NOAO Fundamental Plane Survey. I. Survey Design, Redshifts, and Velocity Dispersion Data

Smith, Russell J.; Hudson, Michael J.; Nelan, Jenica E.; Moore, S. A. W.; Quinney, S. J.; Wegner, Gary A.; Lucey, J. R.; Davies, Roger L.; Malecki, Justin; Schade, David; Suntzeff, Nicholas B.

doi:10.1086/423915

Cited by 143 publications

(161 citation statements)

References 38 publications

(41 reference statements)

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“…This galaxy is listed as a member galaxy of Z8338 (Smith et al 2004; and a spectroscopic redshift of 0.0511 in Cava et al 2009, in agreement with the cluster redshift in P11). According to F11, this is the galaxy with the highest mass, by far the highest star formation (SF) rate in the past (5.5 M /yr, while no SF is detected in current age), and the highest age within Z8338.…”

Section: Counterparts In Other Wavelengthssupporting

confidence: 78%

The long X-ray tail in Zwicky 8338

Schellenberger

Reiprich

2015

A&A

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The interaction processes in galaxy clusters between the hot ionized gas (ICM) and the member galaxies are of crucial importance to understand the dynamics in galaxy clusters, the chemical enrichment processes, and the validity of their hydrostatic mass estimates. Recently, several X-ray tails associated with gas that was partly stripped of galaxies have been discovered. We report on the X-ray tail in the 3 keV galaxy cluster Zwicky 8338, which might be the longest galaxy-scale stripping process ever observed. We derive the properties of the galaxy cluster environment and give hints on the substructure present in this X-ray tail, which is very likely associated with the galaxy CGCG254-021. The X-ray tail is extraordinarily luminous (2 × 10 42 erg s −1 ), the thermal emission has a temperature of 0.8 keV, and the X-ray luminous gas might be stripped off completely from the galaxy. From assumptions about the 3D geometry, we estimate the gas mass fraction (<0.1%) and conclude that the gas has been compressed and/or heated.

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Section: Counterparts In Other Wavelengthssupporting

confidence: 78%

The long X-ray tail in Zwicky 8338

Schellenberger

Reiprich

2015

A&A

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“…Optical information on A576 can be found in the catalogue of Hudson et al (2001). After the publication of Paper I, the NOAO Fundamental Plane Survey appeared (Smith et al 2004). It includes redshift information on the UGC 3957 galaxy group.…”

Section: Discussionmentioning

confidence: 99%

Giant radio galaxy DA 240 group: content and environment

Chen

Peng

Strom

et al. 2011

A&A

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Context. There is a group of about twenty galaxies around the giant radio galaxy (GRG) DA 240 which we are studying to investigate the environment of the radio source. We have noted that 11 members are aligned with the radio emission (Peng et al. 2004, A&A, 415, 487). The alignment occurs within a small angle similar to the width of the GRG radio lobes, and there may be some physical causal relationship. After finishing observations of the four candidates not included in Paper I, we have completed our study of the brighter members of the sample of galaxies around DA 240. Aims. We aim to see if more galaxies have similar redshifts to the host galaxy of DA 240, to confirm the galaxy grouping and further study their distribution. Methods. Spectra of the four candidate galaxies were obtained with the 2.16 m spectroscopic telescope at XingLong observing station of the NAOC, and the galaxies' positions were established with respect to the radio emission. We have discovered two more members associated with the group of galaxies around DA 240. In addition, the work of other researchers provides one other new member.Results. The number of confirmed galaxies associated with the DA 240 group has increased by almost a quarter to 20. There are now 14 galaxies (including the host) lying along the major axis of the radio source. We further consider the relationship of the group to adjacent galaxy associations, noting that it may form a binary pair with the slightly closer UGC 3957 group. They both lie on the periphery of the much more substantial cluster, Abell 576.

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“…Measurements along the slit are divided in two panels, with left panels referring to the part of the slit close to NGC 4889 and right panels referring to the part of the slit close to NGC 4874. Crosses: data from Mehlert et al (2000) shifted to the systemic velocities, 6495 km s −1 for NGC 4889 (Moore et al 2002) and 7205 km s −1 for NGC 4874 (Smith et al 2004). Filled circles: measurements from this paper for run 1. and the creation of one optimal template for each radial bin minimized errors in the kinematics due to template mismatch.…”

Section: Stellar Kinematicsmentioning

confidence: 96%

Kinematics and line strength indices in the halos of the Coma brightest cluster galaxies NGC 4874 and NGC 4889

Coccato

Arnaboldi

Gerhard

et al. 2010

A&A

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Aims. We investigate the stellar kinematics and line strength indices in the outer halos of brightest cluster galaxies (BCGs) in the Coma cluster to obtain the outer halo V rot and σ profiles and to derive constraints on the formation history of these objects. Methods. We analyzed absorption lines in deep, medium-resolution, long-slit spectra in the wavelength range ∼4500-5900 Å, out to ∼50 kpc for NGC 4874 and ∼65 kpc for NGC 4889, probing regions with a surface brightness down to μ R ∼ 24 mag arcsec −2 . Results. These data provide stellar velocity and velocity dispersion profiles along the major axes of both BCGs, and also along the minor axis of NGC 4889. The kinematic properties of NGC 4874 and NGC 4889 halos extend the previous relations of early-type galaxy halos to bright luminosities and indicate that the stars in the outer regions are still bound to these galaxies. For NGC 4889 we also determine Hβ Mg and Fe line strength indices, finding strong radial gradients for Mg and Fe. The current dataset for NGC 4889 is one of the most extended in radius, including both stellar kinematics and line strength index measurements.

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NOAO Fundamental Plane Survey. I. Survey Design, Redshifts, and Velocity Dispersion Data

Cited by 143 publications

References 38 publications

The long X-ray tail in Zwicky 8338

The long X-ray tail in Zwicky 8338

Giant radio galaxy DA 240 group: content and environment

Kinematics and line strength indices in the halos of the Coma brightest cluster galaxies NGC 4874 and NGC 4889

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