3 Results

  

Table 1: HI detections of BCGs

 

Table 1: continued

Notes to Table 1:
0012-018 $\equiv$ UM 219 $\equiv$ KUG 0012-018.
0034+356 - [61, Wegner et al. (1993)] found F = 1.67 Jy km s^-1, W(50)=94 km s^-1 and W(20)=156 km s^-1 in good agreement with our data.
0111+075 - Sc galaxy of the same brightness at 22' to North. No velocity.
0125-065 - Our unpublished VLA data show a large HI envelope around the BCG. A HST study by [58, Thuan et al. (1996)] indicates an extremely compact and dense HII region in this galaxy. There is a galaxy at 10.5$^{\rm s}$ to the West and 13' to the South with no measured velocity.
0142+046 $\equiv$ MCG 1-5-30. Comet-like structure ($\sim$5/h kpc), with a very compact (7'') HII region at the S edge.
0143+346 $\equiv$ KUG 0143+346. [61, Wegner et al. (1993)] obtained F=3.26 Jy km s^-1 and W₂₀=122 km s^-1, about 30% higher than our flux measurement. In group: 3 Sc galaxies within inside 30' with V=5677, 5653 and 5577 km s^-1.
0144+024A - UM370 at 10.2$^{\rm s}$ to the East and 4' to the South is an O or B star according to [50, Terlevich et al. (1991)].
0214+292 $\equiv$ V Zw 212. Possible satellite galaxy from HI spectrum at V=5365 km s^-1 with F=1.04 Jy km s^-1, W₅₀=52 km s^-1, W₂₀=62 km s^-1 (compact galaxy with d(25) = 5 kpc 22'' away). [17, Keel & van Soest (1992)] found that this is a "probably paired'' Markarian galaxy. The possible companion galaxy is at 2.9', with no known velocity and 1 mag fainter than SBS 0214+292.
0225-103 $\equiv$ MCG -2-7-10 $\equiv$ KUG 0225-103. Galaxy 1 mag fainter at $5\hbox{$.\!\!^{\rm s}$}$8 to the East and 14' to the North. In group: 2 galaxies inside of 30' radius with velocities equal to in 2100 km s^-1.
0225-104 $\equiv$ KUG 0225-104. In group with 0225-103.
0335-052 - With a metallicity of $Z_\odot$/41, this is the most metal-deficient BCG known after I Zw 18 ($Z_\odot$/50). Detailed studies with the HST [56, (Thuan et al. 1997]; [56, Thuan & Izotov 1997)], MMT [15, (Izotov et al. 1997)], Russian 6 m [38, (Pustilnik et al. 1997)] and Keck [24, (Lipovetsky et al. 1999a)] telescopes suggest that this galaxy is a young galaxy, containing stars not older than 100 Myr. A VLA map [39, (Pustilnik et al. 1999)] shows that the HI envelope is unusually large (64 $\times$ 24 kpc²) and seen nearly edge-on. As the HI gas structure is not well approximated by our adopted model of a gaussian disk, the beam correction is somewhat uncertain. However the single-dish and VLA HI masses agree quite well. NGC 1376 is at $37\hbox{$.\!\!^{\rm s}$}$3 to the West at V=4155 km s^-1 ($\sim$ 100/h kpc in projection). The BCG is at the outskirts of a medium density group GH 47 [7, (Garcia 1993)].
0741+535 - Galaxy at 7.2$^{\rm s}$ to the East and 17' to the North. In the same group with 2 SB galaxies with velocities of 5641 km s^-1 and 5679 km s^-1, inside a radius of 30'.
0743+550 $\equiv$ MCG 9-13-55 $\equiv$ VV 654, pair? In group? Sb galaxy NGC 2446 at $\sim 25'$ with $\Delta V=180$ km s^-1.
0749+568 - Possible HI satellite at V=5339 km s^-1, $F = 0.24~\pm~0.11$ Jy km s^-1, W₅₀ = 70 km s^-1. This HI component may be associated with a brighter galaxy at $\sim 2'$ to the West and $\sim 1.7'$ to the North, or with a fainter galaxy at 0.2' to the East and $\sim 6'$ to the South, or with a very faint fuzz at 10'' to the East and 30'' to the South.
0847+612 $\equiv$ MCG 10-13-25. Compact galaxy with a bright nucleus and two tails.
0917+527 $\equiv$ KUG 0917+527.
0930+554 $\equiv$ I Zw 18 $\equiv$ UGCA 166. The most metal-deficient BCG known (1/50 of solar metallicity) and a young galaxy (stars not older than 100 Myr, [13, Izotov & Thuan 1998)].
0939+592 $\equiv$ UGC 5179. Spiral galaxy seen almost face-on. The bright SO galaxy NGC 2950 is 3.5 mag brighter at 25.3$^{\rm s}$ to the West and 7' to the South, V = 1378 km s^-1 ($\sim$ 30/h kpc in projection).
0940+662 $\equiv$ NGC 2909 $\equiv$ UGC 5188. [9, Haynes et al. (1988)] obtained F = 2.02 Jy km s^-1 and W₅₀=130 km s^-1, W₂₀=188 km s^-1 consistent with our data.
0940+544 $\equiv$ KUG 0940+544. KUG 0940+543, 1 mag brighter galaxy at 10$^{\rm s}$ to the West and 1.5' to the South. Its velocity is about 27000 km s^-1 (6 m data).
0942+573 $\equiv$ KUG 0942+573.
0946+487 $\equiv$ KUG 0946+487.
0946+558 $\equiv$ UGCA 184 $\equiv$ KUG 0946+588, spiral, [55, Thuan & Martin (1981)] obtained $F=1.23~\pm~0.8$ Jy km s^-1, W₅₀=69 km s^-1, W₂₀=104 km s^-1.
1001+555 $\equiv$ UGC 5421 $\equiv$ MCG 9-17-18, Dwarf ($\sim$ 9 kpc) galaxy seen edge-on. [44, Schneider et al. (1992)] obtained $F=4.19~\pm~0.6$ Jy km s^-1, W₅₀=100 km s^-1, W₂₀=116 km s^-1), [10, Haynes & Giovanelli (1991)] obtained F=4.53 Jy km s^-1, W₅₀=105 km s^-1, W₂₀=127 km s^-1 and [51, Theureau et al. (1998)] obtained $F=4.4~\pm~0.5$ Jy km s^-1, W₅₀=110 km s^-1, W₂₀= 119 km s^-1 in good agreement with our data.
