6. Tables only in electronic form

   
Table 1: Observing log of Perseus galaxies
Notes :
feb93: CCD Thompson 1024x1024, pixel size=0.24
dec93: CCD Thompson 1024x1024, pixel size=0.48 (0.24 2x2 binned)
feb94: CCD Thompson 1024x1024, pixel size=0.24 (the observations in the x filter were done with an unknown filter, because of a mechanical fault).
dec94: CCD Tektronics 1024x1024, pixel size=0.30
feb95: CCD Tektronics 1024x1024, pixel size=0.30

   
Table 2: Galaxies classified as S from visual inspection of the plates OCA2842 and OCA2849 (all but two not presented in Paper I)
Notes:
BO= Butcher & Oemler 1985
GavI= Gavazzi, Garilli & Boselli 1990
GavIII= Gavazzi & Randone 1994
GavIV= Gavazzi, Boselli & Carrasco 1994
D80= Dressler 1980
kp1608= KPNO photographic plate (see Paper I)
run 7= CCD observations in March 1993 (see Paper I)

   
Table 3: Morphological description of spiral galaxies in Perseus

Description of Table 4 (Coma galaxies)

(1) and (2) Number in the abridged and unabridged versions of the Godwin, Metcalf & Peach (GMP) catalogue. (3) Number in Dressler's catalogue (Dressler 1980). (4) Usual designation, such as NGC, IC (Dreyer 1888), and RB (Rood & Baum 1967) numbers. (5) Asymptotic magnitude, in V (Johnson's system). (6) Logarithm of the effective radius, in units of arcsec (). (7) Logarithm of the semi major axis of the effective isophote, in units of arcsec (). (8) Mean SuBr inside the effective isophote, in V mag arcmin^-2. (9) Photometric evidence for a disk, coded as st (strong), cl (clear), ft (faint), or no (none). (10) Typical axis ratio, either its minimum value, if clearly defined, or its value at the effective isophote otherwise. (11) Location where the axis ratio was estimated, coded as ex (at its extremum), re (at the effective isophote), or co (if the value is the same at both locations). (12) Typical e₄ parameter, either its extremum value, if clearly defined, or its value at the effective isophote otherwise. The estimates are in %. (13) Location where the e₄ parameter was estimated, coded as ex (at its extremum), re (at the effective isophote), or co (if the value is the same at both locations). (14) Axis ratio in the envelope, i.e. at the isophote = 24.85 mag arcsec^-2. (15) Amplitude of isophotal twist in the range of reliable measurements, in degrees. (16) Detection of a bar, coded as follows : bar (bar seen), bar? (bar suspected), -no (no bar seen). (17) Detection and classification of a disk, coded as follows: emDi (embedded disk), miDi (mixed disk), exDi (extended disk), -?Di (detected but unclassified disk), -no- (no disk seen). (18) Detection of a spiral pattern, coded as follows: spiP (spiral pattern seen), spiP? (spiral pattern suspected), -no- (no spiral pattern seen). (19) Classification of an envelope, coded as follows: spH (spheroidal halo), thD (thick disk), exD (extended disk), pec (peculiar envelope), -?- (unclassified envelope). (20) Our morphological classification, coded as follows: boE (boxy E), unE (undetermined E), diE (disky E), SA0, SAB0, SB0, Sa, etc., S... (spiral of unknown stage). (21) An asterisk refers to a note in Sect. 5 about specific features such as important dust pattern, ring or lens, low SuBr, f₄-asymmetry, etc., and about uncertainties of various sources.

Note that, when a parameter has not been measured, or when a specific morphological component has not been studied, the relevant code is replaced by a dash.

   
Table 4: Morphological description of early-type galaxies in Coma

Notes to Table 4 (Coma galaxies)

