[ITAL]V[/ITAL]- and [ITAL]R[/ITAL]-band Galaxy Luminosity Functions and Low Surface Brightness Galaxies in the Century Survey

Brown, Warren R.; Geller, Margaret J.; Fabricant, Daniel G.; Kurtz, Michael J.

doi:10.1086/321176

Cited by 59 publications

(85 citation statements)

References 51 publications

(99 reference statements)

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“…For N ≥ 6 the cumulative distribution of the LSB galaxies follows the HSB distribution. Figure 1 shows that the spatial distribution of LSB galaxies follows in general the LSS defined by HSB galaxies which is in good agreement with the results from investigations on LSB galaxies in the Century Survey (Brown et al 2001). However, as mentioned before, there are some extremely isolated LSB galaxies located in voids of the LSS.…”

Section: Letter To the Editorsupporting

confidence: 89%

The environment of Low Surface Brightness galaxies

Rosenbaum

Bomans

2004

A&A

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Abstract. Using the Early Data Release of the Sloan Digital Sky Survey (SDSS) we investigated the clustering properties of Low Surface Brightness (LSB) galaxies in comparison to normal, High Surface Brightness (HSB) galaxies. We selected LSB galaxies and HSB galaxies with well measured redshifts from the SDSS data base and performed three-dimensional neighbour counting analysis within spheres of radii between 0.8 Mpc and 8.0 Mpc. As a second analysis method we used an Nth neighbour analysis with N varying from one to ten galaxies. Our results show significant differences between the galaxy densities of LSB galaxies and HSB galaxies on scales from 2 to 5 Mpc. At scales larger than 5 Mpc LSB and HSB galaxies share the same clustering properties. In the pie-slice diagrams the LSB galaxies appear to favour the inner rims of filaments as defined by the HSB galaxies, with a couple of LSB galaxies even being located inside the voids. Our results support the idea of gas-rich LSB galaxies forming and developing in low density regions without many galaxy interactions and just now reaching the filaments of the large scale structure.

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Section: Letter To the Editorsupporting

confidence: 89%

The environment of Low Surface Brightness galaxies

Rosenbaum

Bomans

2004

A&A

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“…For further details see [7]. Figure 1 shows that the spatial distribution of LSB galaxies follows in general the LSS defined by HSB galaxies which is in good agreement with the results from investigations of LSB galaxies in the Century Survey ( [2]). However, the LSB galaxies seem to favour the outer parts of the filaments and there is a handful of extremely isolated LSB galaxies located in voids of the LSS.…”

Section: Pos(bdmh2004)025supporting

confidence: 84%

The enviroment of Low Surface Brightness Galaxies

Rosenbaum¹,

Bomans²

2004

Proceedings of Baryons in Dark Matter Halos — PoS(BDMH2004)

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The formation and evolution scenarios that led to the existence of Low Surface Brightness (LSB) galaxies are not well understood yet. Although LSBs have HI components with low surface densities (systematically below the Kennicutt criterion), they can be regarded as gas-rich in general. Hence, the key in understanding LSBs lies in the answer to the question what prevented them from sufficient star formation. Using the public data releases of the Sloan Digital Sky Survey (SDSS), we investigated the galaxy density around LSBs in comparison to High Surface Brightness (HSB) galaxies. We performed a number counting analysis in three dimensions within spheres of several radii on a sample of HSBs and LSBs with well measured SDSS redshifts. On scales between 2 and 5 Mpc our results show significantly lower galaxy densities in the vicinity of LSBs compared to HSBs. At larger scales than 5 Mpc LSBs and HSBs share the same clustering properties but on scales below 2 Mpc the galaxy densities in the neighbourhood of LSBs lie systematically (but only with a slight significance) below that of HSBs. In the pie slice diagrams LSBs favour the outer rims of the filaments of the Large Scale Structure and some LSBs are even found in voids. These results give strong evidence to a formation and evolution scenario where LSBs were formed in low density environments. Hence, the lack of tidal interactions with companions must have caused the absence of an effective trigger for a sufficient starburst. Baryons in Dark Matter PoS(BDMH2004)025The enviroment of Low Surface Brightness Galaxies Stefan Dominik Rosenbaum • (right) are plotted containing a total of ∼800 LSB galaxies (black dots) and ∼16000 HSB galaxies (green/grey dots).

