VII/64 CO Observations of Galaxies (Verter 1985)

VII/64/notes.dat Notes (96 records)

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DaVelocities of some galaxies south of -2 deg. 30 min. declination from RSA.
DbGalaxies whose magnitudes are labelled (a) are not listed in the main
Dbcatalog of the RSA but appear in Appendix A of the RSA which compiles
Dbadditional bright (B<13.4) galaxies. Their magnitudes have not been
Dbcorrected for galactic and internal absorption.
DcVelocity of NGC 660 from Benvenuti, Capaccioli, and D'Odorico 1976,
DcAstr. Ap., 53, 141.
DdHI flux of NGC 1068 from Allen, Darchy, and Lauque 1971, Astr. Ap., 10, 198.
DeHI observations carry this quality code: "close multiple system".
DfHI flux and velocity width of NGC 4258 from van Albada 1980, Astr. Ap., 90,
Df123.
DgVelocities of NGC 5506 and Mk231 from BMB.
DhHI flux and HI velocity width of NGC 7371 from Gallagher et al. 1985, in
Dhpreparation.
DiMorphological type, photographic magnitude, and velocity of IC 4553 from
DiStocke, Tifft, and Kaftan-Kissim 1978, A. J., 83, 322. The magnitude is
Dionly corrected for galactic absorption.
DjThe "megamaser" galaxy IC 4553, #220 in the Arp Catalog (Arp 1967, Ap. J.
DjSuppl., 14, 1), has been interpreted as two merging galaxies. Its optical
Djnucleus is double (Stocke, Tifft, and Kaftan-Kissim 1978, A. J., 83, 322),
Djit has the strongest and widest HI absorption line (Mirabel 1982, Ap. J.,
Dj260, 75) known to date, contains the strongest OH maser (Baan and Haschick
Dj1984, Ap. J., 279, 541) known to date, and is the brightest galaxy detected
Djby IRAS (Soifer et al. 1984, Bull. AAS, 16, 470).
DkVelocities of LMC and SMC, with respect to Sun, from Kerr and de Vaucouleurs
Dk1955, Australian J. Phys., 8, 508.
DlHI flux of LMC from McGee and Milton 1966, Australian J. Phys., 19, 343.
DmMaffei 2 is a diffuse infrared object close to the galactic plane that has
Dmbeen identified as a heavily obscured spiral galaxy. Its total size and
Dmdetailed structure are not accurately known. See RTP77, and references
Dmtherein.
DnHI flux and velocity width of Maffei 2 from Wright and Seielstad 1973, Ap.
DnLetters, 13, 1.
DoHI flux of SMC from Hindman 1967, Australian J. Phys., 20, 147.
DpDiameter and magnitude of NGC 1023 companion from Barbon and Capaccioli
Dp1975, Astr. Ap., 42, 103.
DqVelocity, HI flux and velocity width of the dwarf companion of NGC 1023 from
DqSancisi et al. 1984, M. N. R. A. S. preprint.
DrHI upper limit on NGC 2314 (<4mJY) from Shostak, Roberts, and Peterson 1975,
DrA. J., 80, 581.
DsHI upper limit on NGC 2639 (<2mJy) from Thonnard 1982, private communication
DtVelocity, HI flux, and HI velocity width of NGC 2902 from Gallagher et al.
Dt1985, in preparation.
DuHI flux and velocity width from Fisher and Tully 1975, Astr. Ap., 44, 151.
TaGHE upper limits are peak-to-peak temperature limits. The limits in Table 3
Taare one-half the values in the reference.
TbM upper limits are given in integrated intensities. The limits in Table 3
Tbwere obtained by dividing these values by the HI line widths with which they
Tbwere calculated.
TcWFB upper limits are one-half the peak-to-peak noise in the final averaged
Tcprofile.
MaInclination of M31 from Deharveng and Pellet 1975, Astr. Ap., 38, 15.
MbInclination of NGC 253 from Pence 1980, Ap. J., 239, 54.
McAlong the MA of M33 and NGC 2403, there are some points with no detectable
Mcemission that lie within the maximum radius at which emission was seen: the
Mcdistribution is patchy.
MdInclinations of NGC 598, NGC 2403, M101, NGC 6946, and IC 342 from Rogstad
Mdand Shostak 1972, Ap. J., 176, 315.
MeBecause NGC 891 is essentially edge-on, the observed emission from the
Mecentral parts is limited by cloud overlap along the line of sight.
MfInclination of NGC 891 from Sancisi and Allen 1979, Astr. Ap., 74, 73.
MgInclination of NGC 1068 from Walker 1968, Ap. J., 151, 71.
MhInclinations of NGC 2841 and NGC 7331 from Bosma 1978, Ph D. Thesis, Univ.
Mhof Groningen.
MiIt is impossible to accurately assign a distribution type to NGC 2903 on the
Mibasis of the 3 points in E**2; this entry should be treated as a best guess.
MjInclination of NGC 2903 from Burbidge, Burbidge, and Prendergast 1960,
MjAp. J., 132, 640.
MkReference S82 presents evidence suggesting that the CO emission from the
Mkpeculiar galaxy M82 is associated with dusty filaments above and below the
Mkstellar disk.
MlInclination of NGC 4258 from van Albada 1980, Astr. Ap., 90, 123.
MmInclination of NGC 4303 from Fraser 1977, Astr. Ap. Suppl., 29, 61.
MnInclination of NGC 4321 from van der Kruit 1973, Ap. J., 186, 807.
MoEmission along the major axis of NGC 4654 is stronger on one side of the
Mogalaxy than the other; it does not fit into any of the distribution types
Mogiven.
MpInclination of M51 from Tully 1974, Ap. J. Suppl., 27, 437.
MqInclination of NGC 5236 from Rogstad, Lockhart, and Wright 1974, Ap. J.,
Mq193, 309.
MrInclination of NGC 5248 from Burbidge, Burbidge, and Prendergast 1962,
MrAp. J., 136, 128.
MsInclination of LMC and SMC from de Vaucouleurs and Freeman 1972, in Vistas
Msin Astronomy, Vol 14, ed. A. Beer (Oxford: Pergamon), p. 163.
MtMaffei 2 is a diffuse infrared object close to the galactic plane that has
Mtbeen identified as a heavily obscured spiral galaxy. Its total size and
Mtdetailed structure are not accurately known. See RTP77, and references
Mttherein.
MuResolution 65 arcsec. Gordon and Burton 1976, Ap. J., 208, 346.
MvResolution 65 arcsec; number of map points is approximate. Solomon,
MvSanders, and Scoville 1979, in IAU Symposium 84, Large Scale Characteristics
Mvof the Galaxy, ed. W. B. Burton (Dordrecht: Reidel), p. 35.
MwResolution 65 and 50 arcsec; number of map points is approximate. Sanders,
MwSolomon, and Scoville 1984, Ap. J., 276, 182.
MxNumber of map points is approximate. Knapp, Stark, and Wilson 1984, in
Mxpreparation.