1006+578 $\equiv$ KUG 1006+578.
1114+587 - In group? Two galaxies inside a 30' radius with velocities of 1772 km s^-1 and 1808 km s^-1.
1119+586 - Galaxy 2 mag brighter, 11.4$^{\rm s}$ to the West and 18' to the South, with no known velocity. Background HI emission at V=1943 km s^-1 with $F=0.37~\pm~0.18$ Jy km s^-1, W₅₀=36 km s^-1. It may come from either a pair of galaxies at $\sim 1'$ to the East and $\sim 4'$ to the South, or a faint galaxy at 8'' to the East and $\sim 7.3'$ to the North.
1123+644 $\equiv$ UGC 6448 $\equiv$ MCG 11-14-25. Dwarf Irr disk with 2 bright knots. [55, Thuan & Martin (1981)] obtained $F=4.2~\pm~1.06$ Jy km s^-1, W₅₀ = 60 km s^-1, W₂₀ = 87 km s^-1. In group? UGC 6390 inside of 30' radius at V = 1009 km s^-1 ($\sim$ 75/h kpc in projection).
1211+540 - One of the smallest objects in our sample.
1213+597 $\equiv$ MCG 10-18-13. Spiral seen almost face-on. In group? NGC 4195 inside 30' radius at V=4350 km s^-1.
1317+523A $\equiv$ MCG 9-22-47. Observation was made at 13$^{\rm s}$ to the West. A correction factor of 1.27 has been taken into account for the integrated flux density. With this offset, the integrated flux density contribution of the nearby galaxy SBS 1317+523B ($\equiv$ MK251, at 20$^{\rm s}$ to the East and 1.5$^\prime$to the North, at V=4618 km s^-1) is less than 15% of the measured integrated flux density of SBS 1317+523A, which is, after subtraction, of 4.2 Jy km s^-1. In group with the companion galaxy MCG 9-22-48, located at 3$^{\rm s}$ to the East and 30$^{\prime\prime}$ to the South, with $V = 4444~\pm~40$ km s^-1, yielding no confusion, with SBS 1317+523B, and with SBS 1318+520 at 25$^{\rm s}$ to the East, 18' to the South and V= 4740 km s^-1.
1318+520 $\equiv$ MCG 9-22-51. In group with SBS 1317+523A and B and MCG 9-22-48 (see the note for SBS 1317+523A).
1323+483 - Foreground HI source at V=4602 km s^-1 with $F=0.15~\pm~0.07$ Jy km s^-1, W₅₀=32 km s^-1. Fainter galaxy at 3'' to the West and 24'' to the South.
1332+518 $\equiv$ NGC 5238 $\equiv$ UGC 8565 $\equiv$ I Zw 64 $\equiv$ VV 828 $\equiv$ CP 384ab.
1358+554E - Edge-on spiral NGC 5422 ($B=12\hbox{$.\!\!^{\rm m}$}8$) about 6' to the SE with V=1785 km s^-1.
1422+573 $\equiv$ KUG 1422+573. Spheroid with 2 tails along major axis.
1430+596 - Edge-on Spiral. There is also a HI component at V=1955 km s^-1 with $F=0.43~\pm~0.17$ Jy km s^-1, W₅₀=46 km s^-1. This may be associated with a galaxy 2 mag fainter at 4' to the North. In group. Two SBc galaxies inside 30' radius at velocities of 2001 km s^-1 and 1918 km s^-1.
1430+526A $\equiv$ KUG 1430+526.
1504+514N $\equiv$ KUG 1504+514 $\equiv$ CGCG 274-13. Sc galaxy UGC 9702 at 8' to the SW with unknown velocity.
1506+553 $\equiv$ Sc galaxy UGC 9737 $\equiv$ MCG 9-25-23. In group. 2 Sc galaxies inside 30' radius at velocities 3128 km s^-1 and 3421 km s^-1.
1509+527 $\equiv$ KUG 1509+527. Paired with Sdm galaxy MCG 9-25-31, 0.4 mag brighter and with a(25)=1', at 36'' to the West and 6' to the South, at V=3314 km s^-1 ($F=0.34~\pm~0.14$ Jy km s^-1, W₅₀=86 km s^-1). In group. 3 galaxies with velocities equal to 3526 km s^-1, 3360 km s^-1 and 3470 km s^-1 inside a 30' radius.
1519+496 - Two galaxies at 3.7$^{\rm s}$ to the West and 23' to the South, with unknown velocities.
1551+601A - The HI and optical velocities differ by 300 km s^-1. Possible faint foreground HI emission at V = 2516 km s^-1, $F=0.16~\pm~0.11$ Jy km s^-1, W₅₀ = 28 km s^-1 which could be associated either to a faint galaxy at 3.3' to the South, or to a faint galaxy with bright knots 76'' to the East and $\sim 6'$ to the South.
1714+602 - There is a second component of the HI profile with V = 6070 km s^-1 and $F=0.36~\pm~0.12$ Jy km s^-1. It may correspond to faint galaxy at $\sim 1.5'$ to South.
1809+318 [17, Keel & van Soest (1992)] found that this is a "probably paired'' Markarian galaxy. The possible companion galaxy is at 0.3', with no known velocity and 2.2 mag fainter than SBS 1809+318.
2116+020 [17, Keel & van Soest (1992)] found that this is a "probably paired'' Markarian galaxy. The possible companion galaxy is at 2.2', with no known velocity and 1.8 mag fainter than SBS 2116+020.
2127+021 $\equiv$ NGC 7077 $\equiv$ Arakelian 549. [21, Lewis (1987)] obtained F=1.97 Jy km s^-1, W₅₀=121 km s^-1, W₂₀=131 km s^-1, in good agreement with our data.
2220+377 $\equiv$ UGC 12009. [61, Wegner et al. (1993)] obtained F = 8.78 Jy km s^-1, W₅₀=202 km s^-1 and W₂₀=189 km s^-1 in good agreement with our data.
2221+409 - Sm galaxy UGC 12027 at $\sim 10'$ with V=4130 km s^-1 [44, (Schneider et al. 1992)]. In group?
2246+315 - [16, Jackson et al. (1987)] obtained F=3.37 Jy km s^-1, W₂₀=206 km s^-1, 60% higher than our flux.
2311+129 $\equiv$ UGC 12434.