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“…4 gathers the few intrinsic LF estimates from redshift surveys with 0.01 < ∼ z max < ∼ 0.15. The R c LFs for the CS are calculated for the same 1/3 red and 1/3 blue subsamples as the V LFs (see Table 3 Table 2 of Brown et al 2001; see also comments on these shifts in Sect. 3.1.1).…”

Section: R C Bandmentioning

confidence: 99%

“…-When LFs are measured for 2 sub-samples separated by color (as in the Canada-France Redshift Survey, Lilly et al 1995; the CNOC1 survey, Lin et al 1997; and the Century Survey, Brown et al 2001), or separated by the equivalent width of characteristic emission lines (as in the ESO Slice Project, Zucca et al 1997; the Norris survey, Small et al 1997; and the Stromlo-APM survey, Loveday et al 1999; see also Lin et al 1996) they are insufficient for estimation of the intrinsic LFs as they not only fail to separate the various populations of giant and dwarf galaxies, but they also mix giant galaxies of different morphological type; this effect is illustrated using the ESO-Sculptor Survey (de Lapparent et al 2003b), for which PCA spectral types, colors and equivalent width of [OII] emission are available. -Although the COMBO-17 LFs in the B band (Wolf et al 2003) are consistent with those from the comparable CADIS (Fried et al 2001), and with those from the CNOC2 (Lin et al 1999) and ESO-Sculptor (de Lapparent et al 2003b) surveys, the COMBO-17 LFs converted into the U and R c bands shows significant differences with the CNOC2 and ESO-Sculptor for the intermediate spectral types corresponding to Spiral galaxies.…”

Section: Conclusion and Prospectsmentioning

confidence: 99%

“…At redshifts larger than ∼0.1, visual morphological classification becomes highly uncertain and is replaced by spectral classification (Heyl et al 1997;Bromley et al 1998;Lin et al 1999;Folkes et al 1999;Fried et al 2001;Madgwick et al 2002;Wolf et al 2003;de Lapparent et al 2003b). Other redshifts surveys for which a spectral classification is not available use either colors (Lilly et al 1995;Lin et al 1997;Metcalfe et al 1998;Brown et al 2001) or the strength of the emission lines (Lin et al 1996;Small et al 1997;Zucca et al 1997;Loveday et al 1999) for estimating the LFs of the different galaxy types. The widely varying criteria used for galaxy classification in systematic redshift surveys however complicate the interpretation and inter-comparison of the derived LFs.…”

Section: Introductionmentioning

confidence: 99%

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Critical analysis of the luminosity functions per galaxy type measured from redshift surveys

Lapparent

2003

A&A

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Abstract. I perform a quantitative comparison of the shape of the optical luminosity functions as a function of galaxy class and filter, which have been obtained from redshift surveys with an effective depth ranging from z 0.01 to z 0.6. This analysis is based on the M * and α Schechter parameters which are systematically measured for all galaxy redshift surveys. I provide complete tables of all the existing measurements, which I have converted into the UBVR c I c Johnson-Cousins system wherever necessary.By using as reference the intrinsic luminosity functions per morphological type, I establish that the variations in the luminosity functions from survey to survey and among the galaxy classes are closely related to the criteria for galaxy classification used in the surveys, as these determine the amount of mixing of the known morphological types within a given class. When using a spectral classification, the effect can be acute in the case of inaccurate spectrophotometric calibrations: the luminosity functions are then biased by type contamination and display a smooth variation from type to type which might be poorly related to the intrinsic luminosity functions per morphological type. In the case of surveys using multi-fiber spectroscopy, galaxy classification based on rest-frame colors might provide better estimates of the intrinsic luminosity functions.It is noticeable that all the existing redshift surveys fail to measure the Gaussian luminosity function for Spiral galaxies, presumably due to contamination by dwarf galaxies. Most existing redshift surveys based on visual morphological classification also appear to have their Elliptical/Lenticular luminosity functions contaminated by dwarf galaxies. In contrast, the analyses using a reliable spectral classification based on multi-slit spectroscopy or medium-filter spectrophotometry, and combined with accurate CCD photometry succeed in measuring the Gaussian luminosity function for E/S0 galaxies. The present analysis therefore calls for a more coherent approach in separating the relevant giant and dwarf galaxy types, a necessary step towards measuring reliable intrinsic luminosity functions.

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[ITAL]V[/ITAL]- and [ITAL]R[/ITAL]-band Galaxy Luminosity Functions and Low Surface Brightness Galaxies in the Century Survey

Cited by 59 publications

References 51 publications

The environment of Low Surface Brightness galaxies

The environment of Low Surface Brightness galaxies

The enviroment of Low Surface Brightness Galaxies

Critical analysis of the luminosity functions per galaxy type measured from redshift surveys

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