AWhat changed
Hauser and colleagues analyzed ten COBE DIRBE infrared bands after modeling local foregrounds, reporting isotropic residuals consistent with a cosmic infrared background at 140 and 240 micrometres and upper limits at shorter wavelengths. Fixsen and colleagues used COBE FIRAS spectra and three foreground-separation approaches to estimate the far-infrared background spectrum from 125 to 2000 micrometres, finding consistency with the DIRBE measurements within their stated calibration uncertainties.
Scientific scope
Hauser and colleagues analyzed ten COBE DIRBE infrared bands after modeling local foregrounds, reporting isotropic residuals consistent with a cosmic infrared background at 140 and 240 micrometres and upper limits at shorter wavelengths. Fixsen and colleagues used COBE FIRAS spectra and three foreground-separation approaches to estimate the far-infrared background spectrum from 125 to 2000 micrometres, finding consistency with the DIRBE measurements within their stated calibration uncertainties. The DIRBE values depend on foreground subtraction and selected low-foreground regions; isotropy tests cover approximately 2% of the sky, and systematic foreground uncertainties dominate. The FIRAS methods share data, use a DIRBE zodiacal-light model and one explicitly assumes the DIRBE background; their agreement is therefore not three fully independent confirmations. The color method assumes an invariant Galactic spectrum and the line-template method has uncertain nonlinear foreground relationships. Derived spectral-fit parameters have strongly correlated uncertainties. Both teams credit a 1996 tentative FIRAS result by Puget and colleagues; the 1998 papers describe significant differences in inferred spectra. Extragalactic origin and implications for dust-obscured stellar history depend on models. The DIRBE contributor list shown here is incomplete.
Evidence
The linked original works support the scoped statement and contribution attribution. WRS has not independently replayed experiments or reconstructed a full mathematical proof. The DIRBE values depend on foreground subtraction and selected low-foreground regions; isotropy tests cover approximately 2% of the sky, and systematic foreground uncertainties dominate. The FIRAS methods share data, use a DIRBE zodiacal-light model and one explicitly assumes the DIRBE background; their agreement is therefore not three fully independent confirmations. The color method assumes an invariant Galactic spectrum and the line-template method has uncertain nonlinear foreground relationships. Derived spectral-fit parameters have strongly correlated uncertainties. Both teams credit a 1996 tentative FIRAS result by Puget and colleagues; the 1998 papers describe significant differences in inferred spectra. Extragalactic origin and implications for dust-obscured stellar history depend on models. The DIRBE contributor list shown here is incomplete.
Contributors
- The named authors in the research record · SCIENCE: These are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged.
- The COBE Diffuse Infrared Background Experiment Search for the Cosmic Infrared Background: I. Limits and Detections
- The Spectrum of the Extragalactic Far Infrared Background from the COBE FIRAS Observations
Provisional WRS assessment, edition 2026-10-28.1. Independent expert calibration is pending. This grade does not certify correctness or assign ownership.
Full scientific record · Browse contribution grades · Request a correction