In Figure 3 we present greyscale maps corresponding to the R-band and to continuum-subtracted H images obtained for the 114 galaxies in our sample. A blow-up of the nuclear region is also shown in the upper right-hand corner of each image, rescaled in intensity to emphasize details. The size of the compass shown in each of the images is 0.5 kpc at the distance of the corresponding galaxy. The average limiting surface brightness of the main images (3) are 24.6 mag arcsec-2, 24.3 mag arcsec-2, and 7 × 10-17 ergs-1 cm-2 arcsec-2 for B, R, and H, respectively.
Figure 3. R (left) and continuum-subtracted H (right) images of the galaxies in the sample. The compass is 0.5kpc in size in each image. A blow-up image of the galaxy nuclear region is also shown. |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Figure 3. R and continuum-subtracted H images of the galaxies in the sample (cont.) |
Within the galaxy sample studied only three galaxies were not detected by us in H emission, namely Mrk 709, UCM 1446+2312, and UGC 4703 NOTES02. In the case of Mrk 709 the galaxy recession velocity provided by NED (1,197 km s-1), which was taken from the 21 cm-line velocity data published by van Zee, Haynes, & Giovanelli (1995), differs significantly from that published by Terlevich et al. (1991) (~ 15,000 km s-1) and recently confirmed by E. Pérez-Montero (private communication). This leads us to suggest that the low-redshift HI emission detected by van Zee et al. (1995) is not related to Mrk 709, but maybe with another object in the beam that, according to our data, does not show significant ionized gas emission. For UCM 1446+2312 the uncertainty in the recession velocity (determined from the position of the H line in objective-prism photographic plates; Alonso et al. 1999) is ~ ± 1,200 km s-1. Therefore, the line-emission arising from this object might well be beyond the wavelength region covered by the 20Å-wide filter used. Finally, UGC 4703 NOTES02 forms with UGC 4703 NOTES01 an interacting pair where only the latter shows H emission. This suggests that UGC 4703 NOTES02 may have either exhausted most of its gas early during its evolution, or it may have lost it as consequence of the interaction with UGC 4703 NOTES01. Is it important to note that, as already pointed out by Cairós et al. (2001a) and we have discussed in Section 3, most of the BCD galaxies were originally identified by their high surface brightness and blue optical colors. Therefore, some of them may be expected to show very low H equivalent widths (EW) (i.e. they are BCDs but they should not be then classified as HII galaxies). Some examples of this may be Mrk 1423 and I Zw 115 (see Section 8).
The maps presented in Figure 3 show that most of the galaxies in our sample have an extended, low-surface-brightness halo visible in the continuum images. Such halos, commonly associated with an evolved stellar population (Papaderos et al. 1996; Cairós et al. 2001a, b and references therein), are usually more extended than the region showing H emission, except perhaps in the case of the most compact objects (I Zw 18, HS 0822+3542, Pox 186). In Paper II we analyze the structural properties of this low-surface brightness component. With regard to the morphology in H the inspection of our images show that 83 galaxies in our sample (73%) show star formation activity distributed over more than one region. In particular, in 45 galaxies (39%) we are able to distinguish 4 regions or more. Only 28 galaxies show their morphology in the light of H to be dominated by only a single, nuclear HII region. It is worth noting that the median distance and seeing for those galaxies showing only one single star-forming region are 23 Mpc and 1.4 arcsec respectively, while the galaxies with multiple regions are typically at 19 Mpc and have 1.5 arcsec seeing. Clearly, the difference between these values is not large enough to explain the different number of regions detected purely in terms of a differing spatial resolution.
Based only on broad-band optical imaging data, Loose & Thuan (1986) undertook a morphological classification of BCD galaxies. They defined four different groups:
The classification of a galaxy as nE or iE BCD is been mainly determined by the shape of the inner isophotes: regular in the case of nE, and irregular for the iE BCDs. However, the greyscale maps presented in Figure 3 show that, in some cases, despite the continuum isophotes in the inner region being regular, the H images may show a complex structure composed of several individual HII regions. An example of this behavior is seen in Mrk 409, where the inner R-band isophotes are regular (which would lead one to classify this galaxy as a nE BCD), but the H emission shows the presence of a ring composed of at least 5 HII regions (see Figure 3). In cases like that of Mrk 409 we have made use of the information provided by the H images, and the galaxies have been reclassified as iE BCDs. The presence of a ring of star-forming regions around the nucleus of the galaxy has been observed in a total of 4 objects in our sample including Mrk 409, namely Mrk 86 (see Gil de Paz et al. 2000b, c; 2002), Mrk 400, Mrk 409, and VCC 0655. The radius of this ring ranges from 0.5 to 1.0 kpc. In these cases we have added a letter `r' to the morphological type of the objects.
