A First Look at Spatially Resolved Balmer Decrements at 1.0 < z < 2.4 from JWST NIRISS Slitless Spectroscopy

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Bibliographic Details
Published inAstrophysical journal. Letters Vol. 949; no. 1; p. L11
Main Authors Matharu, Jasleen, Muzzin, Adam, Sarrouh, Ghassan T. E., Brammer, Gabriel, Abraham, Roberto, Asada, Yoshihisa, Bradač, Maruša, Desprez, Guillaume, Martis, Nicholas, Mowla, Lamiya, Noirot, Gaël, Sawicki, Marcin, Strait, Victoria, Willott, Chris J., Gould, Katriona M. L., Grindlay, Tess, Harshan, Anishya T.
Format Journal Article
LanguageEnglish
Published Austin The American Astronomical Society 01.05.2023
IOP
IOP Publishing
Subjects
Attenuation
Bins
Cosmic dust
Dust
Galaxies
Galaxy evolution
Galaxy stellar content
H alpha line
High-redshift galaxies
Occultation
Red shift
Shutters
Spatial distribution
Spectroscopy
Spectrum analysis
Star & galaxy formation
Star formation
Stellar mass
Surface brightness
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Abstract NRC publication: Yes
We present the first results on the spatial distribution of dust attenuation at 1.0 < z < 2.4 traced by the Balmer decrement, Hα/Hβ, in emission-line galaxies using deep JWST NIRISS slitless spectroscopy from the CAnadian NIRISS Unbiased Cluster Survey (CANUCS). Hα and Hβ emission-line maps of emission-line galaxies are extracted and stacked in bins of stellar mass for two grism redshift bins, 1.0 < zgrism < 1.7 and 1.7 < zgrism < 2.4. Surface brightness profiles for the Balmer decrement are measured and radial profiles of the dust attenuation toward Hα, AHα, are derived. In both redshift bins, the integrated Balmer decrement increases with stellar mass. Lower-mass (7.6 ,, Log(M*/Me) < 10.0) galaxies have centrally concentrated, negative dust attenuation profiles whereas higher-mass galaxies (10.0 ,, Log(M*/Me) < 11.1) have flat dust attenuation profiles. The total dust obscuration is mild, with on average 0.07 ± 0.07 and 0.14 ± 0.07 mag in the low- and high-redshift bins respectively. We model the typical light profiles of star-forming galaxies at these redshifts and stellar masses with GALFIT and apply both uniform and radially varying dust attenuation corrections based on our integrated Balmer decrements and radial dust attenuation profiles. If the Hα star formation rates (SFRs) of these galaxies were measured after slit-loss corrections assuming uniform dust attenuation with typical JWST NIRSpec slit spectroscopy (0 2 × 0 5 shutters), the total SFR will be overestimated by 6% ± 21% and 26% ± 9% at 1.0 ,, z < 1.7 and 1.7 ,, z < 2.4 respectively.
AbstractList We present the first results on the spatial distribution of dust attenuation at 1.0 < z < 2.4 traced by the Balmer decrement, H α /H β , in emission-line galaxies using deep JWST NIRISS slitless spectroscopy from the CAnadian NIRISS Unbiased Cluster Survey (CANUCS). H α  and H β  emission-line maps of emission-line galaxies are extracted and stacked in bins of stellar mass for two grism redshift bins, 1.0 < z grism < 1.7 and 1.7 < z grism < 2.4. Surface brightness profiles for the Balmer decrement are measured and radial profiles of the dust attenuation toward  H α , A H α , are derived. In both redshift bins, the integrated Balmer decrement increases with stellar mass. Lower-mass (7.6 ≤ Log( M * / M ⊙ ) < 10.0) galaxies have centrally concentrated, negative dust attenuation profiles whereas higher-mass galaxies (10.0 ≤ Log( M * / M ⊙ ) < 11.1) have flat dust attenuation profiles. The total dust obscuration is mild, with on average 0.07 ± 0.07 and 0.14 ± 0.07 mag in the low- and high-redshift bins respectively. We model the typical light profiles of star-forming galaxies at these redshifts and stellar masses with GALFIT and apply both uniform and radially varying dust attenuation corrections based on our integrated Balmer decrements and radial dust attenuation profiles. If the H α  star formation rates (SFRs) of these galaxies were measured after slit-loss corrections assuming uniform dust attenuation with typical JWST NIRSpec slit spectroscopy (0.″2 × 0.″5 shutters), the total SFR will be overestimated by 6% ± 21% and 26% ± 9% at 1.0 ≤ z < 1.7 and 1.7 ≤ z < 2.4 respectively.
NRC publication: Yes
We present the first results on the spatial distribution of dust attenuation at 1.0 < z < 2.4 traced by the Balmer decrement, Hα/Hβ, in emission-line galaxies using deep JWST NIRISS slitless spectroscopy from the CAnadian NIRISS Unbiased Cluster Survey (CANUCS). Hα and Hβ emission-line maps of emission-line galaxies are extracted and stacked in bins of stellar mass for two grism redshift bins, 1.0 < zgrism < 1.7 and 1.7 < zgrism < 2.4. Surface brightness profiles for the Balmer decrement are measured and radial profiles of the dust attenuation toward Hα, AHα, are derived. In both redshift bins, the integrated Balmer decrement increases with stellar mass. Lower-mass (7.6 ≤ Log(M*/M⊙) < 10.0) galaxies have centrally concentrated, negative dust attenuation profiles whereas higher-mass galaxies (10.0 ≤ Log(M*/M⊙) < 11.1) have flat dust attenuation profiles. The total dust obscuration is mild, with on average 0.07 ± 0.07 and 0.14 ± 0.07 mag in the low- and high-redshift bins respectively. We model the typical light profiles of star-forming galaxies at these redshifts and stellar masses with GALFIT and apply both uniform and radially varying dust attenuation corrections based on our integrated Balmer decrements and radial dust attenuation profiles. If the Hα star formation rates (SFRs) of these galaxies were measured after slit-loss corrections assuming uniform dust attenuation with typical JWST NIRSpec slit spectroscopy (0.″2 × 0.″5 shutters), the total SFR will be overestimated by 6% ± 21% and 26% ± 9% at 1.0 ≤ z < 1.7 and 1.7 ≤ z < 2.4 respectively.
