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10 results on '"Baugh, Carlton"'

1. The 2dF Galaxy Redshift Survey: luminosity functions by density environment and galaxy type

Author

Croton, Darren J, Farrar, Glennys R, Norberg, Peder, Colless, Matthew, Peacock, John A, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Croton, Darren J, Farrar, Glennys R, Norberg, Peder, Colless, Matthew, Peacock, John A, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

We use the 2dF Galaxy Redshift Survey to measure the dependence of the b J-band galaxy luminosity function on large-scale environment, defined by density contrast in spheres of radius 8h -1 Mpc, and on spectral type, determined from principal component analysis. We find that the galaxy populations at both extremes of density differ significantly from that at the mean density. The population in voids is dominated by late types and shows, relative to the mean, a deficit of galaxies that becomes increasingly pronounced at magnitudes brighter than M bJ, - 5 log 10 h ≲ -18.5. In contrast, cluster regions have a relative excess of very bright early-type galaxies with M bJ, - 5 log 10 h ≲ -21. Differences in the mid- to faint-end population between environments are significant: at M bJ, -5 log 10 h = -18 early- and late-type cluster galaxies show comparable abundances, whereas in voids the late types dominate by almost an order of magnitude. We find that the luminosity functions measured in all density environments, from voids to clusters, can be approximated by Schechter functions with parameters that vary smoothly with local density, but in a fashion that differs strikingly for early- and late-type galaxies. These observed variations, combined with our finding that the faint-end slope of the overall luminosity function depends at most weakly on density environment, may prove to be a significant challenge for models of galaxy formation.

Published
2005

2. The 2dF Galaxy Redshift Survey: stochastic relative biasing between galaxy populations

Author

Wild, Vivienne, Peacock, John A, Lahav, Ofer, Conway, Edward, Maddox, Steve J, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, de Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole, Lewis, Ian, Lumsden, Stuart, Madgwick, Darren, Norberg, Peder, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Wild, Vivienne, Peacock, John A, Lahav, Ofer, Conway, Edward, Maddox, Steve J, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, de Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole, Lewis, Ian, Lumsden, Stuart, Madgwick, Darren, Norberg, Peder, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

It is well known that the clustering of galaxies depends on galaxy type. Such relative bias complicates the inference of cosmological parameters from galaxy redshift surveys, and is a challenge to theories of galaxy formation and evolution. In this paper

Published
2005

3. Galaxy groups in the 2dFGRS: the group-finding algorithm and the 2PIGG catalogue

Author

Eke, Vincent R, Baugh, Carlton M, Cole, Shaun, Frenk, Carlos S, Norberg, Peder, Peacock, John A, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Glazebrook, Karl, Jackson, Carole, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Eke, Vincent R, Baugh, Carlton M, Cole, Shaun, Frenk, Carlos S, Norberg, Peder, Peacock, John A, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Glazebrook, Karl, Jackson, Carole, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Red-shift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ∼190 000 galaxies considered are placed into groups containing at least two members of which ∼29 000 are found. Of these, ∼7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260 km s -1. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups. It is publicly available on the World Wide Web.

Published
2004

4. The 2dF Galaxy Redshift Survey: Wiener reconstruction of the cosmic web

Author

Erdogdu, Pirin, Lahav, Ofer, Zaroubi, Saleem, Efstathiou, George, Moody, Stephen, Peacock, John A, Colless, Matthew, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Norberg, Peder, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Erdogdu, Pirin, Lahav, Ofer, Zaroubi, Saleem, Efstathiou, George, Moody, Stephen, Peacock, John A, Colless, Matthew, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Norberg, Peder, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

We reconstruct the underlying density field of the Two-degree Field Galaxy Redshift Survey (2dFGRS) for the redshift range 0.035 < z < 0.200 using the Wiener filtering method. The Wiener filter suppresses shot noise and accounts for selection and incompleteness effects. The method relies on prior knowledge of the 2dF power spectrum of fluctuations and the combination of matter density and bias parameters, however the results are only slightly affected by changes to these parameters. We present maps of the density field. We use a variable smoothing technique with two different effective resolutions: 5 and 10 h-1 Mpc at the median redshift of the survey. We identify all major superclusters and voids in the survey. In particular, we find two large superclusters and two large local voids. The full set of colour maps can be viewed on the World Wide Web at http://www.ast.cam.ac.uk/~pirin.

Published
2004

5. Substructure analysis of selected low-richness 2dFGRS clusters of galaxies

Author

Burgett, William, Vick, Michael, Davis, David, Colless, Matthew, De Propris, Roberto, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Cross, Nicholas J G, Dalton, Gavin, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Hawkins, Edward, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Norberg, Peder, Peacock, John A, Percival, Will J, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Burgett, William, Vick, Michael, Davis, David, Colless, Matthew, De Propris, Roberto, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Cross, Nicholas J G, Dalton, Gavin, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Hawkins, Edward, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Norberg, Peder, Peacock, John A, Percival, Will J, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

Complementary one-, two- and three-dimensional tests for detecting the presence of substructure in clusters of galaxies are applied to recently obtained data from the 2dF Galaxy Redshift Survey. The sample of 25 clusters used in this study includes 16 clusters not previously investigated for substructure. Substructure is detected at or greater than the 99 per cent confidence level in at least one test for 21 of the 25 clusters studied here. From the results, it appears that low-richness clusters commonly contain subclusters participating in mergers. About half of the clusters have two or more components within 0.5 h -1 Mpc of the cluster centroid, and at least three clusters (Abell 1139, Abell 1663 and Abell S333) exhibit velocity-position characteristics consistent with the presence of possible cluster rotation, shear, or infall dynamics. The geometry of certain features is consistent with influence by the host supercluster environments. In general, our results support the hypothesis that low-richness clusters relax to structureless equilibrium states on very long dynamical time-scales (if at all).