The results of the morphological classification are given in Table 5. For the objects with detected H emission 27 out of 111 (24%) were classified as nE BCDs, 37 (33%) as iE, and 39 (35%) as iI. For the 39 iI BCDs, 11 are "cometary" (iI,C) and 10 are "mergers" (iI,M). In only 8 galaxies did we not detect any underlying/extended R-band continuum light (that would be otherwise be associated with an old stellar population) and, consequently, they were classified as i0 BCDs. Within this group are the objects with the lowest metallicity in our sample (I Zw 18, Tol 65, UCM 1612+1308). For comparison, within their sample of 28 BCDs, Cairós et al. (2001a, b) found 21% of nE, 39% of iE, and 32% of iI BCDs (7% and 14% of the total were iI,C and iI,M BCDs, respectively).
Object Name | B | R | B-R | fH | MB | log LH | T | EWH |
(mag) | (mag) | (mag) | (10-14 erg/s/cm2) | (mag) | (erg/s) | (Å) | ||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
IC 10 | 5.75±0.03 | 5.45±0.08 | 0.30±0.08 | 51000±3700 | -19.25 | 40.79 | iI,C | 36 |
HS 0029+1748 | 16.74±0.05 | 15.93±0.14 | 0.81±0.15 | 19.1±2.5 | -15.87 | 40.40 | nE | 228 |
Haro 14 | 13.65±0.05 | 12.91±0.14 | 0.74±0.15 | 34±4 | -17.08 | 39.90 | iE | 22 |
UM 285 | 17.00±0.03 | 17.03±0.08 | -0.02±0.08 | 5.8±0.4 | -15.25 | 39.74 | iI,C | 187 |
UCM 0049-0045 | 14.76±0.04 | 13.36±0.25 | 1.39±0.25 | 20±4 | -17.18 | 40.14 | iE | 20 |
UM 323 | 16.09±0.04 | 15.24±0.08 | 0.85±0.09 | 14.1±1.2 | -16.17 | 40.13 | iE | 83 |
Mrk 996 | 15.01±0.03 | 14.08±0.14 | 0.93±0.14 | 54±7 | -16.87 | 40.56 | nE | 109 |
UM 133 | 15.41±0.03 | 14.51±0.14 | 0.90±0.14 | 20±3 | -16.50 | 40.15 | iI,C | 60 |
UM 382 | 18.20±0.04 | 17.83±0.22 | 0.37±0.22 | 2.6±0.5 | -15.33 | 39.90 | iI,C | 170 |
UM 404 | 18.48±0.05 | 18.40±0.12 | 0.08±0.13 | 3.6±0.4 | -15.09 | 40.06 | i0 | 455 |
KUG 0207-016A | 15.24±0.05 | 14.77±0.12 | 0.47±0.13 | 14.3±1.5 | -18.28 | 40.64 | iI | 54 |
UM 408 | 17.46±0.16 | 16.70±0.12 | 0.75±0.20 | 6.8±0.8 | -16.12 | 40.34 | nE | 161 |
UM 417 | 18.37±0.07 | 17.73±0.13 | 0.64±0.15 | 4.4±0.5 | -14.58 | 39.90 | iI,C | 279 |
Mrk 370 | 13.49±0.03 | 12.21±0.12 | 1.28±0.13 | 70±7 | -16.94 | 40.10 | iE | 24 |
Mrk 600 | 14.85±0.03 | 14.82±0.15 | 0.03±0.15 | 24±3 | -15.97 | 39.78 | iE | 96 |
NGC 1522 | 14.03±0.01 | 13.22±0.06 | 0.81±0.06 | 59.9±0.6 | -16.10 | 39.91 | iE | 54 |
