The Luminosity Function and Clustering of H$α$ Emitting Galaxies at $z\approx4-6$ from a Complete NIRCam Grism Redshift Survey Article Swipe
Xiaojing Lin
,
Eiichi Egami
,
Fengwu Sun
,
Haowen Zhang
,
Xiaohui Fan
,
Jakob M. Helton
,
Feige Wang
,
Andrew J. Bunker
,
Zheng Cai
,
Daniel J. Eisenstein
,
D. T. Jaffe
,
Zhiyuan Ji
,
Xiangyu Jin
,
Maria Pudoka
,
Sandro Tacchella
,
Wei Leong Tee
,
Pierluigi Rinaldi
,
Brant Robertson
,
Yang Sun
,
Christopher N. A. Willmer
,
Chris J. Willott
,
Junyu Zhang
,
Yongda Zhu
·
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.48550/arxiv.2504.08028
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.48550/arxiv.2504.08028
We study the luminosity function (LF) and clustering properties of 888 H$α$ emitters (HAEs) at $3.75 < z < 6$ in the GOODS-N field. The sample, built from JWST CONGRESS and FRESCO NIRCam grism surveys using a novel redshift assignment algorithm, spans $\sim$62 arcmin$^2$ and reaches $L_{\rm Hα} \sim 10^{41.2} {\rm erg s^{-1}}$. We identify two prominent filamentary protoclusters at $z \approx 4.41$ and $z \approx 5.19$, hosting 98 and 144 HAEs, respectively. The observed H$α$ LFs show similar shallow faint-end slopes for both protocluster and field galaxies at $z=3.75-5$, and for the protocluster at $z=5-6$ ($α\approx 1.2$ to $-1.3$). In contrast, the field LF at $z=5-6$ is much steeper ($α=-1.87_{-0.23}^{+0.30}$), suggesting that protocluster galaxies at $z > 5$ are more evolved, resembling those at $z=3.75-5$. The observed star formation rate density from H$α$, integrated down to 0.45 ${\rm M_\odot yr^{-1}}$, is $0.050^{+0.002}_{-0.003}$ and $0.046^{+0.006}_{-0.004} M_\odot {\rm yr}^{-1} {\rm Mpc}^{-3}$ at $z=3.75-5$ and $z=5-6$, with protoclusters contributing $\sim$25% and 55%, respectively. This implies that a large fraction of star formation at $z > 4$ occurs in protoclusters. We conduct the first star-formation-rate-limited 3D clustering analysis at $z > 4$. We find the filamentary protocluster geometry flattens the power-law shape of the HAE auto-correlation functions, with slopes much shallower than typically assumed. The auto-correlation function of field HAEs have correlation lengths of $r_0 = 4.61^{+1.00}_{-0.68} h^{-1}{\rm Mpc}$ at $z \approx 4-5$ and $r_0 = 6.23^{+1.68}_{-1.13} h^{-1}{\rm Mpc}$ at $z=5-6$. Comparing the observed correlation functions with the UniverseMachine simulation, we infer the dark matter (sub-)halo masses of HAEs to be $\log (M_h/M_\odot)=11.0-11.2$ at $z\approx 4-6$, with a scatter of 0.4 dex.
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- preprint
- Language
- en
- Landing Page
- http://arxiv.org/abs/2504.08028
- https://arxiv.org/pdf/2504.08028
- OA Status
- green
- OpenAlex ID
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https://openalex.org/W4414827345Canonical identifier for this work in OpenAlex
- DOI
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The Luminosity Function and Clustering of H$α$ Emitting Galaxies at $z\approx4-6$ from a Complete NIRCam Grism Redshift SurveyWork title
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preprintOpenAlex work type
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enPrimary language
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2025Year of publication
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2025-04-10Full publication date if available
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Xiaojing Lin, Eiichi Egami, Fengwu Sun, Haowen Zhang, Xiaohui Fan, Jakob M. Helton, Feige Wang, Andrew J. Bunker, Zheng Cai, Daniel J. Eisenstein, D. T. Jaffe, Zhiyuan Ji, Xiangyu Jin, Maria Pudoka, Sandro Tacchella, Wei Leong Tee, Pierluigi Rinaldi, Brant Robertson, Yang Sun, Christopher N. A. Willmer, Chris J. Willott, Junyu Zhang, Yongda ZhuList of authors in order
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greenOpen access status per OpenAlex
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https://arxiv.org/pdf/2504.08028Direct OA link when available
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| abstract_inverted_index.$3.75 | 15 |
| abstract_inverted_index.$\log | 258 |
| abstract_inverted_index.${\rm | 138 |
| abstract_inverted_index.4-6$, | 262 |
| abstract_inverted_index.4.41$ | 62 |
| abstract_inverted_index.H$α$ | 11, 75 |
| abstract_inverted_index.HAEs, | 71 |
| abstract_inverted_index.Mpc}$ | 225, 235 |
| abstract_inverted_index.built | 26 |
| abstract_inverted_index.field | 86, 103, 215 |
| abstract_inverted_index.first | 180 |
| abstract_inverted_index.grism | 33 |
| abstract_inverted_index.infer | 248 |