We present the first results on the spatial distribution of dust attenuation at 1.0 < z < 2.4 traced by the Balmer decrement, H α /H β , in emission-line galaxies using deep JWST NIRISS slitless spectroscopy from the CAnadian NIRISS Unbiased Cluster Survey (CANUCS). H α  and H β  emission-line maps of emission-line galaxies are extracted and stacked in bins of stellar mass for two grism redshift bins, 1.0 < z _grism < 1.7 and 1.7 < z _grism < 2.4. Surface brightness profiles for the Balmer decrement are measured and radial profiles of the dust attenuation toward  H α , A _H _α , are derived. In both redshift bins, the integrated Balmer decrement increases with stellar mass. Lower-mass (7.6 ≤ Log( M _* / M _⊙ ) < 10.0) galaxies have centrally concentrated, negative dust attenuation profiles whereas higher-mass galaxies (10.0 ≤ Log( M _* / M _⊙ ) < 11.1) have flat dust attenuation profiles. The total dust obscuration is mild, with on average 0.07 ± 0.07 and 0.14 ± 0.07 mag in the low- and high-redshift bins respectively. We model the typical light profiles of star-forming galaxies at these redshifts and stellar masses with GALFIT and apply both uniform and radially varying dust attenuation corrections based on our integrated Balmer decrements and radial dust attenuation profiles. If the H α  star formation rates (SFRs) of these galaxies were measured after slit-loss corrections assuming uniform dust attenuation with typical JWST NIRSpec slit spectroscopy (0.″2 × 0.″5 shutters), the total SFR will be overestimated by 6% ± 21% and 26% ± 9% at 1.0 ≤ z < 1.7 and 1.7 ≤ z < 2.4 respectively.
Author Muzzin, Adam
Asada, Yoshihisa
Grindlay, Tess
Desprez, Guillaume
Harshan, Anishya T.
Mowla, Lamiya
Strait, Victoria
Noirot, Gaël
Sawicki, Marcin
Brammer, Gabriel
Gould, Katriona M. L.
Martis, Nicholas
Matharu, Jasleen
Willott, Chris J.
Abraham, Roberto
Sarrouh, Ghassan T. E.
Bradač, Maruša
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  organization: Kyoto University Department of Astronomy, Sakyo-ku, Kyoto 606-8502, Japan
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  organization: University of California Davis Department of Physics and Astronomy, 1 Shields Avenue, Davis, CA 95616, USA
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  surname: Desprez
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  organization: Saint Mary’s University Department of Astronomy and Physics and Institute for Computational Astrophysics, 923 Robie Street, Halifax, Nova Scotia, B3H 3C3, Canada
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  givenname: Nicholas
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  organization: National Research Council of Canada , Herzberg Astronomy & Astrophysics Research Centre, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
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  organization: Saint Mary’s University Department of Astronomy and Physics and Institute for Computational Astrophysics, 923 Robie Street, Halifax, Nova Scotia, B3H 3C3, Canada
– sequence: 12
  givenname: Marcin
  orcidid: 0000-0002-7712-7857
  surname: Sawicki
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  organization: Saint Mary’s University Department of Astronomy and Physics and Institute for Computational Astrophysics, 923 Robie Street, Halifax, Nova Scotia, B3H 3C3, Canada
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  givenname: Victoria
  orcidid: 0000-0002-6338-7295
  surname: Strait
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  organization: University of Copenhagen Niels Bohr Institute, Jagtvej 128, DK-2200 Copenhagen N, Denmark
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  givenname: Chris J.
  orcidid: 0000-0002-4201-7367
  surname: Willott
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  organization: National Research Council of Canada , Herzberg Astronomy & Astrophysics Research Centre, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
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  givenname: Katriona M. L.
  orcidid: 0000-0003-4196-5960
  surname: Gould
  fullname: Gould, Katriona M. L.
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  givenname: Tess
  orcidid: 0009-0006-4881-3299
  surname: Grindlay
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  organization: University of Victoria Department of Physics and Astronomy, Victoria, BC V8P 5C2, Canada
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  givenname: Anishya T.
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  surname: Harshan
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  organization: University of Ljubljana , Department of Mathematics and Physics, Jadranska ulica 19, SI-1000 Ljubljana, Slovenia
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We present the first results on the spatial distribution of dust attenuation at 1.0 < z < 2.4 traced by the Balmer decrement, H α /H β , in emission-line...
We present the first results on the spatial distribution of dust attenuation at 1.0 < z < 2.4 traced by the Balmer decrement, Hα/Hβ, in emission-line galaxies...
We present the first results on the spatial distribution of dust attenuation at 1.0 < z < 2.4 traced by the Balmer decrement, H α /H β , in emission-line...
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SubjectTerms Attenuation
Bins
Cosmic dust
Dust
Galaxies
Galaxy evolution
Galaxy stellar content
H alpha line
High-redshift galaxies
Occultation
Red shift
Shutters
Spatial distribution
Spectroscopy
Spectrum analysis
Star & galaxy formation
Star formation
Stellar mass
Surface brightness
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Title A First Look at Spatially Resolved Balmer Decrements at 1.0 < z < 2.4 from JWST NIRISS Slitless Spectroscopy
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