TY - JOUR
T1 - JWST UNCOVER
T2 - Extremely Red and Compact Object at z phot ≃ 7.6 Triply Imaged by A2744
AU - Furtak, Lukas J.
AU - Zitrin, Adi
AU - Plat, Adèle
AU - Fujimoto, Seiji
AU - Wang, Bingjie
AU - Nelson, Erica J.
AU - Labbé, Ivo
AU - Bezanson, Rachel
AU - Brammer, Gabriel B.
AU - van Dokkum, Pieter
AU - Endsley, Ryan
AU - Glazebrook, Karl
AU - Greene, Jenny E.
AU - Leja, Joel
AU - Price, Sedona H.
AU - Smit, Renske
AU - Stark, Daniel P.
AU - Weaver, John R.
AU - Whitaker, Katherine E.
AU - Atek, Hakim
AU - Chevallard, Jacopo
AU - Curtis-Lake, Emma
AU - Dayal, Pratika
AU - Feltre, Anna
AU - Franx, Marijn
AU - Fudamoto, Yoshinobu
AU - Marchesini, Danilo
AU - Mowla, Lamiya A.
AU - Pan, Richard
AU - Suess, Katherine A.
AU - Vidal-García, Alba
AU - Williams, Christina C.
N1 - Funding Information:
The authors would like to thank the anonymous referee for providing very useful comments, which greatly helped to improve the paper. L.F. thanks Pierre Boldrini for very useful discussions about high-redshift star clusters. A.Z. thanks Erik Zackrisson for a useful discussion regarding Population III stars. L.F. and A.Z. acknowledge support by grant No. 2020750 from the United States–Israel Binational Science Foundation (BSF) and grant No. 2109066 from the United States National Science Foundation (NSF), and by the Ministry of Science & Technology, Israel. R.B. acknowledges support from the Research Corporation for Scientific Advancement (RCSA) Cottrell Scholar Award ID No.: 27587. E.C.L. acknowledges the support of an STFC Webb Fellowship (ST/W001438/1). H.A. acknowledges support from CNES (Centre National d’Etudes Spatiales). J.C. acknowledges funding from the “FirstGalaxies” Advanced Grant from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 789056). P.D. acknowledges support from the NWO grant No. 016.VIDI.189.162 (“ODIN”) and from the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. The work of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation (DNRF) under grant #140. Support for the program JWST-GO-02561 was provided through a grant from the STScI under NASA contract NAS 5-03127. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program.
Funding Information:
The authors would like to thank the anonymous referee for providing very useful comments, which greatly helped to improve the paper. L.F. thanks Pierre Boldrini for very useful discussions about high-redshift star clusters. A.Z. thanks Erik Zackrisson for a useful discussion regarding Population III stars. L.F. and A.Z. acknowledge support by grant No. 2020750 from the United States-Israel Binational Science Foundation (BSF) and grant No. 2109066 from the United States National Science Foundation (NSF), and by the Ministry of Science & Technology, Israel. R.B. acknowledges support from the Research Corporation for Scientific Advancement (RCSA) Cottrell Scholar Award ID No.: 27587. E.C.L. acknowledges the support of an STFC Webb Fellowship (ST/W001438/1). H.A. acknowledges support from CNES (Centre National d’Etudes Spatiales). J.C. acknowledges funding from the “FirstGalaxies” Advanced Grant from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 789056). P.D. acknowledges support from the NWO grant No. 016.VIDI.189.162 (“ODIN”) and from the European Commission’s and University of Groningen’s CO-FUND Rosalind Franklin program. The work of C.C.W. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation (DNRF) under grant #140. Support for the program JWST-GO-02561 was provided through a grant from the STScI under NASA contract NAS 5-03127. Cloud-based data processing and file storage for this work is provided by the AWS Cloud Credits for Research program.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/8/1
Y1 - 2023/8/1
N2 - Recent JWST/NIRCam imaging taken for the ultra-deep UNCOVER program reveals a very red dropout object at z phot ≃ 7.6, triply imaged by the galaxy cluster A2744 (z d = 0.308). All three images are very compact, i.e., unresolved, with a delensed size upper limit of r e ≲ 35 pc. The images have apparent magnitudes of m F444W ∼ 25−26 AB, and the magnification-corrected absolute UV magnitude of the source is M UV,1450 = −16.81 ± 0.09. From the sum of observed fluxes and from a spectral energy distribution (SED) analysis, we obtain estimates of the bolometric luminosities of the source of L bol ≳ 1043 erg s−1 and L bol ∼ 1044-1046 erg s−1, respectively. Based on its compact, point-like appearance, its position in color-color space, and the SED analysis, we tentatively conclude that this object is a UV-faint dust-obscured quasar-like object, i.e., an active galactic nucleus at high redshift. We also discuss other alternative origins for the object’s emission features, including a massive star cluster, Population III, supermassive, or dark stars, or a direct-collapse black hole. Although populations of red galaxies at similar photometric redshifts have been detected with JWST, this object is unique in that its high-redshift nature is corroborated geometrically by lensing, that it is unresolved despite being magnified—and thus intrinsically even more compact—and that it occupies notably distinct regions in both size-luminosity and color-color space. Planned UNCOVER JWST/NIRSpec observations, scheduled in Cycle 1, will enable a more detailed analysis of this object.
AB - Recent JWST/NIRCam imaging taken for the ultra-deep UNCOVER program reveals a very red dropout object at z phot ≃ 7.6, triply imaged by the galaxy cluster A2744 (z d = 0.308). All three images are very compact, i.e., unresolved, with a delensed size upper limit of r e ≲ 35 pc. The images have apparent magnitudes of m F444W ∼ 25−26 AB, and the magnification-corrected absolute UV magnitude of the source is M UV,1450 = −16.81 ± 0.09. From the sum of observed fluxes and from a spectral energy distribution (SED) analysis, we obtain estimates of the bolometric luminosities of the source of L bol ≳ 1043 erg s−1 and L bol ∼ 1044-1046 erg s−1, respectively. Based on its compact, point-like appearance, its position in color-color space, and the SED analysis, we tentatively conclude that this object is a UV-faint dust-obscured quasar-like object, i.e., an active galactic nucleus at high redshift. We also discuss other alternative origins for the object’s emission features, including a massive star cluster, Population III, supermassive, or dark stars, or a direct-collapse black hole. Although populations of red galaxies at similar photometric redshifts have been detected with JWST, this object is unique in that its high-redshift nature is corroborated geometrically by lensing, that it is unresolved despite being magnified—and thus intrinsically even more compact—and that it occupies notably distinct regions in both size-luminosity and color-color space. Planned UNCOVER JWST/NIRSpec observations, scheduled in Cycle 1, will enable a more detailed analysis of this object.
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U2 - 10.3847/1538-4357/acdc9d
DO - 10.3847/1538-4357/acdc9d
M3 - Article
AN - SCOPUS:85166239264
SN - 0004-637X
VL - 952
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 142
ER -