Studying [C ii] emission in low-mass galaxies at z ∼ 7

Kelsey Glazer; Maruša Bradǎc; Ryan L. Sanders; Seiji Fujimoto; Patricia Bolan; Andrea Ferrara; Victoria Strait; Tucker Jones; Brian C. Lemaux; Livia Vallini; Russell Ryan

doi:10.1093/mnras/stae1178

Studying [C ii] emission in low-mass galaxies at z ∼ 7

Kelsey Glazer, Maruša Bradǎc, Ryan L. Sanders, Seiji Fujimoto, Patricia Bolan, Andrea Ferrara, Victoria Strait, Tucker Jones, Brian C. Lemaux, Livia Vallini, Russell Ryan

Physics And Astronomy

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

5 Scopus citations

Abstract

We report on a [CII] 158 μm search using the Atacama Large Millimeter/submillimeter Array (ALMA) on three lensed, confirmed Ly αemitting galaxies at z 7. Our targets are ultraviolet (UV) faint systems with stellar masses on the order of M 10 9 M. We detect a single [C II ] line emission (4 σ) from the brightest ( L 2.4 ×10 10 L) galaxy in our sample, MACS0454- 1251. We determine a systemic redshift ( z [C II ] = 6.3151 ±0.0005) for MACS0454-1251 and measure a Ly αvelocity offset of v ≈300 ±70 km s −1 . The remaining two galaxies we detect no [C II ] but provide 3 σupper limits on their [C II ] line luminosities which we use to investigate the L [CII] −SFR relation. Overall our single [C II ] detection shows agreement with the relation for local dwarf galaxies. Our [C II ] deficient galaxies could potentially be exhibiting low metallicities ( Z < Z). Another possible explanation for weaker [C II ] emission could be strong feedback from star formation disrupting molecular clouds. We do not detect continuum emission in any of the sources, placing upper limits on their dust masses. Assuming a single dust temperature of T d = 35K dust masses ( M dust ) range from < 4.8 ×10 7 M to 2.3 ×10 8 M. Collectively, our results suggest faint reionization era sources could be metal poor and/or could have strong feedback suppressing [C II ] emission..

Original language	English
Pages (from-to)	945-952
Number of pages	8
Journal	Monthly Notices of the Royal Astronomical Society
Volume	531
Issue number	1
DOIs	https://doi.org/10.1093/mnras/stae1178
State	Published - Jun 1 2024

Bibliographical note

Publisher Copyright:
© 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

Funding

We acknowledge support from the program HST-GO-16667, provided through a grant from the STScI under NASA contract NAS5-26555. MB also acknowledges support from the ERC Advanced Grant FIRSTLIGHT and Slovenian national research agency ARRS through grants N1-0238 and P1-0188. RLS acknowledges support provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51469.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120.

Funders	Funder number
Engineering Research Centers
FIRSTLIGHT
Slovenian national research agency ARRS	N1-0238, P1-0188
Space Telescope Science Institute	INTERSTELLAR H2020/740120
National Aeronautics and Space Administration	NAS5-26555
Horizon 2020 Framework Programme	740120

Keywords

galaxies
gravitational lensing
high-redshift
strong

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/stae1178

Cite this

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title = "Studying [C ii] emission in low-mass galaxies at z ∼ 7",

abstract = "We report on a [CII] 158 μm search using the Atacama Large Millimeter/submillimeter Array (ALMA) on three lensed, confirmed Ly αemitting galaxies at z 7. Our targets are ultraviolet (UV) faint systems with stellar masses on the order of M 10 9 M. We detect a single [C II ] line emission (4 σ) from the brightest ( L 2.4 ×10 10 L) galaxy in our sample, MACS0454- 1251. We determine a systemic redshift ( z [C II ] = 6.3151 ±0.0005) for MACS0454-1251 and measure a Ly αvelocity offset of v ≈300 ±70 km s −1 . The remaining two galaxies we detect no [C II ] but provide 3 σupper limits on their [C II ] line luminosities which we use to investigate the L [CII] −SFR relation. Overall our single [C II ] detection shows agreement with the relation for local dwarf galaxies. Our [C II ] deficient galaxies could potentially be exhibiting low metallicities ( Z < Z). Another possible explanation for weaker [C II ] emission could be strong feedback from star formation disrupting molecular clouds. We do not detect continuum emission in any of the sources, placing upper limits on their dust masses. Assuming a single dust temperature of T d = 35K dust masses ( M dust ) range from < 4.8 ×10 7 M to 2.3 ×10 8 M. Collectively, our results suggest faint reionization era sources could be metal poor and/or could have strong feedback suppressing [C II ] emission..",

