The MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) Survey

Jarvis, Matt J.; Taylor, Andrew; Agudo, I.; Allison, J. R.; Deane, Roger; Frank, B. S.; Gupta, N.; Heywood, Ian; Maddox, Natasha; McAlpine, K.; Santos, Mário G.; Scaife, Anna M. M.; Vaccari, Mattia; Zwart, Jonathan T. L.; Adams, Elizabeth A. K.; Bacon, David; Baker, A. J.; Bassett, Bruce A.; Best, P.; Beswick, R.; Blyth, S. L.; Brown, Michael L.; Brüggen, M.; Cluver, Michelle; Colafranceso, S.; Cotter, Garrett; Cress, C. M.; Davé, Romeel; Ferrari, Chiara; Hardcastle, Martin; Hale, C. L.; Harrison, I.; Hatfield, Peter; Klöckner, H. R.; Kolwa, Sthabile; Malefahlo, Eliab; Marubini, T.; Mauch, T.; Moodley, Kavilan; Morganti, Raffaella; Norris, Ray; Peters, J. A.; Prandoni, I.; Prescott, M.; Oliver, S.; Oozeer, Nadeem; Röttgering, H. J. A.; Seymour, N.; Simpson, Christine M.; Smirnov, O.; Smith, Daniel; Spekkens, Kristine; Stil, J. M.; Tasse, C.; Heyden, K. van der; Whittam, I. H.; Williams, W. L.

doi:10.48550/arxiv.1709.01901

Cited by 19 publications

(26 citation statements)

References 1 publication

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“…These properties are amongst the most critical properties in galaxy evolution and their bias will also help us understand the biases of various other observable properties. The H i bias can be compared against measurements of the completed H i surveys, such as HIPASS and ALFAFA (Barnes et al 2001;Haynes et al 2018), and forecast for the next generation of extragalactic H i surveys, such as MIGH-TEE (Jarvis et al 2017), WALLABY (Koribalski et al, in preparation) and SKA (Yahya et al 2015).…”

Section: Large-scale Galaxy Bias Dependence On Physical Propertiesmentioning

confidence: 99%

Multiwavelength consensus of large-scale linear bias

Pan

Obreschkow

Howlett

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We model the large-scale linear galaxy bias b g (x, z) as a function of redshift z and observed absolute magnitude threshold x for broadband continuum emission from the far infrared to ultra-violet, as well as for prominent emission lines, such as the Hα, Hβ, Lya and [OII] lines. The modelling relies on the semi-analytic galaxy formation model GALFORM, run on the state-of-the-art N-body simulation SURFS with the Planck 2015 cosmology. We find that both the differential bias at observed absolute magnitude x and the cumulative bias for magnitudes brighter than x can be fitted with a five-parameter model:. We also find that the bias for the continuum bands follows a very similar form regardless of wavelength due to the mixing of star-forming and quiescent galaxies in a magnitude limited survey. Differences in bias only become apparent when an additional colour separation is included, which suggest extensions to this work could look at different colours at fixed magnitude limits. We test our fitting formula against observations, finding reasonable agreement with some measurements within 1σ statistical uncertainties, and highlighting areas of improvement. We provide the fitting parameters for various continuum bands, emission lines and intrinsic galaxy properties, enabling a quick estimation of the linear bias in any typical survey of large-scale structure.

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Section: Large-scale Galaxy Bias Dependence On Physical Propertiesmentioning

confidence: 99%

Multiwavelength consensus of large-scale linear bias

Pan

Obreschkow

Howlett

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Our sample sizes are roughly comparable to the expected numbers of galaxies to be detected in LADUMA: below redshifts of z < 0.4, 630 to 1,300 detections are predicted (dependent on the effect of radio frequency interference (RFI)-afflicted frequencies), between redshifts 0.4-0.56 ∼1,200 sources, and between redshifts 0.56-1.4 around ∼700 galaxies in total (based on Oxford S 3 simulations; Obreschkow et al 2009b). By not using the larger volume snapshot galaxies, we also minimise the number of massive (M * >10 10 M ) galaxies, which we do not expect to see large numbers of in LADUMA compared to shallower Hi surveys covering a larger area, such as MIGHTEE-HI (Jarvis et al 2017). LADUMA is also predicted to probe dwarf galaxies down to Hi masses of MHI ∼ 1 × 10 8 M at low redshifts, making Simba-hires a good sample to use for predictions for LADUMA.…”

