D a Velocities of some galaxies south of -2 deg. 30 min. declination from RSA. D b Galaxies whose magnitudes are labelled (a) are not listed in the main D b catalog of the RSA but appear in Appendix A of the RSA which compiles D b additional bright (B<13.4) galaxies. Their magnitudes have not been D b corrected for galactic and internal absorption. D c Velocity of NGC 660 from Benvenuti, Capaccioli, and D'Odorico 1976, D c Astr. Ap., 53, 141. D d HI flux of NGC 1068 from Allen, Darchy, and Lauque 1971, Astr. Ap., 10, 198. D e HI observations carry this quality code: "close multiple system". D f HI flux and velocity width of NGC 4258 from van Albada 1980, Astr. Ap., 90, D f 123. D g Velocities of NGC 5506 and Mk231 from BMB. D h HI flux and HI velocity width of NGC 7371 from Gallagher et al. 1985, in D h preparation. D i Morphological type, photographic magnitude, and velocity of IC 4553 from D i Stocke, Tifft, and Kaftan-Kissim 1978, A. J., 83, 322. The magnitude is D i only corrected for galactic absorption. D j The "megamaser" galaxy IC 4553, #220 in the Arp Catalog (Arp 1967, Ap. J. D j Suppl., 14, 1), has been interpreted as two merging galaxies. Its optical D j nucleus is double (Stocke, Tifft, and Kaftan-Kissim 1978, A. J., 83, 322), D j it has the strongest and widest HI absorption line (Mirabel 1982, Ap. J., D j 260, 75) known to date, contains the strongest OH maser (Baan and Haschick D j 1984, Ap. J., 279, 541) known to date, and is the brightest galaxy detected D j by IRAS (Soifer et al. 1984, Bull. AAS, 16, 470). D k Velocities of LMC and SMC, with respect to Sun, from Kerr and de Vaucouleurs D k 1955, Australian J. Phys., 8, 508. D l HI flux of LMC from McGee and Milton 1966, Australian J. Phys., 19, 343. D m Maffei 2 is a diffuse infrared object close to the galactic plane that has D m been identified as a heavily obscured spiral galaxy. Its total size and D m detailed structure are not accurately known. See RTP77, and references D m therein. D n HI flux and velocity width of Maffei 2 from Wright and Seielstad 1973, Ap. D n Letters, 13, 1. D o HI flux of SMC from Hindman 1967, Australian J. Phys., 20, 147. D p Diameter and magnitude of NGC 1023 companion from Barbon and Capaccioli D p 1975, Astr. Ap., 42, 103. D q Velocity, HI flux and velocity width of the dwarf companion of NGC 1023 from D q Sancisi et al. 1984, M. N. R. A. S. preprint. D r HI upper limit on NGC 2314 (<4mJY) from Shostak, Roberts, and Peterson 1975, D r A. J., 80, 581. D s HI upper limit on NGC 2639 (<2mJy) from Thonnard 1982, private communication D t Velocity, HI flux, and HI velocity width of NGC 2902 from Gallagher et al. D t 1985, in preparation. D u HI flux and velocity width from Fisher and Tully 1975, Astr. Ap., 44, 151. T a GHE upper limits are peak-to-peak temperature limits. The limits in Table 3 T a are one-half the values in the reference. T b M upper limits are given in integrated intensities. The limits in Table 3 T b were obtained by dividing these values by the HI line widths with which they T b were calculated. T c WFB upper limits are one-half the peak-to-peak noise in the final averaged T c profile. M a Inclination of M31 from Deharveng and Pellet 1975, Astr. Ap., 38, 15. M b Inclination of NGC 253 from Pence 1980, Ap. J., 239, 54. M c Along the MA of M33 and NGC 2403, there are some points with no detectable M c emission that lie within the maximum radius at which emission was seen: the M c distribution is patchy. M d Inclinations of NGC 598, NGC 2403, M101, NGC 6946, and IC 342 from Rogstad M d and Shostak 1972, Ap. J., 176, 315. M e Because NGC 891 is essentially edge-on, the observed emission from the M e central parts is limited by cloud overlap along the line of sight. M f Inclination of NGC 891 from Sancisi and Allen 1979, Astr. Ap., 74, 73. M g Inclination of NGC 1068 from Walker 1968, Ap. J., 151, 71. M h Inclinations of NGC 2841 and NGC 7331 from Bosma 1978, Ph D. Thesis, Univ. M h of Groningen. M i It is impossible to accurately assign a distribution type to NGC 2903 on the M i basis of the 3 points in E**2; this entry should be treated as a best guess. M j Inclination of NGC 2903 from Burbidge, Burbidge, and Prendergast 1960, M j Ap. J., 132, 640. M k Reference S82 presents evidence suggesting that the CO emission from the M k peculiar galaxy M82 is associated with dusty filaments above and below the M k stellar disk. M l Inclination of NGC 4258 from van Albada 1980, Astr. Ap., 90, 123. M m Inclination of NGC 4303 from Fraser 1977, Astr. Ap. Suppl., 29, 61. M n Inclination of NGC 4321 from van der Kruit 1973, Ap. J., 186, 807. M o Emission along the major axis of NGC 4654 is stronger on one side of the M o galaxy than the other; it does not fit into any of the distribution types M o given. M p Inclination of M51 from Tully 1974, Ap. J. Suppl., 27, 437. M q Inclination of NGC 5236 from Rogstad, Lockhart, and Wright 1974, Ap. J., M q 193, 309. M r Inclination of NGC 5248 from Burbidge, Burbidge, and Prendergast 1962, M r Ap. J., 136, 128. M s Inclination of LMC and SMC from de Vaucouleurs and Freeman 1972, in Vistas M s in Astronomy, Vol 14, ed. A. Beer (Oxford: Pergamon), p. 163. M t Maffei 2 is a diffuse infrared object close to the galactic plane that has M t been identified as a heavily obscured spiral galaxy. Its total size and M t detailed structure are not accurately known. See RTP77, and references M t therein. M u Resolution 65 arcsec. Gordon and Burton 1976, Ap. J., 208, 346. M v Resolution 65 arcsec; number of map points is approximate. Solomon, M v Sanders, and Scoville 1979, in IAU Symposium 84, Large Scale Characteristics M v of the Galaxy, ed. W. B. Burton (Dordrecht: Reidel), p. 35. M w Resolution 65 and 50 arcsec; number of map points is approximate. Sanders, M w Solomon, and Scoville 1984, Ap. J., 276, 182. M x Number of map points is approximate. Knapp, Stark, and Wilson 1984, in M x preparation.