The COSMOS/UKST Catalog of the Southern Sky

Yentis, D.; Cruddace, R. G.; Gursky, H.; Stuart, Brian; Wallin, John F.; MacGillivray, H. T.; Collins, Chris

doi:10.1007/978-94-011-2472-0_10

Cited by 62 publications

(41 citation statements)

References 4 publications

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“…It is approximately centered on image A of a lensed QSO discovered by Tinney (1995) and located at ( ; ) ¼ (02 h 40 m 07:73 s ; À34 34 0 19:8 00 ) (J2000.0) (Yentis et al 1992). Image B of the QSO is 6.1 00 away from image A.…”

Section: Observations and Datamentioning

confidence: 99%

Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. V. Final Measurement for Fornax

Piatek¹,

Pryor²,

Bristow³

et al. 2007

100

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The measured proper motion of Fornax, expressed in the equatorial coordinate system, is ( ; ) ¼ (47:6 AE 4:6; À36:0 AE 4:1) mas century À1 . This proper motion is a weighted mean of four independent measurements for three distinct fields. Each measurement uses a quasi-stellar object as a reference point. Removing the contribution of the motion of the Sun and of the local standard of rest to the measured proper motion produces a Galactic restframe proper motion of ( Grf ; Grf ) ¼ (24:4 AE 4:6; À14:3 AE 4:1) mas century À1 . The implied space velocity with respect to the Galactic center has a radial component of V r ¼ À31:8 AE 1:7 km s À1 and a tangential component of V t ¼ 196 AE 29 km s À1 . Integrating the motion of Fornax in a realistic potential for the Milky Way produces orbital elements. The perigalacticon and apogalacticon are 118 (66, 137) and 152 (144, 242) kpc, respectively, where the values in the parentheses represent the 95% confidence intervals derived from Monte Carlo experiments. The eccentricity of the orbit is 0.13 (0.11, 0.38), and the orbital period is 3.2 (2.5, 4.6) Gyr. The orbit is retrograde and inclined by 101 (94 , 107 ) to the Galactic plane. Fornax could be a member of a proposed ''stream'' of galaxies and globular clusters; however, the membership of another proposed galaxy in the stream, Sculptor, has been previously ruled out. Fornax is in the Kroupa-Theis-Boily plane, which contains 11 of the Galactic satellite galaxies, but its orbit will take it out of that plane.

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Section: Observations and Datamentioning

confidence: 99%

Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. V. Final Measurement for Fornax

Piatek¹,

Pryor²,

Bristow³

et al. 2007

100

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“…For the analysis in the next sections it is important to estimate the completeness level of the velocity sample as a function of the magnitude. To do that (and also to study the cluster galaxy projected distribution) we extracted from the ROE/NRL COSMOS UKST Southern Sky Object Catalogue, supplied by the Anglo-Australian Observatory (Yentis et al 1992), a sample of galaxies in the direction of the cluster. An examination of Table 1 indicates that, with one exception, all velocities were measured in a region of ∼27 × 22 (in RA and DEC, …”

Section: Observations and Data Reductionsmentioning

confidence: 99%

The cluster of galaxies Abell 970

Sodré¹,

Proust²,

Capelato³

et al. 2001

A&A

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Abstract. We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.

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“…Starting with the pioneer attempt of Rose (1977) and the well known catalogue of Hickson (1982), several other authors have embarked themselves in the work of building CGs catalogues, such as Prandoni et al (1994); McConnachie et al (2009); Díaz-antotaverna@gmail.com Giménez et al (2012) and Hernández-Fernández & Mendes de Oliveira (2015). We mention only these particular catalogues because they are examples of surveys characterised by galaxy detections with different photometry: B (Johnson & Morgan 1953), R (Cousins 1976), bj (COSMOS-UKST, Yentis et al 1992), r (Sloan Digital Sky Survey, SDSS, York & SDSS Collaboration 2000), Ks (Two Micron All-Sky Survey, 2MASS, Skrutskie et al 2006) and FUV (Galaxy Evolution Explorer, GALEX, Bianchi 2014) bands. All these surveys span a wide range of the electromagnetic spectrum (roughly from 1400 to 23000Å), implying that objects with very different physical properties could be detected depending on which part of the spectrum is adopted to construct the galaxy surveys.…”

Section: Introductionmentioning

confidence: 99%

On the properties of compact groups identified in different photometric bands

Taverna

Díaz-Giménez

Zandivarez

et al. 2016

Mon. Not. R. Astron. Soc.

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Historically, compact group catalogues vary not only in their identification algorithms and selection functions, but also in their photometric bands. Differences between compact group catalogues have been reported. However, it is difficult to assess the impact of the photometric band in these differences given the variety of identification algorithms. We used the mock lightcone built by Henriques et al. (2012) to identify and compare compact groups in three different photometric bands: K, r, and u. We applied the same selection functions in the three bands, and found that compact groups in the u-band look the smallest in projection, the difference between the two brightest galaxies is the largest in the K-band, while compact groups in the r-band present the lowest compactness. We also investigated the differences between samples when galaxies are selected only in one particular band (pure compact groups) and those that exist regardless the band in which galaxies were observed (common compact groups). We found that the differences between the total samples are magnified, but also some others arise: pure-r compact groups are the largest in projection; pure-u compact groups have the brightest first ranked galaxies, and the most similar two first ranked galaxies; pure-K compact groups have the highest compactness and the most different two first ranked galaxies; and common compact groups show the largest percentage of physically dense groups. Therefore, without a careful selection and identification of the samples, the characteristic features of group properties in a particular photometric band could be overshadowed.

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The COSMOS/UKST Catalog of the Southern Sky

Cited by 62 publications

References 4 publications

Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. V. Final Measurement for Fornax

Proper Motions of Dwarf Spheroidal Galaxies fromHubble Space TelescopeImaging. V. Final Measurement for Fornax

The cluster of galaxies Abell 970

On the properties of compact groups identified in different photometric bands

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