THE ARECIBO LEGACY FAST ALFA SURVEY. X. THE H i MASS FUNCTION AND FROM THE 40% ALFALFA SURVEY

By Ann M. Martin, E. Papastergis, R. Giovanelli, M. Haynes, C. Springob, S. Stierwalt. 2010

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The Arecibo Legacy Fast ALFA (ALFALFA) survey has completed source extraction for 40% of its total sky area, resulting in the largest sample of H i-selected galaxies to date. We measure the H i mass function from a sample of 10,119 galaxies with and with well-described mass errors that accurately reflect our knowledge of low-mass systems. We characterize the survey sensitivity and its dependence on profile velocity width, the effect of large-scale structure, and the impact of radio frequency interference in order to calculate the H i mass function with both the 1/Vmax and 2DSWML methods. We also assess a flux-limited sample to test the robustness of the methods applied to the full sample. These measurements are in excellent agreement with one another; the derived Schechter function parameters are ϕ* (h370 Mpc−3 dex−1) = 4.8 ± 0.3 × 10−3, log (M*/M☉) + 2 log h70 = 9.96 ± 0.02, and α = −1.33 ± 0.02. We find 4.3 ± 0.3 ×10−4 h−170, 16% larger than the 2005 HIPASS result, and our Schechter function fit extrapolated to = 11.0 predicts an order of magnitude more galaxies than HIPASS. The larger values of and of M* imply an upward adjustment for estimates of the detection rate of future large-scale H i line surveys with, e.g., the Square Kilometer Array. A comparison with simulated galaxies from the Millennium Run and a treatment of photoheating as a method of baryon removal from H i-selected halos indicate that the disagreement between dark matter mass functions and baryonic mass functions may soon be resolved.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/364d7e4bf9adda0259ad6c25bc61f25b130fbe81

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Citations in the corpus

Evolution of the atomic and molecular gas content of galaxies (2013, methodology): “The local Hi mass function down to masses of log (MHI/M⊙) = 7, and global Hi density ΩHI, has been quantified by blind surveys such as ALFALFA (Giovanelli et al. 2005; Martin et al. 2010).”
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).”
The ESO UVES advanced data products quasar sample: II. Cosmological evolution of the neutral gas mass density (2013, background): “Atz = 0 the 21-cm radio surveys (Zwaan et al. 2005a; Martin et al. 2010; Braun 2012) indicate a decrease inΩg by at most a factor of 2 and a constant compatible with uncertainties.”
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): “For these reasons, Martin et al. (2010) included only objects with Code 1, detected within 15000 km s−1.”
UPDATED NEARBY GALAXY CATALOG (2013, methodology): “We also have made extensive use of the following Web services of surveys: the Galaxy Evolution Explorer (GALEX), the Two Micron All Sky Survey (2MASS), the HI Parkes All Sky Survey (HIPASS), the Arecibo Legacy Fast ALFA Survey (ALFALFA), the Extragalactic Distance Database (EDD), the Sloan Digital S”
THE COS-HALOS SURVEY: PHYSICAL CONDITIONS AND BARYONIC MASS IN THE LOW-REDSHIFT CIRCUMGALACTIC MEDIUM (2014, background): “The gas in the ISM of these galaxies will vary from very little to nearly as much as the stellar contribution (McGaugh et al. 2010; Martin et al. 2010).”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, methodology): “We note however that there might be a variation between Martin et al. (2010)’s field HI mass function at low redshift, and that of A963 1.”
THE ARECIBO LEGACY FAST ALFA SURVEY: THE GALAXY POPULATION DETECTED BY ALFALFA (2012, methodology): “But HIPASS suffered from limitations in its volume sensitivity, and in fact, ALFALFA detects more HI sources at the highMHI end (Martin et al. 2010).”
THE VELOCITY WIDTH FUNCTION OF GALAXIES FROM THE 40% ALFALFA SURVEY: SHEDDING LIGHT ON THE COLD DARK MATTER OVERABUNDANCE PROBLEM (2011, background): “The normalization is fixed by matching the integral of the distribution to the average number density of galaxies in the survey volume (see Martin et al. 2010, Appendix B.1 for more details).”
Cold gas properties of the Herschel Reference Survey - II. Molecular and total gas scaling relations (2014, methodology): “…gas mass function from the HRS galaxies, which is comparable to the Hi mass function determined by Zwaan et al. (2005) using HIPASS data and Martin et al. (2010) with ALFALFA data, is impossible since our set of data is not a sample of galaxies extracted from a blind CO survey of a…”
Is there a "too big to fail" problem in the field? (2014, methodology): “The distances adopted here are the ones listed in theα.40 catalog, which are primarily based on the flow model of Masters (2005) (for details refer to §3.2 in Martin et al. 2010).”
The Arecibo Legacy Fast ALFA Survey: The ALFALFA Extragalactic H i Source Catalog (2018, methodology): “Because of the large percentage of channels corrupted by the FAA radar systems at frequencies below 1350 MHz, statistical studies requiring volume completeness should be restricted to galaxies within the corresponding velocity limit of cz < 15000 km s−1 (Martin et al. 2010).”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, methodology): “This conclusion, however, would require a “steep” HI mass function (HIMF) in the local universe, in contrast to what is measured (Zwaan et al. 2005; Martin et al. 2010).”
Cosmic evolution of the atomic and molecular gas contents of galaxies (2011, methodology): “6 shows thez = 0 HI mass functions (HI MF) for the Bow06 and Bau05 models using the BR and the KMT SF laws, and observational results from Zwaan et al. (2005) and Martin et al. (2010).”
Ingredients for 21 cm Intensity Mapping (2018, methodology): “In this plot we also indicate measurements from different observations (Zwaan & Prochaska 2006; Rao et al. 2006; Lah et al. 2007; Songaila & Cowie 2010; Martin et al. 2010; Noterdaeme et al. 2012; Braun 2012; Rhee et al. 2013; Delhaize et al. 2013; Crighton et al. 2015).”