The HIPASS catalogue - I. Data presentation

By M. Meyer, M. Zwaan, Rachel L. Webster, L. Staveley-Smith, E. Ryan-Weber, Michael Drinkwater, David G. Barnes, M. Howlett, Virginia A. Kilborn, Jason Stevens and 27 more. 2004

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The H I Parkes All-Sky Survey (HIPASS) catalogue forms the largest uniform catalogue of H I sources compiled to date, with 4315 sources identified purely by their H I content. The catalogue data comprise the southern region δ< + 2 ◦ of HIPASS, the first blind H I survey to cover the entire southern sky. The rms noise for this survey is 13 mJy beam −1 and the velocity range is −1280 to 12 700 km s −1 . Data search, verification and parametrization methods are discussed along with a description of measured quantities. Full catalogue data are made available to the astronomical community including positions, velocities, velocity widths, integrated fluxes and peak flux densities. Also available are on-sky moment maps, position‐velocity moment maps and spectra of catalogue sources. A number of local large-scale features are observed in the space distribution of sources, including the super-Galactic plane and the Local Void. Notably, large-scale structure is seen at low Galactic latitudes, a region normally obscured at optical wavelengths.

Subfields: Astronomy and Astrophysics, Computational Mechanics

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Citations in the corpus

Physical properties and environments of nearby galaxies (2009, background): “…the Sloan Digital Sky Survey in the optical (SDSS; York et al. 2000), the Two-Micron All Sky Survey in the near infrared (2MASS; Skrutskie et al. 2006), as well as 21-cm radio surveys such as the Hi Parkes All Sky Survey (HIPASS; Meyer et al. 2004) and ALFALFA on Arecibo (Giovanelli et al. 2007).”
Cosmic evolution of the atomic and molecular gas contents of galaxies (2011, methodology): “…measurements of the21 cm emission in large surveys of local galaxies have been presented by Zwaan et al. (2005) using theHI Parkes All-Sky Survey (HIPASS; Meyer et al. 2004) and more recently by Martin et al. (2010) using the Arecibo Legacy Fast ALF Survey (ALFALFA; Giovanelli et al. 2005).”
UPDATED NEARBY GALAXY CATALOG (2013, background): “…number of new irregular dwarf galaxies with radial velocities VLG < 500 km s −1 were observed within the “blind” HI survey of the southern sky performed at the Parks radio telescope (Staveley-Smith et al. 1998, Kilborn et al. 2002, Zwaan et al. 2003, Koribalski et al. 2004, Meyer et al. 2004).”
THE ARECIBO LEGACY FAST ALFA SURVEY: THE GALAXY POPULATION DETECTED BY ALFALFA (2012, methodology): “Compared to the HI Parkes All Sky Survey (HIPASS: Barnes et al. 2001; Meyer et al. 2004; Wong et al. 2006), ALFALFA is 8 times more sensitive, its spectral coverage extends over 1.6 times the bandwidth of HIPASS, and the angular resolution of ALFA is 4 times better than that of the Parkes multifeed…”
THE VELOCITY WIDTH FUNCTION OF GALAXIES FROM THE 40% ALFALFA SURVEY: SHEDDING LIGHT ON THE COLD DARK MATTER OVERABUNDANCE PROBLEM (2011, methodology): “The ALFALFA survey is more sensitive than the previous generation HIPASS survey (Meyer et al. 2004; Zwaan et al. 2004), with a 5σ detection limit of 0.72 Jy km s−1 for a source with a profile width of 200 km s−1 as compared to a 5σ sensitivity of 5.6 Jy km s−1 for the same source in HIPASS…”
THE ARECIBO LEGACY FAST ALFA SURVEY: THE α.40 H i SOURCE CATALOG, ITS CHARACTERISTICS AND THEIR IMPACT ON THE DERIVATION OF THE H i MASS FUNCTION (2011, methodology): “A reasonable comparison of the impact of the different source detection schemes (including the absolute level of flux density sensitivity) may be made by comparing the distribution of the highest-mass galaxies in HIPASS and ALFALFA.”
The HIPASS catalogue - III. Optical counterparts and isolated dark galaxies (2005, background): “In Paper I, Meyer et al. (2004) describe the selection procedure, global sample properties and the catalogue.”
THE ARECIBO LEGACY FAST ALFA SURVEY. X. THE H i MASS FUNCTION AND FROM THE 40% ALFALFA SURVEY (2010, methodology): “The final α.40 sample contains 10,119 Code 1 galaxies, for a detection rate 3.9 deg−2 compared with the HIPASS detection rate ∼ 0.2 deg−2 (5317 extragalactic sources over 29,000 deg2; Meyer et al. (2004) and Wong et al. (2006)).”
The Survey for Ionization in Neutral Gas Galaxies. III. Diffuse, Warm Ionized Medium and Escape of Ionizing Radiation (2007, methodology): “As detailed in Paper I, H iYrelated quantities were derived fromHIPASS data, in particular, HICAT, the full HIPASS catalog (Meyer et al. 2004), and the HIPASS Bright Galaxy Catalog (Koribalski et al. 2004).”
THE CLUSTERING CHARACTERISTICS OF H i-SELECTED GALAXIES FROM THE 40% ALFALFA SURVEY (2012, background): “…the lack of large and deep HI-selected galaxy samples to date (the HIPASS main catalog and its northern extension contain, respectively, 4,315 and 1,002 galaxies; Meyer et al. (2004); Wong et al. (2006)), this population, its evolution, and its bias compared to dark matter are poorly understood.”
Science with the Australian Square Kilometre Array Pathfinder (2007, methodology): “This has been possible at z ∼< 0.04 using the H i Parkes All-Sky Survey HIPASS (Koribalski et al. 2004; Meyer et al. 2004), which mapped the distribution of H i in the nearby Universe that is observable from the Parkes radio telescope.”
The neutral hydrogen content of galaxies in cosmological hydrodynamic simulations (2013, methodology): “The H i Parkes AllSky Survey (HIPASS; Meyer et al. 2004) provided a comprehensive deep census of the H i content of low-redshift galaxies.”
Galaxy and Mass Assembly (GAMA): survey diagnostics and core data release (2010, background): “…the Millennium Galaxy Catalogue (MGC; Driver et al. 2005), the 6dF Galaxy Survey (6dFGS; Jones et al. 2004, 2009), the H I Parkes All Sky Survey (Meyer et al. 2004) and the Galaxy Evolution Explorer (GALEX; Martin et al. 2005) mission, each of which is opening up new avenues of extragalactic…”
Reconciling the local galaxy population with damped Lyman α cross-sections and metal abundances (2005, methodology): “In order to compare our findings with numbers calculated in models of galaxy formation, we first transform theB-band luminosities of our WHISP galaxies into rotational velocities via the Tully-Fisher relation.1 We choose here to use the Tully-Fisher relation determined by Meyer et al. (2005), based ”
THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, background): “(16) At low redshift, we learn from all-sky H i surveys (e.g. Zwaan & et al. 2003; Rosenberg & Schneider 2003; Meyer et al. 2004; Giovanelli et al. 2005; Wong et al. 2006; Catinella et al. 2010) that the gas fractions in SFGs vary systematically with stellar mass (e.g. Baldry et al. 2008, and…”