Published
2004

6. The 2dF Galaxy Redshift Survey: the clustering of galaxy groups

Author

Padilla, Nelson, Baugh, Carlton M, Eke, Vincent R, Norberg, Peder, Cole, Shaun, Frenk, Carlos S, Croton, Darren J, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Glazebrook, Karl, Jackson, Carole, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peacock, John A, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Padilla, Nelson, Baugh, Carlton M, Eke, Vincent R, Norberg, Peder, Cole, Shaun, Frenk, Carlos S, Croton, Darren J, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Glazebrook, Karl, Jackson, Carole, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peacock, John A, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

We measure the clustering of galaxy groups in the 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue. The 2PIGG sample has 28 877 groups with at least two members. The clustering amplitude of the full 2PIGG catalogue is weaker than that of 2dFGRS

Published
2004

7. The 2dF Galaxy Redshift Survey: voids and hierarchical scaling models

Author

Croton, Darren, Colless, Matthew, Gaztanaga, Enrique, Baugh, Carlton M, Norberg, Peder, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peacock, John A, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Croton, Darren, Colless, Matthew, Gaztanaga, Enrique, Baugh, Carlton M, Norberg, Peder, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Couch, Warrick, Dalton, Gavin, De Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peacock, John A, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

We measure the redshift-space reduced void probability function (VPF) for 2dFGRS volume-limited galaxy samples covering the absolute magnitude range M bJ -5log 10 h = -18 to -22. Theoretically, the VPF connects the distribution of voids to the moments of

Published
2004

8. Galaxy groups in the Two-degree Field Galaxy Redshift Survey: the luminous content of the groups

Author

Eke, Vincent R, Frenk, Carlos S, Baugh, Carlton M, Cole, Shaun, Norberg, Peder, Peacock, John A, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry, Cannon, Russell, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, de Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Glazebrook, Karl, Jackson, Carole, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peterson, Bruce, Sutherland, William J, Taylor, Keith, Eke, Vincent R, Frenk, Carlos S, Baugh, Carlton M, Cole, Shaun, Norberg, Peder, Peacock, John A, Baldry, Ivan K, Bland-Hawthorn, Joss, Bridges, Terry, Cannon, Russell, Colless, Matthew, Collins, Chris, Couch, Warrick, Dalton, Gavin, de Propris, Roberto, Driver, Simon, Efstathiou, George, Ellis, Richard S, Glazebrook, Karl, Jackson, Carole, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

The Two-degree Field Galaxy Redshift Survey (2dFGRS) Percolation-Inferred Galaxy Group (2PIGG) catalogue of ∼29 000 objects is used to study the luminous content of galaxy systems of various sizes. Mock galaxy catalogues constructed from cosmological si

Published
2004

9. The 2dF Galaxy Redshift Survey: the blue galaxy fraction and implications for the Butcher-Oemler effect

Author

De Propris, Roberto, Colless, Matthew, Peacock, John A, Couch, Warrick, Driver, Simon, Balogh, Michael, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Cross, Nicholas J G, Dalton, Gavin, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Hawkins, Edward, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Norberg, Peder, Percival, Will J, Peterson, Bruce, Sutherland, William J, Taylor, Keith, De Propris, Roberto, Colless, Matthew, Peacock, John A, Couch, Warrick, Driver, Simon, Balogh, Michael, Baldry, Ivan K, Baugh, Carlton M, Bland-Hawthorn, Joss, Bridges, Terry C, Cannon, Russell, Cole, Shaun, Collins, Chris, Cross, Nicholas J G, Dalton, Gavin, Efstathiou, George, Ellis, Richard S, Frenk, Carlos S, Glazebrook, Karl, Hawkins, Edward, Jackson, Carole A, Lahav, Ofer, Lewis, Ian, Lumsden, Stuart, Maddox, Steve J, Madgwick, Darren, Norberg, Peder, Percival, Will J, Peterson, Bruce, Sutherland, William J, and Taylor, Keith

Abstract

We derive the fraction of blue galaxies in a sample of clusters at z < 0.11 and the general field at the same redshift. The value of the blue fraction is observed to depend on the luminosity limit adopted, cluster-centric radius and, more generally, local galaxy density, but it does not depend on cluster properties. Changes in the blue fraction are due to variations in the relative proportions of red and blue galaxies but the star formation rate for these two galaxy groups remains unchanged. Our results are most consistent with a model where the star formation rate declines rapidly and the blue galaxies tend to be dwarfs and do not favour mechanisms where the Butcher-Oemler effect is caused by processes specific to the cluster environment.

Published
2004

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