The 2dF Galaxy Redshift Survey: galaxy clustering per spectral type

By D. Madgwick, E. Hawkins, Ofer Lahav, S. Maddox, P. Norberg, J. Peacock, I. Baldry, C. Baugh, Joss Bland-Hawthorn, T. Bridges and 18 more. 2003

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We have calculated the two-point correlation functions in redshift space, �(�,�), for galaxies of different spectral types in the 2dF Galaxy Redshift Survey. Using these correlation functions we are able to estimate values of the linear redshi ft-space distortion parameter, � ≡ 0.6 m /b, the pairwise velocity dispersion, a, and the real-space correlation function, �(r), for galaxies with both relatively low star-formation rates (for which the present rate of star formation is less than 10% of its past averaged value) and galaxies with higher current starformation activity. At small separations, the real-space c lustering of passive galaxies is very much stronger than that of the more actively star-forming galaxies; the correlation-function slopes are respectively 1.93 and 1.50, and the relative bias between the two classes is a declining function of radius. On scales larger than 10h 1 Mpc there is evidence that the relative bias tends to a constant, bpassive/bactive ≃ 1. This result is consistent with the similar degrees of redshift-space distortions seen in the correlation func tions of the two classes ‐ the contours

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

GALAXY CLUSTERING IN THE NEWFIRM MEDIUM BAND SURVEY: THE RELATIONSHIP BETWEEN STELLAR MASS AND DARK MATTER HALO MASS AT 1 < z < 2 (2010, background): “…properties, such as luminosity, color, star formation rate, and morphology (Norberg et al. 2001, 2002; Zehavi et al. 2002; Budavári et al. 2003; Madgwick et al. 2003; Zehavi et al. 2005; Li et al. 2006; Swanson et al. 2008; Ross & Brunner 2009; Loh et al. 2010; Ross et al. 2010; Zehavi et al.…”
The DEEP2 Galaxy Redshift Survey: Color and Luminosity Dependence of Galaxy Clustering at z ∼ 1 (2007, methodology): “…da Costa, & Pellegrini 1998), with the most statistically-significant results provided by the latest large surveys, the 2dF Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey (SDSS) (Norberg et al. 2002b; Zehavi et al. 2002; Madgwick et al. 2003a; Li et al. 2006a; Zehavi et al. 2005).”
The DEEP2 Galaxy Redshift Survey: Clustering of Galaxies in Early Data (2003, methodology): “Madgwick et al. (2003a) find using 2dFGRS data that locally, absorption-line galaxies have a relative bias about twice that of emission-line galaxies on scales of r ∼ 1 h−1 Mpc, but that the relative bias decreases to unity on scales >10 h−1 Mpc.”
The 6dF Galaxy Survey: z \approx 0 measurement of the growth rate and sigma_8 (2012, methodology): “The parameter σp depends on galaxy type (e.g. Madgwick et al. 2003) and hence its use for cosmological constraints is limited.”
The Intermediate-Scale Clustering of Luminous Red Galaxies (2004, background): “…al. 1996; Willmer et al. 1998; Brown et al. 2000; Carlberg et al. 2001; Norberg et al. 2001, 2002; Zehavi et al. 2002, 2004b; Budavari et al. 2003; Madgwick et al. 2003; Hogg et al. 2003), and these trends can be connected to their small-scale environments, notably the masses of their host dark…”
The 2dF-SDSS LRG and QSO Survey: the LRG 2-point correlation function and redshift-space distortions (2006, background): “Whether it be the detection of baryonic acoustic oscillations (Eisenstein et al. 2005), clustering properties of different spectral types of galaxy (Madgwick et al. 2003), or the evolution of active galactic nucleus black hole mass (Croom et al. 2005), the two-point correlation function (2PCF)…”
The 2dF Galaxy Redshift Survey: correlation functions, peculiar velocities and the matter density of the Universe (2002, methodology): “…correlation functions have been measured from many redshift surveys, but direct comparisons between different surveys are not straightforward because galaxy clustering depends on the spectral type and luminosity of galaxies (e.g. Guzzo et al. 2000; Norberg et al. 2002b; Madgwick et al. 2003).”
Theoretical Models of the Halo Occupation Distribution: Separating Central and Satellite Galaxies (2004, background): “Population age should be a fairly good proxy for galaxy color or spectral type, so this division mimics the red/blue or early/late divisions studied by Zehavi et al. (2002; 2005) in the SDSS and Norberg et al. (2002) and Madgwick et al. (2003) in the 2dFGRS.”
HALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES (2008, unknown): “…et al. 1997; Benoist et al. 1996; Norberg et al. 2001; Zehavi et al. 2002, 2005b; Coil et al. 2006, 2008), color (e.g., Willmer et al. 1998; Brown et al. 2000; Zehavi et al. 2002, 2005b; Coil et al. 2008), and spectral type (e.g., Norberg et al. 2002; Budavari et al. 2003; Madgwick et al. 2003).”
A semi-empirical simulation of the extragalactic radio continuum sky for next generation radio telescopes (2008, background): “We note, however, that tuning the starburst clustering to match the high-redshift submillimetre population will not accurately reproduce the much weaker clustering ofthe local starburst galaxies, which is much lower than that of passive galaxies (e.g. Madgwick et al. 2003).”
Statistical analysis of galaxy surveys – I. Robust error estimation for two-point clustering statistics (2008, background): “…al. 2000), satisfies both of these requirements and can be divided into large subsamples to study clustering trends with galaxy properties (e.g. Norberg et al. 2001, 2002; Zehavi et al. 2002, 2004, 2005; Madgwick et al. 2003; Croton et al. 2004, 2007; Gaztañaga et al. 2005; Li et al. 2006, 2007).”
Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources (2007, background): “…source populations contributing to the sub-mm counts, whose clustering is relatively weak, as in the case of spiral and starburst galaxies (cf. e.g. Madgwick et al. 2003) or highly diluted because of the very broad redshift distribution, as in the case of radio sources (Magliocchetti et al. 1999;…”
The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications (2005, background): “At smaller scales, there is an increasingly significant deviation, with the red galaxies being more clustered than the blue (in agreement with Madgwick et al. 2003).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, unknown): “…et al. 1989; Loveday et al. 1995; Benoist et al. 1996; Guzzo et al. 1997; Willmer et al. 1998; Brown, Webster & Boyle 2000; Norberg et al. 2001, 2002; Zehavi et al. 2002; Budavari et al. 2003; Madgwick et al. 2003; Zehavi et al. 2005b; Li et al. 2006; Swanson et al. 2008; Loh et al. 2010).”
The dependence of clustering on galaxy properties (2005, background): “…on a variety of factors, including luminosity (Norberg et al. 2001, Zehavi et al. 2002, Zehavi et al. 2005), colour (Zehavi et al. 2002, Zehavi et al. 2005), concentration (Zehavi et al. 2002, Goto et al. 2003), and spectral type (Norberg et al. 2002, Budavári et al. 2003, Madgwick et al. 2003).”
HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “The former, known to be weakly clustered (e.g. Madgwick et al. 2003; Guo et al. 2011; van Kampen et al. 2011), dominate the 250µm selected sample, while the selection at longer wavelengths emphasizes strongly clustered galaxies with intense star-formation activity at z ≈ 2 − 3, with typical halo…”