Erratum: “The Thermal Sunyaev–Zel’dovich Effect from Massive, Quiescent 0.5 ≤ z ≤ 1.5 Galaxies” (2021, ApJ, 913, 88)

Meinke, Jeremy; Böckmann, K.; Cohen, Seth H.; Mauskopf, Philip; Scannapieco, Evan; Sarmento, Richard; Lunde, Emily; Cottle, J’Neil

doi:10.3847/1538-4357/ace532

Cited by 1 publication

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“…We used the EAZY redshifts as input to a custom IDL SED fitting code that was also recently used by Meinke et al (2021Meinke et al ( , 2023. This code starts with Bruzual & Charlot (2003, hereafter BC03) SED models assuming a Salpeter initial mass function (IMF) and an exponentially decaying star formation history specified by the decay scale, τ, which ranges from 0.01 to 100 Gyr in 16 logarithmically spaced steps.…”

Section: Photometric Redshift Estimation and Sed Fitsmentioning

confidence: 99%

TREASUREHUNT: Transients and Variability Discovered with HST in the JWST North Ecliptic Pole Time-domain Field

O’Brien,

Jansen,

Grogin

et al. 2024

ApJS

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The James Webb Space Telescope (JWST) North Ecliptic Pole (NEP) Time-domain Field (TDF) is a >14′ diameter field optimized for multiwavelength time-domain science with JWST. It has been observed across the electromagnetic spectrum both from the ground and from space, including with the Hubble Space Telescope (HST). As part of HST observations over three cycles (the “TREASUREHUNT” program), deep images were obtained with the Wide Field Camera on the Advanced Camera for Surveys in F435W and F606W that cover almost the entire JWST NEP TDF. Many of the individual pointings of these programs partially overlap, allowing an initial assessment of the potential of this field for time-domain science with HST and JWST. The cumulative area of overlapping pointings is ∼88 arcmin2, with time intervals between individual epochs that range between 1 day and 4+ yr. To a depth of m AB ≃ 29.5 mag (F606W), we present the discovery of 12 transients and 190 variable candidates. For the variable candidates, we demonstrate that Gaussian statistics are applicable and estimate that ∼80 are false positives. The majority of the transients will be supernovae, although at least two are likely quasars. Most variable candidates are active galactic nuclei (AGNs), where we find 0.42% of the general z ≲ 6 field galaxy population to vary at the ∼3σ level. Based on a 5 yr time frame, this translates into a random supernova areal density of up to ∼0.07 transients arcmin−2 (∼245 deg−2) per epoch and a variable AGN areal density of ∼1.25 variables arcmin−2 (∼4500 deg−2) to these depths.

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Section: Photometric Redshift Estimation and Sed Fitsmentioning

confidence: 99%