The K-band luminosity function of galaxies

Gardner, Jonathan P.; Sharples, R. M.; Frenk, Carlos S.; Carrasco, B. E.

doi:10.1063/1.52763

Cited by 23 publications

(43 citation statements)

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“…In the top panel, the bold lines show the observed B ‐band luminosity function from the 2dF survey (higher line) and the APM survey (lower line). In the bottom panel, the bold lines show the observed K ‐band luminosity function from Szokoly et al 1998; Gardner et al (1997).…”

Section: Summary and Discussionmentioning

confidence: 99%

“…12. The wide‐field K ‐band survey discussed in Gardner et al (1997) covers an area of ∼4.4 square degrees, and probably provides the best existing determination of the bright end of the K ‐band LF. The survey discussed in Szokoly et al (1998) has a smaller area (0.6 square degrees) but has a fainter limiting magnitude, and thus presumably provides a more reliable estimate of the faint‐end slope.…”

Section: Comparison With Local Observationsmentioning

confidence: 99%

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Semi-analytic modelling of galaxy formation: the local Universe

Somerville¹,

Primack²

1999

Monthly Notices of the Royal Astronomical Society

1,011

1,135

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Using semi‐analytic models of galaxy formation, we investigate galaxy properties such as the Tully–Fisher relation, the B‐ and K‐band LFs, cold gas contents, sizes, metallicities and colours, and compare our results with observations of local galaxies. We investigate several different recipes for star formation and supernova feedback, including choices that are similar to the treatment by Kauffmann, White & Guiderdoni and Cole et al., as well as some new recipes. We obtain good agreement with all of the key local observations mentioned above. In particular, in our best models, we simultaneously produce good agreement with both the observed B‐ and K‐band LFs and the I‐band Tully–Fisher relation. Improved cooling and supernova feedback modelling, inclusion of dust extinction and an improved Press–Schechter model all contribute to this success. We present results for several variants of the CDM family of cosmologies, and find that models with values of Ω0≃0.3–0.5 give the best agreement with observations.

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Section: Summary and Discussionmentioning

confidence: 99%

Section: Comparison With Local Observationsmentioning

confidence: 99%

Semi-analytic modelling of galaxy formation: the local Universe

Somerville¹,

Primack²

1999

Monthly Notices of the Royal Astronomical Society

1,011

1,135

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“…However, these compensation effects are likely to be fairly small since, first, any change in the model normalization would affect the excellent agreement the model has with fainter K ‐band data (e.g. Glazebrook et al 1995; Gardner et al 1996; Huang et al 1996), and secondly, since any significant recalculation of the effective areas would upset the excellent agreement of the 2dF optical magnitude counts with the 2MASS counts for the 2dF fields (Fig. 4), which are normalized using the same method as the two sets of six 2MASS strips in Fig.…”

Section: Bright Galaxy Countsmentioning

confidence: 99%

The local hole in the galaxy distribution: evidence from 2MASS

Frith

Busswell

Fong

et al. 2003

Monthly Notices of the Royal Astronomical Society

108

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Using the bright galaxy counts from the 2 Micron All‐sky Survey (2MASS) second incremental release, two techniques for probing large‐scale structure at distances of ∼150 h−1 Mpc are investigated. First, we study the counts from two sets of six 5°×∼80° strips in the two galactic caps. In the six southern strips a deficit of ∼30 per cent was found relative to a predicted homogeneous distribution at Ks∼ 11. These strips were also in good agreement with a model incorporating the radial density function of the southern 2dF Galaxy Redshift Survey (2dFGRS), which shows a deep underdensity between ∼90 and 180 h−1 Mpc. These results indicate a very large ‘local hole’ in the Southern Galactic Cap (SGC) to ≳150 h−1 Mpc with a linear size across the sky of ∼200 h−1 Mpc, but with a significantly lower mean underdensity of ∼30 per cent compared with that suggested by the bright APM SGC counts. The counts in the northern set of strips are low overall but indicate a more varied pattern. When all the available 2MASS data with |b| > 30° were aggregated, they indicated underdensities of ∼18 and ∼30 per cent at Ks∼ 11 for the northern and southern areas, respectively. Our second method uses the ratio of the counts between 11.38 < Ks < 12.38 and 12.88 < Ks < 13.38 to the ratio of the corresponding counts of the homogeneous model binned in 25 deg2 areas; the counts from these areas provide a smoothed map over the sky of the slope in the counts between Ks= 11.38 and 13.38. Visually, the resulting map shows the expected complex form of the cosmic web and picks out known rich clusters, demonstrating the usefulness of this ‘slope statistic’ as a probe of large‐scale structure at distances of ≲150 h−1 Mpc. Most interestingly, the map also shows large regions, ∼100° across, of steep counts in both hemispheres. Thus, the present 2MASS data suggest the presence of a potentially huge contiguous void stretching from south to north. Not only would this delineate further the limits for the cosmological principle but it would also show the possible presence of significant power on scales of ≳300 h−1 Mpc in the galaxy power spectrum.

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“…Figure 5 shows number magnitude relations for K-band selected samples. The slope of the full K-selected counts, d(log(N))/dm, is 0.26 (Djorgovski et al 1995, Gardner et al 1996, Huang et al 2001, Moustakas et al 1997, Yan et al 1998). The lower curves show the counts for various color cuts (R − K > 5.3 and 6.0 on the right and I − K > 4, 4.5, 5, 5.5 on the left).…”

Section: Surface Density On the Skymentioning

confidence: 99%

Eros and Faint Red Galaxies

McCarthy

2004

Annu. Rev. Astron. Astrophys.

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■ Abstract This chapter reviews the properties of faint IR-selected field galaxies and the extremely red color-selected populations in particular. These populations are a mix of passively evolving stellar systems and heavily obscured star-forming galaxies. The star-forming component appears to constitute 20-50% of the population depending on the magnitude and color cuts employed. The remaining objects are a mix of passively evolving ellipticals and early-type disk galaxies. The passively evolving red galaxies are strongly clustered in space and are likely the high-mass high-luminosity end of the elliptical galaxy progenitor population at redshifts between one and two. These galaxies have masses and space densities that appear to be in conflict with late-forming hierarchical galaxy-formation models. The red galaxies appear to be a population that is distinct from the moderately star-forming Lyman-Break galaxies but may be related to the starburst population at z > 2 seen in deep submillimeter surveys.

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The K-band luminosity function of galaxies

Cited by 23 publications

References 0 publications

Semi-analytic modelling of galaxy formation: the local Universe

Semi-analytic modelling of galaxy formation: the local Universe

The local hole in the galaxy distribution: evidence from 2MASS

Eros and Faint Red Galaxies

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