The IRAS Revised Bright Galaxy Sample

By D. Sanders, J. Mazzarella, D.-C. Kim, J. Surace, B. Soifer. 2003

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IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60 μm flux density greater than 5.24 Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b| > 5°. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2), which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May. The RBGS also makes use of more accurate and consistent automated methods to measure the flux of objects with extended emission. The RBGS contains 39 objects that were not present in the BGS1+BGS2, and 28 objects from the BGS1+BGS2 have been dropped from RBGS because their revised 60 μm flux densities are not greater than 5.24 Jy. Comparison of revised flux measurements for sources in both surveys shows that most flux differences are in the range ∼5%–25%, although some faint sources at 12 and 25 μm differ by as much as a factor of 2. Basic properties of the RBGS sources are summarized, including estimated total infrared luminosities, as well as updates to cross identifications with sources from optical galaxy catalogs established using the NASA/IPAC Extragalactic Database. In addition, an atlas of images from the Digitized Sky Survey with overlays of the IRAS position uncertainty ellipse and annotated scale bars is provided for ease in visualizing the optical morphology in context with the angular and metric size of each object. The revised bolometric infrared luminosity function, ϕ(Lir), for infrared-bright galaxies in the local universe remains best fit by a double power law, ϕ(L) ∝ Lα, with α = -0.6(±0.1) and α = -2.2(±0.1) below and above the "characteristic" infrared luminosity L ∼ 1010.5 L⊙, respectively. A companion paper provides IRAS High Resolution (HIRES) processing of over 100 RBGS sources where improved spatial resolution often provides better IRAS source positions or allows for deconvolution of close galaxy pairs.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ba125dbe9f0b86224a0a546da11a4570a7d40978

