Streaming motions of galaxy clusters within 12 000 km s-1 -- I. New spectroscopic data

Smith, Russell J.; Lucey, J. R.; Hudson, Michael J.; Schlegel, David J.; Davies, Roger L.

doi:10.1046/j.1365-8711.2000.03251.x

Cited by 165 publications

(50 citation statements)

References 47 publications

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“…be υ p = −234±41 km s −1 , which is consistent with the previous measurement υ p = −244 ± 5 km s −1 (Smith et al 2000). We also measured the radial velocities for two faint galaxies: υ p = 777 ± 38 km s −1 for VCC 0833 and υ p = 949 ± 23 km s −1 for NGC 4406B.…”

Section: Velocity Measurementsupporting

confidence: 91%

Subaru Spectroscopy of the Globular Clusters in the Virgo Giant Elliptical Galaxy M86

Park¹,

Lee²,

Hwang³

2012

ApJ

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We present the first spectroscopic study of the globular clusters (GCs) in the giant elliptical galaxy (gE) M86 in the Virgo Cluster. Using spectra obtained in the Multi-Object Spectroscopy mode of the Faint Object Camera and Spectrograph on the Subaru telescope, we measure the radial velocities for 25 GCs in M86. The mean velocity of the GCs is derived to be v p = −354 +81 −79 km s −1 , which is different from the velocity of the M86 nucleus (v gal = −234 ± 41 km s −1 ). We estimate the velocity dispersion of the GCs, σ p = 292 +32 −32 km s −1 , and find a hint of rotation in the M86 GC system. A comparison of the observed velocity dispersion profiles of the GCs and stars with a prediction based on the stellar mass profile strongly suggests the existence of an extended dark matter halo in M86. We also estimate the metallicities and ages for 16 and 8 GCs, respectively. The metallicities of M86 GCs are in the range of −2.0 < [Fe/H] < −0.2 with a mean value of −1.13 ± 0.47. These GCs show a wide age distribution from 4 to 15 Gyr.

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Section: Velocity Measurementsupporting

confidence: 91%

Subaru Spectroscopy of the Globular Clusters in the Virgo Giant Elliptical Galaxy M86

Park¹,

Lee²,

Hwang³

2012

ApJ

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“…The values obtained by the code for the radial velocity and velocity dispersion of the stellar component of the galaxy were Vr = 1726 ± 3 km s −1 and σ = 255 ± 4 km s −1 , respectively, which are in agreement with those obtained by Smith et al (2000). In addition, the calculated values of age and metallicity for NGC 1395 are 12.1 ± 0.2 Gyr and [Z/H]=0.34 ± 0.01 dex, respectively.…”

Section: Stellar Population Analysissupporting

confidence: 88%

Tracing the assembly history of NGC 1395 through its Globular Cluster System

Escudero

Faifer

Castelli

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We used deep Gemini-South/GMOS g ′ r ′ i ′ z ′ images to study the globular cluster (GC) system of the massive elliptical galaxy NGC 1395, located in the Eridanus supergroup. The photometric analysis of the GC candidates reveals a clear colour bimodality distribution, indicating the presence of "blue" and "red" GC subpopulations. While a negative radial colour gradient is detected in the projected spatial distribution of the red GCs, the blue GCs display a shallow colour gradient. The blue GCs also display a remarkable shallow and extended surface density profile, suggesting a significant accretion of low-mass satellites in the outer halo of the galaxy. In addition, the slope of the projected spatial distribution of the blue GCs in the outer regions of the galaxy, is similar to that of the X-ray halo emission. Integrating up to 165 kpc the profile of the projected spatial distribution of the GCs, we estimated a total GC population and specific frequency of 6000±1100 and S N =7.4±1.4, respectively. Regarding NGC 1395 itself, the analysis of the deep Gemini/GMOS images shows a low surface brightness umbrella-like structure indicating, at least, one recent merger event. Through relations recently published in the literature, we obtained global parameters, such as M stellar = 9.32 × 10 11 M⊙ and M h = 6.46 × 10 13 M⊙. Using public spectroscopic data, we derive stellar population parameters of the central region of the galaxy by the full spectral fitting technique. We have found that, this region, seems to be dominated for an old stellar population, in contrast to findings of young stellar populations from the literature.

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“…Throughout this paper, we adopt a Hubble constant H 0 = 70 km s −1 Mpc −1 . We take the redshift of NGC 383 (the parent galaxy of 3C 31) to be 0.0169; this is the mean of values from Smith et al (2000), Huchra, Vogeley & Geller (1999) and De Vaucouleurs et al (1991). The resulting conversion factor between angular and linear size is 0.34 kpc arcsec −1 .…”

Section: Introductionmentioning

confidence: 99%

Dynamical models for jet deceleration in the radio galaxy 3C 31

Laing

Bridle

2002

Monthly Notices of the Royal Astronomical Society

196

212

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We present a dynamical analysis of the flow in the jets of the low-luminosity radio galaxy 3C 31 based on our earlier geometrical and kinematic model and on estimates of the external pressure and density distributions from Chandra observations. We apply conservation of particles, energy and momentum to derive the variations of pressure and density along the jets and show that there are self-consistent solutions for deceleration by injection of thermal matter. We initially take the jets to be in pressure equilibrium with the external medium at large distances from the nucleus and the momentum flux to be energy flux/c; we then progressively relax these constraints. We infer that the jets are over-pressured compared with the external medium where they start to expand rapidly. Local minima in the density and pressure and maxima in the mass injection rate and Mach number occur at approximately 3 kpc. Further out, the jets decelerate smoothly with a Mach number close to 1. The mass injection rate we infer is comparable with that expected from stellar mass loss at 1 - 2 kpc, but significantly exceeds it at large distances. We conclude that entrainment from the galactic atmosphere is the dominant mass input process far from the nucleus, but that stellar mass loss may also contribute closer in. The occurrence of a significant over-pressure where expansion begins leads us to suggest that there is a stationary shock system, perhaps caused by reconfinement of an initially free jet. Our results are compatible with a jet consisting of electron-positron plasma on parsec scales which picks up thermal matter from stellar mass loss to reach the inferred density and mass flux at 1 kpc, but we cannot rule out an electron-proton composition with a low-energy cut-off. [Abridged]Comment: 23 pages, 22 figures, accepted for publication in MNRA

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Streaming motions of galaxy clusters within 12 000 km s-1 -- I. New spectroscopic data

Cited by 165 publications

References 47 publications

Subaru Spectroscopy of the Globular Clusters in the Virgo Giant Elliptical Galaxy M86

Subaru Spectroscopy of the Globular Clusters in the Virgo Giant Elliptical Galaxy M86

Tracing the assembly history of NGC 1395 through its Globular Cluster System

Dynamical models for jet deceleration in the radio galaxy 3C 31

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