  

Table 2: Uncertain and confused HI detections

 

Table 2: continued

Notes to Table 2:
0028+081 $\equiv$ Holmberg 11. Confusion. The BCG is a member of the Hickson compact group No. 2B [11, (Hickson 1982)]. Three galaxies in beam. The nearest one is UGC 312, an Sc galaxy 0.7 mag brighter at 5$^{\rm s}$ to the East and 27'' to the South with V=4335 km s^-1.
0127+307A - Confusion? galaxy 0.5 mag brighter, at 2.3$^{\rm s}$ to the East and 4' to the North, with no known velocity.
0136+328 - Confusion? Scd galaxy KUG 0136+329, 0.5 mag fainter, at 3.6$^{\rm s}$ to the West and 6' to the North, with no known velocity.
0201+284 $\equiv$ KUG 0201+284. No confusion. Uncertain parameters. In group with the SO galaxy NGC 805 at 11$^{\rm s}$ to the East and 9.3' to the North with V=4573 km s^-1 and with NGC 807 at 21' with V=4764 km s^-1.
0207-080 $\equiv$ KUG 0207-080. Confusion by E-S0 galaxy NGC 842 at 1.3$^{\rm s}$ to the East and 1' to the North, at V=3836 km s^-1? No beam correction was made.
0310-054 $\equiv$ KUG 0310-054. Confusion? S0 galaxy NGC 1248, 2.5$^{\rm m}$ brighter, at 1.1$^{\rm s}$ to the East and 2.7' to the North with V=2209 km s^-1 (17/h kpc in projection).
0335-057A - Confusion? Scd galaxy PGC 13407, 4 mag brighter, no velocity, at 6$^{\rm s}$ to the East and 8' to the South.
0743+591B - Confusion. Irr galaxy 14.7 mag at 11.4$^{\rm s}$ to the East and 16'' to the North, V=6420 km s^-1.
0750+603AB - Pair of BCGs with $\Delta V \sim 200$ km s^-1, separated by 3$^{\rm s}$ in the EW direction and 32'' in the SN direction, corresponding to a projected distance of 24/h kpc. Not resolved by the single-dish telescope beam.
0755+587 $\equiv$ MCG 10-12-47. Flux corrected by 25% due to a large offset in the pointing. Confusion with MCG 10-12-51 ($\equiv$ KUG 0755+588) at 17$^{\rm s}$ to the East and 5.7' to the North, at V=5760 km s^-1.
0756+611 - No confusion. Uncertain parameters.
0814+579A - Confusion with the BCG SBS 0814+579B with V = 7918 km s^-1, 2.2$^{\rm s}$ to the East, 1.1' to the North, and faint galaxy at 5.1$^{\rm s}$ to the West.
0844+703 $\equiv$ KUG 0844+703. In group. Confused by Sm galaxy UGC 4593 at V=3626 km s^-1 at 5.1' and NGC 2650 at V=3826 km s^-1 at 8'. F(NGC 4953) = 4.66 Jy km s^-1 and W₅₀=241 km s^-1 [30, (Mebold et al. 1979)], in good agreement with our data.
0912+599 - Interacting galaxies in contact.
0926+606 A and B - Pair of BCGs of similar brightnesses, separated by 2.5$^{\rm s}$ in the EW direction and by 1.2' in the SN direction, corresponding to 14/h kpc in projection. $\Delta V \sim$ 100 km s^-1. We have modeled the two peak HI-profile to derive parameters for each component of the pair. For 0926+606A (RA(1950) = 09$^{\rm h}$26$^{\rm m}$20.1$^{\rm s}$, DEC(1950) = 60$\hbox{$^\circ$}$40$\hbox{$^\prime$}$02$\hbox{$^{\prime\prime}$}$), V(HI) = 4090 km s^-1, W₅₀ = 78 $\pm$ 23 km s^-1, W₂₀ = 120 $\pm$ 37 km s^-1, and log $M\rm (HI)= 9.04$; For 0926+606B (RA(1950) = 09$^{\rm h}$26$^{\rm m}$23.0$^{\rm s}$, DEC(1950) = 60$\hbox{$^\circ$}$41$\hbox{$^\prime$}$15$\hbox{$^{\prime\prime}$}$), V(HI) = 4002 km s^-1, W₅₀ = 67 $\pm$ 23 km s^-1, W₂₀ = 120 $\pm$ 37 km s^-1, and log $M\rm (HI)= 8.96$.
1011+601 - Paired with another BCG (SBS 1011+600) which is also included in the statistical sample. The separation is 1.0$^{\rm s}$ in the EW direction and 3' in the NS direction, corresponding to 20/h kpc in projection. The pair is not resolved by the single-dish beam.
