Deep H I Survey of the Spiral Galaxy NGC 2403

By Filippo Fraternali, G. van Moorsel, R. Sancisi, T. Oosterloo. 2002

179 citations recorded by the source corpus.

High-sensitivity H I observations of the nearby spiral galaxy NGC 2403 obtained with the VLA are presented and discussed. The properties of the extended, differentially rotating H I layer with its H I holes, spiral structure, and outer warp are described. In addition, these new data reveal the presence of a faint, extended, and kinematically anomalous component. This shows up in the H I line profiles as extended wings of emission toward the systemic velocity. In the central regions these wings are very broad (up to 150 km s-1) and indicate large deviations from circular motion. We have separated the anomalous gas component from the cold disk and have obtained for it a separate velocity field and a separate rotation curve. The mass of the anomalous component is 1/10 of the total H I mass. The rotation velocity of the anomalous gas is 25–50 km s-1 lower than that of the disk. Its velocity field has nonorthogonal major and minor axes that we interpret as due to an overall inflow motion of 10–20 km s-1 toward the center of the galaxy. The picture emerging from these observations is that of a cold H I disk surrounded by a thick and clumpy H I layer characterized by slower rotation and inflow motion toward the center. The origin of this anomalous gas layer is unclear. It is likely, however, that it is related to the high rate of star formation in the disk of NGC 2403 and that its kinematics is the result of a galactic fountain–type of mechanism. We suggest that these anomalous H I complexes may be analogous to a part of the high-velocity clouds of our Galaxy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/823d768f1a74b21d1f7c74a05c4ca956ca5a8f98

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Citations in the corpus

3D BAROLO: a new 3D algorithm to derive rotation curves of galaxies (2015, methodology): “We selected 4 galaxies (NGC 2403, NGC 2903, NGC 3198 and NGC 5055) for which we have both very high resolution Hi data (Fraternali et al. 2002, and THINGS) and single-dish observations.”
Analysis of rotation curves in the framework of Rn gravity (2007, unknown): “…UGC 8017, UGC 10981, UGC 11455 (Vogt et al. 2004); M31, M33 (Corbelli & Salucci 2007); IC 2574 (Martimbeau, Carignan & Roy 1994), NGC 5585 (Côté, Carignan & Sancisi 1991), NGC 6503 (Wevers, van der Kruit & Allen 1986), NGC 2403 (Fraternali et al. 2002), NGC 55 (Puche, Carignan & Wainscoat 1991).”
HIGH-RESOLUTION ROTATION CURVES AND GALAXY MASS MODELS FROM THINGS (2008, background): “◦9, whereas Fraternali et al. (2002) derived 62.”
On the Continuing Formation of the Andromeda Galaxy: Detection of H I Clouds in the M31 Halo (2003, background): “NGC 628, Kamphuis & Briggs (1992)), but only recently have instruments had sufficient sensitivity to begin revealing complete systems of peculiar velocity H I (eg. the slowly rotating “halo” component of NGC 2403, Fraternali et al. (2002)).”
A Search for Extended Ultraviolet Disk (XUV-Disk) Galaxies in the Local Universe (2007, background): “The outermost XUV disk complexes lie near local maxima within the HI filament which begins near the NW end of the major axis and wraps counterclockwise around the N side of the galaxy (Fraternali et al. 2002).”
Gaseous Galaxy Halos (2012, background): “…the spiral galaxies observed to deep enough levels show a disk-halo component that lags the rotation of the disk (often referred to as an ‘HI beard’; Sancisi et al., 2001) with a typical gradient of magnitude 15-30 km s−1 kpc−1 (Fraternali et al., 2002; Oosterloo et al., 2007; Heald et al., 2011).”
A dynamical model for the extraplanar gas in spiral galaxies (2005, methodology): “For NGC 2403, we have considered only atomic gas, being the dominant component, and used the exponential fit to the H I surface density given in Fraternali et al. (2002).”
The Cold Gaseous Halo of NGC 891 (2007, background): “These complexes would be similar to those observed in non-edge-on galaxies like NGC 2403 and NGC 6946, where projection effects are less important (Fraternali et al. 2002; Boomsma et al. 2005a; Boomsma 2007).”
Outer structure of the Galactic warp and flare: explaining the Canis Major over-density (2006, background): “An interesting specific study, which reminds us that the dynamics of outer galaxies may not always require current active mergers, is that by Fraternali et al. (2002) of NGC2403.”
Accretion of gas on to nearby spiral galaxies (2008, methodology): “Interestingly, both NGC891 and NGC2403 do show warping of the outer discs (Garćıa-Ruiz, Sancisi & Kuijken 2002; Fraternali et al. 2002).”