Section: Simbamentioning

confidence: 99%

The redshift evolution of the baryonic Tully-Fisher relation in Simba

Glowacki,

Elson,

Davé

2020

Preprint

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The baryonic Tully-Fisher relation (BTFR) is an important tool for constraining galaxy evolution models. As 21-cm Hi emission studies have been largely restricted to low redshifts, the redshift evolution of the BTFR is yet to be fully studied. The upcoming LADUMA survey (Looking At the Distant Universe with the MeerKAT Array) will address this. As preparation for LADUMA, we use the Simba hydrodynamical galaxy formation simulation from the Simba-hires (25 h −1 Mpc) 3 run to generate rotational velocity measures from galaxy rotation curves (V flat ) and Hi spectral line profile widths (W 50 and W 20) at three different redshifts (z = 0, 0.5, and 1). Using these measures, together with the dark matter velocity dispersion, we consider the redshift evolution of the BTFR of Simba galaxies. We find that LADUMA will be successful in detecting redshift evolution of the BTFR, provided that auxiliary data is used to distinguish galaxies with disky morphologies. W 20 spectral line widths give lower scatter and more pronounced redshift evolution compared to W 50. We also compare these rotational velocity measures to the dark matter velocity dispersion across redshift and galaxy morphology. We find weak redshift evolution between rotational velocity and the dark matter halo mass, and provide fits for estimating a galaxy's dark matter halo mass from Hi spectral line widths. This study with Simba showcases the importance of upcoming, deep SKA pathfinder surveys such as LADUMA, and provides predictions to compare with redshift evolution of the BTFR and galaxy dark matter content from Hi rotational velocity measures.

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“…For this they use a Bayesian stacking analysis to probe below the 1-mJy flux-limit of the FIRST survey (Becker et al, 1995). White et al will test the radio-quiet distribution of these RLFs using optical spectroscopy from the Southern African Large Telescope (PI: White) and deep radio data that has been obtained as part of the MIGHTEE survey (Jarvis et al, 2016). Following this is the need to disentangle the star-formation and AGN contributions to the total radio emission, for which very long baseline interferometry would offer excellent spatial information to supplement multi-wavelength analysis.…”

Section: Implications and Future Workmentioning

confidence: 99%

Accretion and star formation in 'radio-quiet' quasars

White¹,

Jarvis²,

Kalfountzou³

et al. 2019

Preprint

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Radio observations allow us to identify a wide range of active galactic nuclei (AGN), which play a significant role in the evolution of galaxies. Amongst AGN at low radio-luminosities is the 'radio-quiet' quasar (RQQ) population, but how they contribute to the total radio emission is under debate, with previous studies arguing that it is predominantly through star formation. In this talk, SVW summarised the results of recent papers on RQQs, including the use of farinfrared data to disentangle the radio emission from the AGN and that from star formation. This provides evidence that black-hole accretion, instead, dominates the radio emission in RQQs. In addition, we find that this accretion-related emission is correlated with the optical luminosity of the quasar, whilst a weaker luminosity-dependence is evident for the radio emission connected with star formation. What remains unclear is the process by which this accretion-related emission is produced. Understanding this for RQQs will then allow us to investigate how this type of AGN influences its surroundings. Such studies have important implications for modelling AGN feedback, and for determining the accretion and star-formation histories of the Universe.

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The MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) Survey

Cited by 19 publications

References 1 publication

Multiwavelength consensus of large-scale linear bias

Multiwavelength consensus of large-scale linear bias

The redshift evolution of the baryonic Tully-Fisher relation in Simba

Accretion and star formation in 'radio-quiet' quasars

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