Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog

Merlin, E.; Bonchi, Andrea; Paris, D.; Belfiori, D.; Fontana, A.; Castellano, M.; Nonino, M.; Polenta, G.; Santini, P.; Yang, Lilan; Glazebrook, Karl; Treu, Tommaso; Roberts-Borsani, Guido; Trenti, Michele; Birrer, Simon; Brammer, Gabriel; Grillo, C.; Calabró, Antonello; Marchesini, Danilo; Mason, Charlotte; Mercurio, A.; Morishita, Takahiro; Strait, Victoria; Boyett, Kristan; Leethochawalit, Nicha; Nanayakkara, Themiya; Vulcani, Benedetta; Bradač, Maruša; Wang, Xin

doi:10.3847/2041-8213/ac8f93

Cited by 42 publications

(39 citation statements)

References 25 publications

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“…Details of the GLASS-ERS data acquisition and observing strategy can be found in Treu et al (2022). Details of the image reduction, stacking, and catalog creation can be found in Merlin et al (2022).…”

Section: Observationsmentioning

confidence: 99%

“…This object immediately appeared to be a potential cool brown dwarf. To search for other cool brown dwarf candidates, we selected from the extracted catalog of Merlin et al (2022) all sources with CLASS_STAR 0.9 (point sources), flags = 0, F444W 28 (for reliable photometry in the other bands, see also Castellano et al 2022), F356W−F444 1.5, and F115W−F444W 2. The color selection criteria were motivated by the infrared colors of T and Y dwarfs, specifically Spitzer IRAC CH1 −CH2 and J−CH2 colors (Meisner et al 2020).…”

Section: Observationsmentioning

confidence: 99%

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Early Results from GLASS-JWST. XIII. A Faint, Distant, and Cold Brown Dwarf*

Nonino

Glazebrook

Burgasser

et al. 2023

ApJL

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We present the serendipitous discovery of a late T-type brown dwarf candidate in JWST NIRCam observations of the Early Release Science Abell 2744 parallel field. The discovery was enabled by the sensitivity of JWST at 4 μm wavelengths and the panchromatic 0.9–4.5 μm coverage of the spectral energy distribution. The unresolved point source has magnitudes F115W = 27.95 ± 0.15 and F444W = 25.84 ± 0.01 (AB), and its F115W−F444W and F356W−F444W colors match those expected for other known T dwarfs. We can exclude it as a reddened background star, high redshift quasar, or a very high redshift galaxy. Comparison with stellar atmospheric models indicates a temperature of T eff ≈ 650 K and surface gravity log g ≈ 5.25 , implying a mass of 0.03 M ⊙ and age of 5 Gyr. We estimate the distance of this candidate to be 570–720 pc in a direction perpendicular to the Galactic plane, making it a likely thick disk or halo brown dwarf. These observations underscore the power of JWST to probe the very low-mass end of the substellar mass function in the Galactic thick disk and halo.

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Section: Observationsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Early Results from GLASS-JWST. XIII. A Faint, Distant, and Cold Brown Dwarf*

Nonino

Glazebrook

Burgasser

et al. 2023

ApJL

Self Cite

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“…For this reason, fitting a plane to each one of the detectors is risky, more so when the gradients in the different detectors are not consistent in direction, as was the case for the long-wavelength channel. In this case, we opted for a more conservative approach: to correct for the readout pattern per detector (see Merlin et al 2022;Pontoppidan et al 2022) and scale the four detectors.…”

Section: Appendix B Short-wavelength Channel Rereductionmentioning

confidence: 99%

A New Era of Intracluster Light Studies with JWST

Montes

Trujillo

2022

ApJL

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Still largely unexplored, the diffuse light in clusters of galaxies traces the past and ongoing buildup of these massive structures. Here we present the first comprehensive study of the intracluster light (ICL) of the cluster SMACS J0723.3–7327 (z = 0.39) using the JWST Early Release Observations. These deep and high spatial resolution images allow the study of the ICL with a high signal-to-noise ratio up to a radial distance of ∼400 kpc, twice as far with respect to previous HST studies of intermediate-redshift clusters. This opens up the possibility of exploring the rich mixture of processes that are building the ICL. We find that the inner parts of this cluster (R < 100 kpc) are built through a major merger, while the outer parts (R > 100 kpc) are mainly produced by the tidal stripping of Milky Way–like satellites. We also find that the slope of the stellar mass density radial profile of the ICL of this cluster (α 3D = −2.47 ± 0.13) closely follows the predicted dark matter halo slope (α 3D,DM = −2.6 to −2), supporting the idea that both components have a similar shape and thus the potential of using the ICL as a tracer of the dark matter distribution in clusters of galaxies. Future JWST studies of the ICL are set to revolutionize our understanding of cluster formation and will be crucial to improve the gravitational lensing mass maps of these structures and thus accurately characterize the properties of the first galaxies.

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“…We noticed the 1/f noise causing small bias shifts in the calibrated stage 2 data products (see Section 2 of Merlin et al 2022). We corrected them by subtracting the median value of each row and then each column before the JWST pipeline stage 3 process.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…We corrected them by subtracting the median value of each row and then each column before the JWST pipeline stage 3 process. Similar to Merlin et al (2022), we masked all sources when computing the median values for row and column subtractions.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

A First Look at Cepheids in a Type Ia Supernova Host with JWST

Yuan

Riess

Casertano

et al. 2022

ApJL

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We report the first look at extragalactic Cepheid variables with the James Webb Space Telescope (JWST), obtained from an archival observation of NGC 1365, host of SNIa 2012fr, a calibration path used to measure the Hubble constant. As expected, the high-resolution observations with NIRCam through F200W show better source separation from line-of-sight companions than Hubble Space Telescope (HST) images at similar near-infrared wavelengths, the spectral region that has been used to mitigate the impact of host dust on distance measurements. Using the standard star P330E as a zero-point and point-spread function reference, we photometered 31 previously known Cepheids in the JWST field, spanning 1.15 < log P < 1.75 including 24 Cepheids in the longer-period interval of 1.35 < log P < 1.75 . We compared the resultant period–luminosity (P-L) relations to that of 49 Cepheids in the full period range including 38 in the longer-period range observed with WFC3/IR on HST and transformed to the JWST photometric system (F200W, Vega). The P-L relations measured are in good agreement, with intercepts (at log P = 1 ) of 25.74 ± 0.04 and 25.72 ± 0.05 for HST and JWST, respectively. Our baseline result comes from the longer-period, higher signal-to-noise ratio Cepheids where we find 25.75 ± 0.05 and 25.75 ± 0.06 mag for HST and JWST, respectively. We find good consistency between this first JWST measurement and HST, and no evidence that HST Cepheid photometry is “biased bright” at the ∼0.2 mag level needed to mitigate the Hubble tension, though comparisons from more SN hosts are warranted and anticipated. We expect future optimized JWST observations to surpass these in quality.

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Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog

Cited by 42 publications

References 25 publications

Early Results from GLASS-JWST. XIII. A Faint, Distant, and Cold Brown Dwarf*

Early Results from GLASS-JWST. XIII. A Faint, Distant, and Cold Brown Dwarf*

A New Era of Intracluster Light Studies with JWST

A First Look at Cepheids in a Type Ia Supernova Host with JWST

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