1028+566 - No confusion. Uncertain parameters.
1054+504 - No confusion. Uncertain parameters.
1057+511A $\equiv$ UGC 6074. Sdm galaxy MCG 9-18-67, 1.3 mag fainter, at 2.8$^{\rm s}$ to the West, 4.3' to the South, with a velocity of 230 $\pm$ 100 km s^-1 larger (6 m data). Physical pair (45 kpc/h in projection). [1, Armstrong & Wooten (1986)] obtained F=2.2 Jy km s^-1.
1114+517 - Confusion with Sb galaxy UGC 6309, 2.7 mag brighter, at 14.4$^{\rm s}$ to the East and 3' to the North with V=2876 km s^-1 and F=4.35 Jy km s^-1. W₅₀=220 km s^-1, W₂₀=264 km s^-1 [10, (Haynes & Giovanelli 1991)]. Pair? $\sim$ 40/h kpc in projection.
1114+5145 $\equiv$ UGC 6309, not a BCG. See the note for SBS 1114+5145.
1123+576 - No confusion. Uncertain parameters.
1125+562 - Flux corrected by 42% due to offset of pointing relative to correct position. Possible confusion by Sc galaxy MCG 9-19-82 at 22.6$^{\rm s}$ to the West, 63$^{\prime\prime}$to the South (13.1$^{\rm s}$ from telescope position). No known radial velocity.
1125+524 - Possible confusion with MCG 9-19-85, at 9.5$^{\rm s}$ to the East and 4.1' to the North; unknown velocity.
1129+576 - Confusion with a close Irr galaxy (MCG 10-17-10) 1.7 mag brighter, 1.3$^{\rm s}$ to the East, 3.8' to the North, V=1296 km s^-1. Pair? (15/h kpc in projection).
1136+607 - Confusion with Sc galaxy UGC 6619, 2.6 mag brighter, at 19$^{\rm s}$ to the East and 2' to the North, with V(HI) = 3465 km s^-1, F=10.9 Jy km s^-1, W₅₀= 279 km s^-1, W₅₀=327 km s^-1 [10, (Haynes & Giovanelli 1991)]. Pair? (28/h kpc in projection). Also a close companion, a galaxy of the same brightness at 4.1$^{\rm s}$ to the West.
1137+589 - Uncertain parameters. No confusion. Galaxy 0.5 mag fainter at 15.5$^{\rm s}$ to the West and 2' to the South, with V=25440 km s^-1.
1144+591 No confusion. MCG 10-17-56, 1.2 mag brighter, at 8$^{\rm s}$ to the West and 9' to the South, at $V \sim 3500$ km s^-1 (6 m data). In group or pair? UGC 6732 with V= 2285 km s^-1, at 14' ($\sim$ 80/h kpc in projection).
1147+520 - Confusion with the Sc UGC 6802 at 13.9$^{\rm s}$ to the East and 7' to the North with V=1253 km s^-1.
1149+596 - No confusion. In group. Inside 30' radius: NGC 3894 (V = 3242 km s^-1) and NGC 3895 (V = 3129 km s^-1).
1159+516B - Possible confusion by faint galaxy at $\sim 5'$ to the North. Uncertain parameters.
1216+460 - Elongated edge-on spiral galaxy. Possible confusion with low-surface brightness galaxy at 1' to the South and with unknown velocity. Pair?
1216+551 - No confusion. Uncertain parameters.
1221+585 - Confusion? Large difference between optical and HI velocities. Sc galaxy (a=30'') at 7.8$^{\rm s}$ to the West and 11.5' to the North. No velocity. In group: 3 bright galaxies inside 30' radius with velocities near 4500 km s^-1.
1221+545B - No confusion. Uncertain parameters.
1222+614 - Confusion? Sab galaxy of similar brightness (MCG 10-18-43) at 8$^{\rm s}$ to the West and 9.5' to the South with no known velocity.
1240+554C $\equiv$ UGC 7887. Confusion with SBb galaxy of the same brightness (NGC 4644) at 12$^{\rm s}$ to the West with V=4764 km s^-1. In group: 5 galaxies of similar brightnesses inside 30' radius with velocities around 4800 km s^-1.
1242+549 - Confusion with the S galaxy NGC 4669, at 10$^{\rm s}$ to the East and 11' to the North, with V=4835 km s^-1 [2, (Bottinelli et al. 1999)].
