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- 01GQF14GFDSPNB303EV10EBSA7 classification A1.
- 01GQF14GFDSPNB303EV10EBSA7 date "2022".
- 01GQF14GFDSPNB303EV10EBSA7 language "eng".
- 01GQF14GFDSPNB303EV10EBSA7 type journalArticle.
- 01GQF14GFDSPNB303EV10EBSA7 hasPart 01GQF178818T3QKH67N78NNF1P.pdf.
- 01GQF14GFDSPNB303EV10EBSA7 subject "Physics and Astronomy".
- 01GQF14GFDSPNB303EV10EBSA7 doi "10.1051/0004-6361/202243930".
- 01GQF14GFDSPNB303EV10EBSA7 issn "0004-6361".
- 01GQF14GFDSPNB303EV10EBSA7 issn "1432-0746".
- 01GQF14GFDSPNB303EV10EBSA7 volume "664".
- 01GQF14GFDSPNB303EV10EBSA7 abstract "Context. The far-infrared (FIR) and sub-millimeter (submm) emissivity, ϵν, of the Milky Way (MW) cirrus is an important benchmark for dust grain models. Dust masses in other galaxies are generally derived from the FIR/submm using the emission properties of these MW-calibrated models. Aims: We seek to derive the FIR/submm ϵν in nine nearby spiral galaxies to check its compatibility with MW cirrus measurements. Methods: We obtained values of ϵν at 70-500 μm, using maps of dust emission from the Herschel satellite and of gas surface density from the THINGS and HERACLES surveys on a scale generally corresponding to 440 pc. We studied the variation of ϵν with the surface brightness ratio Iν(250 μm)/Iν(500 μm), a proxy for the intensity of the interstellar radiation field heating the dust. Results: We find that the average value of ϵν agrees with MW estimates for pixels sharing the same color as the cirrus, namely, for Iν(250 μm)/Iν(500 μm)=4.5. For Iν(250 μm)/Iν(500 μm)> 5, the measured emissivity is instead up to a factor ∼2 lower than predicted from MW dust models heated by stronger radiation fields. Regions with higher Iν(250 μm)/Iν(500 μm) are preferentially closer to the galactic center and have a higher overall (stellar+gas) surface density and molecular fraction. The results do not depend strongly on the adopted CO-to-molecular conversion factor and do not appear to be affected by the mixing of heating conditions. Conclusions: Our results confirm the validity of MW dust models at low density, but are at odds with predictions for grain evolution in higher density environments. If the lower-than-expected ϵν at high Iν(250 μm)/Iν(500 μm) is the result of intrinsic variations in the dust properties, it would imply an underestimation of the dust mass surface density of up to a factor ∼2 when using current dust models.".
- 01GQF14GFDSPNB303EV10EBSA7 author 03A93704-F0EE-11E1-A9DE-61C894A0A6B4.
- 01GQF14GFDSPNB303EV10EBSA7 author ECF3615A-5EA8-11E7-897A-F52FAE28A064.
- 01GQF14GFDSPNB303EV10EBSA7 author F551D4EA-F0ED-11E1-A9DE-61C894A0A6B4.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:1f82006e-7349-48bb-a7cf-89ca9017a0f0.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:23034695-6ba0-482c-91b7-26b97c24e4b2.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:301dfe38-94c4-4a29-b20e-8be3fe095ce0.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:46efddda-998a-4ac6-9d11-00b7ccc19dbe.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:6ca0574d-5a4a-4381-a933-72904ebaa076.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:80fa01c4-1a98-4386-883e-78335d46b0b1.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:8833e6a7-6933-49a4-b53d-e87f32563413.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:9c75c1c6-423a-44d1-b25e-8ede25f9ba71.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:ae1e1f67-179a-4618-92dd-5448cc77265b.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:b3a389e5-1f17-4185-82c9-8c46dbe6f7bb.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:f967ee94-269e-4fbc-9372-ea5a1481e55e.
- 01GQF14GFDSPNB303EV10EBSA7 author urn:uuid:fa375227-c254-4821-9651-df70242cb6af.
- 01GQF14GFDSPNB303EV10EBSA7 dateCreated "2023-01-23T10:00:16Z".
- 01GQF14GFDSPNB303EV10EBSA7 dateModified "2024-07-09T14:50:19Z".
- 01GQF14GFDSPNB303EV10EBSA7 name "Dust emissivity in resolved spiral galaxies".
- 01GQF14GFDSPNB303EV10EBSA7 pagination urn:uuid:2544c505-78fa-40e4-8325-624583f4b95c.
- 01GQF14GFDSPNB303EV10EBSA7 sameAs LU-01GQF14GFDSPNB303EV10EBSA7.
- 01GQF14GFDSPNB303EV10EBSA7 sourceOrganization urn:uuid:e428397f-cf89-4104-9c29-fba27e21a474.
- 01GQF14GFDSPNB303EV10EBSA7 type A1.