An Optical Study of a Sample of Spiral Galaxies

Cabrera-Lavers, A.; Garzón, F.

doi:10.1086/381924

Cited by 14 publications

(12 citation statements)

References 59 publications

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“…While listed in the RC3 as a non-barred galaxy, it is classified as showing a bar in the PGC (Paturel 1989). Chapelon et al (1999) and Cabrera-Lavers & Garzón (2004) show in their photometric analyses that this galaxy has a central isophotal twist that they interprete as a bar with a diameter of ≈38 . Analysing photometric observations, Coccato et al (2004) do not confirm the presence of a bar, but find a strong velocity gradient along the minor axis of the galaxy in their long-slit data.…”

Section: The Galaxies Studiedmentioning

confidence: 97%

Kinematic modelling of disk galaxies

Józsa¹

2007

A&A

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This is the second of a series of papers in which the kinematics of disk galaxies is studied by analysing spectroscopic data. Making use of the methods presented in Paper I, this work focuses on the large-scale distribution of disk and Dark Matter halo material by analysing the structure of warped galaxies. H i observations of three disk galaxies showing regular large-scale ("grand-design") warps are presented and their structure is analysed. The kinematics and geometry of the galaxies are modelled by fitting a tilted-ring model directly to the data cube, thereby avoiding problems due to orbit crowding or beam smearing.The galaxies follow the previously known "rules for the behaviour of warps". Furthermore, at large radii the H i disk settles into a relatively coplanar disk that is inclined with respect to the inner one. With increasing radius, the measured rotation velocity shows a rise. In one of the cases, NGC 5204, the rotation curve shows a jump at the transition radius. While the best fits in the other two cases also suggest that such a jump is present, the change in rotation velocity is compatible with a gradual rise. In two cases, the surface density of the warped H i layer shows a clear drop at the transition radius and decreases only very slowly further out, while this feature is not as clear for UGC 3580. A literature search shows that these properties are shared by a number of other galaxies. In all cases, an additional, slowly rotating gas layer is found to be present. The change in the rotation velocity and the remarkable geometry of the disks together indicate that the radius at which the warp starts marks the transition between two dynamical regimes, an inner one governed by the stellar disk and an outer one determined by the Dark Matter halo.

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Section: The Galaxies Studiedmentioning

confidence: 97%

Kinematic modelling of disk galaxies

Józsa¹

2007

A&A

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“…We have inserted in Fig. 10a the extent of the stellar bar, proposed from photometric measurements by Cabrera-Lavers & Garzon (2004). The bar extends through the entire starburst region, but a kinematic signature is not evident.…”

Section: The Central Region Radial Velocities (R ≤ 4 Kpc)mentioning

confidence: 99%

“…The starburst galaxy NGC 2146 of type Sb II pec (Sandage & Tammann 1987), at a distance of 14.5 Mpc (with 1 ≈ 70 pc), is large and massive and has some outstanding features: a distorted outer shape, although three spiral arms seem to be distinguishable (de Vaucouleurs 1950;Burbidge et al 1959;Benvenuti et al 1975); H i tails, at least at the southern side of an extension up to ∼150 kpc (Caspers & Shane 1986;Taramopoulos et al 2001); a large amount of dust concentrated near the center, with part of it visible as a prominent dust lane and dust "fingers" and polarisation of the visible light (Benvenuti et al 1975;Sandage & Bedke 1994;Draper et al 1995); it has relatively high infrared luminosity L IR = 6 × 10 10 L (Sanders et al 1986); a central condensation, a weak ring, and extended and warped emission of molecular gas (CO) inside which the starburst occurs (Jackson & Ho 1988;Young et al 1988); two H 2 O kilo-masers in the starburst region (Tarchi et al 2002), along with radio supernovae, supernova remnants, and ultra-dense H ii regions (Kronberg & Biermann 1981;Tarchi et al 2000); strong nonthermal continuum radiation produced to a large extent by supernova explosions (Lisenfeld et al 1996); X-ray point sources and diffuse X-ray emission (Armus et al 1995;Della Ceca et al 1999;Inui et al 2005); a cone-like outflow along the minor axis (Armus et al 1995;Greve et al 2000); and maybe a stellar bar (Cabrera-Lavers & Garzon 2004). In short, NGC 2146 is a distorted, dusty, and molecule-rich galaxy with a strong central starburst and a superwind driven out along the minor axis.…”

Section: Introductionmentioning

confidence: 99%

NGC 2146's starburst region and extended structure

Greve¹,

Neininger

Sievers

et al. 2006

A&A

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We present mm-wavelength and optical observations of the starburst region in NGC 2146. This region of ∼4 kpc diameter contains a well-ordered distribution of stars, gas, and dust, and a well-ordered rotation. The possible anomalies found in our observation are a warped CO distribution and an increase in the CO line width at the NW edge of the starburst region. The investigation of a possible encounter or merger origin of the starburst may therefore have to concentrate on the distorted outer structure of the galaxy. There are three large-scale features of ∼20 kpc extent, two of which give the impression of being stellar sub-systems. The third feature is an incomplete and expanding ring of H ii regions and stars, apparently indicating an event that occurred some 300 Myr ago.

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“…The distance to NGC 6217 is listed between ∼19 and 35 Mpc (Tully & Fisher 1977;Hummel 1980;Condon et al 1990;Tutui & Sofue 1997;Pietsch & Arp 2001;Paturel et al 2003). We adopt the same distance to NGC 6217 as F17 of z=0.0045 (20.1 Mpc with an angular scale of 97 pc per arcsecond, see also Cabrera-Lavers & Garzón 2004). It is of morphological type (R'L)SB(rs)b (Sandage & Tammann 1981;de Vaucouleurs et al 1991;Buta et al 2015) i.e.…”

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confidence: 99%

Unveiling the 100 pc scale nuclear radio structure of NGC 6217 with e-MERLIN and the VLA

Williams

McHardy

Baldi

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present high-sensitivity 1.51 GHz e-MERLIN radio images of the nearby galaxy NGC 6217. We resolve the compact radio source at the centre of NGC 6217 for the first time, finding a twin-lobed structure with a total linear size of ∼4 arcsec (∼400 pc). The radio source does not have a compact central core but there is an unresolved hot spot near the outer edge of the southern lobe. Combining our e-MERLIN data with new VLA A-Array data and archival multi-wavelength data, we explore possible scenarios which might explain this complex radio morphology. We conclude that this radio source is most likely powered by a low-luminosity AGN (LLAGN) but with a possible important contribution from nuclear star formation. We also investigate the origin of a putative X-ray jet in NGC 6217, previously suggested in the literature. This 'jet' consists of three X-ray 'knots' in a line, pointed away from the nucleus, with a total size of ∼3 arcmin (∼15 kpc). We find no extended radio emission coincident with the 'jet'. An additional compact radio source, aligned with the knots but without an X-ray counterpart is detected. We detect IR/optical sources falling within the Xray extraction regions of the 'knots', but note that these sources could be chance associations due to high source density around the target field and we estimate the probability of three randomly aligned X-ray sources to be 0.3 per cent in this field.

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An Optical Study of a Sample of Spiral Galaxies

Cited by 14 publications

References 59 publications

Kinematic modelling of disk galaxies

Kinematic modelling of disk galaxies

NGC 2146's starburst region and extended structure

Unveiling the 100 pc scale nuclear radio structure of NGC 6217 with e-MERLIN and the VLA

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