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

By Russell J. Smith, J. Lucey, M. Hudson, David Schlegel, Roger Davies. 2000

144 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f67666dff316fe36db7ae19aee7dbc2a9d5e39c0

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In Astronomy and Astrophysics

1. A. Romanowsky
2. J. Strader
3. J. Brodie
4. M. Hudson
5. D. Merritt
6. A. Bridle
7. M. Colless
8. Lee R. Spitler

In Instrumentation

1. J. Strader
2. J. Brodie
3. D. Merritt
4. A. Bridle
5. A. Romanowsky
6. M. Beasley
7. N. Caldwell
8. J. Rose

Citations in the corpus

• Mass Deficits, Stalling Radii, and the Merger Histories of Elliptical Galaxies (2006, methodology): “In the case of NGC 5903, for which M was computed from the M.- relation, we note that published velocity dispersions for this galaxy range from 192 (Smith et al. 2000) to 245 km s 1 (Davies et al. 1987); the corresponding range in the inferred black hole mass is 1:36 ; 108 PM /M P 4:45 ; 108, and…”
• An expanded Mbh–σ diagram, and a new calibration of active galactic nuclei masses (2010, unknown): “…2 = Rekola et al. (2005); 3 = Madore et al. (1999); 4 = Gillessen et al. (2009); 5 = Karachentsev et al. (2007); 6 = Dalla Bontà et al. (2009); 7 = Smith et al. (2000); 8 = Oliva et al. (1995); 9 = Nelson & Whittle (1995); 10 = Merritt & Ferrarese (2001); 11 = Rodrı́guez-Rico et al. (2006), a…”
• VLA IMAGING OF VIRGO SPIRALS IN ATOMIC GAS (VIVA). I. THE ATLAS AND THE H i PROPERTIES (2009, background): “The velocities and the surface brightness fluctuation (SBF) distances of M87, M86, and M49, which are noted in black in Figure 1, are 1307, −244, and 997 km s−1 (Smith et al. 2000), and 16.1, 18.4 (West & Blakeslee 2000), and 16.3 Mpc (Ferrarese et al. 2003), respectively.”
• Relativistic models and the jet velocity field in the radio galaxy 3C 31 (2002, methodology): “We adopt a redshift of 0.0169 for the galaxy (the mean of values from Smith et al. 2000, Huchra, Vogeley & Geller 1999 and De Vaucouleurs et al. 1991), so the projected linear scale of the images is 0.34 kpc/arcsec.”
• WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, methodology): “We adopt vsys = 1307 km s −1 as the systemic velocity (Smith et al. 2000).”
• The 6dF Galaxy Survey: final redshift release (DR3) and southern large-scale structures (2009, background): “The redshift offsets were found to be consistent between a 2004 comparison of 16 127 6dFGS and ZCAT redshifts, and a 2007 comparison of 443 redshifts from various peculiar velocity surveys (Bernardi et al. 2003; Smith et al. 2000, 2004; Wegner et al. 2003).”
• Dynamical models for jet deceleration in the radio galaxy 3C 31 (2002, methodology): “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 2MASS REDSHIFT SURVEY—DESCRIPTION AND DATA RELEASE (2011, unknown): “…et al. (2000) 2000ApJS..126..209R Romer et al. (2000) 2000ApJS..129..547B Bauer et al. (2000) 2000MNRAS.312..540B Bardelli et al. (2000) 2000MNRAS.313..469S Smith et al. (2000) 2000MNRAS.313..515I Iwasawa et al. (2000) 2000MNRAS.316..326H Hasegawa et al. (2000) 2000MNRAS.317...55S Saunders…”
• The 400 Square Degree ROSAT PSPC Galaxy Cluster Survey: Catalog and Statistical Calibration (2006, unknown): “D, 64, 123527 Jones, C. & Forman, W. 1999, ApJ, 511, 65 Jones, L. R., Ponman, T. J., Horton, A., Babul, A., Ebeling, H., & Burke, D. J. 2003, MNRAS, 343, 627 Jones, L. R., Scharf, C., Ebeling, H., Perlman, E., Wegner, G., Malkan, M., & Horner, D. 1998, ApJ, 495, 100 Katgert, P., Mazure, A., den Hart”
• On the dependence of spectroscopic indices of early-type galaxies on age, metallicity and velocity dispersion (2000, methodology): “The data reported here is from the SMAC I97MA spectroscopic run (see Smith et al. 2000 for further details).”
• Streaming motions of galaxy clusters within 12 000 km s−1– V. The peculiar velocity field (2004, background): “Searches in the ZOA have revealed the presence of massive clusters such as A3627 (Kraan-Korteweg et al. 1996) but the integrated overdensity within c© 0000 RAS the ZOA appears still insufficient to generate substantial infall at the LG (Staveley-Smith et al. 2000).”
• Star Formation Histories of Early-Type Galaxies. I. Higher Order Balmer Lines as Age Indicators (2003, result): “A comparison with the literature values of Smith et al. (2000) for 25 galaxies in common gives a mean difference of 13 km s 1 and rms of 58 km s 1.”