1314+605 - No confusion. Uncertain parameters.
1317+523B $\equiv$ MCG 9-22-49. Confusion with the BCG SBS 1317+523A, which is at 20$^{\rm s}$ to the West and 1.5' to the North, and has the same HI velocity (V=4619 km s^-1) and HI line widths. After subtraction of the integrated flux density contribution from SBS 1317+523A, we find F=3.7 Jy km s^-1. In a group with SBS 1317+523A, MCG 9-22-48 and SBS 1318+520 at 11.4$^{\rm s}$ to the East and 17' to the South, with V=4740 km s^-1 (see the note for SBS 1317+523A, in Table 1).
1319+579AB $\equiv$ NGC 5113, edge-on Sbc with two HII regions at the ends (A and B). Confusion with Sc galaxy NGC 5109 1.7 mag brighter at 29$^{\rm s}$ to the West and 2.7' to the South with V=2131 km s^-1. Possible confusion with MCG 10-19-63 at 12 ' to the North. Unknown velocity.
1340+529 - Paired with MK 1481, a BCG which is 0.5 mag fainter, at 8$^{\rm s}$to the East and 1.2' to the South, with $V=1880~\pm~78$ km s^-1. The Green Bank flux of the pair is a factor of 1.6 larger than that measured at Nançay. No confusion.
1341+529 - Paired with MK 1480, a BCG 0.5 mag brighter, at 8$^{\rm s}$ to the West and 1.2' to the North, with $V=1847~\pm~48$ km s^-1. No confusion.
1401+490 - Confusion? There are another compact galaxy of about the same brightness at 1.6' to the South, and a slightly brighter galaxy at 4.5$^{\rm s}$ to the West and 2' to the North. Unknown velocities.
1450+439 $\equiv$ UGC 9569. Confusion with UGC 9567 (a(25) = 60'') at 13.5$^{\rm s}$ to the West and 4.3' to the South with $V= 2504~\pm~5$ km s^-1. ($\sim$30/h kpc in projection). Interaction? [44, Schneider et al. (1992)] give F=10.0 Jy km s^-1, W₅₀= 154 km s^-1, W₅₀= 183 km s^-1. We have attempted a decomposition to estimate fluxes for each galaxy: F(UGC 9569) = 4.9 $\pm$ 0.8 Jy km s^-1, F(UGC 9567) = 5.9 $\pm$ 1.0 Jy km s^-1.
1523+519 - No confusion, uncertain parameters.
1533+574 $\equiv$ VII Zw 611. Confusion? Pair or two components in the process of merging? Difference in optical velocities is about 150 km s^-1. Sc galaxy MCG 10-22-21, 0.5 mag brighter, at 12$^{\rm s}$ to the West and 4' to the North. No known velocity.
1533+469 - Pair or interacting system, Galaxy 1.5 mag fainter at 2.2$^{\rm s}$ to the West and 18'' to the North. No confusion.
1542+573B $\equiv$ UGC 10002. SBc galaxy. Interacting system with the BCG 1542+573A. In group. Sc galaxy UGC 10022 with V=3957 km s^-1 and galaxy MCG+10-22-36 inside 30' radius. The flux is highly uncertain due to a large correction for pointing offset.
1555+515 - Confusion? Optical and radio velocities differ by $\Delta V = 200$ km s^-1. Sc galaxy (a(25) = 1'), 2 mag brighter, at 1.1$^{\rm s}$ to the East and 7' to the North. No known velocity. In group? Sab galaxy at V=3706 km s^-1 inside 30' radius.
1558+585 - Pair with SBS 1559+585 ($\equiv$ MCG 10-23-15), 2 mag brighter, at 16.5$^{\rm s}$ to the East and 17'' to the North (26/h kpc in projection). Parameters are given for the decomposed profile.
1632+578 - No confusion. Uncertain parameters. The V=4900 km s^-1 feature may be due to some faint radio interference, or may be associated with a brighter galaxy at $\sim 0.9'$ to the East and 3' to the North.
2304+097 - No confusion. Uncertain parameters.
2311+235 - No confusion. Uncertain parameters.

