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Appendix A: Individual galaxy properties

A.1 HCG 37

This group is formed by five galaxies. The brighter member, HCG 37a, has a morphological type E7 (Hickson 1992). Coziol et al. (2004) classified galaxies HCG 37a, HCG 37b, HCG 37c, and HCG 37d as a dwarf LINER (dLINER), LINER, low luminosity AGN, and a star forming galaxy (SFG), respectively. HCG 37b is a near IR source (Allam et al. 1996). Verdes-Montenegro et al. (2001) report that 87% of the expected HI is missing in HCG 37. Four of the five galaxies of HCG 37 were observed (thanks to the field of view of the observations) and we detect H emission only in two of them. HCG 37a shows a central H emission, as was reported in Vilchez et al. (1998), however, the H profiles have a low signal-to-noise ratios. For this galaxy it was impossible to perform a rotation curve.

The monochromatic map of HCG 37d shows an extension of 13 arcsec (5.2 kpc). It has two peaks in the emission, as was found in Vilchez et al. (1998), the peak located in the northwest side of the galaxy being stronger. The continuum image shows the same peaks as the monochromatic image. The velocity field of this object is regular. The kinematic position angle is aligned with the optical one (as derived by Mendes de Oliveira 1992, at 2 h^-1 kpc), differing by only 2. The rotation curve of HCG 37d is not symmetric, and both sides do not match. The receding and approaching sides reach velocities of 60 km s^-1 and 53 km s^-1, respectively. The rotation curve does not reach the optical radius of the galaxy (R₂₅).

A.2 HCG 40

This quintet is composed by two early-type and three late-type galaxies. HCG 40a, HCG 40d, and HCG 40e were classified as radio sources (dLNR, LNR, and Sy2, respectively) in Coziol et al. (1998) and re-classified as no-emission galaxy, SFG and SFG in Coziol et al. (2004). HCG 40b is a no-emission galaxies and HCG 40c is an SFG (Coziol et al. 2004). HCG 40e is an FIR source (Allam et al. 1996). In the evolutive scenario of Verdes-Montenegro et al. (2001), HCG 40 is a type 3a group, where 89% of the expected HI mass is missing, which converts this group into a very evolved group.

The strongest H emission of the group is detected in two peaks, in the barred early-type spiral HCG 40d. This emission is very concentrated in the central region, probably associated with star formation at the end of the bar. We could not derive the rotation curve for this object.

We also detected H emission in the central regions of HCG 40a, and HCG 40b. Both galaxies were classified as early-type galaxies by Hickson (1992), E3 and S0, respectively. Interestingly, no emission was detected in Coziol et al. (2000) for these objects. As for HCG 40d, we could not obtain the rotation curve for these objects.

HCG 40c displays an extended monochromatic map. We detected a peak in the H emission in the southeast side of HCG 40c, coincident with the peak in the HI distribution shown in Verdes-Montenegro et al. (2001). Its velocity field is regular. The kinematic position angle does not change with radius. The rotation curve is symmetric, reaching a plateau at 6 kpc; however, this curve does not reach the optical radius R₂₅. At radii greater than 10 kpc, there is no more H emission, can be noted from the monochromatic image. HCG 40e shows a weak H emission on its disk. Both sides of the rotation curve do not match.

A.3 HCG 47

This quartet is formed by two pairs of galaxies. HCG 47a is an SBb (Hickson 1993) galaxy, showing a ring-shape structure on its southwest side (Fasano et al. 1994). Shimada et al. (2000) classify HCG 47a as an absorption-line galaxy. Hickson classify HCG 47b, HCG 47c and, HCG 47d as E3, Sc and Sd galaxies. HCG 47a, and HCG 47b are radio and FIR sources (Allam et al. 1996).

We detected a strong H emission in the ring of HCG 47a. On the other hand, HCG 47b shows weak intensity on its monochromatic map. The north side of HCG 47d shows the strongest H emission in this galaxy. However, we also note an extended emission in its disk. HCG 47c only shows a central knot in its monochromatic image, at the same position as for the continuum peak.

The velocity field shows higher velocities in the eastern part of the approaching side than in the western region, probably due to the presence of the ring. The kinematic position angle differs from the optical one, at 2 h^-1 kpc and at R₂₅, in 14 in both cases.

HCG 47d shows a regular velocity field. However, there is an offset between the kinematic and optical position angles of 32 and 23 (Mendes de Oliveira 1992, and HyperLeda, respectively). For HCG 47a and 47d it was impossible to obtain the rotation curves. The procedure developed by Epinat et al. (2008a) does not converge for these galaxies.

