Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical Emissions
We present a star formation rate function (SFRF) at z ∼ 6 based on star formation rates (SFRs) derived by spectral energy distribution fitting on data from rest-frame UV to optical wavelengths of galaxies in the CANDELS GOODS-South and North fields. The resulting SFRF shows an excess compared to the...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad0e67 |
| _version_ | 1797349031523909632 |
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| author | Yoshihisa Asada Kouji Ohta |
| author_facet | Yoshihisa Asada Kouji Ohta |
| author_sort | Yoshihisa Asada |
| collection | DOAJ |
| description | We present a star formation rate function (SFRF) at z ∼ 6 based on star formation rates (SFRs) derived by spectral energy distribution fitting on data from rest-frame UV to optical wavelengths of galaxies in the CANDELS GOODS-South and North fields. The resulting SFRF shows an excess compared to the previous estimations by using rest-frame UV luminosity functions (LFs) corrected for the dust attenuation and is comparable to that estimated from a far-infrared LF. This suggests that the number density of dust-obscured intensively star-forming galaxies at z ∼ 6 has been underestimated in the previous approach based only on rest-frame UV observations. We parameterize the SFRF using the Schechter function and obtain the best-fit parameter of the characteristic SFR (SFR*) when the faint-end slope and characteristic number density are fixed. The best-fit SFR* at z ∼ 6 is comparable to that at z ∼ 2, when the cosmic star formation activity reaches its peak. Together with SFRF estimations with a similar approach using rest-frame UV to optical data, the SFR* is roughly constant from z ∼ 2 to ∼6 and may decrease above z ∼ 6. Since the SFR* is sensitive to the high-SFR end of the SFRF, this evolution of SFR* suggests that the high-SFR end of the SFRF grows rapidly during the epoch of reionization and reaches a similar level observed at z ∼ 2. |
| first_indexed | 2024-03-08T12:15:00Z |
| format | Article |
| id | doaj.art-7bf0bb283b544efd875bf22b9b4829fb |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T12:15:00Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-7bf0bb283b544efd875bf22b9b4829fb2024-01-22T14:04:43ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01961215210.3847/1538-4357/ad0e67Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical EmissionsYoshihisa Asada0https://orcid.org/0000-0003-3983-5438Kouji Ohta1https://orcid.org/0000-0003-3844-1517Department of Astronomy, Kyoto University Sakyo-ku , Kyoto 606-8502, Japan ; asada@kusastro.kyoto-u.ac.jpDepartment of Astronomy, Kyoto University Sakyo-ku , Kyoto 606-8502, Japan ; asada@kusastro.kyoto-u.ac.jpWe present a star formation rate function (SFRF) at z ∼ 6 based on star formation rates (SFRs) derived by spectral energy distribution fitting on data from rest-frame UV to optical wavelengths of galaxies in the CANDELS GOODS-South and North fields. The resulting SFRF shows an excess compared to the previous estimations by using rest-frame UV luminosity functions (LFs) corrected for the dust attenuation and is comparable to that estimated from a far-infrared LF. This suggests that the number density of dust-obscured intensively star-forming galaxies at z ∼ 6 has been underestimated in the previous approach based only on rest-frame UV observations. We parameterize the SFRF using the Schechter function and obtain the best-fit parameter of the characteristic SFR (SFR*) when the faint-end slope and characteristic number density are fixed. The best-fit SFR* at z ∼ 6 is comparable to that at z ∼ 2, when the cosmic star formation activity reaches its peak. Together with SFRF estimations with a similar approach using rest-frame UV to optical data, the SFR* is roughly constant from z ∼ 2 to ∼6 and may decrease above z ∼ 6. Since the SFR* is sensitive to the high-SFR end of the SFRF, this evolution of SFR* suggests that the high-SFR end of the SFRF grows rapidly during the epoch of reionization and reaches a similar level observed at z ∼ 2.https://doi.org/10.3847/1538-4357/ad0e67Galaxy evolutionGalaxy formationHigh-redshift galaxies |
| spellingShingle | Yoshihisa Asada Kouji Ohta Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical Emissions The Astrophysical Journal Galaxy evolution Galaxy formation High-redshift galaxies |
| title | Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical Emissions |
| title_full | Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical Emissions |
| title_fullStr | Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical Emissions |
| title_full_unstemmed | Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical Emissions |
| title_short | Early Growth of the Star Formation Rate Function in the Epoch of Reionization: An Approach with Rest-frame Optical Emissions |
| title_sort | early growth of the star formation rate function in the epoch of reionization an approach with rest frame optical emissions |
| topic | Galaxy evolution Galaxy formation High-redshift galaxies |
| url | https://doi.org/10.3847/1538-4357/ad0e67 |
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