  

Table 3: HI non-detections of BCGs

Notes to Table 3:
All optical velocities have been obtained with the 6m telescope IPCS with a typical accuracy of 100-150 km s^-1. They come either from [, Stepanian et al. 1993] (a-d), or Lipovetsky et al.'s unpublished catalog of BCGs.
0155+021 $\equiv$ UM 151
0200+023 $\equiv$ UM 391
0223+009 $\equiv$ IC 0225
0323-003 $\equiv$ KUG 0323-003
0715+594 $\equiv$ UGC 3789
0745+587 $\equiv$ KUG 0745+587
0943+543 $\equiv$ KUG 0943+543
1030+583 $\equiv$ KUG 1030+583
1135+581 - Observed in the G92 and N93 runs, with F(peak) = 22 $\pm$ 4.1 mJy, and 5.4 $\pm$ 2.8 mJy respectively. In both cases $V \sim 950$ km s^-1 as compared to V(opt) = 896 $\pm$ 21 km s^-1. This HI emission may come from a galaxy with similar brightness at 14$^{\rm s}$ to the East and 45'' to the South, which is entirely in the beam of the 140 ft telescope but only partially in the beam of the Nançay telescope.
1503+531 - Elongated edge-on S galaxy. Uncertain parameters.
1614+600 - Confusion? Sc galaxy, 3 mag brighter. At 16.5$^{\rm s}$ to the West and 1.8' to the North. No known velocity.

