CHILES. IX. Observational and Simulated H i Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments

Nicholas M. Luber; Farhanul Hasan; J. H. van Gorkom; D. J. Pisano; Joseph N. Burchett; Julia Blue Bird; Hansung B. Gim; Kelley M. Hess; Lucas R. Hunt; David C. Koo; Sushma Kurapati; Danielle Lucero; Nir Mandelker; Martin Meyer; Emmanuel Momjian; Daisuke Nagai; Joel R. Primack; Min S. Yun

doi:10.3847/1538-4357/adc448

CHILES. IX. Observational and Simulated H i Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments

Nicholas M. Luber^*, Farhanul Hasan, J. H. van Gorkom, D. J. Pisano, Joseph N. Burchett, Julia Blue Bird, Hansung B. Gim, Kelley M. Hess, Lucas R. Hunt, David C. Koo, Sushma Kurapati, Danielle Lucero, Nir Mandelker, Martin Meyer, Emmanuel Momjian, Daisuke Nagai, Joel R. Primack, Min S. Yun

^*Corresponding author for this work

Racah Institute of Physics

Research output: Contribution to journal › Article › peer-review

1 Scopus citations

Abstract

We examine the redshift evolution of the relationship between the neutral atomic hydrogen (H i) content and star formation properties of blue galaxies, along with their location in the cosmic web. Using the COSMOS H i Large Extragalactic Survey (CHILES) and the IllustrisTNG (TNG100) cosmological simulation, and the DisPerSE algorithm, we identify the filamentary structure in both observations and simulations, measure the distance of galaxies to the nearest filament spine D_fil, and calculate the mean H i gas fraction and the relative specific star formation rate (sSFR) of blue galaxies in three different cosmic web environments—0 < D_fil/Mpc < 2 (filament cores), 2 < D_fil/Mpc < 4 (filament outskirts), and 4 < D_fil/Mpc < 20 (voids). We find that, although there are some similarities between CHILES and TNG, there exist significant discrepancies in the dependence of H i and star formation on the cosmic web and on redshift. TNG overpredicts the observed H i fraction and relative sSFR at z = 0-0.5, with the tension being strongest in the voids. CHILES observes a decline in the H i fraction from filament cores to voids, exactly the opposite of the trend predicted by TNG. CHILES observes an increase in H i fraction at z = 0.5 → 0 in the voids, while TNG predicts an increase in this time in all environments. Further dividing the sample into stellar mass bins, we find that the H i in log ( M_*/M_⊙) > 10 galaxies is better reproduced by TNG than H i in log ( M_*/ M_⊙) = 9 − 10 galaxies.

Original language	English
Article number	214
Journal	Astrophysical Journal
Volume	985
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/adc448
State	Published - 1 Jun 2025

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© 2025. The Author(s). Published by the American Astronomical Society.

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Luber, N. M., Hasan, F., van Gorkom, J. H., Pisano, D. J., Burchett, J. N., Bird, J. B., Gim, H. B., Hess, K. M., Hunt, L. R., Koo, D. C., Kurapati, S., Lucero, D., Mandelker, N., Meyer, M., Momjian, E., Nagai, D., Primack, J. R., & Yun, M. S. (2025). CHILES. IX. Observational and Simulated H i Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments. Astrophysical Journal, 985(2), Article 214. https://doi.org/10.3847/1538-4357/adc448

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title = "CHILES. IX. Observational and Simulated H i Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments",

abstract = "We examine the redshift evolution of the relationship between the neutral atomic hydrogen (H i) content and star formation properties of blue galaxies, along with their location in the cosmic web. Using the COSMOS H i Large Extragalactic Survey (CHILES) and the IllustrisTNG (TNG100) cosmological simulation, and the DisPerSE algorithm, we identify the filamentary structure in both observations and simulations, measure the distance of galaxies to the nearest filament spine Dfil, and calculate the mean H i gas fraction and the relative specific star formation rate (sSFR) of blue galaxies in three different cosmic web environments—0 < Dfil/Mpc < 2 (filament cores), 2 < Dfil/Mpc < 4 (filament outskirts), and 4 < Dfil/Mpc < 20 (voids). We find that, although there are some similarities between CHILES and TNG, there exist significant discrepancies in the dependence of H i and star formation on the cosmic web and on redshift. TNG overpredicts the observed H i fraction and relative sSFR at z = 0-0.5, with the tension being strongest in the voids. CHILES observes a decline in the H i fraction from filament cores to voids, exactly the opposite of the trend predicted by TNG. CHILES observes an increase in H i fraction at z = 0.5 → 0 in the voids, while TNG predicts an increase in this time in all environments. Further dividing the sample into stellar mass bins, we find that the H i in log ( M*/M⊙) > 10 galaxies is better reproduced by TNG than H i in log ( M*/ M⊙) = 9 − 10 galaxies.",

