The very local Hubble flow

By I. Karachentsev, M. Sharina, Dmitry I. Makarov, A. Dolphin, E. Grebel, Doug Geisler, P. Guhathakurta, P. Hodge, V. Karachentseva, A. Sarajedini and 1 more. 2002

137 citations recorded by the source corpus.

We present Hubble Space Telescope/WFPC2 images of eighteen galaxies situated in the vicinity of the Local Group (LG) as part of an ongoing snapshot survey of nearby galaxies. Their distances derived from the magnitude of the tip of the red giant branch are $1.92\pm0.10$ Mpc (ESO 294-010), $3.06\pm0.37$ (NGC 404), $3.15\pm0.32$ (UGCA 105), $1.36\pm0.07$ (Sex B), $1.33\pm0.08$ (NGC 3109), $2.64\pm0.21$ (UGC 6817), $2.86\pm0.14$ (KDG 90), $2.27\pm0.19$ (IC 3104), $2.54\pm0.17$ (UGC 7577), $2.56\pm0.15$ (UGC 8508), $3.01\pm0.29$ (UGC 8651), $2.61\pm0.16$ (KKH 86), $2.79\pm0.26$ (UGC 9240), $1.11\pm0.07$ (SagDIG), $0.94\pm0.04$ (DDO 210), $2.07\pm0.18$ (IC 5152), $2.23\pm0.15$ (UGCA 438), and $2.45\pm0.13$ (KKH 98). Based on the velocity-distance data for 36 nearest galaxies around the LG, we find the radius of the zero-velocity surface of the LG to be $R_0 = (0.94\pm0.10)$ Mpc, which yields a total mass $M_{\rm LG} = (1.3\pm0.3)\times 10^{12}~M_{\odot}$. The galaxy distribution around the LG reveals a Local Minivoid which does not contain any galaxy brighter than M V =-11 mag within a volume of ~100 Mpc 3 . The local Hubble flow seems to be very cold, having a one-dimensional mean random motion of ~30 km s -1 . The best-fit value of the local Hubble parameter is $73\pm15$ km s -1 Mpc -1 . The luminosity function for the nearby field galaxies is far less steep than one for members of the nearest groups.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/78a1571e15e1fc0bad5af518e4c8bce8ee5e05f6

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Citations in the corpus

New distances to galaxies in the Centaurus A group (2002, methodology): “6, where the data on M 81/NGC 2403 group are taken from Karachentsev et al. (2002) and the data on the Milky Way/M 31 (the Local Group), are from the book of van den Bergh (2000b).”
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).”
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.…”
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.”
ELVIS: Exploring the Local Volume in Simulations (2013, background): “The velocity field within the Local Volume contains a wealth of information on the assembly history and mass of the Local Group (Kahn & Woltjer 1959; Karachentsev et al. 2002; Karachentsev 2005; Peirani & de Freitas Pacheco 2006; Teyssier et al. 2012; van der Marel et al. 2012).”
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).”
Our Peculiar Motion Away from the Local Void (2007, background): “Then the motion of the Galaxy within the Local Group is V GSRLG = VLG − VGSR = −95x̂+ 87ŷ − 41ẑ (14) or 135 ± 25 km s−1 toward ` = 137 ± 10, b = −18 ± 10 (L = 342, B = −3).”
Distances to nearby galaxies in Sculptor (2003, background): “Together with earlier published TRGB distances to four other galaxies (Karachentsev et al. 2000, 2002) and the distance to NGC 300 from Cepheids (Freedman et al. 1992), this gives us a basis for a more detailed study of the structure of the Sculptor complex.”
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).”
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. ”
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.”