  

Figure 1: HI profiles of the 79 certain BCG detections (Table 1). The ordinate is line flux density in mJy and the abscissa is heliocentric velocity in km s-1

 

Figure 1: continued

 

Figure 1: continued

 

Figure 1: continued

 

Figure 1: continued

  

Figure 2: HI profiles of the 53 less secure or confused BCG detections (Table 2). The ordinate is line flux density in mJy and the abscissa is heliocentric velocity in km s-1

 

Figure 2: continued

 

Figure 2: continued

 

Figure 2: continued

We present the data in three tables. Table 1 gives the data for the galaxies for which we feel the HI results are secure. This means we are relatively certain that the signal is not produced by confusion or receiver baseline anomalies, and that the signal-to-noise value is adequate. Table 2, on the other hand, lists detections of emission which may be all right, but for various reasons such as confusion or a low signal-to-noise ratio, we feel should be used more cautiously. Table 3 lists the undetected galaxies and upper limits for their HI flux densities.

The cut-off between Table 1 and Table 2 is not rigorously defined as it is based on a mixture of subjective evaluation of the HI profiles as well as more objective guidelines. The possibility of confusion was checked for every galaxy by using the Lyon-Meudon Extragalactic Database (LEDA) to generate sky plots of a circular area of radius 30' centered on the galaxy. This allows also to check for the environment of the galaxy, whether it is isolated or in a group. The properties and angular separations of possible companion galaxies are given in the Notes to Tables 1 and 2. There is generally a signal-to-noise ratio lower limit of 4 for inclusion in Table 1. The signal is measured as the peak flux in the galaxy's HI profile, while the noise is measured in the baseline away from the observed signal. In a few cases, repeated observations yielded essentially the same parameters, and although the signal-to-noise ratio remained low, we have included the galaxies in Table 1.

Tables 1 and 2 include all of the basic information about the galaxies and the observations, along with the optical angular size information used in calculating corrections to the measured HI fluxes. They are organized as follows:

Column (1). Name following the IAU nomenclature. Some BCGs in physical pairs are characterized by additional letters (A, B, N = North, E = East), but in the tables the two components are lumped together in the same name entry, as they are not resolved by the radio telescope beam. The BCGs which are in the statistical sample are marked by a cross in all tables. Galaxies marked by an asterisk in Table 2 are non-confused.

Column (2). Cross-references to other names in the Markarian (MK, [29, Markarian et al. 1989)], Michigan (UM, [40, Salzer et al. 1989)] or in the Case (CG, [34, Pesch et al. 1991)] lists. When the galaxy is from the Second Byurakan Survey [28, (Markarian et al. 1983]; [46, Stepanian et al. 1993a-d)], it is designated by the initials SBS.

Columns (3) and (4). Right ascension and declination at the epoch 1950. The coordinates have been measured either from the Palomar Sky Survey prints or plates, or taken to be the pointing coordinates of the 6 m telescope during the spectroscopic observations. The errors in each coordinate are typically between 1 and 5 arcsec.

Column (5). Holmberg (H) major and minor diameters in arcsec to the limiting surface brightness of B = 26.5 mag arcsec^-2, derived mainly from CCD surface photometry [25, (Lipovetsky et al. 1999b]; [18, Kniazev 1995)]. When CCD data was not available, Holmberg diameters were derived from measurements on the Palomar Sky Survey (PSS) blue prints and the relation obtained by least-square fitting to the diameter data from a subsample of 48 of our BCGs with CCD photometry:

$$d_{\rm H}~{\rm (arcsec)} = 2.53 d_{\rm PSS}~{\rm (arcsec)} + 7.4''.$$

Diameters derived in this way are marked by the letter e. They are less accurate than the CCD diameters and serve only to correct the HI fluxes for beam effects (Col. 12). We are in the process of deriving accurate CCD diameters for all BCGs in the statistical sample. Diameters are given only for BCGs observed at Nançay, which require a beam-flux correction (see Col. 12).

Column (6). Position angle in degrees of the major axis of the galaxy measured eastward from north.

Column (7). Heliocentric HI velocity in km s^-1 determined as the midpoint between the half-peak points on both sides of the HI profile. The velocity error is estimated from the peak signal-to-noise ratio as decribed by [42, Schneider et al. (1986)], and includes an estimate of errors based on the slope of the profile edges. It is calculated as:

$$\Delta V = 1.5 (W_{20} - W_{50}) (S/N)^{-1}$$

where S/N is the ratio of the peak signal to the rms noise.

Column (8). Distance D in Mpc to the galaxy. We have used the Virgocentric flow model described by [19, Kraan-Korteweg (1986)] with a Virgocentric infall motion of 220 km s^-1 and a Hubble constant of 75 km s^-1 Mpc^-1.

