MeerKAT 21-cm H I imaging of Abell 2626 and beyond

Healy, J.; Deb, Tirna; Verheijen, Marc; Blyth, S. L.; Serra, P.; Ramatsoku, M.; Vulcani, Benedetta

doi:10.1051/0004-6361/202141377

Cited by 9 publications

(12 citation statements)

References 97 publications

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“…The LEDA 1630451 redshift places it in the Swarm. This galaxy's spiral morphology and detection in H I (Healy et al 2021a) suggest that it is probably not close to the center of a cluster. LEDA 97482, on the other hand, is a cD galaxy (Yuan et al 2016).…”

Section: Identifying A2625mentioning

confidence: 86%

“…The new spectroscopy presented in this paper complements new radio observations centered on A2626 with MeerKAT (Healy et al 2021a). Because radio-frequency interference at the MeerKAT site is so low, the new observations provide previously unattainable neutral hydrogen (H I) measurements of galaxies in the cluster and its surroundings.…”

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confidence: 81%

“…To determine z cl , we selected all galaxies within a radius of 1.5 Mpc of the cluster center and with −3σ cl < v < 3σ cl . We discarded all galaxies detected in H I (Healy et al 2021a) because they do not typically trace the virialized population of a cluster (Colless & Dunn 1996). We applied the biweight location estimator to the redshifts of the sample of galaxies representing the virialized galaxy population (Beers et al 1990) to determine z cl .…”

Section: A2626 and Friendsmentioning

confidence: 99%

“…The radius of 1. • 5 was chosen so that we could identify the known galaxies that are located in the area covered by the MeerKAT H I cube (Healy et al 2021a), which covers 2 × 2 deg 2 centered on A2626. Despite falling into the SDSS spectroscopic footprint, as well as being part of the WINGS-SPE, the spectroscopic coverage across the entire 2 × 2 deg 2 field was very sparse and incomplete, especially for R > 0.7 R 200 from the cluster center.…”

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confidence: 99%

“…The groups identified using the DS test are indicated by the colored points. Black outlines indicate galaxies detected in H I(Healy et al 2021a). Gray points show galaxies associated with the overdensity but not part of any identified substructure.…”

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confidence: 99%

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Abell 2626 and friends: large and small scale structure

Healy,

Willner,

Verheijen

et al. 2021

Preprint

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New MMT/Hectospec spectroscopy centered on the galaxy cluster A2626 and covering a ∼1.8 deg 2 area out to z ∼ 0.46 more than doubles the number of galaxy redshifts in this region. The spectra confirm four clusters previously identified photometrically. A2625, which was previously thought to be a close neighbor of A2626, is in fact much more distant. The new data show six substructures associated with A2626 and five more associated with A2637. There is also a highly collimated collection of galaxies and galaxy groups between A2626 and A2637 having at least three and probably four substructures. At larger scales, the A2626-A2637 complex is not connected to the Pegasus-Perseus filament. 1. INTRODUCTION Large, wide-area spectroscopic surveys such as the Sloan Digital Sky Survey (SDSS; Strauss et al. 2002; Smee et al. 2012), 2dF Galaxy Redshift Survey (2dF-GRS; Colless et al. 2001), and VIMOS Public Extragalactic Survey (VIPERS; Guzzo et al. 2013) have revealed the distribution of galaxies in the Universe.The emerging picture, now referred to as the "Cosmic Web," is a complex and interconnected set of structures (de Lapparent et al. 1986;Bond et al. 1996). These include megaparsec-long one-dimensional structures ("filaments"), thin two-dimensional sheets ("walls"), and vast empty spaces ("voids") surrounded by walls. Galaxy clusters are located where multiple filaments intersect (e.g., Aragón-Calvo et al. 2010;Cautun et al. 2014;Malavasi et al. 2017).The early catalogs of galaxy clusters (Abell 1958;Zwicky et al. 1961) were constructed by identifying apparent over-densities of galaxies on photographic plates. Lucey (1983) and Struble & Rood (1987) estimated that as many as 25% of such identified clusters may be chance superpositions. The only way to confirm cluster members or even the existence of clusters at all is through extensive spectroscopy or at least multi-band imaging. Identifying cluster members can become par-

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Section: Identifying A2625mentioning

confidence: 86%

mentioning

confidence: 81%

Section: A2626 and Friendsmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Abell 2626 and friends: large and small scale structure

Healy,

Willner,

Verheijen

et al. 2021

Preprint

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An H I story of galaxies in Abell 2626 and beyond

