Distances to nearby galaxies in Sculptor

By I. Karachentsev, E. Grebel, M. Sharina, A. Dolphin, D. Geisler, P. Guhathakurta, P. Hodge, V. Karachentseva, A. Sarajedini, Patrick Seitzer. 2003

198 citations recorded by the source corpus.

We present an analysis of Hubble Space Telescope/WFPC2 images of nine nearby galaxies in Sculptor. We derive their distances from the luminosity of the tip of the red giant branch stars with a typical accuracy of ∼12%. Their distances are 4.21 Mpc (Sc 22), 4.92 Mpc (DDO 226), 3.94 Mpc (NGC 253), 3.40 Mpc (KDG 2), 3.34 Mpc (DDO 6), 3.42 Mpc (ESO 540-030), 4.43 Mpc (ESO 245-05), 4.27 Mpc (UGCA 442), and 3.91 Mpc (NGC 7793). The galaxies are concentrated in several spatially separated loose groups around NGC 300, NGC 253, and NGC 7793. The Sculptor galaxy complex together with the CVn I cloud and the Local Group form a 10 Mpc filament, apparently driven by the free Hubble flow.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/be7c7512b5607f8bbdd861a8d0fbece4b321fe7f

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Citations in the corpus

A Catalog of Neighboring Galaxies (2004, background): “+67 54 49 Karachentsev et al. 2003b; ph: Bremnes et al. 1998 09 50 10.0...........”
THE GHOSTS SURVEY. I. HUBBLE SPACE TELESCOPE ADVANCED CAMERA FOR SURVEYS DATA (2011, methodology): “As the likelihood of observing disk galaxies at such high inclinations is low, they are typically observed at distances greater than the limits of the Karachentsev et al. (2003c) catalog and so require longer exposures.”
THE ACS NEARBY GALAXY SURVEY TREASURY (2007, methodology): “We also in- cluded a second high-density environment centered on the NGC 253 clump (D ≈ 3.9 Mpc) in the Sculptor filament (Karachentsev et al. 2003), further increasing the range of environments probed.”
A Search for Extended Ultraviolet Disk (XUV-Disk) Galaxies in the Local Universe (2007, background): “It dominates a “loose quartet” (Karachentsev et al. 2003) of Sculptor galaxies including NGC 55, ESO 410-05 and ESO 294-10 (later two are not listed in the NOG catalog, Giuricin et al. 2000).”
The Carnegie-Chicago Hubble Program. VIII. An Independent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch (2019, methodology): “A number of refinements to the basic technique have continued to be explored and applied over the past few decades (e.g., Madore & Freedman 1995; Sakai et al. 1996; Cioni et al. 2000; Méndez et al. 2002; Karachentsev et al. 2003, 2018; Mager et al. 2008).”
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. ”
XMM–Newton observations of the brightest ultraluminous X-ray sources (2006, unknown): “…Markert & Rallis (1983),3 Colbert et al. (1995), 4 Roberts & Warwick (2000),5 Dewangan et al. (2004),6 Fabbiano (1988),a Stobbart et al. (2004),b Karachentsev et al. (2003),c Read, Ponman & Strickland (1997),d Schlegel, Barrett & Singh (1997),e Foschini et al. (2004),f Ho, Filippenko, & Sargent…”
DETECTION OF GAMMA-RAY EMISSION FROM THE STARBURST GALAXIES M82 AND NGC 253 WITH THE LARGE AREA TELESCOPE ON FERMI (2009, background): “The distance to M82 is 3.63 ± 0.34 Mpc (Freedman et al. 1994), and distance estimates to NGC 253 range from 2.5 Mpc (Turner & Ho 1985, Mauersberger et al. 1996) to 3.9 ± 0.37 Mpc (Karachentsev et al. 2003).”
THE ACS NEARBY GALAXY SURVEY TREASURY. VIII. THE GLOBAL STAR FORMATION HISTORIES OF 60 DWARF GALAXIES IN THE LOCAL VOLUME (2011, methodology): “Similarly, we also included galaxies in the direction of the NGC 253 clump (DN253 ∼ 3.9 Mpc) in the Sculptor Filament (Karachentsev et al. 2003), further extending the range of environments probed by the sample, while maintaining strict volume limits for galaxy selection.”
The Local Group and Other Neighboring Galaxy Groups (2005, methodology): “For the sample of 34 members of the cloud, Karachentsev et al. (2003a) derived the radial velocity dispersion 50 km s −1 , the mean linear projected radius 760 kpc, and the mass estimates: 360 × 10 10 M ⊙ (vir) and 190 × 10 10 M ⊙ (orb).”