The Astrophysical Journal Letters (Jan 2023)
Early Results from GLASS-JWST. XV. Properties of the Faintest Red Sources in the NIRCAM Deep Fields
- K. Glazebrook,
- T. Nanayakkara,
- C. Jacobs,
- N. Leethochawalit,
- A. Calabrò,
- A. Bonchi,
- M. Castellano,
- A. Fontana,
- C. Mason,
- E. Merlin,
- T. Morishita,
- D. Paris,
- M. Trenti,
- T. Treu,
- P. Santini,
- X. Wang,
- K. Boyett,
- Marusa Bradac,
- G. Brammer,
- T. Jones,
- D. Marchesini,
- M. Nonino,
- B. Vulcani
Affiliations
- K. Glazebrook
- ORCiD
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology , PO Box 218, Hawthorn, VIC 3122, Australia ; [email protected]
- T. Nanayakkara
- ORCiD
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology , PO Box 218, Hawthorn, VIC 3122, Australia ; [email protected]
- C. Jacobs
- ORCiD
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology , PO Box 218, Hawthorn, VIC 3122, Australia ; [email protected]
- N. Leethochawalit
- ORCiD
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia; School of Physics, University of Melbourne , Parkville 3010, VIC, Australia; National Astronomical Research Institute of Thailand (NARIT) , Mae Rim, Chiang Mai, 50180, Thailand
- A. Calabrò
- ORCiD
- INAF Osservatorio Astronomico di Roma , Via Frascati 33, I-00078 Monteporzio Catone, Rome, Italy
- A. Bonchi
- INAF Osservatorio Astronomico di Roma , Via Frascati 33, I-00078 Monteporzio Catone, Rome, Italy; ASI-Space Science Data Center , Via del Politecnico, I-00133 Roma, Italy
- M. Castellano
- ORCiD
- INAF Osservatorio Astronomico di Roma , Via Frascati 33, I-00078 Monteporzio Catone, Rome, Italy
- A. Fontana
- ORCiD
- INAF Osservatorio Astronomico di Roma , Via Frascati 33, I-00078 Monteporzio Catone, Rome, Italy
- C. Mason
- ORCiD
- Cosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, Denmark
- E. Merlin
- ORCiD
- INAF Osservatorio Astronomico di Roma , Via Frascati 33, I-00078 Monteporzio Catone, Rome, Italy
- T. Morishita
- ORCiD
- Infrared Processing and Analysis Center , Caltech, 1200 E. California Blvd., Pasadena, CA 91125, USA
- D. Paris
- ORCiD
- INAF Osservatorio Astronomico di Roma , Via Frascati 33, I-00078 Monteporzio Catone, Rome, Italy
- M. Trenti
- ORCiD
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia; School of Physics, University of Melbourne , Parkville 3010, VIC, Australia
- T. Treu
- ORCiD
- Department of Physics and Astronomy, University of California , Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095, USA
- P. Santini
- ORCiD
- INAF Osservatorio Astronomico di Roma , Via Frascati 33, I-00078 Monteporzio Catone, Rome, Italy
- X. Wang
- ORCiD
- Infrared Processing and Analysis Center , Caltech, 1200 E. California Blvd., Pasadena, CA 91125, USA
- K. Boyett
- ORCiD
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia; School of Physics, University of Melbourne , Parkville 3010, VIC, Australia
- Marusa Bradac
- ORCiD
- University of Ljubljana , Department of Mathematics and Physics, Jadranska ulica 19, SI-1000 Ljubljana, Slovenia; Department of Physics and Astronomy, University of California Davis , 1 Shields Avenue, Davis, CA 95616, USA
- G. Brammer
- ORCiD
- Cosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, Denmark
- T. Jones
- ORCiD
- Department of Physics and Astronomy, University of California Davis , 1 Shields Avenue, Davis, CA 95616, USA
- D. Marchesini
- ORCiD
- Department of Physics and Astronomy, Tufts University , 574 Boston Ave., Medford, MA 02155, USA
- M. Nonino
- ORCiD
- INAF-Trieste Astronomical Observatory , Via Bazzoni 2, I-34124, Trieste, Italy
- B. Vulcani
- ORCiD
- INAF- Osservatorio astronomico di Padova , Vicolo Osservatorio 5, I-35122 Padova, Italy
- DOI
- https://doi.org/10.3847/2041-8213/acba8b
- Journal volume & issue
-
Vol. 947,
no. 2
p. L25
Abstract
We present a first look at the reddest 2–5 μ m sources found in deep images from the GLASS Early Release Science program. We undertake a general search, i.e., not looking for any particular spectral signatures, for sources detected only in bands redder than is reachable with the Hubble Space Telescope, and which would likely not have been identified in pre-JWST surveys. We search for sources down to AB ∼27 (corresponding to >10 σ detection threshold) in any of the F200W to F444W filters, with a >1 magnitude excess relative to F090W to F150W bands. Fainter than F444W >25 we find 56 such sources of which 37 have reasonably constrained spectral energy distributions to which we can fit photometric redshifts. We find the majority of this population (∼65%) as 2 2 μ m boosted by a combination of the Balmer break and emission lines. The typical implied rest equivalent widths are ∼200 Å with some extreme objects up to ∼1000 Å. This is in contrast with brighter magnitudes where the red sources tend to be z 11 galaxies and a very cool brown dwarf.
Keywords
