Chiles: H I morphology and galaxy environment at z = 0.12 and z = 0.17

Kelley M. Hess; Nicholas M. Luber; Ximena Fernández; Hansung B. Gim; J. H. Van Gorkom; Emmanuel Momjian; Julia Gross; Martin Meyer; Attila Popping; Luke J.M. Davies; Lucas Hunt; Kathryn Kreckel; Danielle Lucero; D. J. Pisano; Monica Sanchez-Barrantes; Min S. Yun; Richard Dodson; Kevin Vinsen; Andreas Wicenec; Chen Wu; Matthew A. Bershady; Aeree Chung; Julie D. Davis; Jennifer Donovan Meyer; Patricia Henning; Natasha Maddox; Evan T. Smith; J. M. Van Der Hulst; Marc A.W. Verheijen; Eric M. Wilcots

doi:10.1093/mnras/sty3421

Chiles: H I morphology and galaxy environment at z = 0.12 and z = 0.17

Kelley M. Hess, Nicholas M. Luber, Ximena Fernández, Hansung B. Gim, J. H. Van Gorkom, Emmanuel Momjian, Julia Gross, Martin Meyer, Attila Popping, Luke J.M. Davies, Lucas Hunt, Kathryn Kreckel, Danielle Lucero, D. J. Pisano, Monica Sanchez-Barrantes, Min S. Yun, Richard Dodson, Kevin Vinsen, Andreas Wicenec, Chen WuMatthew A. Bershady, Aeree Chung, Julie D. Davis, Jennifer Donovan Meyer, Patricia Henning, Natasha Maddox, Evan T. Smith, J. M. Van Der Hulst, Marc A.W. Verheijen, Eric M. Wilcots

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21 Citations (Scopus)

Abstract

We present a study of 16 H I-detected galaxies found in 178 h of observations from Epoch 1 of the COSMOS H I Large Extragalactic Survey (CHILES). We focus on two redshift ranges between 0.108 ≤ z ≤ 0.127 and 0.162 ≤ z ≤ 0.183 which are among the worst affected by radio frequency interference (RFI). While this represents only 10 per cent of the total frequency coverage and 18 per cent of the total expected time on source compared to what will be the full CHILES survey, we demonstrate that our data reduction pipeline recovers high-quality data even in regions severely impacted by RFI. We report on our in-depth testing of an automated spectral line source finder to produce H I total intensity maps which we present side-by-side with significance maps to evaluate the reliability of the morphology recovered by the source finder. We recommend that this become a common place manner of presenting data from upcoming H I surveys of resolved objects. We use the COSMOS 20k group catalogue and extract the filamentary structure using the topological DisPerSE algorithm to evaluate the H I morphology in the context of both local and large-scale environments and we discuss the shortcomings of both methods. Many of the detections show disturbed H I morphologies suggesting they have undergone a recent interaction which is not evident from deep optical imaging alone. Overall, the sample showcases the broad range of ways in which galaxies interact with their environment. This is a first look at the population of galaxies and their local and large-scale environments observed in H I by CHILES at redshifts beyond the z = 0.1 Universe.

Original language	English
Pages (from-to)	2234-2256
Number of pages	23
Journal	Monthly Notices of the Royal Astronomical Society
Volume	484
Issue number	2
DOIs	https://doi.org/10.1093/mnras/sty3421
Publication status	Published - 2019 Apr 1

Bibliographical note

Funding Information:
The research of K.M.H. and J.M.v.d.H. are supported by the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement nr. 291531. CHILES is supported by National Science Foundation (NSF) grants AST-1413102, AST-1412578, AST-1412843, AST-1413099 and AST-1412503. X.F. is supported by an NSF-Astronomy and Astrophysics Postdoctoral Fellowship (AAPF) under award AST-1501342. Support for M.S.B. is provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. K.K. gratefully acknowledges support from grant KR 4598/1-2 from the DFG Priority Program 1573. We thank Tom Oosterloo for comments on an earlier version of this paper which have led to improvements. We thank the anonymous referee and the scientific editor for their comments which improved the quality of this paper.

