THE H i CONTENT OF THE UNIVERSE OVER THE PAST 10 GYR

Neeleman, Marcel; Prochaska, J. Xavier; Ribaudo, Joseph; Lehner, N.; Howk, J. C.; Rafelski, Marc; Kanekar, Nissim

doi:10.3847/0004-637x/818/2/113

Cited by 99 publications

(119 citation statements)

References 60 publications

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“…The filled triangles are from H I21 cm emission surveys (Zwaan et al 2005;Martin et al 2010), the open squares from H I21 cm emission stacking at low redshifts (Lah et al 2007;Delhaize et al 2013;Rhee et al 2013), and the filled circles from absorption-selected galaxies, Mg II absorbers at z ≈ 0.7-1.2 (Rao et al 2006) and damped Lyα absorbers at z2.2 (Noterdaeme et al 2012;Crighton et al 2015). The open star shows our new GMRT result, for blue star-forming galaxies at z ≈ 1.265; it is clear that this is significantly lower than the Ω GAS estimates at both z=0 and z2.2 (see also Neeleman et al 2016). …”

Section: H Sf H I Imentioning

confidence: 74%

THE GAS MASS OF STAR-FORMING GALAXIES AT z ≈ 1.3

Kanekar

Sethi

Dwarakanath

2016

ApJL

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We report a Giant Metrewave Radio Telescope search for H I 21 cm emission from a large sample of massive starforming galaxies at z ≈ 1.18-1.34, lying in sub-fields of the DEEP2 Redshift Survey. The search was carried out by co-adding ("stacking") the H I 21 cm emission spectra of 857 galaxies, after shifting each galaxy's H I 21 cm spectrum to its rest frame. We obtain the 3σ upper limit S H I <2.5 μJy on the average H I 21 cm flux density of the 857galaxies, at a velocity resolution of ≈315 km s [ ] <´´D - on the average H I mass of the 857 stacked galaxies, the first direct constraint on the atomic gas mass of galaxies at z>1. The implied limit on the average atomic gas mass fraction (relative to stars) is M GAS /M * <0.5, comparable to the cold molecular gas mass fraction in similar star-forming galaxies at these redshifts. We find that the cosmological mass density of neutral atomic gas in massive starforming galaxies at z ≈ 1.3 is Ω GAS <3.7×10 −4 , significantly lower than Ω GAS estimates in both galaxies in the local universe and damped Lyα absorbers at z2.2. Massive blue star-forming galaxies thus do not appear to dominate the neutral atomic gas content of the universe at z ≈ 1.3.

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Section: H Sf H I Imentioning

confidence: 74%

THE GAS MASS OF STAR-FORMING GALAXIES AT z ≈ 1.3

Kanekar

Sethi

Dwarakanath

2016

ApJL

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“…While the general trend of these results indicates a steep decline in the cross-section of DLA absorbers from redshifts 5 to 2, there is less agreement among the various studies at low redshift because of small sample sizes. For example, Meiring et al (2011) found 3 serendipitous DLAs in the COS-Halos survey (the grey diamond in Figure 3); Neeleman et al (2016) identified 4 DLAs in a blind survey of 463 quasars in the HST archives (the orange triangle). The blue cross is a 21 cm follow-up study of Mg ii systems by Kanekar et al (2009) in which they found 9 detections of 21 cm absorption among 55 Mg ii systems.…”

Section: The Cosmic Incidence Of Neutral Gas N Dlamentioning

confidence: 99%

“…The HST Quasar Absorption Line Key Project found only 1 DLA in a blind survey (Bahcall et al 1993), while Meiring et al (2011) found 3 serendipitous DLAs in the COS-Halos survey, and Neeleman et al (2016) identified 4 DLAs in a blind survey of 463 quasars in the HST archives. These results are consistent given the small samples and low statistical accuracies.…”

Section: Introductionmentioning

confidence: 99%

The statistical properties of neutral gas at z < 1.65 from UV measurements of Damped Lyman Alpha systems

Rao

Turnshek

Sardane

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We derive the statistical properties of neutral gas at redshifts 0.11 < z < 1.65 from UV measurements of quasar Lyα absorption lines corresponding to 369 Mg ii systems with W λ2796 0 ≥ 0.3Å. In addition to the 41 damped Lyman alpha (DLA) systems presented in Rao et al. (2006), the current DLA sample includes 29 newly discovered DLAs. Of these, 26 were found in our Hubble Space Telescope (HST) Advanced Camera for Surveys prism survey for DLAs (Turnshek et al. 2015) and three were found in a GALaxy Evolution Explorer (GALEX) archival search. In addition, an HST Cosmic Origins Spectrograph Cycle 19 survey yielded no DLAs that could be used for this study. Formally, this DLA sample includes 70 systems with N HI ≥ 2 × 10 20 atoms cm −2 . We find that the incidence of DLAs, or the product of their gas cross section and their comoving number density, can be described by n DLA (z) = (0.027±0.007)(1+z) (1.682±0.200) over the redshift range 0 < z < 5. The cosmic mass density of neutral gas can be described by Ω DLA (z) = (4.77 ± 1.60) × 10 −4 (1 + z) (0.64±0.27) . The low-redshift column density distribution function is well-fitted by a power law of the form f (N) ∼ N β with β = −1.46 ± 0.20. It is consistent with the high-redshift as well as z = 0 estimates at the high column density end but, lies between them at the low column density end. We discuss possible N HI and metallicity bias in Mg ii-selected DLA samples and show that such biases do not exist in the current data at z < 1.65. Thus, at least at z < 1.65, DLAs found through Mg ii selection statistically represent the true population of DLAs. However, we caution that studies of DLA metallicities should take into the account the relative incidence of DLAs with respect to W λ2796 0 (or gas velocity spread) in order to correctly measure the mean neutral-gas cosmic metallicity of the universe.

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“…1 A comparison of the evolution of the stellar mass density (stars/purple) and atomic gas (HI) mass density (points/green) with redshift (top) and lookback time (bottom). The HI data are from the compilation by Neeleman et al (2016) and Sánchez-Ramírez et al (2016), and the stellar mass densities are taken from the Madau & Dickinson (2014) compilation. The HI measurements are largely based on damped Lyman-α absorption measurements except at z ∼ 0.…”

Section: The Need For Accretion Through Cosmic Timementioning

confidence: 99%

An Introduction to Gas Accretion onto Galaxies

Putman¹

2017

Astrophysics and Space Science Library

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Evidence for gas accretion onto galaxies can be found throughout the universe. In this chapter, I summarize the direct and indirect signatures of this process and discuss the primary sources. The evidence for gas accretion includes the star formation rates and metallicities of galaxies, the evolution of the cold gas content of the universe with time, numerous indirect indicators for individual galaxies, and a few direct detections of inflow. The primary sources of gas accretion are the intergalactic medium, satellite gas and feedback material. There is support for each of these sources from observations and simulations, but the methods with which the fuel ultimately settles in to form stars remain murky.

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THE H i CONTENT OF THE UNIVERSE OVER THE PAST 10 GYR

Abstract: We use the Hubble Space Telescope (HST) archive of ultraviolet (UV) quasar spectroscopy to conduct the first blind survey for damped Lyα absorbers (DLAs) at low redshift ( Show more

Cited by 99 publications

References 60 publications

THE GAS MASS OF STAR-FORMING GALAXIES AT z ≈ 1.3

THE GAS MASS OF STAR-FORMING GALAXIES AT z ≈ 1.3

The statistical properties of neutral gas at z < 1.65 from UV measurements of Damped Lyman Alpha systems

An Introduction to Gas Accretion onto Galaxies

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