JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58
Using the novel James Webb Space Telescope (JWST)/NIRCam observations in the A2744 field, we present a first spatially resolved overview of a Hubble Space Telescope (HST)-dark galaxy, spectroscopically confirmed at z = 2.58 with magnification μ ≈ 1.9. While being largely invisible at ∼1 μ m with NIR...
| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/acbd9d |
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| author | Vasily Kokorev Shuowen Jin Georgios E. Magdis Karina I. Caputi Francesco Valentino Pratika Dayal Maxime Trebitsch Gabriel Brammer Seiji Fujimoto Franz Bauer Edoardo Iani Kotaro Kohno David Blánquez Sesé Carlos Gómez-Guijarro Pierluigi Rinaldi Rafael Navarro-Carrera |
| author_facet | Vasily Kokorev Shuowen Jin Georgios E. Magdis Karina I. Caputi Francesco Valentino Pratika Dayal Maxime Trebitsch Gabriel Brammer Seiji Fujimoto Franz Bauer Edoardo Iani Kotaro Kohno David Blánquez Sesé Carlos Gómez-Guijarro Pierluigi Rinaldi Rafael Navarro-Carrera |
| author_sort | Vasily Kokorev |
| collection | DOAJ |
| description | Using the novel James Webb Space Telescope (JWST)/NIRCam observations in the A2744 field, we present a first spatially resolved overview of a Hubble Space Telescope (HST)-dark galaxy, spectroscopically confirmed at z = 2.58 with magnification μ ≈ 1.9. While being largely invisible at ∼1 μ m with NIRCam, except for sparse clumpy substructures, the object is well detected and resolved in the long-wavelength bands with a spiral shape clearly visible in F277W. By combining ancillary Atacama Large Millimeter/submillimeter Array (ALMA) and Herschel data, we infer that this object is an edge-on dusty spiral with an intrinsic stellar mass log ( M _* / M _⊙ ) ∼ 11.3 and a dust-obscured star formation rate ∼300 M _⊙ yr ^−1 . A massive quiescent galaxy (log ( M _* / M _⊙ ) ∼ 10.8) with tidal features lies 2.″0 away ( r ∼ 9 kpc), at a consistent redshift as inferred by JWST photometry, indicating a potential major merger. The dusty spiral lies on the main sequence of star formation, and shows high dust attenuation in the optical (3 < A _V < 4.5). In the far-infrared, its integrated dust spectral energy distribution is optically thick up to λ _0 ∼ 500 μ m, further supporting the extremely dusty nature. Spatially resolved analysis of the HST-dark galaxy reveals a largely uniform A _V ∼ 4 area spanning ∼57 kpc ^2 , which spatially matches to the ALMA 1 mm continuum emission. Accounting for the surface brightness dimming and the depths of current JWST surveys, unlensed analogs of the HST-dark galaxy at z > 4 would be only detectable in F356W and F444W in an UNCOVER-like survey, and become totally JWST-dark at z ∼ 6. This suggests that detecting highly attenuated galaxies in the Epoch of Reionization might be a challenging task for JWST. |
| first_indexed | 2024-03-12T03:37:12Z |
| format | Article |
| id | doaj.art-ec7e6492e93a425ab0b583a133a03012 |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-12T03:37:12Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj.art-ec7e6492e93a425ab0b583a133a030122023-09-03T13:08:54ZengIOP PublishingThe Astrophysical Journal Letters2041-82052023-01-019452L2510.3847/2041-8213/acbd9dJWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58Vasily Kokorev0https://orcid.org/0000-0002-5588-9156Shuowen Jin1https://orcid.org/0000-0002-8412-7951Georgios E. Magdis2https://orcid.org/0000-0002-4872-2294Karina I. Caputi3https://orcid.org/0000-0001-8183-1460Francesco Valentino4https://orcid.org/0000-0001-6477-4011Pratika Dayal5https://orcid.org/0000-0001-8460-1564Maxime Trebitsch6https://orcid.org/0000-0002-6849-5375Gabriel Brammer7https://orcid.org/0000-0003-2680-005XSeiji Fujimoto8https://orcid.org/0000-0001-7201-5066Franz Bauer9https://orcid.org/0000-0002-8686-8737Edoardo Iani10https://orcid.org/0000-0001-8386-3546Kotaro Kohno11https://orcid.org/0000-0002-4052-2394David Blánquez Sesé12https://orcid.org/0000-0001-7880-8841Carlos Gómez-Guijarro13https://orcid.org/0000-0002-4085-9165Pierluigi Rinaldi14https://orcid.org/0000-0002-5104-8245Rafael Navarro-Carrera15https://orcid.org/0000-0001-6066-4624Kapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The Netherlands ; kokorev@astro.rug.nlCosmic Dawn Center (DAWN) , Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, DK-2800 Kgs. Lyngby, DenmarkCosmic Dawn Center (DAWN) , Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, DK-2800 Kgs. Lyngby, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2100, Copenhagen N, DenmarkKapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The Netherlands ; kokorev@astro.rug.nl; Cosmic Dawn Center (DAWN) , DenmarkCosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2100, Copenhagen N, Denmark; European Southern Observatory , Karl-Schwarzschild-Str. 2, D-85748 Garching bei Munchen, GermanyKapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The Netherlands ; kokorev@astro.rug.nlKapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The Netherlands ; kokorev@astro.rug.nlCosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2100, Copenhagen N, DenmarkCosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2100, Copenhagen N, Denmark; Department of Astronomy, The University of Texas at Austin , Austin, TX 78712, USAInstituto de Astrofísica , Facultad de Física, Pontificia Universidad Católica de Chile, Campus San Joaquín, Av. Vicuña Mackenna 4860, Macul Santiago, 7820436, Chile; Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile , Campus San Joaquín, Av. Vicuña Mackenna 4860, Macul Santiago, 7820436, Chile; Millennium Institute of Astrophysics , Nuncio Monseñor Sótero Sanz 100, Of 104, Providencia, Santiago, ChileKapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The Netherlands ; kokorev@astro.rug.nlInstitute of Astronomy, Graduate School of Science, The University of Tokyo , 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan; Research Center for the Early Universe, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanCosmic Dawn Center (DAWN) , Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, DK-2800 Kgs. Lyngby, DenmarkUniversité Paris-Saclay, Université Paris Cité , CEA, CNRS, AIM, F-91191, Gif-sur-Yvette, FranceKapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The Netherlands ; kokorev@astro.rug.nlKapteyn Astronomical Institute, University of Groningen , P.O. Box 800, 9700AV Groningen, The Netherlands ; kokorev@astro.rug.nlUsing the novel James Webb Space Telescope (JWST)/NIRCam observations in the A2744 field, we present a first spatially resolved overview of a Hubble Space Telescope (HST)-dark galaxy, spectroscopically confirmed at z = 2.58 with magnification μ ≈ 1.9. While being largely invisible at ∼1 μ m with NIRCam, except for sparse clumpy substructures, the object is well detected and resolved in the long-wavelength bands with a spiral shape clearly visible in F277W. By combining ancillary Atacama Large Millimeter/submillimeter Array (ALMA) and Herschel data, we infer that this object is an edge-on dusty spiral with an intrinsic stellar mass log ( M _* / M _⊙ ) ∼ 11.3 and a dust-obscured star formation rate ∼300 M _⊙ yr ^−1 . A massive quiescent galaxy (log ( M _* / M _⊙ ) ∼ 10.8) with tidal features lies 2.″0 away ( r ∼ 9 kpc), at a consistent redshift as inferred by JWST photometry, indicating a potential major merger. The dusty spiral lies on the main sequence of star formation, and shows high dust attenuation in the optical (3 < A _V < 4.5). In the far-infrared, its integrated dust spectral energy distribution is optically thick up to λ _0 ∼ 500 μ m, further supporting the extremely dusty nature. Spatially resolved analysis of the HST-dark galaxy reveals a largely uniform A _V ∼ 4 area spanning ∼57 kpc ^2 , which spatially matches to the ALMA 1 mm continuum emission. Accounting for the surface brightness dimming and the depths of current JWST surveys, unlensed analogs of the HST-dark galaxy at z > 4 would be only detectable in F356W and F444W in an UNCOVER-like survey, and become totally JWST-dark at z ∼ 6. This suggests that detecting highly attenuated galaxies in the Epoch of Reionization might be a challenging task for JWST.https://doi.org/10.3847/2041-8213/acbd9dActive galaxiesDisk galaxies |
| spellingShingle | Vasily Kokorev Shuowen Jin Georgios E. Magdis Karina I. Caputi Francesco Valentino Pratika Dayal Maxime Trebitsch Gabriel Brammer Seiji Fujimoto Franz Bauer Edoardo Iani Kotaro Kohno David Blánquez Sesé Carlos Gómez-Guijarro Pierluigi Rinaldi Rafael Navarro-Carrera JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58 The Astrophysical Journal Letters Active galaxies Disk galaxies |
| title | JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58 |
| title_full | JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58 |
| title_fullStr | JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58 |
| title_full_unstemmed | JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58 |
| title_short | JWST Insight into a Lensed HST-dark Galaxy and Its Quiescent Companion at z = 2.58 |
| title_sort | jwst insight into a lensed hst dark galaxy and its quiescent companion at z 2 58 |
| topic | Active galaxies Disk galaxies |
| url | https://doi.org/10.3847/2041-8213/acbd9d |
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