The HIPASS catalogue: ΩH i and environmental effects on the H i mass function of galaxies

By M. Zwaan, M. Meyer, L. Staveley-Smith, R. Webster. 2005

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We use the catalogue of 4315 extragalactic H i 21-cm emission-line detections from the H i Parkes All Sky Survey (HIPASS) to calculate the most accurate measurement of the H i mass function (HIMF) of galaxies to date. The completeness of the HIPASS sample is well characterized, which enables an accurate calculation of space densities. The HIMF is fitted with a Schechter function with parameters α=−1.37 ± 0.03 ± 0.05, log (M*/M⊙) = 9.80 ± 0.03 ± 0.03 h−275, and θ*= (6.0 ± 0.8 ± 0.6) × 10−3 h375 Mpc−3 dex−1 (random and systematic uncertainties at 68 per cent confidence limit), in good agreement with calculations based on the HIPASS Bright Galaxy Catalogue, which is a complete, but smaller, sub-sample of galaxies. The cosmological mass density of H i in the local Universe is found to be ΩH i= (3.5 ± 0.4 ± 0.4) × 10−4 h−175. This large homogeneous sample allows us to test whether the shape of the HIMF depends on local galaxy density. We find tentative evidence for environmental effects in the sense that the HIMF becomes steeper toward higher density regions, ranging from α≈−1.2 in the lowest density environments to α≈−1.5 in the highest density environments probed by this blind H i survey. This effect appears stronger when densities are measured on larger scales.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3ab6c4e10014fad0687374f0d5da86671b396cc8

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Citations in the corpus

The Neutral Hydrogen Cosmological Mass Density at z = 5 (2015, methodology): “At redshift < 0.3, H I 21 cm emission can be used to measure ΩHI either directly or by stacking analyses (e.g. Zwaan et al. 2005; Martin et al. 2010).”
A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei (2008, methodology): “One can compare the model predictions with the total mass density of H I gas from blind H I surveys at z ∼ 0 (Zwaan et al. 2005), as well as with estimates of cold gas at high redshift from damped Lyman α systems (e.g. Prochaska, Herbert-Fort & Wolfe 2005, and references therein).”
Damped Lyα Systems at z < 1.65: The Expanded Sloan Digital Sky Survey Hubble Space Telescope Sample (2006, methodology): “In Figure 14 we used the most recent estimate of n(z ¼ 0) ¼ 0:045 0:006 derived by Zwaan et al. (2005b).”
The HI content of star-forming galaxies at z = 0.24 (2007, methodology): “Using the HI mass function at z ∼ 0 (Zwaan et al. 2005), we estimate that there is only a ∼15% chance of a direct detection (5σ) of the HI flux from an individual galaxy within the volume probed by our GMRT observations.”
Evolution of the atomic and molecular gas content of galaxies (2013, methodology): “We overplot observations from Zwaan et al. (2005) and Martin et al. (2010) at z = 0.0.”
THE ARECIBO LEGACY FAST ALFA SURVEY. X. THE H i MASS FUNCTION AND FROM THE 40% ALFALFA SURVEY (2010, methodology): “The published HIPASS HIMFs were based on more galaxies than previous blind surveys; the function extracted from the 1000 brightest detections (Zwaan et al. 2003) had a faint-end slope -1.3 and the later paper, with a fuller catalog of 4315 sources (Zwaan et al. 2005), found -1.37.”
Is there a "too big to fail" problem in the field? (2014, background): “…of central importance in extragalactic astronomy, and their measurement and scientific interpretation has been the subject of a large body of literature (see e.g. Martin et al. 2010; Zwaan et al. 2005; Papastergis et al. 2011; Zwaan et al. 2010 for some of the most recent observational results).”
Science with the Australian Square Kilometre Array Pathfinder (2007, methodology): “HIPASS data have allowed accurate measurement of the local H i mass function (HIMF) and ΩHI of galaxies (Zwaan et al. 2003, 2005).”
FIGGS: Faint Irregular Galaxies GMRT Survey – overview, observations and first results (2008, background): “…from, for example, testing the predictions E-mail: ayesha@ast.cam.ac.uk of cold dark matter models (e.g. Blanton, Geha & West 2007; Simon & Geha 2007), checking if such systems could be the host population of quasar absorption line systems (e.g. Kanekar & Chengalur 2005; Zwaan et al. 2005) etc.”
Physical properties and environments of nearby galaxies (2009, methodology): “Finally, in the lower right panel of Figure 3 we show the Hi mass functions determined by the compilation of Springob, Haynes & Giovanelli (2005), which is comparable to the HIPASS result of Zwaan et al. (2005).”
Galacticus: A Semi-Analytic Model of Galaxy Formation (2010, methodology): “Figure 11 explores the gas content of galaxies in the example model, by comparing the model HI mass function with that observed by Zwaan et al. (2005).”
On the impact of empirical and theoretical star formation laws on galaxy formation (2010, methodology): “For the Bow06 model, these changes help to improve the agreement with the local observations by Zwaan et al. (2005).”
Evolution of the cosmological mass density of neutral gas from Sloan Digital Sky Survey II - Data Release 7 (2009, methodology): “TheΓ-function fit to the frequency distribution obtained by Zwaan et al. (2005b) from 21-cm observations atz = 0 is also indicated as a solid grey line for direct comparison.”
MEASUREMENT OF 21 cm BRIGHTNESS FLUCTUATIONS AT z ∼ 0.8 IN CROSS-CORRELATION (2012, methodology): “Below redshiftz = 0.1, H I has been studied using 21 cm emission from its hyperfine splitting (Zwaan et al. 2005; Martin et al. 2010).”