NGC 1705 | 13.09±0.01 | 12.19±0.06 | 0.90±0.06 | 253±3 | -15.45 | 39.90 | iE | 90 |
II Zw 33 | 14.21±0.03 | 13.34±0.11 | 0.86±0.11 | 93±9 | -18.77 | 41.24 | iI | 95 |
II Zw 33B | 16.87±0.04 | 15.67±0.11 | 1.21±0.12 | 5.1±0.5 | -16.12 | 39.98 | iI | 43 |
II Zw 40 | 11.87±0.04 | 11.10±0.09 | 0.77±0.09 | 1554±120 | -18.09 | 41.25 | iI,M | 217 |
Tol 0610-387 | 15.90±0.05 | 14.87±0.06 | 1.03±0.08 | 16±1 | -15.89 | 40.01 | iE | 68 |
Mrk 005 | 15.13±0.04 | 14.56±0.13 | 0.57±0.13 | 28±3 | -15.47 | 39.77 | iI,C | 89 |
Mrk 007 | 14.29±0.03 | 13.49±0.18 | 0.79±0.18 | 36±6 | -19.00 | 40.95 | iI | 41 |
Mrk 86 | 12.07±0.03 | 11.49±0.11 | 0.58±0.11 | 241±23 | -17.13 | 40.14 | iE,r | 44 |
HS 0822+3542 | 17.85±0.03 | 17.76±0.14 | 0.09±0.14 | 7.4±0.9 | -12.18 | 38.95 | iI,C | 546 |
UGC 4483 | 15.14±0.03 | 14.56±0.13 | 0.58±0.13 | 36±4 | -12.38 | 38.64 | iI,C | 115 |
UGC 4703N1 | 15.86±0.04 | 15.01±0.03 | 0.85±0.05 | 24.9±0.5 | -17.58 | 40.85 | iI,M | 120 |
UGC 4703N2 | 17.04±0.04 | 16.10±0.03 | 0.94±0.05 | ... | -16.39 | ... | ... | ... |
Mrk 1416 | 16.32±0.03 | 15.75±0.02 | 0.58±0.04 | 19.4±0.8 | -16.32 | 40.42 | iI | 191 |
Mrk 108 | 15.15±0.03 | 14.66±0.08 | 0.49±0.08 | 73±5 | -16.54 | 40.62 | iI,M | 275 |
Mrk 400 | 14.30±0.04 | 13.63±0.11 | 0.67±0.12 | 39±4 | -18.41 | 40.76 | iE,r | 51 |
NGC 2915 | 11.93±0.01 | 10.96±0.06 | 0.97±0.06 | 209±3 | -15.85 | 39.51 | iE | 23 |
I Zw 18 | 16.05±0.04 | 16.24±0.07 | -0.18±0.08 | 35.2±2.4 | -14.45 | 39.83 | i0 | 679 |
Mrk 1418 | 13.86±0.03 | 12.61±0.19 | 1.25±0.20 | 95±16 | -16.42 | 40.17 | iE | 49 |
Mrk 1423 | 14.90±0.03 | 13.52±0.10 | 1.38±0.11 | 6.8±0.4 | -16.65 | 39.53 | nE | 8 |
SBS 0940+544C | 17.18±0.04 | 17.05±0.10 | 0.13±0.11 | 5.1±0.5 | -14.73 | 39.55 | iI,M | 165 |
Mrk 709 | 16.32±0.03 | 15.65±0.02 | 0.67±0.04 | ... | -14.66 | ... | ... | ... |
Mrk 1426 | 15.88±0.04 | 15.44±0.12 | 0.44±0.12 | 7.8±0.8 | -16.24 | 39.82 | iE | 55 |
UGCA 184 | 15.99±0.04 | 15.80±0.10 | 0.19±0.11 | 14.0±1.4 | -15.82 | 39.95 | iI | 142 |
Mrk 409 | 14.37±0.03 | 13.33±0.05 | 1.04±0.06 | 29.2±1.7 | -17.27 | 40.20 | iE,r | 29 |
Tol 001 | 15.74±0.05 | 15.48±0.07 | 0.26±0.09 | 12.0±0.9 | -16.09 | 39.89 | iE | 88 |
Tol 002 | 14.06±0.01 | 13.34±0.06 | 0.72±0.06 | 121.3±1.8 | -15.19 | 39.86 | iE | 127 |
NGC 3125 | 13.05±0.01 | 12.25±0.06 | 0.80±0.06 | 342±4 | -16.79 | 40.55 | iE | 131 |