A.4 HCG 49

This small and compact quartet of galaxies shows an angular diameter of 0.9 arcmin (Hickson et al. 1982) (36 kpc) and is the most distant group in this sample (140 Mpc). HCG 49a and HCG 49b are late-type spiral galaxies, HCG 49c is an Im and HCG 49d is a E5 (Hickson 1993). In the scenario proposed in Verdes-Montenegro et al. (2001), HCG 49 is a well developed group, in the 3b phase, where the HI gas forms a large cloud containing all galaxies, with a single velocity gradient.

Fasano et al. (1996) note that HCG 49a seems to be a superposition of two galaxies, but our monochromatic map shows that the emission is coming from only one object. We analyzed the H profile in the region where the superposition appears, and we do not detect a defined profile. The monochromatic map of HCG 49a shows H emission across the disk of this object. This emission peaks at the same place in the monochromatic and the continuum map. This object shows a regular velocity field. The kinematic position angle differs only in 7 from the optical position angle at 2 h^-1 kpc. However, the difference is greater if we take the optical position angle at R₂₅ (16). The rotation curve is symmetric, and both sides match relatively well.

HCG 49b shows two strong peaks in the monochromatic map. One of them is located at the same position of the continuum maximum. The other bright knot is placed to the east of the galaxy. This knot shows an amplitude of 40 km s^-1. HCG 49b shows a perturbed velocity field. The kinematic position angle changes along the radius and it differs from the optical one at 2 h^-1 kpc in 17. However, at R₂₅ the optical and kinematic position angles reach a similar value (Table 3). The rotation curve of HCG 49b extended out to 12.5 arcsec (8.5 kpc). Both sides do not match. The receding side reaches values of 70 km s^-1 and the approaching side reaches values of 75 km s^-1.

The monochromatic map of HCG 49c shows a much lower intensity than HCG 49a, and b. We detected a bridge in the H emission between members b and c. The velocity field seems regular. However, a disagreement of 64 is observed between the kinematic, and optical position angles. Both sides of the rotation curve match from the center out to 2.5 kpc. Beyond this radius, no H emission is detected on the approaching side.

A.5 HCG 54

Hickson et al. (1989) classified this group as formed by three irregular galaxies and one Sdm galaxy. Verdes-Montenegro et al. (2002) found HI tidal tails and shells in the environment of HCG 54. They concluded that this group is a merger remnant.

From our monochromatic map, we note that HCG 54b shows the strongest H emission and its velocity field shows an amplitude of 30 km s^-1. HCG 54b and 54d also appear in the monochromatic map; however, it is difficult to get some information from the velocity field. HCG 54a is detected in the continuum image. Our data supports the scenario that HCG 54 is in fact one single galaxy and not a group. The nature of this object (Verdes-Montenegro et al. 2002) made us decide not to obtain any kinematic parameter of its members.

A.6 HCG 56

This quintet if formed by the late-type spiral HCG 56a, the SB0 HCG 56b, and three SO galaxies (c-e). Coziol et al. (2004) classified members a, d and e as star forming galaxies, HCG 56b as a Seyfert galaxy and HCG 56c as a no-emission line galaxy. Allam et al. (1996) detected members b-d at 25, 60, and 100 m. This group only shows 19% of its expected HI mass (Verdes-Montenegro et al. 2001). We present Fabry-Perot data for members a-d of this group. The monochromatic map of HCG 56a shows an extended emission along the disk. Peaks in the H emission are detected in the southern and northern side of this galaxy. Both peaks are located at the same distance with respect to the peak in the continuum image. The velocity field of HCG 56a seems to be regular. We noted that the approaching side is more extended than the receding side. We do not detect any misalignment between the kinematic and optical position angles for this galaxy. The rotation curve of HCG 56a is symmetric. The approaching and receding sides match from 3 to 18 (2 to 10 kpc), where the approaching side reaches a plateau. At radii larger than 18 , there is no data for the receding side; however, the approaching side reaches 35 .

We detected H emission at the center of the S0 galaxies HCG 56b, HCG 56c, and HCG 56d. Given that we only detected H emission at the center of these objects, it was not possible to obtain their rotation curves. No emission was detected in the bridge between members b, and c. Members b-d show a shift of 0.88 (one pixel) between their monochromatic and continuum peaks.

A.7 HCG 68

This group is formed by four early-type galaxies (HCG 68a, b, d, and e) and one barred spiral galaxy (HCG 68c) (Hikcson 1993). Shimada et al. (2000) classified members a-c as AGN; however, Coziol et al. (2004) classified HCG 68a as a no-emission galaxy. Verdes-Montenegro et al. (2001) detected only 33% of the expected HI mass for this group. We detected H emission in the monochromatic map of HCG 68a and b. However, the H profile is not well defined in either galaxies.

