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

Kanekar, Nissim; Sethi, Shiv K.; Dwarakanath, K. S.

doi:10.3847/2041-8205/818/2/l28

Cited by 66 publications

(82 citation statements)

References 46 publications

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“…For the integrations here and below, we do not include the HI mass in galaxies with M * < 10 5 M ⊙ . Our value of Ω HI is consistent with that presented in Paper I ((4.02 ± 0.26) × 10 −4 h −1 70 ), although based on a slightly restricted sample and different technique, as well as with previous literature values determined using either HI stacking (Delhaize et al 2013;Lah et al 2007;Kanekar et al 2016;Rhee et al 2013Rhee et al , 2016Rhee et al , 2018 or 21-cm emission detections (Zwaan et al 2005;Martin et al 2010;Freudling et al 2011;Hoppmann et al 2015;Jones et al 2018).…”

Section: Splitting Centrals and Satellitessupporting

confidence: 92%

“…The HI Parkes All-Sky Survey (HIPASS; Barnes et al 2001) has detected HI emission from 5,317 galaxies at 0 < z < 0.04 over a sky area of 21,341 deg 2 (Meyer et al 2004;Wong et al ⋆ Contact e-mail: wkhu@nao.cas.cn 2006), and the Arecibo Legacy Fast ALFA (ALFALFA) survey (Giovanelli et al 2005) has detected ∼ 31,500 galaxies out to z = 0.06 over a sky area of approximately 7,000 deg 2 . These large-area surveys allow for accurate measurement of the local HI mass function and the cosmic HI gas density (Zwaan et al 2005;Martin et al 2010;Jones et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…The cosmic HI gas density has also been successfully constrained at different redshifts (0.0−0.37) (Lah et al 2007;Delhaize et al 2013;Rhee et al 2013Rhee et al , 2016Rhee et al , 2018. In particular, Kanekar et al (2016) used the Giant Metrewave Radio Telescope (GMRT) to stack HI emission from massive star-forming galaxies at z ∼ 1.18 − 1.34, the highest redshift measurement of HI flux ever made using HI spectral stacking.…”

Section: Introductionmentioning

confidence: 99%

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The cosmic atomic hydrogen mass density as a function of mass and galaxy hierarchy from spectral stacking

Catinella

Cortese

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use spectral stacking to measure the contribution of galaxies of different masses and in different hierarchies to the cosmic atomic hydrogen (HI) mass density in the local Universe. Our sample includes 1793 galaxies at z < 0.11 observed with the Westerbork Synthesis Radio Telescope, for which Sloan Digital Sky Survey spectroscopy and hierarchy information are also available. We find a cosmic HI mass density of Ω HI = (3.99 ± 0.54) × 10 −4 h −1 70 at z = 0.065. For the central and satellite galaxies, we obtain Ω HI of (3.51 ± 0.49) × 10 −4 h −1 70 and (0.90 ± 0.16) × 10 −4 h −1 70 , respectively. We show that galaxies above and below stellar masses of ∼10 9.3 M ⊙ contribute in roughly equal measure to the global value of Ω HI . While consistent with estimates based on targeted HI surveys, our results are in tension with previous theoretical work. We show that these differences are, at least partly, due to the empirical recipe used to set the partition between atomic and molecular hydrogen in semi-analytical models. Moreover, comparing our measurements with the cosmological semi-analytic models of galaxy formation S and GALFORM reveals gradual stripping of gas via ram pressure works better to fully reproduce the properties of satellite galaxies in our sample, than strangulation. Our findings highlight the power of this approach in constraining theoretical models, and confirm the non-negligible contribution of massive galaxies to the HI mass budget of the local Universe.At the same time, studies of the HI gas content of galax-

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Section: Splitting Centrals and Satellitessupporting

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The cosmic atomic hydrogen mass density as a function of mass and galaxy hierarchy from spectral stacking

Catinella

Cortese

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The highest redshift (z = 0.376) H i 21-cm emission detection to date (Fernández et al, 2016) has been possible due to very long integration (178 hours) using the Karl G. Jansky Very Large Array (VLA). Besides direct detection of H i 21-cm emission from galaxies, there have been several H i 21cm emission line stacking experiments which have studied the average H i properties of different samples of galaxies (Lah et al, 2007(Lah et al, , 2009Delhaize et al, 2013;Rhee et al, 2013Rhee et al, , 2018Kanekar et al, 2016). In addition to stacking, intensity mapping and cross-correlation of H i 21-cm emission with optical galaxy surveys (e.g.…”

