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AKARI and IRAS: From Beam Corrections to SEDs
Astrophysics of Galaxies · Submitted 10 Aug 2018
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim This investigation finds that our simple 2MASS-based beam correction scheme is inadequate for these larger and more complex sources.
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The abstract, sentence by sentence
There is significant scientific value to be gained from combining AKARI fluxes with data at other far-IR wavelengths from the IRAS and Herschel missions. To be able to do this we must ensure that there are no systematic differences between the datasets that need to be corrected before the fluxes are compatible with each other. One such systematic effect identified in the BSCv1 data is the issue of beam corrections. We determine these for the BSCv2 data by correlating ratios of appropriate IRAS and AKARI bands with the difference in 2MASS J band extended and point source magnitudes for sources cross matched between the IRAS FSC, AKARI BSCv2 and 2MASS catalogs. We find significant correlations (p<< 10^-13) indicating that beam corrections are necessary in the 65 and 90 micron bands. We then use these corrected fluxes to supplement existing data in spectral energy distribution (SED) fits for ultraluminous infrared galaxies in the HERUS survey. The addition of AKARI fluxes makes little difference to the results of simple (T,beta) fits to the SEDs of these sources, though there is a general decrease in reduced chi^2 values. The utility of the extra AKARI data, however, is in allowing physically more realistic SED models with more parameters to be fit to the data. We also extend our analysis of beam correction issues in the AKARI data by examining the Herschel Reference Sample, which have Herschel photometry from 100 to 500 microns and which are more spatially extended than the HERUS ULIRGs. Thirty-four of the HRS sources have good Herschel SEDs and matching data from AKARI. This investigation finds that our simple 2MASS-based beam correction scheme is inadequate for these larger and more complex sources. There are also indications that additional beam corrections at 140 and 160 microns are needed for these sources, extended on scales >1 arcminute.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | There is significant scientific value to be gained from combining AKARI fluxes with data at other far-IR wavelengths from the IRAS and Herschel missions. | background 1.00 | 0.09 | 0.06 | asserted 0.87 |
| s1 | To be able to do this we must ensure that there are no systematic differences between the datasets that need to be corrected before the fluxes are compatible with each other. | background 0.72 | 0.07 | 0.03 | asserted 0.97 |
| s2 | One such systematic effect identified in the BSCv1 data is the issue of beam corrections. | background 0.89 | 0.18 | 0.04 | asserted 1.00 |
| s3 | We determine these for the BSCv2 data by correlating ratios of appropriate IRAS and AKARI bands with the difference in 2MASS J band extended and point source magnitudes for sources cross matched between the IRAS FSC, AKARI BSCv2 and 2MASS catalogs. | method 1.00 | 0.96 | 0.04 | asserted 0.99 |
| s4 | We find significant correlations (p<< 10^-13) indicating that beam corrections are necessary in the 65 and 90 micron bands. | result 0.99 | 0.97 | 0.16 | asserted 0.93 |
| s5 | We then use these corrected fluxes to supplement existing data in spectral energy distribution (SED) fits for ultraluminous infrared galaxies in the HERUS survey. | contribution 0.66 | 0.93 | 0.07 | asserted 0.96 |
| s6 | The addition of AKARI fluxes makes little difference to the results of simple (T,beta) fits to the SEDs of these sources, though there is a general decrease in reduced chi^2 values. | result 0.98 | 0.94 | 0.09 | asserted 1.00 |
| s7 | The utility of the extra AKARI data, however, is in allowing physically more realistic SED models with more parameters to be fit to the data. | interpretation 0.97 | 0.81 | 0.29 | asserted 1.00 |
| s8 | We also extend our analysis of beam correction issues in the AKARI data by examining the Herschel Reference Sample, which have Herschel photometry from 100 to 500 microns and which are more spatially extended than the HERUS ULIRGs. | contribution 0.92 | 0.87 | 0.04 | asserted 0.97 |
| s9 | Thirty-four of the HRS sources have good Herschel SEDs and matching data from AKARI. | method 0.58 | 0.73 | 0.03 | asserted 1.00 |
| s10 | This investigation finds that our simple 2MASS-based beam correction scheme is inadequate for these larger and more complex sources. | result 0.73 | 0.95 | 0.24 | asserted 1.00 |
| s11 | There are also indications that additional beam corrections at 140 and 160 microns are needed for these sources, extended on scales >1 arcminute. | result 0.96 | 0.94 | 0.17 | hedged possibility 0.99 |
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The paper
Original abstract
There is significant scientific value to be gained from combining AKARI fluxes with data at other far-IR wavelengths from the IRAS and Herschel missions. To be able to do this we must ensure that there are no systematic differences between the datasets that need to be corrected before the fluxes are compatible with each other. One such systematic effect identified in the BSCv1 data is the issue of beam corrections. We determine these for the BSCv2 data by correlating ratios of appropriate IRAS and AKARI bands with the difference in 2MASS J band extended and point source magnitudes for sources cross matched between the IRAS FSC, AKARI BSCv2 and 2MASS catalogs. We find significant correlations (p<< 10^-13) indicating that beam corrections are necessary in the 65 and 90 micron bands. We then use these corrected fluxes to supplement existing data in spectral energy distribution (SED) fits for ultraluminous infrared galaxies in the HERUS survey. The addition of AKARI fluxes makes little difference to the results of simple (T,beta) fits to the SEDs of these sources, though there is a general decrease in reduced chi^2 values. The utility of the extra AKARI data, however, is in allowing physically more realistic SED models with more parameters to be fit to the data. We also extend our analysis of beam correction issues in the AKARI data by examining the Herschel Reference Sample, which have Herschel photometry from 100 to 500 microns and which are more spatially extended than the HERUS ULIRGs. Thirty-four of the HRS sources have good Herschel SEDs and matching data from AKARI. This investigation finds that our simple 2MASS-based beam correction scheme is inadequate for these larger and more complex sources. There are also indications that additional beam corrections at 140 and 160 microns are needed for these sources, extended on scales >1 arcminute.
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