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## (from tabmap V6.0 (2016-08-18)) 2024-03-19T10:19:22 #--------------------------------------------------------------------------- #-- VII/64 CO Observations of Galaxies (Verter 1985) #-------------------------------------------------------------------------- #---Table: VII/64/./notes.dat Notes (96 records) # Fflag A1 --- *[DTM] File flag # Nflag A1 --- *Note flag # Text A76 --- Note text #Note on Fflag: # D if the note is from detect.dat or uprlmits.dat; # T if the note is from temperat.dat; or # M if the note is from CO Maps of Galaxies (maps.dat). #Note on Nflag: # Lowercase letter that corresponds to a note flag from any of the files # listed above. When several lines are required, Fflag and Nflag are # repeated. #------------------------------------------------------------------------------- -------------------------------------------------------------------------------- F|N| f|f| l|l| a|a| g|g|Text -|-|---------------------------------------------------------------------------- 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. --------------------------------------------------------------------------------