Funding Information:
Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020.

Funding Information:
The research of K.M.H. and J.M.v.d.H. are supported by the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement nr. 291531. CHILES is supported by National Science Foundation (NSF) grants AST-1413102, AST-1412578, AST-1412843, AST-1413099 and AST-1412503. X.F. is supported by an NSF-Astronomy and Astrophysics Postdoctoral Fellowship (AAPF) under award AST-1501342. Support for M.S.B. is provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. K.K. gratefully acknowledges support from grant KR 4598/1-2 from the DFG Priority Program 1573. We thank Tom Oosterloo for comments on an earlier version of this paper which have led to improvements. We thank the anonymous referee and the scientific editor for their comments which improved the quality of this paper.

Publisher Copyright:
© 2018 The Author(s).

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/sty3421

Cite this

Hess, K. M., Luber, N. M., Fernández, X., Gim, H. B., Van Gorkom, J. H., Momjian, E., Gross, J., Meyer, M., Popping, A., Davies, L. J. M., Hunt, L., Kreckel, K., Lucero, D., Pisano, D. J., Sanchez-Barrantes, M., Yun, M. S., Dodson, R., Vinsen, K., Wicenec, A., ... Wilcots, E. M. (2019). Chiles: H I morphology and galaxy environment at z = 0.12 and z = 0.17. Monthly Notices of the Royal Astronomical Society, 484(2), 2234-2256. https://doi.org/10.1093/mnras/sty3421

@article{22b99b7762a7429bab1683b751371e0f,

title = "Chiles: H I morphology and galaxy environment at z = 0.12 and z = 0.17",

abstract = "We present a study of 16 H I-detected galaxies found in 178 h of observations from Epoch 1 of the COSMOS H I Large Extragalactic Survey (CHILES). We focus on two redshift ranges between 0.108 ≤ z ≤ 0.127 and 0.162 ≤ z ≤ 0.183 which are among the worst affected by radio frequency interference (RFI). While this represents only 10 per cent of the total frequency coverage and 18 per cent of the total expected time on source compared to what will be the full CHILES survey, we demonstrate that our data reduction pipeline recovers high-quality data even in regions severely impacted by RFI. We report on our in-depth testing of an automated spectral line source finder to produce H I total intensity maps which we present side-by-side with significance maps to evaluate the reliability of the morphology recovered by the source finder. We recommend that this become a common place manner of presenting data from upcoming H I surveys of resolved objects. We use the COSMOS 20k group catalogue and extract the filamentary structure using the topological DisPerSE algorithm to evaluate the H I morphology in the context of both local and large-scale environments and we discuss the shortcomings of both methods. Many of the detections show disturbed H I morphologies suggesting they have undergone a recent interaction which is not evident from deep optical imaging alone. Overall, the sample showcases the broad range of ways in which galaxies interact with their environment. This is a first look at the population of galaxies and their local and large-scale environments observed in H I by CHILES at redshifts beyond the z = 0.1 Universe.",

author = "Hess, {Kelley M.} and Luber, {Nicholas M.} and Ximena Fern{\'a}ndez and Gim, {Hansung B.} and {Van Gorkom}, {J. H.} and Emmanuel Momjian and Julia Gross and Martin Meyer and Attila Popping and Davies, {Luke J.M.} and Lucas Hunt and Kathryn Kreckel and Danielle Lucero and Pisano, {D. J.} and Monica Sanchez-Barrantes and Yun, {Min S.} and Richard Dodson and Kevin Vinsen and Andreas Wicenec and Chen Wu and Bershady, {Matthew A.} and Aeree Chung and Davis, {Julie D.} and Meyer, {Jennifer Donovan} and Patricia Henning and Natasha Maddox and Smith, {Evan T.} and {Van Der Hulst}, {J. M.} and Verheijen, {Marc A.W.} and Wilcots, {Eric M.}",