Columns (9) and (10). Velocity widths in km s^-1 of the HI profile at 50% and 20% of peak. Again, errors are calculated following [42, Schneider et al. (1986)] and are based on the same method as for the velocities in Col. (7). The expected error for the 50% width is

$$3.0 (W_{20}-W_{50}) (S/N)^{-1}~{\rm and}$$

for the 20% width is

4.7 (W₂₀-W₅₀) (S/N)^-1.

Column (11). Observed integrated flux density in Jy km s^-1. Following [43, Schneider et al. (1990)], we assume that the window over which the flux was measured is 20% wider than the velocity width measured at 20% of peak. The statistical error on the flux is then:

$$\sigma = 2 (1.2 W_{20}/\Delta V)^{1/2}\Delta V \sigma_{V}$$

where $\Delta V$ is the velocity resolution of the smoothed data, and $\sigma_{V}$ is the rms dispersion in the baseline measured at that resolution. The factor of 2 accounts for baseline uncertainties.

Column (12). HI flux densities corrected for telescope beam size. This correction is negligible for observations made with the NRAO 43 m telescope, as the FWHP of the telescope beam is 22', much larger than the maximum size of our galaxies ($\leq$ 3'). The same holds for the north-south beam of the Nançay telescope which has a FWHP of 22'. But the east-west beam of the Nançay radio telescope has a FWHP of only 3.7', and a beam correction needs to be applied. We follow [55, Thuan & Martin (1981)] in assuming that the neutral gas is distributed like an elliptical Gaussian with half-power major and minor axis a and b in arcmin. Then:

$$F_{\rm c} = F_{\rm H} \left[ 1 + (a^{2} \sin^{2}~{\rm PA}+ b^{2}\cos^{2}~{\rm PA}) / \theta^{2} \right]^{1/2}$$

where a and b are the Holmberg diameters given in Col. (5), PA is the position angle in degrees given in Col. (6), and $\theta$ is the HPBW of the Nançay telescope in the East-West direction. The beam correction are generally small, between 1.01 and 1.03. For only a few BCGs does the correction factor reach 1.10-1.18.

Column (13). Logarithm of the hydrogen mass $M_{\rm H}$ in solar masses calculated from:

$$M_{\rm H} = 2.36 \times 10^5 F_{\rm c}~{\rm (Jy~km~s}^{-1}) D^2~({\rm Mpc}^2)$$

where $F_{\rm c}$ is the corrected flux density given in Col. (12) and D the distance to the galaxy given in Col. (8).

Column (14). Telescope used (G = Green Bank, N = Nançay) and last two digits of the year of observation (The observation year ranges from 1992 to 1996). An asterisk in Table 1 means that there is additional information in the notes. All entries in Table 2 have supplemental notes.

Table 1 contains 79 entries with 34 galaxies in the statistical sample.

Table 2 contains 54 entries but only 53 are BCGs as 1114+5145 $\equiv$UGC6074 is not a BCG and has been observed to check for confusion with the BCG 1114+517 $\equiv$ MK1445. Out of the 53 BCGs, we have determined that 32 BCGs are confused (see notes). The 21 non-confused BCGs in Table 2 are: 0201+284, 0756+611, 0912+599, 1028+566, 1054+504, 1057+511A, 1123+576, 1137+589, 1144+591, 1149+596, 1216+551, 1221+545B, 1314+605, 1340+529, 1341+529, 1523+519, 1533+469, 1542+573B, 1632+578, 2304+097 and 2311+235. They are marked by an asterisk in Col. 1. Table 2 contains 29 galaxies from the statistical sample, with 11 non-confused galaxies and 18 confused galaxies, among which are the pairs of BCGs 0926+606 A and B and 1011+600 and 1011+601 which are listed in a single entry.

Table 3 lists the BCGs which were not detected. It is organized as follows: the galaxy's IAU name (Col. 1), cross-reference to other names (Col. 2), its 1950 coordinates (Cols. 3 and 4). The heliocentric optical velocity on which the receiver was centered is given in Col. 5. The NRAO and Nançay receivers covered respectively a velocity range of 1350 and 4225 km s^-1. Col. 6 lists the rms noise in mJy of the spectrum smoothed to a velocity resolution of $\sim$ 16 km s^-1 for the Green Bank spectra and of $\sim$ 21 km s^-1 for the Nançay spectra. Finally, Col. 7 gives the telescope used and the year of the observations. An asterisk signifies that more information can be found in the notes.

Figures 1 and 2 show in order of increasing right ascension the HI profiles of the BCGs listed respectively in Tables 1 and 2. Several of the BCGs in Table 1 have previous HI measurements. The detailed references are given in the Notes section. Comparison of our measurements with those of previous authors is given in Appendix A.