| abstract_inverted_index.large | 165 |
| abstract_inverted_index.novel | 37 |
| abstract_inverted_index.shape | 198 |
| abstract_inverted_index.spans | 41 |
| abstract_inverted_index.study | 1 |
| abstract_inverted_index.those | 123 |
| abstract_inverted_index.using | 35 |
| abstract_inverted_index.(HAEs) | 13 |
| abstract_inverted_index.5.19$, | 66 |
| abstract_inverted_index.FRESCO | 31 |
| abstract_inverted_index.H$α$, | 133 |
| abstract_inverted_index.NIRCam | 32 |
| abstract_inverted_index.field. | 23 |
| abstract_inverted_index.masses | 253 |
| abstract_inverted_index.matter | 251 |
| abstract_inverted_index.occurs | 174 |
| abstract_inverted_index.slopes | 81, 205 |
| abstract_inverted_index.$L_{\rm | 46 |
| abstract_inverted_index.$z=5-6$ | 95, 106 |
| abstract_inverted_index.GOODS-N | 22 |
| abstract_inverted_index.M_\odot | 139, 145 |
| abstract_inverted_index.\approx | 61, 65, 228 |
| abstract_inverted_index.conduct | 178 |
| abstract_inverted_index.density | 131 |
| abstract_inverted_index.hosting | 67 |
| abstract_inverted_index.implies | 162 |
| abstract_inverted_index.lengths | 219 |
| abstract_inverted_index.reaches | 45 |
| abstract_inverted_index.sample, | 25 |
| abstract_inverted_index.scatter | 265 |
| abstract_inverted_index.shallow | 79 |
| abstract_inverted_index.similar | 78 |
| abstract_inverted_index.steeper | 109 |
| abstract_inverted_index.surveys | 34 |
| abstract_inverted_index.$-1.3$). | 99 |
| abstract_inverted_index.$\sim$62 | 42 |
| abstract_inverted_index.$z=5-6$, | 153 |
| abstract_inverted_index.$z=5-6$. | 237 |
| abstract_inverted_index.CONGRESS | 29 |
| abstract_inverted_index.analysis | 184 |
| abstract_inverted_index.assumed. | 210 |
| abstract_inverted_index.emitters | 12 |
| abstract_inverted_index.evolved, | 121 |
| abstract_inverted_index.flattens | 195 |
| abstract_inverted_index.fraction | 166 |
| abstract_inverted_index.function | 4, 213 |
| abstract_inverted_index.galaxies | 87, 114 |
| abstract_inverted_index.geometry | 194 |
| abstract_inverted_index.identify | 54 |
| abstract_inverted_index.observed | 74, 127, 240 |
| abstract_inverted_index.redshift | 38 |
| abstract_inverted_index.yr}^{-1} | 147 |
| abstract_inverted_index.$\sim$25% | 157 |
| abstract_inverted_index.$z\approx | 261 |
| abstract_inverted_index.10^{41.2} | 49 |
| abstract_inverted_index.Comparing | 238 |
| abstract_inverted_index.contrast, | 101 |
| abstract_inverted_index.faint-end | 80 |
| abstract_inverted_index.formation | 129, 169 |
| abstract_inverted_index.functions | 242 |
| abstract_inverted_index.power-law | 197 |
| abstract_inverted_index.prominent | 56 |
| abstract_inverted_index.s^{-1}}$. | 52 |
| abstract_inverted_index.shallower | 207 |
| abstract_inverted_index.typically | 209 |
| abstract_inverted_index.$z=3.75-5$ | 151 |
| abstract_inverted_index.(sub-)halo | 252 |
| abstract_inverted_index.Mpc}^{-3}$ | 149 |
| abstract_inverted_index.algorithm, | 40 |
| abstract_inverted_index.arcmin$^2$ | 43 |
| abstract_inverted_index.assignment | 39 |
| abstract_inverted_index.clustering | 7, 183 |
| abstract_inverted_index.functions, | 203 |
| abstract_inverted_index.h^{-1}{\rm | 224, 234 |
| abstract_inverted_index.integrated | 134 |
| abstract_inverted_index.luminosity | 3 |
| abstract_inverted_index.properties | 8 |
| abstract_inverted_index.resembling | 122 |
| abstract_inverted_index.suggesting | 111 |
| abstract_inverted_index.yr^{-1}}$, | 140 |
| abstract_inverted_index.$z=3.75-5$, | 89 |
| abstract_inverted_index.$z=3.75-5$. | 125 |
| abstract_inverted_index.($α\approx | 96 |
| abstract_inverted_index.correlation | 218, 241 |
| abstract_inverted_index.filamentary | 57, 192 |
| abstract_inverted_index.simulation, | 246 |
| abstract_inverted_index.contributing | 156 |
| abstract_inverted_index.protocluster | 84, 93, 113, 193 |
| abstract_inverted_index.protoclusters | 58, 155 |
| abstract_inverted_index.respectively. | 72, 160 |
| abstract_inverted_index.protoclusters. | 176 |
| abstract_inverted_index.UniverseMachine | 245 |
| abstract_inverted_index.auto-correlation | 202, 212 |
| abstract_inverted_index.4.61^{+1.00}_{-0.68} | 223 |
| abstract_inverted_index.6.23^{+1.68}_{-1.13} | 233 |
| abstract_inverted_index.$0.046^{+0.006}_{-0.004} | 144 |
| abstract_inverted_index.(M_h/M_\odot)=11.0-11.2$ | 259 |
| abstract_inverted_index.$0.050^{+0.002}_{-0.003}$ | 142 |
| abstract_inverted_index.star-formation-rate-limited | 181 |
| abstract_inverted_index.($α=-1.87_{-0.23}^{+0.30}$), | 110 |
| cited_by_percentile_year | |
| countries_distinct_count | 0 |
| institutions_distinct_count | 23 |
| citation_normalized_percentile |