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An Empirically Based Model for Predicting Infrared Luminosity Functions, Deep Infrared Galaxy Counts and the Diffuse Infrared Background
Astrophysics · Submitted 29 Sep 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Comparisons of our galaxy count results with existing data indicate that either galaxy luminosity evolution is not much stronger than Q=3.1, where L is proportional to (1+z)^{Q}, or that this evolution does not continue beyond a redshift of 2.
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The abstract, sentence by sentence
We predict luminosity functions and number counts for extragalactic infrared sources at various wavelengths using the framework of our empirically based model. Comparisons of our galaxy count results with existing data indicate that either galaxy luminosity evolution is not much stronger than Q=3.1, where L is proportional to (1+z)^{Q}, or that this evolution does not continue beyond a redshift of 2. However, a derivation of the far infrared background from COBE-DIRBE data suggests a stronger evolution for far infrared emission with Q > 4 in the redshift range beteen 0 and 1. We discuss several interpretations of these results and also discuss how future observations can reconcile this apparent conflict. We also make predictions of the redshift distributions of extragalactic infrared sources at selected flux levels which can be tested by planned detectors. Finally, we predict the fluxes at which various future surveys will become confusion limited.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We predict luminosity functions and number counts for extragalactic infrared sources at various wavelengths using the framework of our empirically based model. | contribution 0.96 | 0.93 | 0.13 | asserted 1.00 |
| s1 | Comparisons of our galaxy count results with existing data indicate that either galaxy luminosity evolution is not much stronger than Q=3.1, where L is proportional to (1+z)^{Q}, or that this evolution does not continue beyond a redshift of 2. | result 0.62 | 0.77 | 0.27 | hedged possibility 0.98 |
| s2 | However, a derivation of the far infrared background from COBE-DIRBE data suggests a stronger evolution for far infrared emission with Q > 4 in the redshift range beteen 0 and 1. | result 0.85 | 0.38 | 0.14 | hedged possibility 0.95 |
| s3 | We discuss several interpretations of these results and also discuss how future observations can reconcile this apparent conflict. | interpretation 0.89 | 0.45 | 0.06 | unclear 0.82 |
| s4 | We also make predictions of the redshift distributions of extragalactic infrared sources at selected flux levels which can be tested by planned detectors. | result 0.49 | 0.93 | 0.07 | asserted 0.97 |
| s5 | Finally, we predict the fluxes at which various future surveys will become confusion limited. | result 0.85 | 0.91 | 0.07 | asserted 1.00 |
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The paper
Original abstract
We predict luminosity functions and number counts for extragalactic infrared sources at various wavelengths using the framework of our empirically based model. Comparisons of our galaxy count results with existing data indicate that either galaxy luminosity evolution is not much stronger than Q=3.1, where L is proportional to (1+z)^{Q}, or that this evolution does not continue beyond a redshift of 2. However, a derivation of the far infrared background from COBE-DIRBE data suggests a stronger evolution for far infrared emission with Q > 4 in the redshift range beteen 0 and 1. We discuss several interpretations of these results and also discuss how future observations can reconcile this apparent conflict. We also make predictions of the redshift distributions of extragalactic infrared sources at selected flux levels which can be tested by planned detectors. Finally, we predict the fluxes at which various future surveys will become confusion limited.
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3 arXiv papers cite this in 3 sentences
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The semi-analytical “model D” proposed by Finke et al [ref] , modeling the star formation rate recently introduced by Hopkins and Beacom [ref] is adopted for CIOB (for a more detailed treatment of infrared and optical background radiations we refer to [ref] and Refs. therein).
HERMES: Simulating the Propagation of Ultra-High Energy Cosmic Rays · Modeling the extragalactic background radiation · 0.97
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