WALLABY Pilot Survey: the diversity of ram pressure stripping of the galactic HI gas in the Hydra Cluster

Wang, Jing; Staveley-Smith, Lister; Westmeier, Tobias; Catinella, Barbara; Shao, Li; Reynolds, T. N.; For, Bi-Qing; Lee, Bumhyun; Liang, Ze-zhong; Wang, Shun; Elagali, A.; Denes, H.; Kleiner, D.; Koribalski, Baerbel S.; Lee-Waddell, K.; Oh, S-H.; Rhee, J.; Serra, P.; Spekkens, K.; Wong, O. I.; Bekki, K.; Bigiel, F.; Courtois, H. M.; Hess, Kelley M.; Holwerda, B. W.; McQuinn, Kristen B. W.; Pandey-Pommier, M.; van der Hulst, J. M.; Verdes-Montenegro, L.

doi:10.48550/arxiv.2104.13052

Cited by 4 publications

(7 citation statements)

References 120 publications

(192 reference statements)

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“…We conclude that the H morphology of ESO 501−G075 is compatible with the galaxy experiencing ram pressure and consistent with ESO 501−G075 falling into Hydra I for the first time. Our results are also in agreement with the ram pressure study of Hydra I by Wang et al (2021), in which ESO 501−G075 is classified as a candidate for experiencing ram pressure.…”

Section: Discussionsupporting

confidence: 91%

WALLABY Pilot Survey: First Look at the Hydra I Cluster and Ram Pressure Stripping of ESO 501-G075

Reynolds,

Westmeier,

Elagali

et al. 2021

Preprint

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We present results from neutral atomic hydrogen (H ) observations of Hydra I, the first cluster observed by the Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) on the Australian Square Kilometre Array Pathfinder. For the first time we show that WALLABY can reach its final survey sensitivity. Leveraging the sensitivity, spatial resolution and wide field of view of WALLABY, we identify a galaxy, ESO 501−G075, that lies near the virial radius of Hydra I and displays an H tail. ESO 501−G075 shows a similar level of morphological asymmetry as another cluster member, which lies near the cluster centre and shows signs of experiencing ram pressure. We investigate possible environmental processes that could be responsible for producing the observed disturbance in the H morphology of ESO 501−G075. We rule out tidal interactions, as ESO 501−G075 has no nearby neighbours within ∼ 0.34 Mpc. We use a simple model to determine that ram pressure can remove gas from the disc at radii 𝑟 25 kpc. We conclude that, as ESO 501−G075 has a typical H mass compared to similar galaxies in the field and its morphology is compatible with a ram pressure scenario, ESO 501−G075 is likely recently infalling into the cluster and in the early stages of experiencing ram pressure.

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Section: Discussionsupporting

confidence: 91%

WALLABY Pilot Survey: First Look at the Hydra I Cluster and Ram Pressure Stripping of ESO 501-G075

Reynolds,

Westmeier,

Elagali

et al. 2021

Preprint

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“…This is the scenario proposed to account for the optical and HI structure in NGC 1427A, member of the Fornax cluster (Lee-Waddell et al 2018). The new WALLABY data for the Hydra I cluster (Wang et al 2021) will help to disentangle the nature of the stellar filaments in NGC 3314A. In this section we describe the main steps adopted to derive the surface photometry and the structural parameters for UDG 32.…”

Section: Discussionmentioning

confidence: 99%

Formation of an ultra-diffuse galaxy in the stellar filaments of NGC3314A: caught in act?

Iodice,

La Marca,

Hilker

et al. 2021

Preprint

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The VEGAS imaging survey of the Hydra I cluster reveals an extended network of stellar filaments to the south-west of the spiral galaxy NGC 3314A. Within these filaments, at a projected distance of ∼ 40 kpc from the galaxy, we discover an ultra-diffuse galaxy (UDG) with a central surface brightness of µ 0,g ∼ 26 mag arcsec −2 and effective radius R e ∼ 3.8 kpc. This UDG, named UDG 32, is one of the faintest and most diffuse low-surface brightness galaxies in the Hydra I cluster. Based on the available data, we cannot exclude that this object is just seen in projection on top of the stellar filaments, thus being instead a foreground or background UDG in the cluster. However, the clear spatial coincidence of UDG 32 with the stellar filaments of NGC 3314A suggests that it might have formed from the material in the filaments, becoming a detached, gravitationally bound system. In this scenario, the origin of UDG 32 depends on the nature of the stellar filaments in NGC 3314A, which is still unknown. They could result from ram-pressure stripping or have a tidal origin. In this letter, we focus on the comparison of the observed properties of the stellar filaments and UDG 32, and speculate about their possible origin. The relatively red colour (g − r = 0.54 ± 0.14 mag) of the UDG, similar to that of the disk in NGC 3314A, combined with an age older than 1 Gyr, and the possible presence of a few compact stellar systems, all point towards a tidal formation scenario inferred for the UDG 32.

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“…Furthermore, the intrinsic lack of zerospacing information in the visibility (uv-) plane translates to a potential for 'resolving out' emission that exists on large angular scales. So far, WALLABY early-science commissioning and pilot observations have successfully recovered the total HI emission from a diverse set of HI observations of galaxies in environments ranging from the field to groups and clusters (Serra et al 2015b;Reynolds et al 2019;Lee-Waddell et al 2019;Elagali et al 2019;Kleiner et al 2019;For et al 2019;Wang et al 2021).…”

Section: Discussionmentioning

confidence: 99%

WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395

Wong,

Stevens,

For

et al. 2021

Preprint

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We present the Australian Square Kilometre Array Pathfinder (ASKAP) WALLABY pre-pilot observations of two 'dark' HI sources (with HI masses of a few times 10 8 M ⊙ and no known stellar counterpart) that reside within 363 kpc of NGC 1395, the most massive early-type galaxy in the Eridanus group of galaxies. We investigate whether these 'dark' HI sources have resulted from past tidal interactions or whether they are an extreme class of low surface brightness galaxies. Our results suggest that both scenarios are possible, and not mutually exclusive. The two 'dark' HI sources are compact, reside in relative isolation and are more than 159 kpc away from their nearest HI-rich galaxy neighbour. Regardless of origin, the HI sizes and masses of both 'dark' HI sources are consistent with the HI size-mass relationship that is found in nearby low-mass galaxies, supporting the possibility that these HI sources are an extreme class of low surface brightness galaxies. We identified three analogues of candidate primordial 'dark' HI galaxies within the TNG100 cosmological, hydrodynamic simulation. All three model analogues are dark matter-dominated, have assembled most of their mass 12-13 Gyr ago, and have not experienced much evolution until cluster infall 1-2 Gyr ago. Our WALLABY pre-pilot science results suggest that the upcoming large area HI surveys will have a significant impact on our understanding of low surface brightness galaxies and the physical processes that shape them.

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WALLABY Pilot Survey: the diversity of ram pressure stripping of the galactic HI gas in the Hydra Cluster

Cited by 4 publications

References 120 publications

WALLABY Pilot Survey: First Look at the Hydra I Cluster and Ram Pressure Stripping of ESO 501-G075

WALLABY Pilot Survey: First Look at the Hydra I Cluster and Ram Pressure Stripping of ESO 501-G075

Formation of an ultra-diffuse galaxy in the stellar filaments of NGC3314A: caught in act?

WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395

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