note = "Funding Information: The research of K.M.H. and J.M.v.d.H. are supported by the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement nr. 291531. CHILES is supported by National Science Foundation (NSF) grants AST-1413102, AST-1412578, AST-1412843, AST-1413099 and AST-1412503. X.F. is supported by an NSF-Astronomy and Astrophysics Postdoctoral Fellowship (AAPF) under award AST-1501342. Support for M.S.B. is provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. K.K. gratefully acknowledges support from grant KR 4598/1-2 from the DFG Priority Program 1573. We thank Tom Oosterloo for comments on an earlier version of this paper which have led to improvements. We thank the anonymous referee and the scientific editor for their comments which improved the quality of this paper. Funding Information: Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020. Funding Information: The research of K.M.H. and J.M.v.d.H. are supported by the European Research Council under the European Union{\textquoteright}s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement nr. 291531. CHILES is supported by National Science Foundation (NSF) grants AST-1413102, AST-1412578, AST-1412843, AST-1413099 and AST-1412503. X.F. is supported by an NSF-Astronomy and Astrophysics Postdoctoral Fellowship (AAPF) under award AST-1501342. Support for M.S.B. is provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. K.K. gratefully acknowledges support from grant KR 4598/1-2 from the DFG Priority Program 1573. We thank Tom Oosterloo for comments on an earlier version of this paper which have led to improvements. We thank the anonymous referee and the scientific editor for their comments which improved the quality of this paper. Publisher Copyright: {\textcopyright} 2018 The Author(s).",

year = "2019",

month = apr,

day = "1",

doi = "10.1093/mnras/sty3421",

language = "English",

volume = "484",

pages = "2234--2256",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

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}

Hess, KM, Luber, NM, Fernández, X, Gim, HB, Van Gorkom, JH, Momjian, E, Gross, J, Meyer, M, Popping, A, Davies, LJM, Hunt, L, Kreckel, K, Lucero, D, Pisano, DJ, Sanchez-Barrantes, M, Yun, MS, Dodson, R, Vinsen, K, Wicenec, A, Wu, C, Bershady, MA, Chung, A, Davis, JD, Meyer, JD, Henning, P, Maddox, N, Smith, ET, Van Der Hulst, JM, Verheijen, MAW & Wilcots, EM 2019, 'Chiles: H I morphology and galaxy environment at z = 0.12 and z = 0.17', Monthly Notices of the Royal Astronomical Society, vol. 484, no. 2, pp. 2234-2256. https://doi.org/10.1093/mnras/sty3421

TY - JOUR

T1 - Chiles

T2 - H I morphology and galaxy environment at z = 0.12 and z = 0.17

AU - Hess, Kelley M.

AU - Luber, Nicholas M.

AU - Fernández, Ximena

AU - Gim, Hansung B.

AU - Van Gorkom, J. H.

AU - Momjian, Emmanuel

AU - Gross, Julia

AU - Meyer, Martin

AU - Popping, Attila

AU - Davies, Luke J.M.

AU - Hunt, Lucas

AU - Kreckel, Kathryn

AU - Lucero, Danielle

AU - Pisano, D. J.

AU - Sanchez-Barrantes, Monica

AU - Yun, Min S.

AU - Dodson, Richard

AU - Vinsen, Kevin

AU - Wicenec, Andreas

AU - Wu, Chen

AU - Bershady, Matthew A.

AU - Chung, Aeree

AU - Davis, Julie D.

AU - Meyer, Jennifer Donovan

AU - Henning, Patricia

AU - Maddox, Natasha

AU - Smith, Evan T.

AU - Van Der Hulst, J. M.

AU - Verheijen, Marc A.W.

AU - Wilcots, Eric M.

