The HI content of star-forming galaxies at z = 0.24

By Philip Lah, J. Chengalur, Frank H. Briggs, M. Colless, R. Propris, M. Pracy, W. D. de Blok, S. Fujita, M. Ajiki, Y. Shioya and 5 more. 2007

146 citations recorded by the source corpus.

We use observations from the Giant Metrewave Radio Telescope (GMRT) to measure the atomic hydrogen gas content of star-forming galaxies at z = 0.24 (i.e. a look-back time of ∼3 Gyr). The sample of galaxies studied were selected from Hα-emitting field galaxies detected in a narrow-band imaging survey with the Subaru Telescope. The Anglo-Australian Telescope was used to obtain precise optical redshifts for these galaxies. We then co-added the H I 21-cm emission signal for all the galaxies within the GMRT spectral line data cube. From the co-added signal of 121 galaxies, we measure an average atomic hydrogen gas mass of (2.26 ± 0.90) × 10 9 M� . We translate this H I signal into a cosmic density of neutral gas at z = 0.24 ‐ ‐

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f10d86f08969c5b8325a6a4f7feb184ef0d2d364

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Citations in the corpus

Column density distribution and cosmological mass density of neutral gas: Sloan Digital Sky Survey-III Data Release 9 (2012, methodology): “Given the sensitivity of current radio telescopes, this technique remains limited to z ≤ 0.2 (e.g. Lah et al. 2007).”
MEASUREMENT OF 21 cm BRIGHTNESS FLUCTUATIONS AT z ∼ 0.8 IN CROSS-CORRELATION (2012, background): “…redshifts are more difficult to measure, and estimates based on Mg-II lines in DLA systems observed with Hubble Space Telescope find ΩHI(z ∼ 1) ≈ (0.97 ± 0.36) × 10−3 (Rao et al. 2006), in rough agreement withz ≈ 0.2 DLA measurements (Meiring et al. 2011) and 21 cm stacking (Lah et al. 2007).”
Ingredients for 21 cm Intensity Mapping (2018, methodology): “In this plot we also indicate measurements from different observations (Zwaan & Prochaska 2006; Rao et al. 2006; Lah et al. 2007; Songaila & Cowie 2010; Martin et al. 2010; Noterdaeme et al. 2012; Braun 2012; Rhee et al. 2013; Delhaize et al. 2013; Crighton et al. 2015).”
Science with ASKAP (2008, background): “04 ∼ z ∼ 1 because of insufficient sensitivity of current-generation radio telescopes (though see [165]), and so next generation telescopes such as ASKAP and ultimately the SKA will be required.”
The enrichment of the intergalactic medium with adiabatic feedback – I. Metal cooling and metal diffusion (2009, background): “…of damped Ly-α systems (DLAs) (Prochaska et al. 2005; Rao et al. 2006; Prochaska & Wolfe 2009) and the H I 21-cm emissions (Zwaan et al. 2005; Lah et al. 2007) (shown in Figure 3) suggest that ΩHI does not evolve substantially through cosmic time, even though the stellar mass density keeps…”
Cosmic evolution of the atomic and molecular gas contents of galaxies (2011, methodology): “The first measurements will come from stacking of stellar mass- or SFRselected galaxy samples, as has been done in the local Universe (e.g. Verheijen et al. 2007; Lah et al. 2007, 2009).”
The ESO UVES advanced data products quasar sample: II. Cosmological evolution of the neutral gas mass density (2013, background): “The measurement atz = 0.24 comes from the radio observations of star-forming galaxies (Lah et al. 2007).”
Evolution of the cosmological mass density of neutral gas from Sloan Digital Sky Survey II - Data Release 7 (2009, background): “However, the limited sensitivity of current radio telescopes prevents direct detectionsof H i emission beyondz ∼ 0.2 (Lah et al. 2007; Verheijen et al. 2007; Catinella et al. 2008).”