The Origin of the X-ray Emission from the Non-Starburst Gas-Rich Luminous Infrared Galaxies Arp 302
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arXiv
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| Format: | Preprint |
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2024
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| _version_ | 1866910288210558976 |
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| author | Jiang, Jiachen Baker, William Young, Andrew Gallo, Luigi |
| author_facet | Jiang, Jiachen Baker, William Young, Andrew Gallo, Luigi |
| contents | We present an analysis of the XMM-Newton observation of luminous infrared merging galaxies Arp 302 and a joint re-analysis of its Chandra observation. In particular, we focus on the more significant X-ray emitter of the pair, Arp 302N. Chandra detects significant soft X-ray emission from the hot gas in the star-forming region of Arp 302N spreading up to 12 kpc. We estimate the star-formation rate of Arp 302N to be around 1-2 $M_{\odot}$ yr$^{-1}$ based on the X-ray luminosity of the star-forming region, similar to previous measurements at longer wavelengths. Chandra and XMM-Newton observations show evidence of a Si XIII emission line with 86% confidence. Our best-fit model infers a super-solar silicon abundance in the star-forming region, likely related to the past core-collapse supernovae in this galaxy. Similar silicon overabundance was reported in the circumstellar medium of core-collapse supernova remnants in our Galaxy.
We also detect narrow Fe K$α$ and Fe K$β$ (98.6% confidence) emission lines as part of the AGN emission. Our best-fit spectral model using Mytorus indicates the evidence of a heavily obscured power-law emission with $N_{\rm H}>3\times10^{24}$ cm$^{-2}$ in addition to a weak, unobscured power-law emission. The scattering fraction of the unobscured power-law emission from Compton-thin materials is 0.7%. All these spectral features suggest evidence of a Seyfert 2-like AGN in Arp 302N. The X-ray measurement of its AGN activity is consistent with the previous Spitzer measurement of the same object. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2401_03117 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Origin of the X-ray Emission from the Non-Starburst Gas-Rich Luminous Infrared Galaxies Arp 302 Jiang, Jiachen Baker, William Young, Andrew Gallo, Luigi High Energy Astrophysical Phenomena We present an analysis of the XMM-Newton observation of luminous infrared merging galaxies Arp 302 and a joint re-analysis of its Chandra observation. In particular, we focus on the more significant X-ray emitter of the pair, Arp 302N. Chandra detects significant soft X-ray emission from the hot gas in the star-forming region of Arp 302N spreading up to 12 kpc. We estimate the star-formation rate of Arp 302N to be around 1-2 $M_{\odot}$ yr$^{-1}$ based on the X-ray luminosity of the star-forming region, similar to previous measurements at longer wavelengths. Chandra and XMM-Newton observations show evidence of a Si XIII emission line with 86% confidence. Our best-fit model infers a super-solar silicon abundance in the star-forming region, likely related to the past core-collapse supernovae in this galaxy. Similar silicon overabundance was reported in the circumstellar medium of core-collapse supernova remnants in our Galaxy. We also detect narrow Fe K$α$ and Fe K$β$ (98.6% confidence) emission lines as part of the AGN emission. Our best-fit spectral model using Mytorus indicates the evidence of a heavily obscured power-law emission with $N_{\rm H}>3\times10^{24}$ cm$^{-2}$ in addition to a weak, unobscured power-law emission. The scattering fraction of the unobscured power-law emission from Compton-thin materials is 0.7%. All these spectral features suggest evidence of a Seyfert 2-like AGN in Arp 302N. The X-ray measurement of its AGN activity is consistent with the previous Spitzer measurement of the same object. |
| title | The Origin of the X-ray Emission from the Non-Starburst Gas-Rich Luminous Infrared Galaxies Arp 302 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2401.03117 |