SBS 1006+578 | 16.42±0.04 | 15.78±0.11 | 0.64±0.12 | 5.6±0.6 | -15.34 | 39.53 | iE | 53 |
Haro 2 | 13.39±0.04 | 12.87±0.11 | 0.52±0.11 | 157±16 | -18.28 | 40.94 | nE | 105 |
Mrk 1434 | 16.77±0.04 | 16.43±0.13 | 0.33±0.14 | 16.4±2.0 | -15.85 | 40.34 | i0 | 324 |
Haro 3 | 13.22±0.04 | 12.61±0.13 | 0.61±0.14 | 275±30 | -17.57 | 40.83 | iE | 148 |
SBS 1054+504 | 16.08±0.04 | 15.46±0.15 | 0.62±0.15 | 4.3±0.5 | -15.44 | 39.32 | nE | 30 |
Haro 4 | 15.59±0.04 | 15.44±0.17 | 0.15±0.17 | 66±12 | -14.14 | 39.79 | iI | 589 |
VII Zw 403 | 14.11±0.04 | 13.58±0.11 | 0.53±0.12 | 59±6 | -14.30 | 39.21 | iE | 75 |
Mrk 178 | 14.15±0.04 | 13.60±0.09 | 0.55±0.10 | 109±9 | -13.96 | 39.36 | iI,M | 146 |
UM 439 | 14.77±0.03 | 14.09±0.06 | 0.67±0.07 | 42.8±2.5 | -15.96 | 40.00 | iE | 88 |
Mrk 1450 | 15.75±0.05 | 15.09±0.09 | 0.67±0.10 | 42±4 | -15.08 | 40.04 | nE | 234 |
UM 452 | 15.25±0.03 | 14.07±0.11 | 1.19±0.12 | 4.7±0.5 | -16.20 | 39.33 | nE | 9 |
SBS 1147+520 | 16.95±0.05 | 15.98±0.09 | 0.97±0.10 | 1.4±0.2 | -14.44 | 38.78 | nE | 16 |
Tol 17 | 15.99±0.05 | 15.05±0.06 | 0.94±0.08 | 17.5±1.0 | -16.20 | 40.20 | iE | 86 |
UM 455 | 17.02±0.03 | 16.26±0.01 | 0.77±0.03 | 6.9±0.3 | -16.62 | 40.38 | iI | 105 |
UM 456 | 15.37±0.03 | 14.66±0.01 | 0.71±0.03 | 24.5±0.9 | -16.48 | 40.21 | iI | 85 |
UM 456A | 16.71±0.03 | 16.05±0.01 | 0.66±0.03 | 4.20±0.16 | -15.24 | 39.48 | iI | 51 |
Pox 4 | 15.27±0.04 | 14.88±0.10 | 0.38±0.11 | 94±9 | -18.18 | 41.43 | iI,M | 478 |
ESO 572-G025 | 15.02±0.04 | 14.07±0.03 | 0.94±0.05 | 60.6±1.6 | -16.80 | 40.59 | nE | 125 |
VCC 0001 | 15.80±0.03 | 14.42±0.01 | 1.37±0.04 | 1.90±0.06 | -15.22 | 38.77 | nE | 5 |
Mrk 1313 | 16.02±0.03 | 15.50±0.06 | 0.52±0.06 | 8.6±0.5 | -16.49 | 40.02 | i0 | 64 |
VCC 0130 | 17.05±0.05 | 16.27±0.01 | 0.78±0.05 | 1.75±0.06 | -13.97 | 38.73 | iE | 26 |
Haro 8 | 14.27±0.03 | 13.20±0.11 | 1.07±0.11 | 43±4 | -16.75 | 40.12 | nE | 38 |
UM 491 | 15.54±0.03 | 14.95±0.07 | 0.59±0.08 | 8.8±0.6 | -16.66 | 39.90 | nE | 39 |
ISZ 399 | 14.18±0.01 | 12.99±0.06 | 1.19±0.06 | 41.8±2.4 | -15.99 | 39.77 | nE | 30 |
VCC 0459 | 14.95±0.05 | 14.13±0.01 | 0.83±0.05 | 20.4±0.5 | -16.07 | 39.80 | iI | 42 |
VCC 0655 | 13.32±0.04 | 12.12±0.03 | 1.20±0.05 | 75.1±2.2 | -17.70 | 40.36 | iE,r | 24 |
Tol 65 | 17.26±0.04 | 16.84±0.03 | 0.42±0.05 | 24.9±1.0 | -15.52 | 40.59 | i0 | 916 |
VCC 0848 | 15.03±0.05 | 14.10±0.01 | 0.93±0.05 | 14.2±0.4 | -15.99 | 39.64 | iI,M | 28 |
