HIGHEST REDSHIFT IMAGE OF NEUTRAL HYDROGEN IN EMISSION: A CHILES DETECTION OF A STARBURSTING GALAXY AT z = 0.376

Fernández, Ximena; Gim, Hansung B.; Gorkom, J. H. van; Yun, Min S.; Momjian, Emmanuel; Popping, Attila; Chomiuk, Laura; Hess, Kelley M.; Hunt, Lucas; Kreckel, Kathryn; Lucero, D. M.; Maddox, Natasha; Oosterloo, Tom; Pisano, D. J.; Verheijen, Marc; Hales, C. A.; Chung, Aeree; Dodson, Richard; Golap, K.; Gross, Julia; Henning, P. A.; Hibbard, J. E.; Jaffé, Yara L.; Meyer, Jennifer Donovan; Meyer, Martin; Sanchez-Barrantes, Monica; Schiminovich, David; Wicenec, A.; Wilcots, Eric M.; Bershady, Matthew A.; Scoville, N.; Strader, Jay; Tremou, Evangelia; Salinas, R.; Chávez, Ricardo

doi:10.3847/2041-8205/824/1/l1

Cited by 128 publications

(73 citation statements)

References 51 publications

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“…This is in good agreement with cosmological simulations that predict the most massive galaxies to be in dense environments. The two most isolated galaxies have very extended HI and a relatively low star formation rate, in good agreement with what has been found in surveys of void galaxies (Kreckel et al 2012) The CHILES collaboration recently published the detection of neutral hydrogen in a star-bursting galaxy at redshift z = 0.376, COSMOS J100054.83+023126.2, the highest redshift HI emission detection to date (Fernández et al 2016). Figure 1b of Fernández et al (2016) shows that the HI morphology is asymmetric within the galaxy and very extended to the south.…”

Section: Preliminary Hi Resultssupporting

confidence: 81%

Large-scale Structure in CHILES Using DisPerSE

Luber

Gorkom

Hess

et al. 2019

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We demonstrate that the Discrete Persistent Source Extractor (DisPerSE) can be used with spectroscopic redshifts to define the cosmic web and its distance to galaxies in small area deepfields. Here we analyze the use of DisPerSE to identify structure in observational data. We apply DisPerSE to the distribution of galaxies in the COSMOS field and find the best parameters to identify filaments. We compile a catalog of 11500 spectroscopic redshifts from the Galaxy and Mass Assembly (GAMA) G10 data release. We analyze two-dimensional slices, extract filaments and calculate the distance for each galaxy to its nearest filament. We find that redder and more massive galaxies are closer to filaments. To study the growth of galaxies across cosmic time, and environment, we are carrying out an HI survey covering redshifts z = 0 -0.45, the COSMOS HI Large Extragalactic Survey (CHILES). In addition we present the predicted HI mass fraction as a function of distance to filaments for the spectroscopically known galaxies in CHILES. Lastly, we discuss the cold gas morphology of a few individual galaxies and their positions with respect to the cosmic web. The identification of the cosmic web, and the ability of CHILES to study the resolved neutral hydrogen morphologies and kinematics of galaxies, will allow future studies of the properties of neutral hydrogen in different cosmic web environments across the redshift range z = 0.1 -0.45.

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Section: Preliminary Hi Resultssupporting

confidence: 81%

Large-scale Structure in CHILES Using DisPerSE

Luber

Gorkom

Hess

et al. 2019

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“…Beyond the local Universe, HI emission has been detected from galaxies up to z ∼ 0.3 with deep integrations (Zwaan et al 2001;Verheijen et al 2007;Catinella et al 2008;Fernández et al 2016). The ongoing COSMOS HI Large Extragalactic Survey (CHILES) with the upgraded Jansky Very Large Array is imaging HI over the z = 0− 0.45 redshift interval and holds the current record for the highest-redshift HI emission detection at z = 0.376 (Fernández et al 2016).…”

Section: Introductionmentioning

confidence: 92%

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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“…For example, the Arecibo Ultra Deep Survey (AUDS) (Freudling et al 2011;Hoppmann et al 2015) has so-far detected 103 galaxies with 400 hrs of integration time in the redshift range of 0 < z < 0.16. The Cosmological Evolution Survey (COSMOS) HI Large Extragalactic Survey (CHILES) over the redshift range z = 0 -0.45 (Fernández et al 2013;Fernández et al 2016) will be able to detect up to 300 galaxies with 1000 hours of observation time on the Very Large Array (VLA). However, even with such large integration times, these surveys have been limited to very small sky areas (1.35 deg 2 for AUDS and 0.3 deg 2 for CHILES), resulting in small effective volumes and large cosmic variance.…”

Section: Introductionmentioning

confidence: 99%

An accurate low-redshift measurement of the cosmic neutral hydrogen density

Hoppmann

Staveley‐Smith

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using a spectral stacking technique, we measure the neutral hydrogen (HI) properties of a sample of galaxies at z < 0.11 across 35 pointings of the Westerbork Synthesis Radio Telescope (WSRT). The radio data contains 1,895 galaxies with redshifts and positions known from the Sloan Digital Sky Survey (SDSS). We carefully quantified the effects of sample bias, aperture used to extract spectra, sidelobes and weighting technique and use our data to provide a new estimate for the cosmic HI mass density. We find a cosmic HI mass density of Ω HI = (4.02 ± 0.26) × 10 −4 h −1 70 at z = 0.066, consistent with measurements from blind HI surveys and other HI stacking experiments at low redshifts. The combination of the small interferometer beam size and the large survey volume makes our result highly robust against systematic effects due to confusion at small scales and cosmic variance at large scales. Splitting into three sub-samples with z = 0.038, 0.067 and 0.093 shows no significant evolution of the HI gas content at low redshift.

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HIGHEST REDSHIFT IMAGE OF NEUTRAL HYDROGEN IN EMISSION: A CHILES DETECTION OF A STARBURSTING GALAXY AT z = 0.376

Cited by 128 publications

References 51 publications

Large-scale Structure in CHILES Using DisPerSE

Large-scale Structure in CHILES Using DisPerSE

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

An accurate low-redshift measurement of the cosmic neutral hydrogen density

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