The Durham/UKST Galaxy Redshift Survey — V. The catalogue

Ratcliffe, A.; Shanks, T.; Parker, Quentin A.; Broadbent, A.; Watson, Fred; Oates, A. P.; Collins, Chris; Fong, R.

doi:10.1046/j.1365-8711.1998.01907.x

Cited by 91 publications

(140 citation statements)

References 13 publications

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“…The Durham/UKST galaxy redshift survey ( [535]) consists of 2500 galaxy redshifts to a limiting apparent magnitude of b J = 17, covering a 1500 sq deg area around the south galactic Pole. The galaxies in this survey were selected from the EDSGC and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three.…”

Section: Namementioning

confidence: 99%

Large-scale structure of the Universe and cosmological perturbation theory

et al. 2002

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We review the formalism and applications of non-linear perturbation theory (PT) to understanding the large-scale structure of the Universe. We first discuss the dynamics of gravitational instability, from the linear to the non-linear regime. This includes Eulerian and Lagrangian PT, non-linear approximations, and a brief description of numerical simulation techniques. We then cover the basic statistical tools used in cosmology to describe cosmic fields, such as correlations functions in real and Fourier space, probability distribution functions, cumulants and generating functions. In subsequent sections we review the use of PT to make quantitative predictions about these statistics according to initial conditions, including effects of possible non Gaussianity of the primordial fields. Results are illustrated by detailed comparisons of PT predictions with numerical simulations. The last sections deal with applications to observations. First we review in detail practical estimators of statistics in galaxy catalogs and related errors, including traditional approaches and more recent developments. Then, we consider the effects of the bias between the galaxy distribution and the matter distribution, the treatment of redshift distortions in three-dimensional surveys and of projection effects in angular catalogs, and some applications to weak gravitational lensing. We finally review the current observational situation regarding statistics in galaxy catalogs and what the future generation of galaxy surveys promises to deliver.

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Section: Namementioning

confidence: 99%

Large-scale structure of the Universe and cosmological perturbation theory

et al. 2002

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“…Columns 2 and 3 present the object identification and the radial velocity from ESO-LV catalogue (Lauberts & Valentijn 1989). Column 3 also exhibits other values for galaxy radial velocity when it was not available in the ESO-LV; in this column, BLA indicates data from Bergvall et al (2003);dCa, da Costa et al (1991);dCb, da Costa (1994;as published in Reduzzi & Rampazzo 1995);dCc, da Costa et al (1998);dS, de Souza et al (1997);F, Fisher et al (1995); FJ, Fairall & Jones (1991); Lo, Loveday (1996); M, Mathewson et al (1992); R., Ratcliffe et al 1998;Sch., Schweizer (1987); and SWa, Sekiguchi & Wolstencroft (1992). Column 4 shows the radial velocity obtained using emission lines; Col. 5, the latter column value dispersion; Col. 6, the number of lines used to determine last column value; Col. 7, the radial velocity obtained using absorption lines; Col. 8, last column dispersion value; Col. 9, the number of lines used to get Col. 8; Col. 10, radial velocity obtained using crosscorrelation method; Col. 11, last value dispersion; and Col. 12, the TDR value, which supplies the confidence degree of crosscorrelation method used to get the radial velocity value (Tonry & Davis 1979).…”

