Is the infrared background excess explained by the isotropic zodiacal light from the outer solar system?

Tsumura, Kohji

doi:10.1093/pasj/psy100

Cited by 3 publications

(2 citation statements)

References 48 publications

(71 reference statements)

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“…Our F150W and F200W NIRCam diffuse light limits in Figure 13 are in line with the 1.1-1.6 μm CIBER detections of Matsuura et al (2017) and Sano et al (2020; purple triangles in Figure 13), and with the SKYSURF upper limits in the HST/ WFC3 F140W and F160M filters of Carleton et al (2022). These papers, as well as Tsumura (2018) and Korngut et al (2022), suggested that some very dim spherical-or nearly spherical-Zodiacal component could be missing from the Kelsall et al (1998) model. Kelsall et al (1998) also noted that a dim spherical Zodiacal component could have been missed in their model of the COBE/DIRBE data.…”

Section: Jwst Sky-sb Estimates and Possible Limits To Diffuse Lightsupporting

confidence: 83%

“…Software: Astropy: http://www.astropy.org (Astropy Collaboration et al 2013, 2018; IDL Astronomy Library: https://idlastro.gsfc.nasa.gov (Landsman 1993); Photutils: https://photutils.readthedocs.io/en/stable/ (Bradley et al 2020); ProFound: https://github.com/asgr/ProFound (Robotham et al 2017(Robotham et al , 2018; ProFit: https://github.com/ICRAR/ProFit (Robotham et al 2018); SourceExtractor: SourceExtractor: https://www.astromatic.net/software/sextractor/ or https:// sextractor.readthedocs.io/en/latest/ (Bertin & Arnouts 1996).…”

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confidence: 99%

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JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results

Windhorst

Cohen

Jansen

et al. 2022

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We give an overview and describe the rationale, methods, and first results from NIRCam images of the JWST “Prime Extragalactic Areas for Reionization and Lensing Science” (PEARLS) project. PEARLS uses up to eight NIRCam filters to survey several prime extragalactic survey areas: two fields at the North Ecliptic Pole (NEP); seven gravitationally lensing clusters; two high redshift protoclusters; and the iconic backlit VV 191 galaxy system to map its dust attenuation. PEARLS also includes NIRISS spectra for one of the NEP fields and NIRSpec spectra of two high-redshift quasars. The main goal of PEARLS is to study the epoch of galaxy assembly, active galactic nucleus (AGN) growth, and First Light. Five fields—the JWST NEP Time-Domain Field (TDF), IRAC Dark Field, and three lensing clusters—will be observed in up to four epochs over a year. The cadence and sensitivity of the imaging data are ideally suited to find faint variable objects such as weak AGN, high-redshift supernovae, and cluster caustic transits. Both NEP fields have sightlines through our Galaxy, providing significant numbers of very faint brown dwarfs whose proper motions can be studied. Observations from the first spoke in the NEP TDF are public. This paper presents our first PEARLS observations, their NIRCam data reduction and analysis, our first object catalogs, the 0.9–4.5 μm galaxy counts and Integrated Galaxy Light. We assess the JWST sky brightness in 13 NIRCam filters, yielding our first constraints to diffuse light at 0.9–4.5 μm. PEARLS is designed to be of lasting benefit to the community.

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Section: Jwst Sky-sb Estimates and Possible Limits To Diffuse Lightsupporting

confidence: 83%

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confidence: 99%

JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results

Windhorst

Cohen

Jansen

et al. 2022

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The Isotropic Interplanetary Dust Cloud and Near-infrared Extragalactic Background Light Observed with COBE/DIRBE

Sano

Matsuura

Yomo

et al. 2020

ApJ

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We report observation of isotropic interplanetary dust (IPD) by analyzing the infrared (IR) maps of the Diffuse Infrared Background Experiment (DIRBE) on board the Cosmic Background Explorer (COBE) spacecraft. To search for the isotropic IPD, we perform new analysis in terms of the solar elongation angle (ϵ), because we expect the zodiacal light (ZL) intensity from the isotropic IPD to decrease as a function of ϵ. We use the DIRBE weekly averaged maps covering 64° ≲ ϵ ≲ 124° and inspect the ϵ dependence of residual intensity after subtracting conventional ZL components. We find the ϵ dependence of the residuals, indicating the presence of the isotropic IPD. However, the mid-IR ϵ dependence is different from that of the isotropic IPD model at ϵ ≳ 90°, where the residual intensity increases as a function of ϵ. To explain the observed ϵ dependence, we assume a spheroidal IPD cloud showing higher density farther away from the Sun. We estimate the intensity of the near-IR extragalactic background light (EBL) by subtracting the spheroidal component, assuming the spectral energy distribution from the residual brightness at 12 μm. The EBL intensity is derived as , , and at 1.25, 2.2, and 3.5 μm, respectively. The EBL is still a few times larger than the integrated light of normal galaxies, suggesting the existence of unaccounted-for extragalactic sources.

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Inferred Measurements of the Zodiacal Light Absolute Intensity through Fraunhofer Absorption Line Spectroscopy with CIBER

Korngut

Kim²,

Arai³

et al. 2022

ApJ

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Scattered sunlight from the interplanetary dust (IPD) cloud in our solar system presents a serious foreground challenge for spectrophotometric measurements of the extragalactic background light (EBL). In this work, we report on inferred measurements of the absolute intensity of the zodiacal light (ZL) using the novel technique of Fraunhofer line spectroscopy on the deepest 8542 Å line of the near-infrared Ca ii absorption triplet. The measurements are performed with the narrow band spectrometer (NBS) on board the Cosmic Infrared Background Experiment sounding rocket instrument. We use the NBS data to test the accuracy of two ZL models widely cited in the literature, the Kelsall and Wright models, which have been used in foreground removal analyses that produce high and low EBL results respectively. We find a mean reduced χ 2 = 3.5 for the Kelsall model and χ 2 = 2.0 for the Wright model. The best description of our data is provided by a simple modification to the Kelsall model, which includes a free ZL offset parameter. This adjusted model describes the data with a reduced χ 2 = 1.5 and yields an inferred offset amplitude of 46 ± 19 nW m−2 sr−1 extrapolated to 12500 Å. These measurements elude to the potential existence of a dust cloud component in the inner solar system whose intensity does not strongly modulate with the Earth’s motion around the Sun.

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Is the infrared background excess explained by the isotropic zodiacal light from the outer solar system?

Cited by 3 publications

References 48 publications

JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results

JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results

The Isotropic Interplanetary Dust Cloud and Near-infrared Extragalactic Background Light Observed with COBE/DIRBE

Inferred Measurements of the Zodiacal Light Absolute Intensity through Fraunhofer Absorption Line Spectroscopy with CIBER

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