The Star Formation Efficiency during Reionization as Inferred from the Hubble Frontier Fields
A recent ultraviolet luminosity function (UVLF) analysis in the Hubble Frontier Fields, behind foreground lensing clusters, has helped solidify estimates of the faint-end of the z ∼ 5–9 UVLF at up to 5 mag fainter than in the field. These measurements provide valuable information regarding the role...
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Published in | The Astrophysical journal Vol. 961; no. 1; pp. 50 - 70 |
---|---|
Main Authors | , |
Format | Journal Article |
Language | English |
Published |
Philadelphia
The American Astronomical Society
01.01.2024
IOP Publishing |
Subjects | |
Online Access | Get full text |
ISSN | 0004-637X 1538-4357 |
DOI | 10.3847/1538-4357/ad06a7 |
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Abstract | A recent ultraviolet luminosity function (UVLF) analysis in the Hubble Frontier Fields, behind foreground lensing clusters, has helped solidify estimates of the faint-end of the
z
∼ 5–9 UVLF at up to 5 mag fainter than in the field. These measurements provide valuable information regarding the role of low-luminosity galaxies in reionizing the universe and can help in calibrating expectations for JWST observations. We fit a semiempirical model to the lensed and previous UVLF data from Hubble. This fit constrains the average star formation efficiency (SFE) during reionization, with the lensed UVLF measurements probing halo mass scales as small as
M
∼ 2 × 10
9
M
⊙
. The implied trend of SFE with halo mass is broadly consistent with an extrapolation from previous inferences at
M
≳ 10
10
M
⊙
, although the joint data prefer a shallower SFE. This preference, however, is partly subject to systematic uncertainties in the lensed measurements. Near
z
∼ 6, we find that the SFE peaks at ∼20% between ∼10
11
and 10
12
M
⊙
. Our best-fit model is consistent with the Planck 2020 determinations of the electron scattering optical depth, and most current reionization history measurements, provided the escape fraction of ionizing photons is
f
esc
∼ 10%–20%. The joint UVLF accounts for nearly 80% of the ionizing photon budget at
z
∼ 8. Finally, we show that recent JWST UVLF estimates at
z
≳ 11 require strong departures from the redshift evolution suggested by the Hubble data. |
---|---|
AbstractList | A recent ultraviolet luminosity function (UVLF) analysis in the Hubble Frontier Fields, behind foreground lensing clusters, has helped solidify estimates of the faint-end of the z ∼ 5–9 UVLF at up to 5 mag fainter than in the field. These measurements provide valuable information regarding the role of low-luminosity galaxies in reionizing the universe and can help in calibrating expectations for JWST observations. We fit a semiempirical model to the lensed and previous UVLF data from Hubble. This fit constrains the average star formation efficiency (SFE) during reionization, with the lensed UVLF measurements probing halo mass scales as small as M ∼ 2 × 10 ^9 M _⊙ . The implied trend of SFE with halo mass is broadly consistent with an extrapolation from previous inferences at M ≳ 10 ^10 M _⊙ , although the joint data prefer a shallower SFE. This preference, however, is partly subject to systematic uncertainties in the lensed measurements. Near z ∼ 6, we find that the SFE peaks at ∼20% between ∼10 ^11 and 10 ^12 M _⊙ . Our best-fit model is consistent with the Planck 2020 determinations of the electron scattering optical depth, and most current reionization history measurements, provided the escape fraction of ionizing photons is f _esc ∼ 10%–20%. The joint UVLF accounts for nearly 80% of the ionizing photon budget at z ∼ 8. Finally, we show that recent JWST UVLF estimates at z ≳ 11 require strong departures from the redshift evolution suggested by the Hubble data. A recent ultraviolet luminosity function (UVLF) analysis in the Hubble Frontier Fields, behind foreground lensing clusters, has helped solidify estimates of the faint-end of the z ∼ 5–9 UVLF at up to 5 mag fainter than in the field. These measurements provide valuable information regarding the role of low-luminosity galaxies in reionizing the universe and can help in calibrating expectations for JWST observations. We fit a semiempirical model to the lensed and previous UVLF data from Hubble. This fit constrains the average star formation efficiency (SFE) during reionization, with the lensed UVLF measurements probing halo mass scales as small as M ∼ 2 × 109M⊙. The implied trend of SFE with halo mass is broadly consistent with an extrapolation from previous inferences at M ≳ 1010M⊙, although the joint data prefer a shallower SFE. This preference, however, is partly subject to systematic uncertainties in the lensed measurements. Near z ∼ 6, we find that the SFE peaks at ∼20% between ∼1011 and 1012M⊙. Our best-fit model is consistent with the Planck 2020 determinations of the electron scattering optical depth, and most current reionization history measurements, provided the escape fraction of ionizing photons is fesc ∼ 10%–20%. The joint UVLF accounts for nearly 80% of the ionizing photon budget at z ∼ 8. Finally, we show that recent JWST UVLF estimates at z ≳ 11 require strong departures from the redshift evolution suggested by the Hubble data. A recent ultraviolet luminosity function (UVLF) analysis in the Hubble Frontier Fields, behind foreground lensing clusters, has helped solidify estimates of the faint-end of the z ∼ 5–9 UVLF at up to 5 mag fainter than in the field. These measurements provide valuable information regarding the role of low-luminosity galaxies in reionizing the universe and can help in calibrating expectations for JWST observations. We fit a semiempirical model to the lensed and previous UVLF data from Hubble. This fit constrains the average star formation efficiency (SFE) during reionization, with the lensed UVLF measurements probing halo mass scales as small as M ∼ 2 × 10 9 M ⊙ . The implied trend of SFE with halo mass is broadly consistent with an extrapolation from previous inferences at M ≳ 10 10 M ⊙ , although the joint data prefer a shallower SFE. This preference, however, is partly subject to systematic uncertainties in the lensed measurements. Near z ∼ 6, we find that the SFE peaks at ∼20% between ∼10 11 and 10 12 M ⊙ . Our best-fit model is consistent with the Planck 2020 determinations of the electron scattering optical depth, and most current reionization history measurements, provided the escape fraction of ionizing photons is f esc ∼ 10%–20%. The joint UVLF accounts for nearly 80% of the ionizing photon budget at z ∼ 8. Finally, we show that recent JWST UVLF estimates at z ≳ 11 require strong departures from the redshift evolution suggested by the Hubble data. |
Author | Sipple, Jackson Lidz, Adam |
Author_xml | – sequence: 1 givenname: Jackson surname: Sipple fullname: Sipple, Jackson organization: University of Pennsylvania Center for Particle Cosmology, Department of Physics and Astronomy, Philadelphia, PA 19104, USA – sequence: 2 givenname: Adam orcidid: 0000-0002-3950-9598 surname: Lidz fullname: Lidz, Adam organization: University of Pennsylvania Center for Particle Cosmology, Department of Physics and Astronomy, Philadelphia, PA 19104, USA |
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SubjectTerms | Astronomical models Astrophysics Estimates Galaxies Galaxy dark matter halos Gravitational lensing Hubble Space Telescope Ionization James Webb Space Telescope Luminosity Luminosity function Markov chain Monte Carlo Model selection Optical analysis Optical thickness Photons Red shift Reionization Star & galaxy formation Star formation Stars & galaxies Stellar feedback |
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Title | The Star Formation Efficiency during Reionization as Inferred from the Hubble Frontier Fields |
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