TY - JOUR
T1 - A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE)
T2 - Spectroscopically Complete Census of Obscured Cosmic Star Formation Rate Density at z = 4-6
AU - Sun, Fengwu
AU - Wang, Feige
AU - Yang, Jinyi
AU - Champagne, Jaclyn B.
AU - Decarli, Roberto
AU - Fan, Xiaohui
AU - Bañados, Eduardo
AU - Cai, Zheng
AU - Colina, Luis
AU - Egami, Eiichi
AU - Hennawi, Joseph F.
AU - Jin, Xiangyu
AU - Jun, Hyunsung D.
AU - Khusanova, Yana
AU - Li, Mingyu
AU - Li, Zihao
AU - Lin, Xiaojing
AU - Liu, Weizhe
AU - Meyer, Romain A.
AU - Pudoka, Maria A.
AU - Rieke, George H.
AU - Shen, Yue
AU - Tee, Wei Leong
AU - Venemans, Bram
AU - Walter, Fabian
AU - Wu, Yunjing
AU - Zhang, Huanian
AU - Zou, Siwei
N1 - This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #2078. The JWST data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi: 10.17909/vt74-kd84 . Support for program #2078 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127.
F.S. acknowledges funding from JWST/NIRCam contract to the University of Arizona, NAS5-02105 and support for JWST program #2883 provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. F.W. and X.F. acknowledge support from NSF Grant AST-2308258. J.B.C. acknowledges funding from the JWST Arizona/Steward Postdoc in Early galaxies and Reionization (JASPER) Scholar contract at the University of Arizona. L.C. acknowledges support by grant PIB2021-127718NB-100 from the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by \u201CERDF A way of making Europe.\u201D Y.K. thanks the support of the German Space Agency (DLR) through the program LEGACY 50OR2303. R.A.M. acknowledges support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. S.Z. acknowledges support from the National Science Foundation of China (no. 12303011).
We thank JWST #2078 program coordinator Weston Eck and ALMA program #2022.1.01077.L contact scientist Catherine Vlahakis for their support of our observing programs. We thank NRAO for providing computational resource support for ALMA data processing. We thank the anonymous referee for helpful comments. F.S. thanks Seiji Fujimoto for helpful discussions. F.S. acknowledges funding from JWST/NIRCam contract to the University of Arizona, NAS5-02105 and support for JWST program #2883 provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. F.W. and X.F. acknowledge support from NSF Grant AST-2308258. J.B.C. acknowledges funding from the JWST Arizona/Steward Postdoc in Early galaxies and Reionization (JASPER) Scholar contract at the University of Arizona. L.C. acknowledges support by grant PIB2021-127718NB-100 from the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/ 10.13039/501100011033 and by \u201CERDF A way of making Europe.\u201D Y.K. thanks the support of the German Space Agency (DLR) through the program LEGACY 50OR2303. R.A.M. acknowledges support from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. S. Z. acknowledges support from the National Science Foundation of China (no. 12303011). This paper makes use of the following ALMA data: ADS/ JAO.ALMA#2022.1.01077.L. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is based on observations made with the NASA/ ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #2078. The JWST data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/vt74-kd84. Support for program #2078 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127.
PY - 2025/2/10
Y1 - 2025/2/10
N2 - We present a stringent measurement of the dust-obscured star formation rate density (SFRD) at z = 4-6 from the ASPIRE JWST Cycle-1 medium and ALMA Cycle-9 large program. We obtained JWST/NIRCam grism spectroscopy and ALMA 1.2 mm continuum map along 25 independent quasar sightlines, covering a total survey area of ∼35 arcmin2 where we search for dusty star-forming galaxies (DSFGs) at z = 0-7. We identify eight DSFGs in seven fields at z = 4-6 through the detection of Hα or [O iii] λ5008 lines, including fainter lines such as Hβ, [O iii] λ4960, [N ii] λ6585, and [S ii] λλ6718,6733 for six sources. With this spectroscopically complete DSFG sample at z = 4-6 and negligible impact from cosmic variance (shot noise), we measure the infrared luminosity function (IRLF) down to LIR ∼ 2 × 1011 L⊙. We find flattening of IRLF at z = 4-6 towards the faint end (power-law slope α = 0.5 9 − 0.45 + 0.39 ). We determine the dust-obscured cosmic SFRD at this epoch to be log [ ρ SFR , IR / ( M ⊙ yr − 1 Mpc − 3 ) ] = − 1.5 2 − 0.13 + 0.14 . This is significantly higher than previous determinations using ALMA data in the Hubble Ultra Deep Field, which is void of DSFGs at z = 4-6 because of strong cosmic variance (shot noise). We conclude that the majority (66% ± 7%) of cosmic star formation at z ∼ 5 is still obscured by dust. We also discuss the uncertainty of SFRD propagated from far-IR spectral energy distribution and IRLF at the bright end, which will need to be resolved with future ALMA and JWST observations.
AB - We present a stringent measurement of the dust-obscured star formation rate density (SFRD) at z = 4-6 from the ASPIRE JWST Cycle-1 medium and ALMA Cycle-9 large program. We obtained JWST/NIRCam grism spectroscopy and ALMA 1.2 mm continuum map along 25 independent quasar sightlines, covering a total survey area of ∼35 arcmin2 where we search for dusty star-forming galaxies (DSFGs) at z = 0-7. We identify eight DSFGs in seven fields at z = 4-6 through the detection of Hα or [O iii] λ5008 lines, including fainter lines such as Hβ, [O iii] λ4960, [N ii] λ6585, and [S ii] λλ6718,6733 for six sources. With this spectroscopically complete DSFG sample at z = 4-6 and negligible impact from cosmic variance (shot noise), we measure the infrared luminosity function (IRLF) down to LIR ∼ 2 × 1011 L⊙. We find flattening of IRLF at z = 4-6 towards the faint end (power-law slope α = 0.5 9 − 0.45 + 0.39 ). We determine the dust-obscured cosmic SFRD at this epoch to be log [ ρ SFR , IR / ( M ⊙ yr − 1 Mpc − 3 ) ] = − 1.5 2 − 0.13 + 0.14 . This is significantly higher than previous determinations using ALMA data in the Hubble Ultra Deep Field, which is void of DSFGs at z = 4-6 because of strong cosmic variance (shot noise). We conclude that the majority (66% ± 7%) of cosmic star formation at z ∼ 5 is still obscured by dust. We also discuss the uncertainty of SFRD propagated from far-IR spectral energy distribution and IRLF at the bright end, which will need to be resolved with future ALMA and JWST observations.
UR - https://www.scopus.com/pages/publications/85217994700
UR - https://www.scopus.com/pages/publications/85217994700#tab=citedBy
U2 - 10.3847/1538-4357/ad9d0e
DO - 10.3847/1538-4357/ad9d0e
M3 - Article
AN - SCOPUS:85217994700
SN - 0004-637X
VL - 980
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 12
ER -