JWST Imaging of Earendel, the Extremely Magnified Star at Redshift z = 6.2
Ikusi/ Ireki
Data
2022Egilea
Welch, Brian
Coe, Dan
Zackrisson, Erik
de Mink, S. E.
Ravindranath, Swara
Anderson, Jay
Brammer, Gabriel
Bradley, Larry
Yoon, Jinmi
Kelly, Patrick
Diego, José
Windhorst, Rogier A.
Zitrin, Adi
Dimauro, Paola
Jiménez Teja, Yolanda
Abdurro'uf
Nonino, Mario
Acebrón, Ana
Andrade Santos, Felipe
Ávila, Roberto J.
Bayliss, Matthew B.
Benítez, Alex
Broadhurst, Thomas
Bhatawdekar, Rachana
Bradac, Marusa
Caminha, Gabriel B.
Chen, Wenlei
Eldridge, Jan
Farag, Ebraheem
Florian, Michael
Frye, Brenda L.
Fujimoto, Seiji
Gómez, Sebastián
Henry, Alaina
Hsiao, Tiger Yu-Yang
Hutchison, Taylor A.
James, Bethan L.
Joyce, Meridith
Jung, Intae
Khullar, Gourav
Larson, Rebecca L.
Mahler, Guillaume
Mandelker, Nir
McCandliss, Stephan
Morishita, Takahiro
Newshore, Rosa
Norman, Colin
O'Connor, Kyle
Oesch, Pascal A.
Oguri, Masamune
Ouchi, Masami
Postman, Marc
Rigby, Jane R.
Ryan, Russell E. Jr.
Sharma, Soniya
Sharon, Keren
Strait, Victoria
Strolger, Louis Gregory
Timmes, F. X
Toft, Sune
Trenti, Michele
Vanzella, Eros
Vikaeus, Anton
The Astrophysical Journal Letters 940(1) : (2022) // Article ID L1
Laburpena
The gravitationally lensed star WHL 0137–LS, nicknamed Earendel, was identified with a photometric redshift zphot = 6.2 ± 0.1 based on images taken with the Hubble Space Telescope. Here we present James Webb Space Telescope (JWST) Near Infrared Camera images of Earendel in eight filters spanning 0.8–5.0 μm. In these higher-resolution images, Earendel remains a single unresolved point source on the lensing critical curve, increasing the lower limit on the lensing magnification to μ > 4000 and restricting the source plane radius further to r < 0.02 pc, or ∼4000 au. These new observations strengthen the conclusion that Earendel is best explained by an individual star or multiple star system and support the previous photometric redshift estimate. Fitting grids of stellar spectra to our photometry yields a stellar temperature of Teff ≃ 13,000–16,000 K, assuming the light is dominated by a single star. The delensed bolometric luminosity in this case ranges from log(L)=5.8 to 6.6 L⊙, which is in the range where one expects luminous blue variable stars. Follow-up observations, including JWST NIRSpec scheduled for late 2022, are needed to further unravel the nature of this object, which presents a unique opportunity to study massive stars in the first billion years of the universe.
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Bestelakorik adierazi ezean, itemaren baimena horrela deskribatzen da:© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.