NGC 922 - a new drop-through ring galaxy★

Wong, O. I.; Meurer, G. R.; Bekki, Kenji; Hanish, D. J.; Kennicutt, Robert C.; Bland-Hawthorn, Joss; Ryan-Weber, E. V.; Koribalski, B. S.; Kilborn, V. A.; Putman, Mary E.; Heiner, J. S.; Webster, R. L.; Allen, R. J.; Dopita, Michael A.; Doyle, M. T.; Drinkwater, Michael J.; Ferguson, Harry; Freeman, K. C.; Heckman, Timothy M.; Hoopes, Charles G.; Knezek, Patricia; Meyer, M.; Oey, M. S.; Seibert, Mark; Smith, R. C.; Staveley‐Smith, L.; Thilker, David A.; Werk, Jessica K.; Zwaan, M. A.

doi:10.1111/j.1365-2966.2006.10589.x

Cited by 25 publications

(48 citation statements)

References 30 publications

(49 reference statements)

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“…We note however that the ring galaxy NGC 922 shows a stronger star formation activity on the side of the nucleus than on the opposite one (e.g. Wong & et al 2006;Meurer & et al 2006), contrarily to our simulations of the Cartwheel. However, the strong asymmetry observed in the distribution of gas and old stars clusters (Pellerin et al 2010;Prestwich et al 2012) indicates that the "ring" structure itself is asymmetric (which thus biases the distribution of star form- ing regions).…”

Section: Star Formation As Function Of Locationsupporting

confidence: 54%

Morphology and enhanced star formation in a Cartwheel-like ring galaxy

Renaud

Athanassoula

Amram

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use hydrodynamical simulations of a Cartwheel-like ring galaxy, modelled as a nearly head-on collision of a small companion with a larger disc galaxy, to probe the evolution of the gaseous structures and flows, and to explore the physical conditions setting the star formation activity. Star formation is first quenched by tides as the companion approaches, before being enhanced shortly after the collision. The ring ploughs the disc material as it radially extends, and almost simultaneously depletes its stellar and gaseous reservoir into the central region, through the spokes, and finally dissolve 200 Myr after the collision. Most of star formation first occurs in the ring before this activity is transferred to the spokes and then the nucleus. We thus propose that the location of star formation traces the dynamical stage of ring galaxies, and could help constrain their star formation histories. The ring hosts tidal compression associated with strong turbulence. This compression yields an azimuthal asymmetry, with maxima reached in the side furthest away from the nucleus, which matches the star formation activity distribution in our models and in observed ring systems. The interaction triggers the formation of star clusters significantly more massive than before the collision, but less numerous than in more classical galaxy interactions. The peculiar geometry of Cartwheel-like objects thus yields a star (cluster) formation activity comparable to other interacting objects, but with notable second order differences in the nature of turbulence, the enhancement of the star formation rate, and the number of massive clusters formed.

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Section: Star Formation As Function Of Locationsupporting

confidence: 54%

Morphology and enhanced star formation in a Cartwheel-like ring galaxy

Renaud

Athanassoula

Amram

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…In this paper we use the results of the X-ray analysis as presented in Wolter & Trinchieri (2004 NGC 922 has been described as a RiG only recently (Wong et al 2006). It contains 7 ULXs and has a SFR = 8 M yr −1 (Prestwich et al 2012;Wong et al 2006) derived from H α measures, which we use hereafter.…”

Section: Cartwheel Galaxy (Am 0035−335)mentioning

confidence: 99%

“…Assuming Z = 0.02, 12+log(O/H) = 8.92 Reference list: 1: Hα data:Appleton & Marston (1997); 2:Fosbury & Hawarden (1977); 3: Hα dataWong et al (2006); 4: Hα data:Romano et al (2008); 5: from log(NII/Hα) in different ring positions(Fogarty et al 2011); 6: Hα dataHigdon & Wallin (1997); 7:Mapelli et al (2009); 8: Higdon et al (1997) citingJeske (1986); 9: Hα dataSchmitt et al (2006); 10:García-Vargas et al (1997). c B-Magnitude of the ring Note-MK and B are from NED, SFR and Z from References in column 6.…”

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confidence: 99%

The X-Ray Luminosity Function of Ultraluminous X-Ray Sources in Collisional Ring Galaxies

Wolter

Fruscione

Mapelli

2018

ApJ

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Ring galaxies are fascinating laboratories: a catastrophic impact between two galaxies (one not much smaller than the other) has produced fireworks especially in the larger one, when hit roughly perpendicularly to the plane. We analyze the point sources, produced by the starburst episode following the impact, in the rings of seven galaxies and determine their X-ray luminosity function (XLF). In total we detect 63 sources, of which 50 have luminosity L X ≥ 10 39 erg s −1 , classifying them as ultra luminous X-ray sources (ULXs). We find that the total XLF is not significantly different from XLFs derived for other kinds of galaxies, with a tendency of having a larger fraction of high X-ray luminosity objects. Both the total number of ULXs and the number of ULXs per unit star formation rate are found in the upper envelope of the more normal galaxies distribution. Further analysis would be needed to address the issue of the nature of the compact component in the binary system.

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“…. General properties of NGC 922 and the intruder S2 from Wong et al (2006) and Pellerin et al (2010).…”

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confidence: 99%

An H i study of the collisional ring galaxy NGC 922

Elagali

Wong

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present new atomic hydrogen (H I) observations of the collisional ring galaxy NGC 922 obtained using the Australia Telescope Compact Array. Our observations reveal for the first time the vast extent of the H I disc of this galaxy. The H I morphology and kinematics of NGC 922 show that this galaxy is not the product of a simple drop-through interaction, but has a more complex interaction history. The integrated H I flux density of NGC 922 from our observations is 24.7 Jy km s −1 , which is within the error of the flux value obtained using the 64-m Parkes radio telescope. This flux density translates to a total H I mass of 1.1 × 10 10 M and corresponds to an H I to total mass fraction (M H I /M tot ) of approximately 0.11. The gaseous structures of NGC 922 are more extended to the north and include an H I tail that has a projected physical length of 8 kpc. Gas warps are also evident in the velocity field of NGC 922 and are more prominent on the approaching and the western side of the disc. In comparison with a large sample of star-forming galaxies in the local Universe, NGC 922 possesses a high gas fraction relative to galaxies with a similar stellar mass of ∼10 10.4 M , and exhibits a high specific star formation rate.

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NGC 922 - a new drop-through ring galaxy★

Cited by 25 publications

References 30 publications

Morphology and enhanced star formation in a Cartwheel-like ring galaxy

Morphology and enhanced star formation in a Cartwheel-like ring galaxy

The X-Ray Luminosity Function of Ultraluminous X-Ray Sources in Collisional Ring Galaxies

An H i study of the collisional ring galaxy NGC 922

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