N1 - Funding Information: The research of K.M.H. and J.M.v.d.H. are supported by the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement nr. 291531. CHILES is supported by National Science Foundation (NSF) grants AST-1413102, AST-1412578, AST-1412843, AST-1413099 and AST-1412503. X.F. is supported by an NSF-Astronomy and Astrophysics Postdoctoral Fellowship (AAPF) under award AST-1501342. Support for M.S.B. is provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. K.K. gratefully acknowledges support from grant KR 4598/1-2 from the DFG Priority Program 1573. We thank Tom Oosterloo for comments on an earlier version of this paper which have led to improvements. We thank the anonymous referee and the scientific editor for their comments which improved the quality of this paper. Funding Information: Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020. Funding Information: The research of K.M.H. and J.M.v.d.H. are supported by the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement nr. 291531. CHILES is supported by National Science Foundation (NSF) grants AST-1413102, AST-1412578, AST-1412843, AST-1413099 and AST-1412503. X.F. is supported by an NSF-Astronomy and Astrophysics Postdoctoral Fellowship (AAPF) under award AST-1501342. Support for M.S.B. is provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. K.K. gratefully acknowledges support from grant KR 4598/1-2 from the DFG Priority Program 1573. We thank Tom Oosterloo for comments on an earlier version of this paper which have led to improvements. We thank the anonymous referee and the scientific editor for their comments which improved the quality of this paper. Publisher Copyright: © 2018 The Author(s).

PY - 2019/4/1

Y1 - 2019/4/1

N2 - We present a study of 16 H I-detected galaxies found in 178 h of observations from Epoch 1 of the COSMOS H I Large Extragalactic Survey (CHILES). We focus on two redshift ranges between 0.108 ≤ z ≤ 0.127 and 0.162 ≤ z ≤ 0.183 which are among the worst affected by radio frequency interference (RFI). While this represents only 10 per cent of the total frequency coverage and 18 per cent of the total expected time on source compared to what will be the full CHILES survey, we demonstrate that our data reduction pipeline recovers high-quality data even in regions severely impacted by RFI. We report on our in-depth testing of an automated spectral line source finder to produce H I total intensity maps which we present side-by-side with significance maps to evaluate the reliability of the morphology recovered by the source finder. We recommend that this become a common place manner of presenting data from upcoming H I surveys of resolved objects. We use the COSMOS 20k group catalogue and extract the filamentary structure using the topological DisPerSE algorithm to evaluate the H I morphology in the context of both local and large-scale environments and we discuss the shortcomings of both methods. Many of the detections show disturbed H I morphologies suggesting they have undergone a recent interaction which is not evident from deep optical imaging alone. Overall, the sample showcases the broad range of ways in which galaxies interact with their environment. This is a first look at the population of galaxies and their local and large-scale environments observed in H I by CHILES at redshifts beyond the z = 0.1 Universe.

AB - We present a study of 16 H I-detected galaxies found in 178 h of observations from Epoch 1 of the COSMOS H I Large Extragalactic Survey (CHILES). We focus on two redshift ranges between 0.108 ≤ z ≤ 0.127 and 0.162 ≤ z ≤ 0.183 which are among the worst affected by radio frequency interference (RFI). While this represents only 10 per cent of the total frequency coverage and 18 per cent of the total expected time on source compared to what will be the full CHILES survey, we demonstrate that our data reduction pipeline recovers high-quality data even in regions severely impacted by RFI. We report on our in-depth testing of an automated spectral line source finder to produce H I total intensity maps which we present side-by-side with significance maps to evaluate the reliability of the morphology recovered by the source finder. We recommend that this become a common place manner of presenting data from upcoming H I surveys of resolved objects. We use the COSMOS 20k group catalogue and extract the filamentary structure using the topological DisPerSE algorithm to evaluate the H I morphology in the context of both local and large-scale environments and we discuss the shortcomings of both methods. Many of the detections show disturbed H I morphologies suggesting they have undergone a recent interaction which is not evident from deep optical imaging alone. Overall, the sample showcases the broad range of ways in which galaxies interact with their environment. This is a first look at the population of galaxies and their local and large-scale environments observed in H I by CHILES at redshifts beyond the z = 0.1 Universe.

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U2 - 10.1093/mnras/sty3421

DO - 10.1093/mnras/sty3421

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JO - Monthly Notices of the Royal Astronomical Society

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ER -

Chiles: H I morphology and galaxy environment at z = 0.12 and z = 0.17

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