Section: Radial Velocitiesmentioning

confidence: 99%

Optical spectroscopy for a sample of southern binary galaxies

Silva

Souza²

2006

A&A

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Aims. This work is part of a joint observational program aiming to get photometric and spectroscopic information on southern pairs of galaxies. We present optical long-slit spectroscopic data on 80 probable components of pairs, 61 of them collected with a spectral resolution of 3.4 Å, and 19 with 12 Å. Nevertheless, our analysis takes into account 53 components of pairs with better spectral resolution, as 8 of these target galaxies actually belong to optical pairs. For the sample with better resolution, the covered wavelength range is 5724 ≤ λ ≤ 7036 Å. The spectroscopic and photometric information is gathered for an analysis relating galaxy morphologies to their spectra. Methods. We use H α + [N II ] and H α equivalent widths as star formation tracers for the central region of our sample galaxies, and we classify the spectra according to the emission lines' relative strength by looking at their behavior. Results. Some of our sample galaxies exhibit high central star formation, most of them belonging to close pairs. However, not all galaxies' components of close pairs show this behavior. This may be a clue that besides interaction, other agents can stimulate central emission in binary galaxies. We suggest an enhancement in the number of galaxies with peculiar spectra (probably Seyferts) in our binary sample, when compared to isolated galaxies. Our data indicates that the morphological types of interacting galaxies are related to their spectral characteristics, as almost all early-type galaxies of our sample do not exhibit central optical emission. We note that the star formation activity is most likely to take place in both pairs' components, with a slightly higher mean strength for the less bright component of the pair. It is interesting to point out that most spirals exhibiting a strong HII emission line spectra present either a bar or a peculiarity, but on a general basis we do not find an enhancement of star formation in our interaction sample.

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“…Columns 2-5 present the object identification from the ESO-LV catalogue (Lauberts & Valentijn 1989): identification, radial velocity, blue band total magnitude, and morphological type. Whenever possible, we complete the radial information in Col. 3 with data from other sources; in this column, CS indicates data from Couto da Silva & de Souza (2006); dCa, da Costa et al (1991);dCb, da Costa (1994); dCc, da dS, de Souza et al (1997); FJ, Fairall & Jones (1991); Lo, Loveday (1996); M, Mathewson et al (1992); R., Ratcliffe et al 1998;Sch., Schweizer (1987a,b); and SWa, Sekiguchi & Wolstencroft (1992). Until now, has been no radial velocity available for the object P151b; however, P151a was studied by Combes et al (1994) as a pair component, and according to Donzelli & Pastoriza (2000), P151 is a merging pair.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Photometric study of a sample of southern binary galaxies

Silva

Souza²

2006

A&A

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Aims. This work exhibits the basic optical photometric data for a sample of 50 probable southern binary galaxies. Our sample covers a broad range of pair separations, stages of interaction, and morphologies. From the initial list of selected pairs, using spectroscopic data from the literature and our own data, we conclude that 84% of these systems are true binary galaxies. Methods. We present residual and asymmetric maps, R major semi-axis profiles of surface brightness, ellipticity, position-angle, harmonic Fourier coefficients of third and fourth order (b 3 and b 4 ) for 50 probable pairs, and B − R color maps for 47 of these pairs. For most galaxies, we present the profiles in two different ways, aiming to verify the influence of random errors on them. Results. We note that random errors in position-angle profiles are at least 2• , but a more significant result must take into account a variation larger than 11• for this distribution. Barred galaxies usually show a typical behavior in ellipticity and position-angle profiles: these profiles display variations when changing from a bar to a disk region. In some cases, the variations also occur along the bar. Some galaxies show distribution profiles that are common for their morphological type, and the interaction signature is only evidenced by their residual maps. Bars are usually redder and rings are bluer, when compared with the galaxy outskirts. Conclusions. Our data indicates that there is a connection between interaction strength and morphological distortions in binary galaxies. If we consider the projected separation of a pair as an indication of interaction strength, distortions such as displaced centers, anomalous shapes of spiral arms, and twistings of external regions are easily detected in some close pairs, although not all components of close pairs show this behavior. Our data suggests that besides interaction, other parameters, like orbital geometry and internal properties of galaxies, can stimulate binary galaxies' peculiarities.

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The Durham/UKST Galaxy Redshift Survey — V. The catalogue

Cited by 91 publications

References 13 publications

Large-scale structure of the Universe and cosmological perturbation theory

Large-scale structure of the Universe and cosmological perturbation theory

Optical spectroscopy for a sample of southern binary galaxies

Photometric study of a sample of southern binary galaxies

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