RECORD
A census of radio-selected AGN on the COSMOS field and of their FIR properties
Astrophysics of Galaxies · Submitted 21 Sep 2017
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim By exploiting the better statistics of the new sample, we confirm the results of Magliocchetti et al. (2014): the probability for a radio-selected AGN to be detected at FIR wavelengths is both a function of radio luminosity and redshift, whereby powerful sources are more likely FIR emitters at earlier epochs.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
We use the new catalogue by Laigle et al. (2016) to provide a full census of VLA-COSMOS radio sources. We identify 90% of such sources and sub-divide them into AGN and star-forming galaxies on the basis of their radio luminosity. The AGN sample is COMPLETE with respect to radio selection at all z<3.5. Out of 704 AGN, 272 have a counterpart in the Herschel maps. By exploiting the better statistics of the new sample, we confirm the results of Magliocchetti et al. (2014): the probability for a radio-selected AGN to be detected at FIR wavelengths is both a function of radio luminosity and redshift, whereby powerful sources are more likely FIR emitters at earlier epochs. Such an emission is due to star-forming processes within the host galaxy. FIR emitters and non-FIR emitters only differentiate in the z<1 universe. At higher redshifts they are indistinguishable from each other, as there is no difference between FIR-emitting AGN and star-forming galaxies. Lastly, we focus on radio AGN which show AGN emission at other wavelengths. We find that MIR emission is mainly associated with ongoing star-formation and with sources which are smaller, younger and more radio luminous than the average parent population. X-ray emitters instead preferentially appear in more massive and older galaxies. We can therefore envisage an evolutionary track whereby the first phase of a radio-active AGN and of its host galaxy is associated with MIR emission, while at later stages the source becomes only active at radio wavelengths and possibly also in the X-ray.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We use the new catalogue by Laigle et al. (2016) to provide a full census of VLA-COSMOS radio sources. | method 0.62 | 0.72 | 0.02 | asserted 0.97 |
| s1 | We identify 90% of such sources and sub-divide them into AGN and star-forming galaxies on the basis of their radio luminosity. | method 0.84 | 0.92 | 0.04 | asserted 1.00 |
| s2 | The AGN sample is COMPLETE with respect to radio selection at all z<3.5. | result 0.76 | 0.71 | 0.10 | asserted 1.00 |
| s3 | Out of 704 AGN, 272 have a counterpart in the Herschel maps. | result 0.95 | 0.87 | 0.04 | asserted 1.00 |
| s4 | By exploiting the better statistics of the new sample, we confirm the results of Magliocchetti et al. (2014): the probability for a radio-selected AGN to be detected at FIR wavelengths is both a function of radio luminosity and redshift, whereby powerful sources are more likely FIR emitters at earlier epochs. | result 0.99 | 0.57 | 0.64 | asserted 1.00 |
| s5 | Such an emission is due to star-forming processes within the host galaxy. | interpretation 0.99 | 0.26 | 0.06 | asserted 1.00 |
| s6 | FIR emitters and non-FIR emitters only differentiate in the z<1 universe. | result 0.98 | 0.84 | 0.11 | asserted 1.00 |
| s7 | At higher redshifts they are indistinguishable from each other, as there is no difference between FIR-emitting AGN and star-forming galaxies. | result 0.80 | 0.80 | 0.14 | asserted 1.00 |
| s8 | Lastly, we focus on radio AGN which show AGN emission at other wavelengths. | contribution 0.97 | 0.52 | 0.02 | asserted 0.60 |
| s9 | We find that MIR emission is mainly associated with ongoing star-formation and with sources which are smaller, younger and more radio luminous than the average parent population. | result 1.00 | 0.95 | 0.08 | asserted 1.00 |
| s10 | X-ray emitters instead preferentially appear in more massive and older galaxies. | result 1.00 | 0.90 | 0.05 | asserted 0.99 |
| s11 | We can therefore envisage an evolutionary track whereby the first phase of a radio-active AGN and of its host galaxy is associated with MIR emission, while at later stages the source becomes only active at radio wavelengths and possibly also in the X-ray. | interpretation 1.00 | 0.68 | 0.26 | speculative 0.73 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
We use the new catalogue by Laigle et al. (2016) to provide a full census of VLA-COSMOS radio sources. We identify 90% of such sources and sub-divide them into AGN and star-forming galaxies on the basis of their radio luminosity. The AGN sample is COMPLETE with respect to radio selection at all z<3.5. Out of 704 AGN, 272 have a counterpart in the Herschel maps. By exploiting the better statistics of the new sample, we confirm the results of Magliocchetti et al. (2014): the probability for a radio-selected AGN to be detected at FIR wavelengths is both a function of radio luminosity and redshift, whereby powerful sources are more likely FIR emitters at earlier epochs. Such an emission is due to star-forming processes within the host galaxy. FIR emitters and non-FIR emitters only differentiate in the z<1 universe. At higher redshifts they are indistinguishable from each other, as there is no difference between FIR-emitting AGN and star-forming galaxies. Lastly, we focus on radio AGN which show AGN emission at other wavelengths. We find that MIR emission is mainly associated with ongoing star-formation and with sources which are smaller, younger and more radio luminous than the average parent population. X-ray emitters instead preferentially appear in more massive and older galaxies. We can therefore envisage an evolutionary track whereby the first phase of a radio-active AGN and of its host galaxy is associated with MIR emission, while at later stages the source becomes only active at radio wavelengths and possibly also in the X-ray.
Human review
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.