We detected several bright HII regions on the well-defined arms of HCG 68c. In the nuclear region, we detected a peak in H; nevertheless, no emission was detected across the bar of this object, as also reported by Vilchez et al. (1998). The maximum intensity in the monochromatic map of HCG 68c corresponds to an HII region located 60 from its center (northwest side of the galaxy). The velocity field of HCG 68c is quite regular. The kinematic and optical (R₂₅) position angles are aligned. The difference between the kinematic and optical position angles at 2 h^-1 is caused by the influence of the bar at this radius. The rotation curve of HCG 68c reaches 115 (19 kpc). In the first 10 , both sides of the rotation curve do not match, and we detected a bump in the approaching side, reaching 250 km s^-1. Both sides of the rotation curve match from 15 to 105 . At 40 , the approaching side shows higher velocities than the receding side, showing some bumps, probably produced by the crossing of spiral arms.

A.8 HCG 79

Mendes de Oliveira et al. (2003) presented the rotation curve of HCG 79d. Inclinations for HCG 79d are 64 and 78 (depending on whether is taken from the axis ratio given in Hickson 1993, or if it is taken from HyperLeda database). Durbala et al. (2008) showed continuum-subtracted H images of HCG 79 (for this group, see details in Durbala et al. 2008).

A.9 HCG 93

This quartet is formed by two barred spiral galaxies, HCG 93b, and HCG 93c, one E1 galaxy (HCG 93a), and the SB0 galaxy HCG 93d (Hickson 1993). Members a and c were classified as AGN by Shimada et al. (2000) and Coziol et al. (2004). HCG 93b is classified as an AGN by Shimada et al. (2004) but Coziol et al. (2004) classified it as a star forming galaxy. About 84% of the expected HI mass in HCG 93 is missing (Verdes-Montenegro et al. 2001). We presented Fabry-Perot data only for the barred spiral HCG 93b. Its monochromatic map shows H emission across the bar and two bright knots at the end of it, produced by star formation resulting from the compression of gas in this place, in agreement with its morphological type (Phillips 1996; Pisano et al. 2000). In the arms, we detected a few HII regions. The velocity field of HCG 93b shows a twist. We detected a disagreement between optical and kinematic position angles of 17 and 134 (Mendes de Oliveira et al. 2003, and HyperLeda, respectively). Both sides of the rotation curve of HCG 93b do not match. From 20 (7 kpc), the approaching side falls, reaching values of 120 km s^-1. The approaching side has an extension of 95  (30 kpc).

Appendix B: Individual maps and rotation curves

	Figure B.1: Maps for HCG 37. North is at the top and east to the left for all images in Figs. B.1 to B.10. HCG 37a is located to the southeast of HCG 37d. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.2: Maps for HCG 40. HCG 40a is located close to the center of the field and to the south west of HCG 40d. HCG 40e, b and c are located to the southeast of HCG 40a. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.3: Maps for HCG 47. HCG 47b and 47a are located at the bottom of the field. HCG 47c and 47d are located at the north of the field. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.4: Maps for HCG 49. From east to west: HCG 49a, 49b, 49c and 49d. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.5: Maps for HCG 54. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.6: Maps for HCG 56. From east to west: HCG 56a, 56b, 56c, and 56d. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.7: Maps for HCG 68. HCG 68a is located to the south of HCG 68b. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.8: Maps for HCG 68c. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.9: Maps for HCG 79. HCG 79b and 79c are located in the north of the field, from east to west. HCG 79a is in the center of the field and HCG 79d placed at the south of 79a. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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	Figure B.10: Maps for HCG 93b. Top left: B band image from DSS. Top right: velocity field. Bottom left: monochromatic image. Bottom right: velocity dispersion map.
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Figure B.11: Rotation curves in this sample. The PA was determinated automatically from the model. The center and inclination were fixed (mophological center and photometic inclination, respectively). The black vertical arrow in the x-axis represents the radius R25 while the smaller grey arrow in the x-axis represents the transition radius that is defined by the first ring that contains more than 25 uncorrelated bins in the velocity field (see Epinat et al. 2008a).

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	Figure B.12: See caption of Fig. B.11.
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	Figure B.13: See caption of Fig. B.11.
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Appendix C: Rotation curve tables (long tables are placed at the end of this Appendix)

Table C.1:   HCG 2b rotation curve.

Table C.2:   HCG 7d rotation curve.

Table C.3:   HCG 22c rotation curve.

Table C.4:   HCG 37d rotation curve.

Table C.5:   HCG 40c rotation curve.

Table C.6:   HCG 40e rotation curve.

Table C.7:   HCG 49a rotation curve.

Table C.8:   HCG 49b rotation curve.

Table C.9:   HCG 49c rotation curve.

Table C.10:   HCG 56a rotation curve.

Table C.11:   HCG 79d rotation curve.

Table C.12:   HCG 93b rotation curve.

Table C.13:   NGC 92 rotation curve.

Table C.14:   HCG 2a rotation curve.

Table C.15:   HCG 2c rotation curve.

Table C.16:   HCG 7a rotation curve.

Table C.17:   HCG 68c rotation curve.