author = "Luber, {Nicholas M.} and Farhanul Hasan and {van Gorkom}, {J. H.} and Pisano, {D. J.} and Burchett, {Joseph N.} and Bird, {Julia Blue} and Gim, {Hansung B.} and Hess, {Kelley M.} and Hunt, {Lucas R.} and Koo, {David C.} and Sushma Kurapati and Danielle Lucero and Nir Mandelker and Martin Meyer and Emmanuel Momjian and Daisuke Nagai and Primack, {Joel R.} and Yun, {Min S.}",

note = "Publisher Copyright: {\textcopyright} 2025. The Author(s). Published by the American Astronomical Society.",

year = "2025",

month = jun,

day = "1",

doi = "10.3847/1538-4357/adc448",

language = "אנגלית",

volume = "985",

journal = "Astrophysical Journal",

issn = "0004-637X",

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Luber, NM, Hasan, F, van Gorkom, JH, Pisano, DJ, Burchett, JN, Bird, JB, Gim, HB, Hess, KM, Hunt, LR, Koo, DC, Kurapati, S, Lucero, D, Mandelker, N, Meyer, M, Momjian, E, Nagai, D, Primack, JR & Yun, MS 2025, 'CHILES. IX. Observational and Simulated H i Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments', Astrophysical Journal, vol. 985, no. 2, 214. https://doi.org/10.3847/1538-4357/adc448

TY - JOUR

T1 - CHILES. IX. Observational and Simulated H i Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments

AU - Luber, Nicholas M.

AU - Hasan, Farhanul

AU - van Gorkom, J. H.

AU - Pisano, D. J.

AU - Burchett, Joseph N.

AU - Bird, Julia Blue

AU - Gim, Hansung B.

AU - Hess, Kelley M.

AU - Hunt, Lucas R.

AU - Koo, David C.

AU - Kurapati, Sushma

AU - Lucero, Danielle

AU - Mandelker, Nir

AU - Meyer, Martin

AU - Momjian, Emmanuel

AU - Nagai, Daisuke

AU - Primack, Joel R.

AU - Yun, Min S.

PY - 2025/6/1

Y1 - 2025/6/1

N2 - We examine the redshift evolution of the relationship between the neutral atomic hydrogen (H i) content and star formation properties of blue galaxies, along with their location in the cosmic web. Using the COSMOS H i Large Extragalactic Survey (CHILES) and the IllustrisTNG (TNG100) cosmological simulation, and the DisPerSE algorithm, we identify the filamentary structure in both observations and simulations, measure the distance of galaxies to the nearest filament spine Dfil, and calculate the mean H i gas fraction and the relative specific star formation rate (sSFR) of blue galaxies in three different cosmic web environments—0 < Dfil/Mpc < 2 (filament cores), 2 < Dfil/Mpc < 4 (filament outskirts), and 4 < Dfil/Mpc < 20 (voids). We find that, although there are some similarities between CHILES and TNG, there exist significant discrepancies in the dependence of H i and star formation on the cosmic web and on redshift. TNG overpredicts the observed H i fraction and relative sSFR at z = 0-0.5, with the tension being strongest in the voids. CHILES observes a decline in the H i fraction from filament cores to voids, exactly the opposite of the trend predicted by TNG. CHILES observes an increase in H i fraction at z = 0.5 → 0 in the voids, while TNG predicts an increase in this time in all environments. Further dividing the sample into stellar mass bins, we find that the H i in log ( M*/M⊙) > 10 galaxies is better reproduced by TNG than H i in log ( M*/ M⊙) = 9 − 10 galaxies.

AB - We examine the redshift evolution of the relationship between the neutral atomic hydrogen (H i) content and star formation properties of blue galaxies, along with their location in the cosmic web. Using the COSMOS H i Large Extragalactic Survey (CHILES) and the IllustrisTNG (TNG100) cosmological simulation, and the DisPerSE algorithm, we identify the filamentary structure in both observations and simulations, measure the distance of galaxies to the nearest filament spine Dfil, and calculate the mean H i gas fraction and the relative specific star formation rate (sSFR) of blue galaxies in three different cosmic web environments—0 < Dfil/Mpc < 2 (filament cores), 2 < Dfil/Mpc < 4 (filament outskirts), and 4 < Dfil/Mpc < 20 (voids). We find that, although there are some similarities between CHILES and TNG, there exist significant discrepancies in the dependence of H i and star formation on the cosmic web and on redshift. TNG overpredicts the observed H i fraction and relative sSFR at z = 0-0.5, with the tension being strongest in the voids. CHILES observes a decline in the H i fraction from filament cores to voids, exactly the opposite of the trend predicted by TNG. CHILES observes an increase in H i fraction at z = 0.5 → 0 in the voids, while TNG predicts an increase in this time in all environments. Further dividing the sample into stellar mass bins, we find that the H i in log ( M*/M⊙) > 10 galaxies is better reproduced by TNG than H i in log ( M*/ M⊙) = 9 − 10 galaxies.

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JO - Astrophysical Journal

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ER -

CHILES. IX. Observational and Simulated H i Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments

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