New distances to galaxies in the Centaurus A group

By I. Karachentsev, M. Sharina, A. Dolphin, E. Grebel, D. Geisler, P. Guhathakurta, P. Hodge, V. Karachentseva, A. Sarajedini, Patrick Seitzer. 2002

169 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fbe527a5d033f5e042559d865b0c2cbaee398328

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Citations in the corpus

Planetary Nebulae as Standard Candles. XII. Connecting the Population I and Population II Distance Scales (2002, background): “Only seven PNLF galaxies have TRGB distances: the LMC (Sakai, Zaritsky, & Kennicutt 2000), M31 (Durrell, Harris, & Pritchet 2001), M33 (Kim et al. 2002), NGC 5102 (Karachentsev et al. 2002), NGC 5128 (Harris, Harris, & Poole 1999), NGC 3379 (Sakai et al. 1997), and NGC 3115 (Elson 1997).”
The very local Hubble flow (2002, background): “The bottom one corresponds to the combined LF of 96 galaxies in the LG, M81 group and CenA group.”
The Hubble Flow around the Centaurus A/M83 Galaxy Complex (2006, background): “Karachentsev et al. (2002a, 2002b, 2003) have shown that the M81/NGC 2403, Cen A/M83, and Maffei 1/ IC 342 groups are all ‘‘dumbbell’’ systems like the Local Group (LG).”
The Ultraluminous State (2009, methodology): “…bFigures shown in brackets relate to following references, from which the assumed distance was taken: (i) SRW06, (ii ) Saha et al. (2002), (iii ) Liu & Di Stefano (2008), (iv) Karachentsev et al. (2002).cobserved X-ray luminosity (0.3–10.0 keV) based on the DKBBFTH model (see lat r).”
The Local Group and Other Neighboring Galaxy Groups (2005, methodology): “…on nearby galaxy distances and radial velocities allowed us to determine virial and total masses of four of the nearest complexes: Milky Way+M31 (Karachentsev et al. 2002c), M81+NGC2403 (Karachentsev et al. 2002a), CenA+M83 (Karachentsev et al. 2002b), and IC342+Maffei (Karachentsev et al.…”
Local galaxy flows within 5 Mpc (2002, background): “…group, (4) mean projected linear radius of the group, (5) radial velocity dispersion, (6) absolute B magnitude of the brightest member, (7) integrated luminosity of the group, (8,9) virial and orbital (Karachentsev et al. 2002a) mass estimate normalized to the luminosity unit, (10) crossing time.”
THE ACS NEARBY GALAXY SURVEY TREASURY (2007, methodology): “Galaxies in the M81 group were drawn from Karachentsev et al. (2002a), but do not include the newest candidate members reported in Chiboucas et al. (2008).”
A Catalog of Neighboring Galaxies (2004, background): “33 34 03 Karachentsev et al. 2002b; ph: Jerjen et al. 2000a 13 24 36.0......”
An Hα Imaging Survey of Galaxies in the Local 11 Mpc Volume (2004, unknown): “—(1) Cote et al. 1997: Cen A group; (2) Ferrerese et al. 2000; (3) Ferrerese et al. 2000: N1023 group (N925 ceph); (4) Fingerhut et al. 2007; (5) Freedman et al. 2001; (6) Irwin et al. 2007; (7) Karachentsev et al. 2006; (8) Karachentsev et al. 2007; (9) KKH04: Cen A group; (10) KKH04: Crone et al. ”
Associations of Dwarf Galaxies (2006, background): “It is a factor two more distant than the zero velocity surface separating Local Group infall from cosmic expansion (Karachentsev et al. 2002a) but still within the zero energy surface (Peirani & Pacheco 2005) so conceivably is bound to the Local Group.”
COSMICFLOWS-2: THE DATA (2013, background): “The TRGB is fit at F814W=25.95, giving a distance of 9.84 Mpc. early users of WFPC2 on HST with the specific interest in measuring galaxy distances (Karachentsev et al. 2002a,b,c, 2003a,b,c,d).”