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The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, methodology): “The total IR LF of Sanders et al. (2003) is plotted as a local reference, in addition to the LFs of Le Floc’h et al. (2005), Rodighiero et al. (2010a), Caputi et al. (2007), Magnelli et al. (2009) and Magnelli et al. (2011) in various redshift intervals.”
THE STRUCTURE AND KINEMATICS OF THE CIRCUMGALACTIC MEDIUM FROM FAR-ULTRAVIOLET SPECTRA OF z ≃ 2–3 GALAXIES (2010, result): “The typical galaxy in our sample has a bolometric luminosity of ≃ 3×1011 L⊙, roughly 5 times higher than that of M82 (cf. Reddy et al. 2006; Sanders et al. 2003).”
DUST-CORRECTED STAR FORMATION RATES OF GALAXIES. I. COMBINATIONS OF Hα AND INFRARED TRACERS (2009, methodology): “Whenever possible we adopted in order of priority the fluxes measured in the IRAS Revised Bright Galaxy Sample (Sanders et al. 2003), followed by IRAS Bright Galaxy Sample (Soifer et al. 1989), then the large optical galaxy catalog (Rice et al. 1988) and finally version 2 of the IRAS Faint Source…”
THE MOLECULAR GAS IN LUMINOUS INFRARED GALAXIES. II. EXTREME PHYSICAL CONDITIONS AND THEIR EFFECTS ON THE Xco FACTOR (2012, methodology): “Mrk 231 This is an archetypal ULIRG/QSO and the most IR luminous galaxy in the Revised IRAS Bright Galaxy Survey (RBGS; Sanders et al. 2003).”
The 0.4 < z < 1.3 star formation history of the Universe as viewed in the far-infrared (2009, background): “This choice is driven by the fact that the ultimate goal of this paper is to derive the evolution of the total infrared LF which is itself best fitted with a double power law function (Sanders et al. 2003).”
Far-infrared spectral energy distribution fitting for galaxies near and far (2012, methodology): “Similarly, dust temperatures estimated for the original RBGS sample (Sanders et al. 2003) were overestimated by ∼10 K, due to the different fitting method used (single greybody versus single greybody plus mid-IR powerlaw).”
Luminous Infrared Galaxies with the Submillimeter Array. I. Survey Overview and the Central Gas to Dust Ratio (2008, methodology): “Out of a total of 39 galaxies above declination -20o (Sanders et al. 2003) which meet these two criteria, we selected for this survey 14 galaxies with previous interferometric observations in the CO J=1-0 transition.”
THE DISRUPTION OF GIANT MOLECULAR CLOUDS BY RADIATION PRESSURE & THE EFFICIENCY OF STAR FORMATION IN GALAXIES (2009, background): “The Starburst M82 M82 is one of the nearest (D = 3.6 Mpc; Freedman et al. 1994) starburst galaxies, with an infrared luminosityLIR = 5.8× 1010L⊙ (Sanders et al. 2003).”
Spitzer Observations of Massive, Red Galaxies at High Redshift (2005, background): “Locally, the space density of ULIRGs is 10 7 h70 Mpc 3 (Sanders et al. 2003), while the DRGs with ULIRG-like luminosities have a space density of (5:8 0:9) ; 10 5 h 370 Mpc 3, an increase by a factor of 600 (and similar to the conclusion for BzK-selected objects; Daddi et al. 2005b).”
GALAXY-WIDE SHOCKS IN LATE-MERGER STAGE LUMINOUS INFRARED GALAXIES (2011, neutral): “B Mag. log(LIR/L⊙) IC 1623 0.0201 01:07:47 -17:30:27 15.04 11.71 NGC 3256 0.00935 10:27:51 -43:54:14 11.83 11.64 extragalactic sources in the local universe (log LIR/L⊙) > 11.0), with redshifts z< 0.088 and is a complete subset of the IRAS Revised Bright Galaxy Sample (RBGS) (Sanders et al. 2003).”
OBSERVATIONS OF Arp 220 USING HERSCHEL-SPIRE: AN UNPRECEDENTED VIEW OF THE MOLECULAR GAS IN AN EXTREME STAR FORMATION ENVIRONMENT (2011, methodology): “We overplot data from IRAS in green-solid squares (Sanders et al. 2003), SCUBA in green - solid triangles (Dunne et al. 2000), ISOPHOT in purple - open diamonds (Klaas et al. 2001) and Planck in orange open triangles (Planck Collaboration 2011, arXiv:1101.2041), which also show good agreement with…”
Near-Infrared and Star-forming Properties of Local Luminous Infrared Galaxies (2006, methodology): “The sample comprises approximately 80% of all the LIRGs in the RBGS in the above velocity interval, and is representative of local LIRGs in general.”
GAS-PHASE OXYGEN GRADIENTS IN STRONGLY INTERACTING GALAXIES. I. EARLY-STAGE INTERACTIONS (2010, background): “The pairs are chosen from both optically-selected (Arp 1966; Barton et al. 2000) and infrared-selected (Sanders et al. 2003; Surace et al. 2004) catalogs of interacting systems.”
THE SPITZER LOCAL VOLUME LEGACY: SURVEY DESCRIPTION AND INFRARED PHOTOMETRY (2009, methodology): “The IRAS data are compiled from Rice et al. (1988), Moshir et al. (1990), Sanders et al. (2003), Lisenfeld et al. (2007), and our own archival extractions.”
Infrared Luminosity Functions from the Chandra Deep Field-South: The Spitzer View on the History of Dusty Star Formation at 0 ≲ z ≲ 1* (2005, methodology): “Regarding the total IR luminosity function φIR(L) at z=0, we show on one hand a recent result from the revised IRAS Bright Galaxy Sample (Sanders et al. 2003), on the other hand an estimate that we derived from the 60µm local LF (Saunders et al. 1990; Takeuchi et al. 2003) assuming the tight…”
X-ray emission from star-forming galaxies – I. High-mass X-ray binaries (2011, methodology): “…UGC 05720 24.9+11.1 −7.7 (2) Im pec 28 0.6 1.8 0.37 4.9 38.36 4 39.68 0.18 38.37 CARTWHEEL 122.8 (17) S pec (Ring) - 0.7 17.6 4.2 4.2 39.20 11 41.23 0.68 40.01 a References for distances: (1) Sanders et al. (2003), (2) Tully (1988), (3) Grisé et al. (2008), (4) Georgiev et al. (2006), (5)…”