Section: H I 21-cm Absorptionmentioning

confidence: 99%

Cold neutral hydrogen gas in galaxies

Dutta

2019

J Astrophys Astron

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This review summarizes recent studies of the cold neutral hydrogen gas associated with galaxies probed via the H i 21-cm absorption line. H i 21-cm absorption against background radio-loud quasars is a powerful tool to study the neutral gas distribution and kinematics in foreground galaxies from kilo-parsec to parsec scales. At low redshifts (z < 0.4), it has been used to characterize the distribution of high column density neutral gas around galaxies and study the connection of this gas with the galaxy's optical properties. The neutral gas around galaxies has been found to be patchy in distribution, with variations in optical depth observed at both kilo-parsec and parsec scales. At high redshifts (z > 0.5), H i 21-cm absorption has been used to study the neutral gas in metal or Lyman − α absorption-selected galaxies. It has been found to be closely linked with the metal and dust content of the gas. Trends of various properties like incidence, spin temperature and velocity width of H i 21-cm absorption with redshift have been studied, which imply evolution of cold gas properties in galaxies with cosmic time. Upcoming large blind surveys of H i 21-cm absorption with next generation radio telescopes are expected to determine accurately the redshift evolution of the number density of H i 21-cm absorbers per unit redshift and hence understand what drives the global star formation rate density evolution.

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“…The spin temperature in turn is determined by coupling with atoms, electrons and Lyman-α line radiation (Wouthuysen, 1952b,a;Purcell & Field, 1956;Furlanetto, Oh, & Briggs, 2006). At intermediate redshifts, techniques such as co-adding (Chengalur, Braun, & Wieringa, 2001;Zwaan, 2000;Lah et al, 2007;Rhee et al, 2013;Delhaize et al, 2013;Rhee et al, 2016;Kanekar, Sethi, & Dwarakanath, 2016) and cross-correlation (Chang et al, 2010;Masui et al, 2013) have been used to detect neutral Hydrogen. As we get to even higher redshifts, statistical detection is the only viable approach for observing the large scale distribution of HI.…”

Section: Methodsmentioning

confidence: 99%

Prospects of Detecting HI using Redshifted 21-cm Radiation at z∼3

Gehlot

Bagla

2017

J Astrophys Astron

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Distribution of cold gas in the post-reionization era provides an important link between distribution of galaxies and the process of star formation. Redshifted 21 cm radiation from the Hyperfine transition of neutral Hydrogen allows us to probe the neutral component of cold gas, most of which is to be found in the interstellar medium of galaxies. Existing and upcoming radio telescopes can probe the large scale distribution of neutral Hydrogen via HI intensity mapping. In this paper we use an estimate of the HI power spectrum derived using an ansatz to compute the expected signal from the large scale HI distribution at z ∼ 3. We find that the scale dependence of bias at small scales makes a significant difference to the expected signal even at large angular scales. We compare the predicted signal strength with the sensitivity of radio telescopes that can observe such radiation and calculate the observation time required for detecting neutral Hydrogen at these redshifts. We find that OWFA (Ooty Wide Field Array) offers the best possibility to detect neutral Hydrogen at z ∼ 3 before the SKA (Square Kilometer Array) becomes operational. We find that the OWFA should be able to make a 3 σ or a more significant detection in 2000 hours of observations at several angular scales. Calculations done using the Fisher matrix approach indicate that a 5σ detection of the binned HI power spectrum via measurement of the amplitude of the HI power spectrum is possible in 1000 hours (Sarkar, Bharadwaj and Ali, 2017).

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

Cited by 66 publications

References 46 publications

The cosmic atomic hydrogen mass density as a function of mass and galaxy hierarchy from spectral stacking

The cosmic atomic hydrogen mass density as a function of mass and galaxy hierarchy from spectral stacking

Cold neutral hydrogen gas in galaxies

Prospects of Detecting HI using Redshifted 21-cm Radiation at z∼3

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