Deb¹,

Verheijen²,

Hulst³

2023

A&A

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Context. To study the effects of environment on galaxies, we use H I observations of galaxies in and around the cluster Abell 2626 (A2626). The cluster can effectively be divided into three different environments: the cluster itself, a group environment in the periphery of the cluster (we call it the Swarm), and substructure in the cluster itself. We use these to study the dependence of the galaxy properties on environment. Aims. We have explored the relation between H I deficiency, H I morphology, and star formation deficiency for the galaxies in and around the A2626 galaxy cluster to investigate the environmental effects on these properties. Methods. To quantify the asymmetries of the outer H I disc of a galaxy, we used 1) three visual classes based on the outermost reliable H I contour (settled, disturbed, and unsettled H I discs), 2) the offset between the H I centre and the optical centre of a galaxy, and 3) the modified asymmetry parameter Amod as defined previously. Results. The H I deficiency of a galaxy is strongly correlated with the projected distance from the centre of A2626. Furthermore, substructure galaxies tend to be more asymmetric than the isolated galaxies in A2626, probably because tidal interactions are more efficient within the substructures than outside the substructures. Moreover, asymmetric, offset, and smaller H I discs are not necessarily the result of the cluster environment because they are also observed in substructures in A2626 and in the Swarm. This signifies that a pre-processing of the H I discs of galaxies in groups or substructures plays an important role, together with the processing in the cluster environment. Finally, the star formation rates for the galaxies in all three environments are slightly lower than the typical star formation rate for normal galaxies, as manifested by their offset from the star formation main sequence. This implies effective gas removal mechanisms in all three environments.

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What drives the wheels of evolution in NGC 1512?

Robin,

Kartha,

Ujjwal

et al. 2023

A&A

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Context. Environmental and secular processes play a pivotal role in the evolution of galaxies. These can be external processes such as interactions or internal processes linked to the action of bar, bulge, and spiral structures. Ongoing star formation in spiral galaxies can be affected by these processes. By studying the star formation progression in the galaxy, we can gain insights into the role of different processes that regulate the overall evolution of a galaxy. Aims. The ongoing interaction between the barred-spiral galaxy NGC 1512 and its satellite NGC 1510 offers an opportunity to investigate how galactic interactions and the presence of a galactic bar influence the evolution of NGC 1512. We aim to understand the recent star formation activity in the galaxy pair and thus gain insight into the evolution of NGC 1512. Methods. The UltraViolet Imaging Telescope (UVIT) on board AstroSat enables us to characterise the star-forming regions in the galaxy with a superior spatial resolution of ∼85 pc in the galaxy rest frame. We identified and characterised 175 star-forming regions in the UVIT far-ultraviolet (FUV) image of NGC 1512 and correlated with the neutral hydrogen (H I) distribution. Extinction correction was applied to the estimated photometric magnitude. We traced the star-forming spiral arms of the galaxy and studied the star formation properties across the galaxy in detail. Results. We detect localised regions of star-formation enhancement and distortions in the galactic disc. We find this to be consistent with the distribution of H I in the galaxy. This is evidence of past and ongoing interactions affecting the star formation properties of the galaxy. We studied the properties of the inner ring. We find that the regions of the inner ring show maximum star-formation-rate density (log(SFRDmean[M⊙ yr−1 kpc−2]) ∼ −1.7) near the major axis of the bar, hinting at a possible crowding effect in these regions. The region of the bar in the galaxy is also depleted of UV emission. This absence suggests that the galactic bar may have played an active role in the redistribution of gas and quenching of star formation inside the identified bar region. We therefore suggest that both secular and environmental factors might be influencing the evolution of NGC 1512.

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MeerKAT 21-cm H I imaging of Abell 2626 and beyond

Cited by 9 publications

References 97 publications

Abell 2626 and friends: large and small scale structure

Abell 2626 and friends: large and small scale structure

An H I story of galaxies in Abell 2626 and beyond

What drives the wheels of evolution in NGC 1512?

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MeerKAT 21-cm H I imaging of Abell 2626 and beyond

Cited by 9 publications

References 97 publications

Abell 2626 and friends: large and small scale structure

Abell 2626 and friends: large and small scale structure

An H I story of galaxies in Abell 2626 and beyond

What drives the wheels of evolution in NGC 1512?

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Product

Resources

About

MeerKAT 21-cm H I imaging of Abell 2626 and beyond

An H I story of galaxies in Abell 2626 and beyond