keywords = "galaxies, gravitational lensing, high-redshift, strong",

author = "Kelsey Glazer and Maru{\v s}a Bradǎc and Sanders, \{Ryan L.\} and Seiji Fujimoto and Patricia Bolan and Andrea Ferrara and Victoria Strait and Tucker Jones and Lemaux, \{Brian C.\} and Livia Vallini and Russell Ryan",

note = "Publisher Copyright: {\textcopyright} 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2024",

month = jun,

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doi = "10.1093/mnras/stae1178",

language = "English",

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T1 - Studying [C ii] emission in low-mass galaxies at z ∼ 7

AU - Glazer, Kelsey

AU - Bradǎc, Maruša

AU - Sanders, Ryan L.

AU - Fujimoto, Seiji

AU - Bolan, Patricia

AU - Ferrara, Andrea

AU - Strait, Victoria

AU - Jones, Tucker

AU - Lemaux, Brian C.

AU - Vallini, Livia

AU - Ryan, Russell

PY - 2024/6/1

Y1 - 2024/6/1

N2 - We report on a [CII] 158 μm search using the Atacama Large Millimeter/submillimeter Array (ALMA) on three lensed, confirmed Ly αemitting galaxies at z 7. Our targets are ultraviolet (UV) faint systems with stellar masses on the order of M 10 9 M. We detect a single [C II ] line emission (4 σ) from the brightest ( L 2.4 ×10 10 L) galaxy in our sample, MACS0454- 1251. We determine a systemic redshift ( z [C II ] = 6.3151 ±0.0005) for MACS0454-1251 and measure a Ly αvelocity offset of v ≈300 ±70 km s −1 . The remaining two galaxies we detect no [C II ] but provide 3 σupper limits on their [C II ] line luminosities which we use to investigate the L [CII] −SFR relation. Overall our single [C II ] detection shows agreement with the relation for local dwarf galaxies. Our [C II ] deficient galaxies could potentially be exhibiting low metallicities ( Z < Z). Another possible explanation for weaker [C II ] emission could be strong feedback from star formation disrupting molecular clouds. We do not detect continuum emission in any of the sources, placing upper limits on their dust masses. Assuming a single dust temperature of T d = 35K dust masses ( M dust ) range from < 4.8 ×10 7 M to 2.3 ×10 8 M. Collectively, our results suggest faint reionization era sources could be metal poor and/or could have strong feedback suppressing [C II ] emission..

AB - We report on a [CII] 158 μm search using the Atacama Large Millimeter/submillimeter Array (ALMA) on three lensed, confirmed Ly αemitting galaxies at z 7. Our targets are ultraviolet (UV) faint systems with stellar masses on the order of M 10 9 M. We detect a single [C II ] line emission (4 σ) from the brightest ( L 2.4 ×10 10 L) galaxy in our sample, MACS0454- 1251. We determine a systemic redshift ( z [C II ] = 6.3151 ±0.0005) for MACS0454-1251 and measure a Ly αvelocity offset of v ≈300 ±70 km s −1 . The remaining two galaxies we detect no [C II ] but provide 3 σupper limits on their [C II ] line luminosities which we use to investigate the L [CII] −SFR relation. Overall our single [C II ] detection shows agreement with the relation for local dwarf galaxies. Our [C II ] deficient galaxies could potentially be exhibiting low metallicities ( Z < Z). Another possible explanation for weaker [C II ] emission could be strong feedback from star formation disrupting molecular clouds. We do not detect continuum emission in any of the sources, placing upper limits on their dust masses. Assuming a single dust temperature of T d = 35K dust masses ( M dust ) range from < 4.8 ×10 7 M to 2.3 ×10 8 M. Collectively, our results suggest faint reionization era sources could be metal poor and/or could have strong feedback suppressing [C II ] emission..

KW - galaxies

KW - gravitational lensing

KW - high-redshift

KW - strong

UR - https://www.scopus.com/pages/publications/85193990735

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U2 - 10.1093/mnras/stae1178

DO - 10.1093/mnras/stae1178

M3 - Article

AN - SCOPUS:85193990735

SN - 0035-8711

VL - 531

SP - 945

EP - 952

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Studying [C ii] emission in low-mass galaxies at z ∼ 7

Abstract

Bibliographical note

Funding

Keywords

ASJC Scopus subject areas

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