Wheels of Fire. II. Neutral Hydrogen in the Cartwheel Ring Galaxy

Higdon, James L.

doi:10.1086/177599

Cited by 87 publications

(188 citation statements)

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“…t ≥ 20 Myr both galaxies develop stellar and gaseous ring structures which are characteristic for head-on galaxy collisions (see, e.g., the Cartwheel galaxy; Higdon et al 1995Higdon et al , 1996.…”

Section: Cloud Size Parameter and Galaxy Inclinationmentioning

confidence: 99%

A dynamical model for the Taffy galaxies UGC 12914/5

Vollmer¹,

Braine²,

Soida³

2012

A&A

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The spectacular head-on collision of the two gas-rich galaxies of the Taffy system, UGC 12914/15, gives us a unique opportunity to study the consequences of a direct ISM-ISM collision. To interpret existing multi-wavelength observations, we made dynamical simulations of the Taffy system including a sticky particle component. To compare simulation snapshots to Hi and CO observations, we assume that the molecular fraction of the gas depends on the square root of the gas volume density. For the comparison of our simulations with observations of polarized radio continuum emission, we calculated the evolution of the 3D large-scale magnetic field for our simulations. The induction equations including the time-dependent gas-velocity fields from the dynamical model were solved for this purpose. Our simulations reproduce the stellar distribution of the primary galaxy, UGC 12914, the prominent Hi and CO gas bridge, the offset between the CO and Hi emission in the bridge, the bridge isovelocity vectors parallel to the bridge, the Hi double-line profiles in the bridge region, the large line-widths (∼200 km s −1 ) in the bridge region, the high field strength of the bridge large-scale regular magnetic field, the projected magnetic field vectors parallel to the bridge and the strong total power radio continuum emission from the bridge. The stellar distribution of the secondary model galaxy is more perturbed than observed. The observed distortion of the Hi envelope of the Taffy system is not reproduced by our simulations which use initially symmetric gas disks. The model allows us to define the bridge region in three dimensions. We estimate the total bridge gas mass (Hi, warm and cold H 2 ) to be 5 to 6× 10 9 M , with a molecular fraction M H 2 /M HI of about unity. Despite the enormous mass of molecular gas in the bridge, very little star formation is present, similar to other systems with extraplanar gas and broad CO lines. The structure of the model gas bridge is bimodal: on kpc-scales there is a dense ( 0.01 M pc −3 ) component with a high velocity dispersion >100 km s −1 and a less dense (∼10 −3 M pc −3 ) component with a smaller, but still high, velocity dispersion ∼50 km s −1 . The synchrotron lifetime of relativistic electrons is only long enough to be consistent with the existence of the radio continuum bridge for the less dense component. On the other hand, only the high-density gas undergoes a high enough mechanical energy input to produce the observed strong emission of warm H 2 . We propose that, despite the high local gas densities, this high input of mechanical energy drives strong turbulence and quenches star formation in the bridge gas except for the giant Hii region near UGC 12915. Our model suggests that we observe this galaxy head-on collision near the time of maximum CO and H 2 emission.

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Section: Cloud Size Parameter and Galaxy Inclinationmentioning

confidence: 99%

A dynamical model for the Taffy galaxies UGC 12914/5

Vollmer¹,

Braine²,

Soida³

2012

A&A

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“…The stripped gas may be found as tidal tails, filaments, and plumes near the interacting galaxies, e.g. in the Abell 1367 cluster (Scott et al 2010) and nearby groups (e.g., Higdon 1996;Koribalski et al 2003;Koribalski & Dickey 2004;English et al 2010). These extended H i structures can be difficult to detect, requiring high sensitivity single-dish observations to measure the low-surface brightness emission and long interferometric observations with emphasis on short baselines such as not to resolve out the diffuse H i emission.…”

Section: Introductionmentioning

confidence: 99%

H i debris in the IC 1459 galaxy group

Saponara

Koribalski

Benaglia

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present H i synthesis imaging of the giant elliptical galaxy IC 1459 and its surroundings with the Australia Telescope Compact Array (ATCA). Our search for extended H i emission revealed a large complex of H i clouds near IC 1459, likely the debris from tidal interactions with neighbouring galaxies. The total H i mass (∼ 10 9 M ) in the detected clouds spans 250 kpc from the north-east of the gas-rich spiral NGC 7418A to the south-east of IC 1459. The extent and mass of the H i debris, which shows rather irregular morphology and kinematics, are similar to those in other nearby groups. Together with H i clouds recently detected near two other IC 1459 group members, namely IC 5270 and NGC 7418, using Phased-Array Feeds (PAFs) on the Australian Square Kilometer Array Pathfinder (ASKAP), the detected debris make up a significant fraction of the group's intergalactic medium.

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“…It is located in a tight, compact group (SCG 0035-3357;Iovino et al 2003) of 4 members, very close in space (∼0.3 Mpc 1 and velocity ∼400 km s −1 from one another, see Taylor & Atherton 1984). Whether the impact was due to G3 (at ∼1 NE, Higdon 1996) or G2 (at ∼3 to the North; Athanassoula et al 1997), two rings are now visible as a result: the outer one has the largest linear diameter measured in ring galaxies: 80 (∼100 kpc) along the major axis; the inner one, close to the core, is elliptical in shape with obvious dust lanes crossing it (Struck et al 1996).…”

Section: Introductionmentioning

confidence: 99%

“…Many detailed observations of the Cartwheel are available, ranging from radio line (Higdon 1996) and continuum (Higdon 1996), to near- (Marcum et al 1992) and far-infrared (Appleton & Struck-Marcell 1987), optical (Theys & Spiegel 1976;Fosbury & Hawarden 1977) and Hα images (Higdon 1995) and line spectroscopy (Fosbury & Hawarden 1977). All have confirmed the presence of a recent starburst in the outer Appendix is only available in electronic form at http://www.edpsciences.org 1 We use H 0 = 75 km s −1 Mpc −1 , which implies a scale of 1.252 kpc/arcsec at the distance of the group, D L = 122 Mpc, throughout the paper.…”

Section: Introductionmentioning

confidence: 99%

A thorough study of the intriguing X-ray emission from the Cartwheel ring

Wolter

Trinchieri

2004

A&A

105

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Abstract. We present the results from the high resolution Chandra observation of the Cartwheel galaxy. Many individual sources are resolved in the image, mostly associated with the outer ring. All detected sources have a very high X-ray luminosity (≥10 39 erg s −1 ) that classifies them as Ultra Luminous X-ray sources (ULX). The brightest of them is possibly the most luminous individual non-nuclear source observed so far, with L X ∼ 10 41 erg s −1 (at D = 122 Mpc). The spatial extent of this source is consistent with a point source at the Chandra resolution. The luminosity function of individual X-ray sources extends about an order of magnitude higher than previously reported in other galaxies. We discuss this in the context of the "universal" luminosity function for High Mass X-ray Binaries and we derive a Star Formation Rate higher than in other starburst galaxies studied so far. A diffuse component, associated with hot gas, is present. However, deeper observations that we will obtain with XMM-Newton are needed to constrain its properties.

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Wheels of Fire. II. Neutral Hydrogen in the Cartwheel Ring Galaxy

Cited by 87 publications

References 0 publications

A dynamical model for the Taffy galaxies UGC 12914/5

A dynamical model for the Taffy galaxies UGC 12914/5

H i debris in the IC 1459 galaxy group

A thorough study of the intriguing X-ray emission from the Cartwheel ring

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