0552: dust along the major axis. Type given in Paper I confirmed. 0718: two bumps on the major axis profile. Inner ring and lens. Type given in Paper I confirmed. 0750R: image of run 9 (see Paper I). 0750: 30 degree twist at r arcsec on the V image. same twist in R, but image not deep enough for full confirmation. Type given in Paper I confirmed. 0754: type given in Paper I fully confirmed. 0828: E boxy outside r_e and possibly disky inside. In Paper I it is classified diE because the boxiness of the outer region is not detected with certainty, partly because of the presence of a companion galaxy at 15 arcsec in the minor axis direction. 0857: the bar suspected in Paper I is not detected in our better images. 0908: slightly boxy isophotes out to r_e, then slightly disky isophotes. Uncertain detailed classification. 0967: focus problems made the PSF slightly elongated in the NS direction and galaxy data inside 3 arcsec not usable. 1109: the bar suspected in Paper I is detected. 1154: asymmetric with respect to its major axis. 1432: classified SA0/a by morphologists, probably because of the low contrast spiP. 1564: ellipticity and e₄ profile unusual for a lenticular galaxy. It seems to be asymmetric. 1594: the better data with respect to Paper I allow us to classify it elliptical. 1625: the bar suspected in Paper I is detected. 1844: isophote twist toward GMP 1852. Type given in Paper I confirmed. 1852: isophote twist opposite to GMP 1844, bar suspected but nearby star slightly elongated in the same direction. Type given in Paper I confirmed. 1925: large isophote twist at low SuBr. 2085: rich in globular clusters. The better data with respect to Paper I allow us to classify it elliptical. 2109: focus problems made the PSF slightly elongated in a direction orthogonal to the galaxy major axis. Data inside 4 arcsec are not usable. Also classified unE with CFH data of Paper I. 2134: rich in globular clusters. Its intensity profile obeys the r^-1.44 law from 1 arcsec out to 60 arcsec, putting this galaxy in the D class following Schombert (1987) and Tonry (1987). Classified as unE in Paper I from a slightly shallower image. 2283: the analysis is made difficult by the crowded field and a nearby saturated star.

Description of Table 5 (Perseus galaxies)

(1) Zwicky name. (2) Usual designation, such as NGC, UGC (Nilson 1976), T (Tifft 1978), BGP (Bucknell, Godwin & Peach 1979) and CR (Chincarini and Rood 1977) numbers. (3) Flag for filter or observational material. (4) Asymptotic magnitude. (5) Logarithm of the effective radius, in units of arcsec. (6) Logarithm of the semi major axis of the effective isophote, in units of arcsec. (7) Mean SuBr inside the effective isophote, in mag arcmin^-2. (8) to (12) Same as columns (9) to (13) of Table 4. (13) Axis ratio in the envelope, i.e. at the isophote V=24.85 or R=24 mag arcsec^-2. (14) to (20) Same as columns (15) to (21) of Table 4.

Note that a "(1)" in the table means that the parameter has not been computed because the night was not photometric, or because of the pan-chromaticity of the plate.

   
Table 5: Morphological description of early-type galaxies in Perseus

Notes to Table 5 (Perseus galaxies)

T40: the identification of Tifft 40 is doubtful. The observed galaxy is the nearest one to the Tifft 40 coordinates. A brighter (spiral) galaxy is 4 arcmin SE, which is more likely Tifft 40, if we believe Kent & Sargent's (1983) classification (S). 540-32: companion of NGC 1177, roundish. 540-33: peanut shaped SA0. 540-41: face on. 540-46: the small field of view did not allow us to image the whole envelope. 540-57: there is a bump on the major axis SuBr profile at V=23 mag arcsec². 540-73: this galaxy is 19 arcsec from a very bright star, preventing the detailed structural analysis. However, bulge and disk are clearly visually detected as a change of axis ratio and as a bump on the major axis profile, leading to our estimated type. The galaxy is edge-on. 540-74: our morphological type fully confirms that of Poulain, Nieto & Davoust (1992). 540-76: strong, but smooth, dust lane on major axis. A second faint dust lane is present with an inclination of about 10 degrees with respect to the galaxy major axis 10 arcsec Southward. 540-81: dust just in the inner part of this galaxy observed near the CCD's edge. 540-89: a very brigh star 20 arcsec from the galaxy center perturbs the isophotal analysis at that radius. e₄ never dominates the Fourier terms, f₄ asymmetry. 540-106: almost edge-on, a bit S-shaped, asymmetric. 540-114: the c/a profile starts to rise at fainter SuBr than sampled by plate, thus explaining the difference in the envelope classification. 541-15S: face on. 541-16N: the galaxy Zw 540-16S and nearby stars prevented us from measuring the shape of this galaxy's envelope. 541-16S: the galaxy 540-16N makes it impossible to measure the SuBr profile at r>12 arcsec.