Discovery of a large H i ring around the quiescent galaxy AGC 203001

Bait, Omkar; Kurapati, Sushma; Duc, Pierre–Alain; Cuillandre, Jean-Charles; Wadadekar, Yogesh; Kamphuis, P.; Barway, Sudhanshu

doi:10.1093/mnras/stz2972

Cited by 13 publications

(14 citation statements)

References 62 publications

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“…For example, the ISM in collisional ring galaxies, which experience compression-triggered star formation, is one such starforming ISM that is H I-rich but CO-poor (e.g., Wong et al 2017;Higdon et al 2011). WALLABY will much increase the H I samples of low-mass and LSB galaxies as well as ring galaxies (see Bait et al 2020).…”

Section: Star Formation In Galaxiesmentioning

confidence: 99%

WALLABY – an SKA Pathfinder H i survey

Koribalski

Staveley‐Smith

Westmeier

et al. 2020

Astrophys Space Sci

201

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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Section: Star Formation In Galaxiesmentioning

confidence: 99%

WALLABY – an SKA Pathfinder H i survey

Koribalski

Staveley‐Smith

Westmeier

et al. 2020

Astrophys Space Sci

201

125

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“…The Parkes gridded beam is ∼15.5 arcmin, the velocity resolution is 18 km s −1 (with 4 arcmin pixel size and 13.2 km s −1 channel width) and the rms noise is ∼13 mJy beam −1 per channel for a typical integration time of eight minutes. A detailed description of the hipass observations, calibration and imaging techniques is given in Barnes et al (2001). Current galaxy catalogues include the 'hipass Bright Galaxy Catalog' (hipass bgc; Koribalski et al 2004; see Fig.…”

Section: Parkes Hi Surveysmentioning

confidence: 99%

“…For example, the ISM in collisional ring galaxies, which experience compression-triggered star formation, is one such starforming ISM that is H i-rich but CO-poor (e.g., Wong et al 2017;Higdon et al 2011). wallaby will much increase the H i samples of low-mass and LSB galaxies as well as ring galaxies (see Bait et al 2019).…”

Section: Star Formation In Galaxiesmentioning

confidence: 99%

WALLABY -- An SKA Pathfinder HI Survey

Koribalski,

Staveley-Smith,

Westmeier

et al. 2020

Preprint

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The Widefield ASKAP L-band Legacy All-sky Blind surveY (wallaby) is a nextgeneration 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 radio-quiet 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 signalto-noise ratio of five, wallaby is expected to detect over 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 previous 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.wallaby data products will be made publicly available in the CSIRO ASKAP Science Data Archive (CASDA).

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“…The H I distribution is traditionally derived from spatially resolved maps (e.g., Rots 1980; Yun et al 1994;Noordermeer et al 2005) or azimuthally averaged radial profiles (e.g., Baldwin et al 1980;Rhee & van Albada 1996;Hunter et al 2012). The H I disk traces the spiral arms and outer disk (e.g., Hunter et al 2012;Wang et al 2013), and often exhibits morphological features such as rings (e.g., Emonts et al 2008;Bait et al 2020), warps (e.g., Martinsson et al 2016), and holes created either by local events in the disk (e.g., Boomsma et al 2008;Warren et al 2011) or dynamic stability of the central regions of galaxies (e.g., Murugeshan et al 2019). The H I radial profile, when scaled to the H I radius, shows a central depression, followed by an exponential (Swaters et al 2002;Wang et al 2014Wang et al , 2016 or Sérsic (1963) function (Hunter et al 2021) further out.…”

Section: Introductionmentioning

confidence: 99%

Centrally Concentrated H i Distribution Enhances Star Formation in Galaxies

Wang

2022

ApJ

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We use a sample of 13,511 nearby galaxies from the ALFALFA and Sloan Digital Sky Survey spectroscopic surveys to study the relation between the spatial distribution of H i 21 cm emission and star formation rate (SFR). We introduce a new nonparametric quantity K, measured from the curve of growth of the line, to describe the shape of the integrated H i profile. The value of K increases from double-horned to single-peaked profiles, depending on projection effects and the spatial and velocity distribution of the gas. Using carefully chosen samples to control for the competing factors that influence the integrated line profile, we argue that useful inferences can be made on the spatial distribution of the gas. We find that galaxies with a high value of K tend to have more centrally concentrated H i distribution within the optical disk of the galaxy at fixed conditions, and that larger values of K are associated with higher levels of total and central SFR. The results suggest that the global concentration of H i plays an important role in facilitating the conversion of neutral atomic hydrogen to molecular hydrogen gas, which, in turn, affects the star formation activity throughout the optical disk. Our sample is biased against quiescent galaxies, and thus the conclusions may not hold for galaxies with low SFR or low H i content.

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Discovery of a large H i ring around the quiescent galaxy AGC 203001

Cited by 13 publications

References 62 publications

WALLABY – an SKA Pathfinder H i survey

WALLABY – an SKA Pathfinder H i survey

WALLABY -- An SKA Pathfinder HI Survey

Centrally Concentrated H i Distribution Enhances Star Formation in Galaxies

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