H i debris in the IC 1459 galaxy group

Saponara, J.; Koribalski, B. S.; Benaglia, P.; López, Manuel Fernández

doi:10.1093/mnras/stx2475

Cited by 22 publications

(47 citation statements)

References 58 publications

(79 reference statements)

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“…This is particularly interesting as substantial H I debris are often found near massive, early-type galaxies (see e.g. Chung et al 2009;Saponara et al 2018). The pair is also part of the subgroup containing NGC 5150.…”

Section: E N V I Ro N M E N T a N D H I M O R P H O L O G Ymentioning

confidence: 95%

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

For

Staveley‐Smith

Westmeier

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present an H i study of the galaxy group LGG 351 using Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) early science data observed with the Australian Square Kilometre Array Pathfinder (ASKAP). LGG 351 resides behind the M 83 group at a velocity range (cz) of ∼3500–4800 km s−1 within the rich Hydra-Centaurus overdensity region. We detect 40 sources with the discovery of a tidally interacting galaxy pair and two new H i sources that are not presented in previous optical catalogues. 23 out of 40 sources have new redshifts derived from the new H i data. This study is the largest WALLABY sub-sample to date and also allows us to further validate the performance of ASKAP and the data reduction pipeline askapsoft. Extended H i emission is seen in six galaxies indicating interaction within the group, although no H i debris is found. We also detect H i in a known ultra-faint dwarf galaxy (dw 1328−29), which demonstrates that it is not a satellite of the M 83 group as previously thought. In conjunction with multiwavelength data, we find that our galaxies follow the atomic gas fraction and baryonic Tully–Fisher scaling relations derived from the GALEX Arecibo SDSS Survey. In addition, majority of our galaxies fall within the star formation main sequence indicating inefficiency of gas removal processes in this loose galaxy group.

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Section: E N V I Ro N M E N T a N D H I M O R P H O L O G Ymentioning

confidence: 95%

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

For

Staveley‐Smith

Westmeier

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The long tidal tails, high gas content and shells are indicative of two merging spirals (e.g., Toomre & Toomre 1972;Toomre 1977;Malin & Carter 1980). Saponara et al (2018) found large HI clouds near IC 1459, concluding these were likely to be debris from tidal interactions with neighbouring galaxies. Being the central galaxy in a relatively small group would mean a high probability of mergers due to the low dispersion of the group (Ostriker 1980;Tremaine 1981).…”

Section: Merging Spiralsmentioning

confidence: 99%

Unravelling the origin of the counter-rotating core in IC 1459 with KMOS and MUSE

Prichard

Vaughan

Davies

2019

Monthly Notices of the Royal Astronomical Society

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The massive early-type galaxy (ETG) IC 1459 is a slowly rotating galaxy that exhibits a rapidly counter-rotating kinematically decoupled core (KDC, R KDC ≈ 5 ≈ 0.1R e ). To investigate the origin of its KDC, we coupled large data mosaics from the nearinfrared (NIR)/optical integral field unit (IFU) instruments K-band Multi-Object Spectrograph (KMOS) and Multi Unit Spectroscopic Explorer (MUSE). We studied IC 1459's stellar populations and, for the first time for a KDC, the spatially resolved initial mass function (IMF). We used full-spectral-fitting to fit the stellar populations and IMF simultaneously, and an alternative spectral-fitting method that does not assume a star-formation history (SFH; although does not constrain the IMF) for comparison. When no SFH is assumed, we derived a negative metallicity gradient for IC 1459 that could be driven by a distinct metal-poor population in the outer regions of the galaxy, and a radially constant old stellar age. We found a radially constant bottom-heavy IMF out to ∼ 1 /3R e . The radially flat IMF and age extend beyond the counter-rotating core. We detected high velocity dispersion along the galaxy's major axis. Our results potentially add weight to findings from orbital modelling of other KDCs that the core is not a distinct population of stars but in fact two smooth co-spatial counter-rotating populations. No clear picture of formation explains the observational results of IC 1459, but we propose it could have included a gas-rich intense period of star formation at early times, perhaps with counter-rotating accreting cold streams, followed by dry and gas-rich mergers through to the present day.

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“…While all forms of hydrogen are typically detected in the inner discs and spiral arms of galaxies in the Local Universe, most often it is the H I 21-cm line that reveals the outermost regions of galaxy discs (e.g., Warren et al 2004;Begum et al 2005;Sancisi et al 2008;Heald et al 2011;Koribalski et al 2018). Occasionally H I is found in filaments, plumes and/or bridges, tracing the gravitational interactions with neighbouring galaxies (e.g., Yun et al 1993Yun et al , 1994Koribalski et al 2003;Koribalski and Dickey 2004;Pearson et al 2016) and in groups/clusters (e.g., Verdes-Montenegro et al 2001;Oosterloo and van Gorkom 2005;Chung et al 2009;English et al 2010;Lee-Waddell et al 2012;Hess et al 2017;Scott et al 2018;Saponara et al 2018). Beyond the inner galaxy disk in which molecular hydrogen is typically the dominant gas component (Leroy et al 2008;Bigiel and Blitz 2012), H I is also an excellent tracer of star formation in the outer discs of galaxies (e.g., Battaglia et al 2006;Koribalski and López-Sánchez 2009;Koribalski 2017).…”

Section: Introductionmentioning

confidence: 99%

WALLABY – an SKA Pathfinder H i survey

Koribalski

Staveley‐Smith

Westmeier

et al. 2020

Astrophys Space Sci

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189

125

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The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (H I) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 × 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radioquiet zone in Western Australia. WALLABY aims to survey three-quarters of the sky (−90 • < δ < +30 • ) to a redshift of z 0.26, and generate spectral line image cubes at ∼30 arcsec resolution and ∼1.6 mJy beam −1 per 4 km s −1 channel sensitivity. ASKAP's instantaneous field of view at 1.4 GHz, delivered by the PAF's 36 beams, is about 30 sq deg. At an integrated signal-to-noise ratio of five, WALLABY is expected to detect around half a million galaxies with a mean redshift of z ∼ 0.05 (∼200 Mpc). The scientific goals of WALLABY include: (a) a census of gas-rich galaxies in the vicinity of the Local Group; (b) a study of the H I properties of galaxies, groups and clusters, in particular the influence of the environment on galaxy evolution; and (c) the refinement of cosmological parameters using the spatial and redshift distribution of low-bias gas-rich galaxies. For context we provide an overview of recent and planned large-scale H I surveys. Combined with existing and new multi-wavelength sky surveys, WALLABY will enable an exciting new generation of panchromatic studies of the Local Universe. -First results from the WALLABY pilot survey are revealed, with initial data products publicly available in the CSIRO ASKAP Science Data Archive (CASDA).

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H i debris in the IC 1459 galaxy group

Cited by 22 publications

References 58 publications

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351

Unravelling the origin of the counter-rotating core in IC 1459 with KMOS and MUSE

WALLABY – an SKA Pathfinder H i survey

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