Brooks et al. 2009 ; Dekel et al. 2009 ; Cornuault et al. 2016 ). This cold mode of delivery may be the most efficient of the mechanisms (Genel et al. 2010 ; Lu et al. 2011 ; van de Voort et al. 2011 ) and Pichon et al. ( 2011 ) have revealed how these cold gas streams can build a disk in a coherent planar manner (see also Danovich et al. 2012 , 2014 ; Prieto et al. 2013 ; and Stewart et al. 2013 ). Examining the kinematics of a larger sample of isolated dwarf ETGs will enable one to compare their properties with cluster dwarf ETGs and in so doing learn about their collective origin. For example, Paudel et al. ( 2010 ) have suggested that old metal-poor dwarf ETGs found in the central high-density regions of clusters may have formed along with the cluster while the younger more metal-rich dwarf ETGs (which tend to have disk features) have fallen in at a later time. While plausible, the assumption that the infalling galaxies were disk galaxies that underwent a structural transformation may need revising if isolated dwarf ETGs already have the same structural and kinematic properties as this cluster population. CG 611 is one such galaxy that suggests they do, and Janz et al. ( 2017 ) presents a further eight such galaxies. A related issue is the dominance at low masses of dwarf ETGs in clusters and the prevalence of (higher mass) Scd-Im galaxies in the field. Although we do not answer this question, obviously past claims that have attempted to answer this solely in terms of harassment and transformation of late-type galaxies need to be reconsidered, because dwarf ETGs similar to those in clusters are now known to also exist in the field. There is a formation channel for dwarf ETGs that does not involve the harassment of disk galaxies. In the Λ cold dark matter (ΛCDM) model of galaxy formation, low-mass dwarf galaxies naturally form, and help to build up bigger galaxies. One can speculate that these small