Physical Sciences and Mathematics | Open Access Articles

Measuring Cosmic Density Of Neutral Hydrogen Via Stacking The Dingo-Vla Data, Qingxiang Chen, Martin Meyer, Attila Popping, Lister Staveley-Smith, Julia Bryant, Jacinta Delhaize, Benne Holwerda, M E. Cluver, J Loveday, Angel R. Lopez-Sanchez, Martin Zwaan, E N. Taylor, A M. Hopkins, Angus Wright, Simon Driver, S Brough Oct 2021

Measuring Cosmic Density Of Neutral Hydrogen Via Stacking The Dingo-Vla Data, Qingxiang Chen, Martin Meyer, Attila Popping, Lister Staveley-Smith, Julia Bryant, Jacinta Delhaize, Benne Holwerda, M E. Cluver, J Loveday, Angel R. Lopez-Sanchez, Martin Zwaan, E N. Taylor, A M. Hopkins, Angus Wright, Simon Driver, S Brough

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We use the 21-cm emission-line data from the Deep Investigation of Neutral Gas Origin-Very Large Array (DINGO-VLA) project to study the atomic hydrogen gas H I of the Universe at redshifts z < 0.1. Results are obtained using a stacking analysis, combining the H I signals from 3622 galaxies extracted from 267 VLA pointings in the G09 field of the Galaxy and Mass Assembly Survey (GAMA). Rather than using a traditional one-dimensional spectral stacking method, a three-dimensional cubelet stacking method is used to enable deconvolution and the accurate recovery of average galaxy fluxes from this high-resolution interferometric data set. By probing down to galactic scales, this experiment also overcomes confusion corrections that have been necessary to include in previous single-dish studies. After stacking and deconvolution, we obtain a 30σ H I mass measurement from the stacked spectrum, indicating an average H I mass of MHI=(1.67±0.18)×109 M⊙" role="presentation" style="box-sizing: border-box; margin: 0px; padding: 0px; border: 0px; font-variant: inherit; font-stretch: inherit; line-height: normal; font-family: inherit; vertical-align: baseline; display: inline; word-spacing: normal; overflow-wrap: normal; white-space: nowrap; float: none; direction: ltr; max-width: none; max-height: none; min-width: 0px; min-height: 0px; position: relative;">MHI=(1.67±0.18)×109 M⊙MHI=(1.67±0.18)×109 M⊙⁠. The corresponding cosmic density of neutral atomic hydrogen is ΩHI=(0.38±0.04)×10−3" role="presentation" style="box-sizing: border-box; margin: 0px; padding: 0px; border: 0px; font-variant: inherit; font-stretch: inherit; line-height: normal; font-family: inherit; vertical-align: baseline; display: inline; word-spacing: normal; overflow-wrap: normal; white-space: nowrap; float: none; direction: ltr; max-width: none; max-height: none; min-width: 0px; min-height: 0px; position: relative;">ΩHI=(0.38±0.04)×10−3ΩHI=(0.38±0.04)×10−3 at redshift of z = 0.051. These values are in good agreement with …

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Galaxy And Mass Assembly (Gama): The Environmental Impact On Sfr And Metallicity In Galaxy Groups, D Sotillo-Ramos, M A. Lara-López, A M. Pérez-García, R Pérez-Martínez, A M. Hopkins, Benne Holwerda, J Liske, A R. López-Sánchez, M S. Owers, K A. Pimbblet Oct 2021

Deep Extragalactic Visible Legacy Survey (Devils): Sed Fitting In The D10-Cosmos Field And The Evolution Of The Stellar Mass Function And Sfr–M⋆ Relation, Jessica E. Thorne, Aaron S G Robotham, Luke J M Davies, Sabine Bellstedt, Simon P. Driver, Matías Bravo, Malcolm N. Bremer, Benne Holwerda, Andrew M. Hopkins, Claudia Del P Lagos, Steven Phillipps, Malgorzata Siudek, Edward N. Taylor, Angus H. Wright May 2021

Deep Extragalactic Visible Legacy Survey (Devils): Sed Fitting In The D10-Cosmos Field And The Evolution Of The Stellar Mass Function And Sfr–M⋆ Relation, Jessica E. Thorne, Aaron S G Robotham, Luke J M Davies, Sabine Bellstedt, Simon P. Driver, Matías Bravo, Malcolm N. Bremer, Benne Holwerda, Andrew M. Hopkins, Claudia Del P Lagos, Steven Phillipps, Malgorzata Siudek, Edward N. Taylor, Angus H. Wright

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We present catalogues of stellar masses, star formation rates (SFRs), and ancillary stellar population parameters for galaxies spanning 0 < z < 9 from the Deep Extragalactic VIsible Legacy Survey (DEVILS). DEVILS is a deep spectroscopic redshift survey with very high completeness, covering several premier deep fields including COSMOS (D10). Our stellar mass and SFR estimates are self-consistently derived using the spectral energy distribution (SED) modelling code PROSPECT, using well-motivated parametrizations for dust attenuation, star formation histories, and metallicity evolution. We show how these improvements, and especially our physically motivated assumptions about metallicity evolution, have an appreciable systematic effect on the inferred stellar masses, at the level of ∼0.2 dex. To illustrate the scientific value of these data, we map the evolving galaxy stellar mass function (SMF) and the SFR–M_⋆ relation for 0 < z < 4.25. In agreement with past studies, we find that most of the evolution in the SMF is driven by the characteristic density parameter, with little evolution in the characteristic mass and low-mass slopes. Where the SFR–M_⋆ relation is indistinguishable from a power law at z > 2.6, we see evidence of a bend in the relation at low redshifts (z < 0.45). This suggests evolution in both the normalization and shape of the SFR–M_⋆ relation since cosmic noon. It is significant that we only clearly see this bend when combining our new DEVILS measurements with consistently derived values for lower redshift galaxies from the Galaxy And Mass Assembly (GAMA) survey: this shows the power of …

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Galaxy And Mass Assembly (Gama): The Environmental Impact On Sfr And Metallicity In Galaxy Groups, D Sotillo-Ramos, M A. Lara-López, A M. Pérez-García, R Pérez-Martínez, A M. Hopkins, Benne Holwerda, J Liske, A R. López-Sánchez, M S. Owers, K A. Pimbblet

Faculty Scholarship

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