Mrk 209 | 14.15±0.03 | 13.94±0.13 | 0.21±0.13 | 173±20 | -14.67 | 39.84 | iE | 349 |
Mrk 1329 | 14.08±0.03 | 13.38±0.09 | 0.70±0.10 | 67±6 | -16.94 | 40.31 | iI,C | 70 |
UGCA 290 | 15.67±0.03 | 15.04±0.13 | 0.63±0.13 | 6.2±0.9 | -13.46 | 38.52 | iI,M | 29 |
VCC 1750 | 16.73±0.03 | 15.93±0.05 | 0.80±0.06 | 3.8±0.2 | -14.29 | 39.06 | iI | 41 |
Haro 9 | 13.02±0.05 | 12.24±0.10 | 0.78±0.11 | 221±21 | -17.91 | 40.79 | nE | 82 |
NGC 4861 | 12.68±0.03 | 11.91±0.09 | 0.76±0.09 | 560±5 | -17.82 | 41.03 | iI,C | 160 |
UM 533 | 14.63±0.04 | 13.64±0.11 | 0.99±0.11 | 31±3 | -15.71 | 39.71 | iE | 41 |
Mrk 450 | 14.44±0.05 | 13.65±0.10 | 0.79±0.11 | 11.8±1.1 | -16.13 | 39.38 | iE | 15 |
NGC 5058 | 14.05±0.03 | 13.37±0.07 | 0.68±0.08 | 45±3 | -16.58 | 39.99 | iI | 47 |
PGC 046448 | 15.47±0.03 | 14.51±0.01 | 0.96±0.03 | 8.9±0.4 | -17.48 | 40.21 | iE | 26 |
Pox 186 | 17.73±0.03 | 17.39±0.01 | 0.35±0.04 | 14.8±0.5 | -13.20 | 39.62 | i0 | 907 |
Tol 35 | 14.17±0.03 | 13.22±0.05 | 0.94±0.06 | 83±4 | -17.99 | 40.86 | iE | 76 |
SBS 1331+493 | 14.87±0.03 | 14.16±0.17 | 0.71±0.17 | 25±4 | -15.11 | 39.47 | iE | 54 |
Tol 85 | 16.51±0.03 | 15.99±0.01 | 0.52±0.03 | 20.5±0.9 | -16.96 | 40.78 | iI | 261 |
Mrk 67 | 16.10±0.03 | 15.34±0.08 | 0.76±0.09 | 25.1±2.0 | -14.67 | 39.79 | nE | 170 |
Mrk 1480 | 16.17±0.03 | 15.56±0.08 | 0.61±0.08 | 13.9±1.0 | -16.01 | 40.09 | nE | 111 |
Mrk 1481 | 16.19±0.03 | 15.57±0.06 | 0.62±0.07 | 4.4±0.3 | -15.99 | 39.60 | iI,M | 34 |
Tol 1345-420 | 15.87±0.03 | 15.00±0.03 | 0.87±0.05 | 33.5±1.1 | -16.67 | 40.62 | nE | 165 |
HS 1400+3927 | 17.04±0.05 | 15.94±0.10 | 1.10±0.12 | 8.6±0.8 | -14.58 | 39.66 | nE | 97 |
SBS 1415+437 | 15.43±0.03 | 14.77±0.12 | 0.66±0.13 | 50±6 | -14.59 | 39.79 | iI,C | 203 |
SBS 1428+457 | 15.42±0.05 | 14.67±0.09 | 0.75±0.10 | 48±4 | -17.32 | 40.85 | iI | 173 |
Tol 1434+032 | 15.86±0.03 | 15.42±0.06 | 0.44±0.07 | 11.3±0.7 | -15.80 | 39.79 | iI | 78 |
Mrk 475 | 16.20±0.03 | 15.67±0.07 | 0.53±0.08 | 35.6±2.4 | -13.73 | 39.60 | nE | 355 |
HS 1440+4302 | 17.58±0.05 | 16.54±0.11 | 1.04±0.12 | 4.1±0.4 | -15.32 | 39.85 | nE | 80 |
HS 1442+4250 | 15.55±0.05 | 15.01±0.07 | 0.54±0.09 | 14.7±1.1 | -14.90 | 39.42 | iE | 69 |
UCM 1446+2312 | 15.77±0.03 | 14.52±0.09 | 1.25±0.10 | ... | -16.96 | ... | ... | ... |
