continuum of galaxy properties across both samples. The LVL sample [@dale09] includes both early- and late-type galaxies, and in particular includes 7 objects which identified as BCDs in the Palomar/Las Campanas Atlas of BCDs [@gildepaz03; @kennicutt08].

On subsequent plots and figures we take care to indicate these individual populations (BCD, irregular/spiral, early-type) within the LVL sample. Our goal is not to demarcate BCDs from “normal” dwarf galaxies, but rather to explore the extremes of dwarf galaxy evolution. BCDs are often characterized by their significant star formation rates, but they are unique in other aspects as well. Throughout this work we will discuss the continuum of dwarf galaxy properties, and show the extreme position that BCDs occupy.

[sed\_biggrid-crop.eps]{} (20.91,81.6) [![image](UM323_i.eps){width="1.1cm"}]{} (20.91,45.0) [![image](Mk36_i.eps){width="1.1cm"}]{} (20.91,26.69) [![image](UM462_i.eps){width="1.1cm"}]{} (20.91, 8.32) [![image](Mk324_i.eps){width="1.1cm"}]{}

(39.2,81.6) [![image](UM408_i.eps){width="1.1cm"}]{} (39.2,63.3) [![image](CG10_i.eps){width="1.1cm"}]{} (39.2,45.0) [![image](UM439_i.eps){width="1.1cm"}]{} (39.2,26.69) [![image](Mk67_i.eps){width="1.1cm"}]{} (39.2, 8.32) [![image](Mk328_i.eps){width="1.1cm"}]{}

(57.49,81.6) [![image](Mk600_i.eps){width="1.1cm"}]{} (57.49,63.3) [![image](IZw18_i.eps){width="1.1cm"}]{} (57.49,45.0) [![image](Mk750_i.eps){width="1.1cm"}]{} (57.49,26.69) [![image](Mk475_i.eps){width="1.1cm"}]{}

(75.84,63.3) [![image](Was5_i.eps){width="1.1cm"}]{} (75.84,45.0) [![image](UM461_i.eps){width="1.1cm"}]{} (75.84,26.69) [![image](Mk900_i.eps){width="1.1cm"}]{} (75.21,81.65) [![image](IIZw40_i.eps){width="1.1cm"}]{}

SEDs
----

Figure \[allsed\] shows the complete set of observed SEDs for our sample of BCDs. The SEDs have been corrected for Galactic extinction [via @sfd98 for consistency with the LVL photometry] and are shown in flux units of mJy. Also shown are $100''$$\times$$100''$ color cutout images 