2018
DOI: 10.1093/mnras/sty741
|View full text |Cite
|
Sign up to set email alerts
|

An H i study of the collisional ring galaxy NGC 922

Abstract: 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 o… Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
4
1

Citation Types

3
17
0

Year Published

2018
2018
2024
2024

Publication Types

Select...
5
1

Relationship

2
4

Authors

Journals

citations
Cited by 10 publications
(20 citation statements)
references
References 59 publications
3
17
0
Order By: Relevance
“…This will advance our understanding of the collisional ring galaxies' number density, their evolution and whether the drop-through interaction proposed in non-cosmological isolated interaction simulations is frequent enough to explain the observed number density of ring galaxies (Lavery et al 2004;Elmegreen & Elmegreen 2006). Further, observations of collisional ring galaxies suggests that these systems contain on average high amounts of HI gas in comparison with galaxies that have the same stellar mass (Elagali et al 2018), yet are H2 deficient (Higdon et al 2015;Wong et al 2017) especially at the outer rings where the atomic hydrogen surface density is the highest (e.g., in the Cartwheel galaxy ΣHI = 19 − 65 M pc −2 ; Higdon et al 2015). The reason behind this deficiency is not yet well understood, however Wong et al (2017) and Higdon et al (2015) hypothesise that the ISM in ring galaxies behaves differently as a result of the extreme conditions in, e.g., pressure, temperature and metallicity, induced by the drop-through collision.…”
Section: Introductionmentioning
confidence: 80%
See 2 more Smart Citations
“…This will advance our understanding of the collisional ring galaxies' number density, their evolution and whether the drop-through interaction proposed in non-cosmological isolated interaction simulations is frequent enough to explain the observed number density of ring galaxies (Lavery et al 2004;Elmegreen & Elmegreen 2006). Further, observations of collisional ring galaxies suggests that these systems contain on average high amounts of HI gas in comparison with galaxies that have the same stellar mass (Elagali et al 2018), yet are H2 deficient (Higdon et al 2015;Wong et al 2017) especially at the outer rings where the atomic hydrogen surface density is the highest (e.g., in the Cartwheel galaxy ΣHI = 19 − 65 M pc −2 ; Higdon et al 2015). The reason behind this deficiency is not yet well understood, however Wong et al (2017) and Higdon et al (2015) hypothesise that the ISM in ring galaxies behaves differently as a result of the extreme conditions in, e.g., pressure, temperature and metallicity, induced by the drop-through collision.…”
Section: Introductionmentioning
confidence: 80%
“…This agrees with the current theoretical and observational understanding of ring galaxies in the local Universe. For instance, in most of the observed ring galaxies the intruder lies within a physical distance of less than 100 kpc (Elagali et al 2018;Conn et al 2016;Fogarty et al 2011). Figure 9(a) shows a scatter plot of EAGLE galaxies in the ( u − r ) colour-stellar mass plane at z = 0 (left) and z = 0.5 (right).…”
Section: The Host Halos Of Eagle Ring Galaxiesmentioning
confidence: 99%
See 1 more Smart Citation
“…Enormous effort is aimed towards understanding how such interactions relate to the observed H i content in galaxies and conversely how H i distribution and kinematics uncover the physics of interaction (e.g. Bekki 2008;Pisano et al 2011;Mihos et al 2012;Elagali et al 2018;Bosma 2017, and references therein). Spiral galaxies have a lower H i fraction in high density environments, for instance, near the centers of galaxy clusters (Giovanelli & Haynes 1985;Chung et al 2009) or in HCGs (Verdes-Montenegro et al 2001), than spiral galaxies that reside in the field.…”
Section: Introductionmentioning
confidence: 99%
“…It has a recession velocity 𝑣 𝑟 = 3082.46±5.40 km/s corresponding to a distance of 42.46±2.48 Mpc (Koribalski et al 2004). It contains a higher abundance of neutral gas for a galaxy of its size, compared to typical star-forming galaxies (Elagali et al 2018a). The interaction with the dwarf companion has triggered a star-formation episode in the bulge ∼ 300 Myr ago, that continues until now.…”
Section: Introductionmentioning
confidence: 99%