Tol 1448+116 | 16.15±0.05 | 15.95±0.10 | 0.21±0.12 | 8.9±0.9 | -16.02 | 39.90 | iE | 101 |
II Zw 70 | 14.84±0.12 | 14.29±0.13 | 0.55±0.18 | 83±11 | -16.52 | 40.54 | iI | 217 |
II Zw 71 | 14.45±0.15 | 13.54±0.12 | 0.91±0.19 | 40±4 | -16.91 | 40.23 | iI | 49 |
I Zw 115 | 15.04±0.09 | 14.14±0.08 | 0.91±0.12 | 1.88±0.16 | -15.24 | 38.47 | iE | 4 |
SBS 1533+574 | 16.02±0.10 | 15.30±0.10 | 0.72±0.14 | 30±3 | -17.46 | 40.95 | iE | 198 |
I Zw 123 | 15.42±0.10 | 14.85±0.08 | 0.57±0.13 | 35±3 | -14.92 | 39.76 | nE | 151 |
HS 1609+4827 | 15.11±0.11 | 14.55±0.09 | 0.56±0.14 | 20.9±1.8 | -18.04 | 40.66 | nE | 64 |
UCM 1612+1308 | 17.21±0.14 | 17.31±0.07 | -0.10±0.15 | 7.1±0.5 | -16.42 | 40.38 | i0 | 313 |
UGCA 412 | 15.55±0.05 | 14.62±0.09 | 0.92±0.11 | 35±3 | -17.52 | 40.85 | nE | 120 |
HS 1704+4332 | 18.41±0.03 | 17.87±0.08 | 0.54±0.09 | 3.3±0.3 | -14.13 | 39.61 | i0 | 236 |
NGC 6789 | 13.74±0.03 | 12.69±0.07 | 1.05±0.08 | 32.7±2.0 | -14.04 | 38.70 | iE | 18 |
Tol 1924-416 | 13.97±0.04 | 13.50±0.03 | 0.47±0.05 | 297±5 | -19.09 | 41.78 | iE | 413 |
Tol 1937-423 | 15.14±0.04 | 14.25±0.03 | 0.89±0.05 | 21.7±0.4 | -17.96 | 40.66 | iE | 50 |
Mrk 900 | 14.17±0.03 | 13.56±0.12 | 0.61±0.13 | 55±6 | -17.20 | 40.37 | nE | 68 |
Mrk 314 | 13.55±0.03 | 13.12±0.24 | 0.43±0.24 | 64±13 | -18.99 | 40.90 | iI,M | 53 |
Mrk 324 | 15.17±0.03 | 14.60±0.13 | 0.57±0.14 | 16.0±1.9 | -16.84 | 40.09 | nE | 51 |
Mrk 328 | 14.93±0.05 | 14.18±0.09 | 0.74±0.10 | 17.4±1.4 | -16.82 | 40.02 | nE | 38 |
Note. - Columns stand for: (1) Galaxy name (2) B-band integrated magnitude and its 1- error. (3) R-band integrated magnitude and its 1- error. (4) (B - R) integrated color its 1- error. (5) Integrated H flux and error in units of 10-14 erg s-1 cm-2 (corrected for underlying stellar absorption). (6) B-band absolute magnitude. (7) H luminosity in erg s-1. (8) Morphological type according to the classification of Loose & Thuan (1986). (9) Equivalent width of H in Å. Magnitudes, colors, fluxes, and luminosities are corrected for Galactic extinction but not for internal extinction. |
It is worth mentioning that, although the fraction of BCDs with elliptical envelopes is < 60 per cent, the four galaxies where a ring of star-forming regions was found are all iE BCDs. This fact suggests that the shaping of these rings requires a highly symmetric distribution of the galaxy stellar and total mass.