TY - JOUR
T1 - Comparison of diffuse infrared and far-ultraviolet emission in the Large Magellanic Cloud
T2 - The data
AU - Saikia, Gautam
AU - Shalima, P.
AU - Gogoi, Rupjyoti
AU - Pathak, Amit
N1 - Publisher Copyright:
© 2016 Elsevier Ltd
PY - 2016/11/15
Y1 - 2016/11/15
N2 - Dust scattering is the main source of diffuse emission in the far-ultraviolet (FUV). For several locations in the Large Magellanic Cloud (LMC), Far Ultraviolet Spectroscopic Explorer (FUSE) satellite has observed diffuse radiation in the FUV with intensities ranging from 1000 to 3×105 photon units and diffuse fraction between 5% and 20% at 1100 Å. Here, we compare the FUV diffuse emission with the mid-infrared (MIR) and far-infrared (FIR) diffuse emission observed by the Spitzer Space Telescope and the AKARI satellite for the same locations. The intensity ratios in the different MIR and FIR bands for each of the locations will enable us to determine the type of dust contributing to the diffuse emission as well as to derive a more accurate 3D distribution of stars and dust in the region, which in turn may be used to model the observed scattering in the FUV. In this work we present the infrared (IR) data for two different regions in LMC, namely N11 and 30 Doradus. We also present the FUV~IR correlation for different infrared bands.
AB - Dust scattering is the main source of diffuse emission in the far-ultraviolet (FUV). For several locations in the Large Magellanic Cloud (LMC), Far Ultraviolet Spectroscopic Explorer (FUSE) satellite has observed diffuse radiation in the FUV with intensities ranging from 1000 to 3×105 photon units and diffuse fraction between 5% and 20% at 1100 Å. Here, we compare the FUV diffuse emission with the mid-infrared (MIR) and far-infrared (FIR) diffuse emission observed by the Spitzer Space Telescope and the AKARI satellite for the same locations. The intensity ratios in the different MIR and FIR bands for each of the locations will enable us to determine the type of dust contributing to the diffuse emission as well as to derive a more accurate 3D distribution of stars and dust in the region, which in turn may be used to model the observed scattering in the FUV. In this work we present the infrared (IR) data for two different regions in LMC, namely N11 and 30 Doradus. We also present the FUV~IR correlation for different infrared bands.
UR - https://www.scopus.com/pages/publications/84961120923
UR - https://www.scopus.com/inward/citedby.url?scp=84961120923&partnerID=8YFLogxK
U2 - 10.1016/j.pss.2016.03.001
DO - 10.1016/j.pss.2016.03.001
M3 - Article
AN - SCOPUS:84961120923
SN - 0032-0633
VL - 133
SP - 90
EP - 96
JO - Planetary and Space Science
JF - Planetary and Space Science
ER -