The Shape of the H i Mass Function for Late-Type Galaxies over the Range M H I 10 7--10 10 M sub sun

Briggs, F.; Rao, S. Sumangala

doi:10.1086/173328

Cited by 31 publications

(41 citation statements)

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“…Most of the shallower slopes (a B [1.2) for the H I mass function have been derived from optically selected samples in the Ðeld (Huchtmeier, Karachentsev, & Karachentseva 2000 ;Briggs & Rao 1993) or in clusters (Briggs & Rao 1993) or H IÈselected samples in high-density regions like the Canes Venatici group (Kraan-Korteweg et al 1999), Centaurus A (Banks et al 1999), or Ursa Major (Verheijen et al 2000). The results for the faint-end slope in the Ðeld have been more varied.…”

Section: Introductionmentioning

confidence: 99%

The Arecibo Dual‐Beam Survey: The HiMass Function of Galaxies

Rosenberg

Schneider

2002

ApJ

118

182

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We use the H IÈselected galaxy sample from the Arecibo Dual-Beam Survey of Rosenberg and Schneider to determine the shape of the H I mass function of galaxies in the local universe using both the stepwise maximum likelihood and the methods. Our survey region spanned all 24 hours of right 1/V tot ascension at selected declinations between 8¡ and 29¡ covering D430 deg2 of sky in the main beam. The survey is not as deep as some previous Arecibo surveys, but it has a larger total search volume and samples a much larger area of the sky. We conducted extensive tests on all aspects of the galaxy detection process, allowing us to empirically correct for our sensitivity limits, unlike the previous surveys. The mass function for the entire sample is quite steep, with a power-law slope of a B [1.5. We Ðnd indications that the slope of the H I mass function is Ñatter near the Virgo Cluster, suggesting that evolutionary e †ects in high-density environments may alter the shape of the H I mass function. These evolutionary e †ects may help to explain di †erences in the H I mass function derived by di †erent groups. We are sensitive to the most massive sources (log M [ 5 ] 1010 over most of the declination range, M _ ) D1 sr, and do not detect any massive low surface brightness galaxies. These statistics restrict the population of Malin 1Èlike galaxies to less than 5.5 ] 10~6 Mpc~3.

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Section: Introductionmentioning

confidence: 99%

The Arecibo Dual‐Beam Survey: The HiMass Function of Galaxies

Rosenberg

Schneider

2002

ApJ

118

182

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“…Log of velocity width (50%) as a function of H i mass, MHI, for the confirmed detections. The line is a boundary to the H i mass versus line-width relation derived from a much larger sample of galaxies (Briggs & Rao 1993), ∆V = 0.35(MHI/M ) 1/3 km s −1 . H i masses computed using distance d = V hel /H0 are marked by solid dots.…”

Section: Properties Of the Detected Galaxiesmentioning

confidence: 90%

“…4 the measured velocity width is plotted as a function of H i mass. There is a well known trend (a sort of H i Tully-Fisher Relation) that larger M HI masses are strongly correlated with higher rotation speeds (cf., Briggs & Rao 1993). Figure 4 displays H i masses based on observed velocities as well as H i masses corrected for Virgocentric flow using the POTENT program (solid respectively open circles) including the shifts in galaxy masses due to the perturbed velocity field.…”

Section: Properties Of the Detected Galaxiesmentioning

confidence: 99%

Nançay "blind” 21 cm line survey of the Canes Venatici group region

Kraan-Korteweg

Driel

Briggs

et al. 1999

Astron. Astrophys. Suppl. Ser.

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Abstract. A radio spectroscopic driftscan survey in the 21 cm line with the Nançay decimetric radio telescope of 0.08 steradians of sky in the direction of the constellation Canes Venatici covering a heliocentric velocity range of −350 < V hel < 2350 km s −1 produced 53 spectral features, which was further reduced to a sample of 33 reliably detected galaxies by extensive follow-up observations. With a typical noise level of rms = 10 mJy after Hanning smoothing, the survey is -depending on where the detections are located with regard to the centre of the beamsensitive to M HI = 1 − 2 10 8 h −2 M at 23 h −1 Mpc and to M HI = 4 − 8 10 7 h −2 M throughout the CVn groups. The survey region had been previously examined on deep optical plates by Binggeli et al. (1990) and contains loose groups with many gas-rich galaxies as well as voids. No galaxies that had not been previously identified in these deep optical surveys were uncovered in our H i survey, neither in the groups nor the voids. The implication is that no substantial quantity of neutral hydrogen contained in gas-rich galaxies has been missed in these well-studied groups. All late-type members of our sample are listed in the Fisher & Tully (1981b) optically selected sample of nearby late-type galaxies; the only system not contained in Fisher and Tully's Catalog is the S0 galaxy NGC 4203. Within the well-sampled CVn group volume with distances corrected for flow motions, the H i mass function is best fitted with the Zwaan et al. (1997) H i mass function (α = −1.2) scaled by a factor of f = 4.5 in account of the locally overdense region.

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“…Early studies of the possible environmental dependence of the HIMF were limited to comparisons of the HIMF derived for galaxies in the Virgo cluster with that derived for galaxies in the The ALFALFA Search for (Almost) Dark Galaxies 7 field (Hoffman et al 1992;Briggs & Rao 1993;Rosenberg & Schneider 2002;Davies et al 2004;Gavazzi et al 2004). While all of these studies suffer to varying degrees from poor statistics and incompleteness, their results marginally suggest that the HIMF in Virgo is missing the low HI mass dwarfs found in the field or is at least flatter at the faint end than the field HIMF.…”

Section: The Environment and Clustering Of Gas-rich Galaxiesmentioning

confidence: 99%

The ALFALFA Search for (Almost) Dark Galaxies across the HI Mass Function

Haynes¹

2007

Proc. IAU

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Abstract. The Arecibo Legacy Fast ALFA (ALFALFA) survey is a second generation blind extragalactic HI survey currently in progess which is exploiting Arecibo's superior sensitivity, angular resolution and digital technology to derive a census of the local HI universe over a cosmologically significant volume. As of the time of this meeting, some 4500 good quality extragalactic HI line sources have been identified in about 15% of the final survey area. ALFALFA is detecting HI masses as low as 10 6 M⊙ and as large as 10 10.8 M⊙ with positional accuracies typically better than 20′′ , allowing immediate identification of the most probable optical counterparts. Only 3% of all extragalactic HI sources and less than 1% of detections with MHI > 10 9.5 M⊙ cannot be identified with a stellar component. Because ALFALFA is far from complete, the discussion here focuses on limitations of past surveys that ALFALFA will overcome because of its greater volume, sensitivity and reduced susceptibility to source confusion and on a sampling of illustrative preliminary results. First ALFALFA results already suggest, in agreement with previous studies, that there does not appear to be a cosmologically significant population of optically dark but HI rich galaxies. ALFALFA promises a wealthy dataset for the exploration of many issues in near-field cosmology and galaxy evolution studies, setting the stage for their extension to higher redshifts in the future with the Square Kilometer Array (SKA).

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The Shape of the H i Mass Function for Late-Type Galaxies over the Range M H I 10 7--10 10 M sub sun

Cited by 31 publications

References 0 publications

The Arecibo Dual‐Beam Survey: The HiMass Function of Galaxies

The Arecibo Dual‐Beam Survey: The HiMass Function of Galaxies

Nançay "blind” 21 cm line survey of the Canes Venatici group region

The ALFALFA Search for (Almost) Dark Galaxies across the HI Mass Function

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