JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16
We report the initial result of our Pa β narrowband imaging on a protocluster with the JWST Near Infrared Camera (NIRCam). As NIRCam enables deep narrowband imaging of rest-frame near-infrared lines at z > 1, we target one of the most studied protoclusters, the Spiderweb protocluster at z = 2.16,...
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| 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/ad8155 |
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| author | Rhythm Shimakawa J. M. Pérez-Martínez Helmut Dannerbauer Yusei Koyama Tadayuki Kodama Pablo G. Pérez-González Chiara D’Eugenio Yuheng Zhang Abdurrahman Naufal Kazuki Daikuhara |
| author_facet | Rhythm Shimakawa J. M. Pérez-Martínez Helmut Dannerbauer Yusei Koyama Tadayuki Kodama Pablo G. Pérez-González Chiara D’Eugenio Yuheng Zhang Abdurrahman Naufal Kazuki Daikuhara |
| author_sort | Rhythm Shimakawa |
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| description | We report the initial result of our Pa β narrowband imaging on a protocluster with the JWST Near Infrared Camera (NIRCam). As NIRCam enables deep narrowband imaging of rest-frame near-infrared lines at z > 1, we target one of the most studied protoclusters, the Spiderweb protocluster at z = 2.16, in which previous studies have confirmed more than a hundred member galaxies. The NIRCam F405N narrowband filter covers in the Pa β line the protocluster redshift given by known protocluster members, allowing for the search for new member candidates. The weight-corrected color–magnitude diagram obtained 57 sources showing narrowband excesses, 41 of which satisfy further color selection criteria for limiting the sample to Pa β emitter candidates at z ∼ 2.16, and 24 of them do not have H α emitter counterparts. The Pa β emitter candidates appear to follow the spatial distribution of known protocluster members; however, follow-up spectroscopic confirmation is required. Only 17 out of 58 known H α -emitting cluster members are selected as Pa β emitters in the current data, albeit the rest fall out of the narrowband selection owing to their small Pa β equivalent widths. We derive the Pa β luminosity function in the Spiderweb protocluster, showing a normalization density of $\mathrm{log}{\phi }^{* }=-2.53\pm 0.15$ at a characteristic Pa β luminosity of $\mathrm{log}{L}^{* }=42.33\pm 0.17$ . Furthermore, we examine the possibility of detecting faint line emitters visible only in the narrowband image but find no promising candidates. |
| format | Article |
| id | doaj-art-e94cbe5f93464f11baedd9877f16a32b |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-e94cbe5f93464f11baedd9877f16a32b2024-12-04T12:56:18ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0197717310.3847/1538-4357/ad8155JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16Rhythm Shimakawa0https://orcid.org/0000-0003-4442-2750J. M. Pérez-Martínez1https://orcid.org/0000-0002-5963-6850Helmut Dannerbauer2https://orcid.org/0000-0001-7147-3575Yusei Koyama3https://orcid.org/0000-0002-0479-3699Tadayuki Kodama4https://orcid.org/0000-0002-2993-1576Pablo G. Pérez-González5https://orcid.org/0000-0003-4528-5639Chiara D’Eugenio6Yuheng Zhang7https://orcid.org/0000-0001-5757-5719Abdurrahman Naufal8https://orcid.org/0000-0001-7713-0434Kazuki Daikuhara9https://orcid.org/0000-0002-9509-2774Waseda Institute for Advanced Study (WIAS), Waseda University , 1-21-1, Nishi-Waseda, Shinjuku, Tokyo, 169-0051, Japan ; rhythm.shimakawa@aoni.waseda.jp; Center for Data Science, Waseda University , 1-6-1, Nishi-Waseda, Shinjuku, Tokyo, 169-0051, JapanInstituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna , Dpto. Astrofísica, E-38206 La Laguna, Tenerife, SpainInstituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna , Dpto. Astrofísica, E-38206 La Laguna, Tenerife, SpainSubaru Telescope, National Astronomical Observatory of Japan, National Institutes of Natural Sciences 650 North A’ohoku Place , Hilo, HI 96720, USAAstronomical Institute, Tohoku University , 6-3, Aramaki, Aoba, Sendai, Miyagi 980-8578, JapanCentro de Astrobiología (CAB) , CSIC-INTA, Ctra. de Ajalvir km 4, Torrejǿn de Ardoz, E-28850, Madrid, SpainInstituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna , Dpto. Astrofísica, E-38206 La Laguna, Tenerife, SpainInstituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna , Dpto. Astrofísica, E-38206 La Laguna, Tenerife, Spain; Purple Mountain Observatory, Chinese Academy of Sciences , 10 Yuanhua Road, Nanjing, 210023, People's Republic of China; School of Astronomy and Space Science, University of Science and Technology of China , Hefei, Anhui 230026, People's Republic of ChinaDepartment of Astronomical Science, The Graduate University for Advanced Studies , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanAstronomical Institute, Tohoku University , 6-3, Aramaki, Aoba, Sendai, Miyagi 980-8578, JapanWe report the initial result of our Pa β narrowband imaging on a protocluster with the JWST Near Infrared Camera (NIRCam). As NIRCam enables deep narrowband imaging of rest-frame near-infrared lines at z > 1, we target one of the most studied protoclusters, the Spiderweb protocluster at z = 2.16, in which previous studies have confirmed more than a hundred member galaxies. The NIRCam F405N narrowband filter covers in the Pa β line the protocluster redshift given by known protocluster members, allowing for the search for new member candidates. The weight-corrected color–magnitude diagram obtained 57 sources showing narrowband excesses, 41 of which satisfy further color selection criteria for limiting the sample to Pa β emitter candidates at z ∼ 2.16, and 24 of them do not have H α emitter counterparts. The Pa β emitter candidates appear to follow the spatial distribution of known protocluster members; however, follow-up spectroscopic confirmation is required. Only 17 out of 58 known H α -emitting cluster members are selected as Pa β emitters in the current data, albeit the rest fall out of the narrowband selection owing to their small Pa β equivalent widths. We derive the Pa β luminosity function in the Spiderweb protocluster, showing a normalization density of $\mathrm{log}{\phi }^{* }=-2.53\pm 0.15$ at a characteristic Pa β luminosity of $\mathrm{log}{L}^{* }=42.33\pm 0.17$ . Furthermore, we examine the possibility of detecting faint line emitters visible only in the narrowband image but find no promising candidates.https://doi.org/10.3847/1538-4357/ad8155ProtoclustersHigh-redshift galaxy clustersEmission line galaxiesNear infrared astronomyGalaxy formationGalaxy evolution |
| spellingShingle | Rhythm Shimakawa J. M. Pérez-Martínez Helmut Dannerbauer Yusei Koyama Tadayuki Kodama Pablo G. Pérez-González Chiara D’Eugenio Yuheng Zhang Abdurrahman Naufal Kazuki Daikuhara JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16 The Astrophysical Journal Protoclusters High-redshift galaxy clusters Emission line galaxies Near infrared astronomy Galaxy formation Galaxy evolution |
| title | JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16 |
| title_full | JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16 |
| title_fullStr | JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16 |
| title_full_unstemmed | JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16 |
| title_short | JWST/NIRCam Narrowband Survey of Paβ Emitters in the Spiderweb Protocluster at z = 2.16 |
| title_sort | jwst nircam narrowband survey of paβ emitters in the spiderweb protocluster at z 2 16 |
| topic | Protoclusters High-redshift galaxy clusters Emission line galaxies Near infrared astronomy Galaxy formation Galaxy evolution |
| url | https://doi.org/10.3847/1538-4357/ad8155 |
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