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Table 1 presents the summary data for all of the sources in the IRAS RBGS. The complete sample contains 629 galaxies that met our threshold criteria of S60 > 5.24 Jy. The column entries are as follows:

(1) Common Name - Common name taken in decreasing priority order from the NGC, UGC, ESO, IC, A, MCG, CGCG, Zwicky compact galaxies, Markarian, and IRAS catalogs. "N" follows the common name for "new" RBGS objects which were not included in the compilation of the BGS1 (Soifer et al. 1989) or BGS2 (Sanders et al. 1995); "1" flags objects from the BGS1, and "2" flags objects from the BGS2.

(2) IRAS Name - Names from the IRAS Faint Source Catalog (FSC) are given using the standard "F" prefix; if the source is not in the FSC, the name from the Point Source Catalog (PSC) is given, which has no letter prefix. IRAS source names are based on equinox B1950.0 coordinates. Names from the IRAS Faint Source Catalog Rejects (FSCR) are given using the standard "Z" prefix. (NGC 4151 is the only FSCR object in the RBGS; see Section 2.) IRAS catalog names are not listed for a few very large galaxies (indicated by "--") because entries in the IRAS catalogs do not represent the total flux and generally correspond only to the nucleus or other bright component. Flags following the IRAS name are as follows: "R" indicates large galaxies with for which total flux densities derived from IRAS images were published by Rice et al. (1988) or Rice (1993); the Rice et al. values are adopted here only in cases listing an "R" value for the Method code in columns (8) - (11); see text for details. "*" identifies objects located in regions of the Milky Way, LMC, or SMC with high source confusion. [Note: The objects are listed in order of increasing B1950 right ascension (R.A.), as reflected in the source names from the IRAS catalogs; this places some objects out of order in terms of their J2000 coordinates.]

(3-4) R.A., Dec - Equinox J2000.0 R.A. and declination (Dec), transformed from equinox B1950.0 coordinates published in the IRAS FSC (Version 2.0) or PSC (Version 2), as indicated in Col. (2). These coordinates correspond to the centroid of the IRAS positional uncertainty ellipse as superimposed on the Digitized Sky Survey fields shown in Figure 1. Exceptions are for the large galaxies NGC55, SMC, NGC300, LMC, NGC6744, and NGC6822 whose positions are taken from Rice et al. (1988).

(5-6) ell, b - Galactic latitude and longitude in decimal degrees.

(7) HIRES code - IRAS HIRES code from Surace, Sanders & Mazzarella (2003). A listing here indicates that the infrared source contains two or more objects that were confused in one or more of the IRAS detectors. The high-resolution image restoration algorithm HIRES (Aumann, Fowler, & Melnyk 1990) was applied to these sources in an attempt to resolve flux from individual galaxies. "R" means the source was resolved into two or more components, resulting in new IRAS positions and fluxes; "*" means the source was resolved, but the IRAS position lies between the two galaxies as seen on the DSS; "S" means the source was partially resolved into two or more components, and fluxes were estimated for each object, but no new reliable positions were derived; "U" means HIRES was unsuccessful at resolving separate components. See Surace et al. (2003) for detailed HIRES results for these objects. For consistency, the fluxes listed in Table 1 were derived using SCANPI in the same manner as the single objects in the table. There are known calibration problems with the HIRES data product (Surace et al. 1993), and while the flux ratio between individual galaxies within a system can be more accurately measured using HIRES, the absolute calibration of the galaxy system flux is better determined by SCANPI. Since in many cases a single galaxy dominates the far-infrared flux of a multiple galaxy system, there are only a handful of systems that would have not been selected in the RBGS but which are included by virtue of having an integrated flux above the selection limit.

(8-11) Flux Densities - Total IRAS flux densities (Jy) in the 12 µm, 25 µm, 60 µm, and 100 µm, respectively. Following each flux density value are the uncertainty (1sigma in mJy) followed by three code letters (SMF) indicating the infrared Size (U = "unresolved", M = "marginally extended", R = "resolved"); the Method chosen as the best flux estimate from SCANPI (Z = "zero crossing", I = "in-band total", T = "template fit", P = "peak value", S = "deconvolution with SCLEAN" (see Appendix), R = from Rice et al. (1988); and a Flag indicating the type of confusion (c = "cirrus", g = "nearby galaxy", n = "excessive noise", b = "blended objects") causing large uncertainty as indicated by a colon (":") prefix on the flux density. Note that some large galaxies flagged with "R" in Col. (2) have new SCANPI zero-crossing estimates, indicated here using "Z" for the second flag, which are judged to have more accurate calibration than previously adopted values from Rice et al. (1988).

(12) cz - The Heliocentric radial velocity (kms-1) of the IRAS source computed as c times the redshift z. The source for the redshift is given in Col. (2) of Table 2 as a 19 digit reference code from NED. In cases where either a millimeter (e.g. CO) or HI 21-cm line measurement has been reported we have chosen to adopt these redshifts given that they better reflect the systemic velocity of the galaxy, as opposed to optical measurements which are often biased (typically blue-shifted) due to optical depth effects.

(13) Distance - The estimated source distance in Mpc; metric ("proper") distance is listed, not luminosity distance. For most objects this was calculated from cz using the cosmic attractor model outlined in Appendix A of Mould et al. (2000), using Ho = 75 km s-1 Mpc-1 and adopting a flat cosmology in which OmegaM = 0.3 and OmegaLambda = 0.7 (which corresponds to q0 = - 0.55). Superscripts are defined as follows: "P" indicates the distance is not computed by correcting the heliocentric redshift using the cosmic attractor model, but comes from a direct primary distance measurement; "S" flags a direct secondary distance measurement; "V" indicates that the cosmic attractor flow model places the object within the Virgo cluster at a distance of 15.3 Mpc; "G" indicates that the cosmic attractor flow model places the object within the Great Attractor. References for the adopted primary and secondary distance indicators are Freedman et al. (2001), Madore & Freedman (1998), Ferrarese et al. (2000), Mould et al. (1991), Tully & Shaya (1984), Aaronson & Mould (1983), Aaronson et al. 1982, and Aaronson, Mould & Huchra (1980).

(14-15) Luminosities - The base10 logarithm of the far-infrared luminosity, Lfir = L(40 - 400µm), determined using the prescription described in Appendix B of Cataloged Galaxies and Quasars Observed in the IRAS Survey (1989), and the infrared luminosity, Lir = L(8 - 1000µm), determined using the fluxes in all four IRAS bands (Perault 1987; see also Table 1 in Sanders & Mirabel 1996), in units of solar bolometric luminosity, Lodot = 3.83 × 1033 ergs-1.

(16) Rank - The object's sequential rank in the distribution of Lir values, where 1 is the most luminous source.

(17) Other Names - Other names from catalogs of interacting galaxies (IG) or active galactic nuclei (AGN). Spaces between catalog name prefix and number (as standard in NED) are omitted here to save space.

Table 1 in data format.

Table 1 in postscript format.

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