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ISM conditions in low z QSOs

ISM conditions in low z QSOs. background. Star formation, AGN activity and the ISM Quasi-stellar objects (QSO) : are the most energetic AGN and are thought to be an important phase of massive galaxy evolution. photodissociation region (PDR). PDR. PDR is created by UV radiation

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ISM conditions in low z QSOs

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  1. ISM conditions in low z QSOs

  2. background • Star formation, AGN activity and the ISM • Quasi-stellar objects (QSO) : are the most energetic AGN and are thought to be an important phase of massive galaxy evolution. • photodissociation region (PDR)

  3. PDR • PDR is created by UV radiation • (Kaufman et al. 1999) established the PDR model • [CII] 158μm, [OI] 63μm, [CO(1-0)] 115.271GHz(2.6mm) and so on can be the ISM diagnostics

  4. task • measure CO luminosity from the LMT/RSR spectra  • use CLOUDY or other PDR modeling (PDR toolbox) to get ISM condition constraints from available lines: CO, CII, OI

  5. Samples 5/9 have all 3 emission lines and FIR luminosity (W1005+43, W1355+20, W1422+29, W1634+20, W1659+18) (Zhao, Yan, & Tsai 2016)

  6. Fit CO emission line W0752+19 & W0946+13 did not find the CO(1-0)

  7. Convert spectra to Luminosity • integrate under the Gaussian to get line intensity I in unit of K km s^-1 • use the special factor 7 for LMT early work to get S_coδνin unit of Jy km s^-1 • convert S_coδνto Luminosity (Kirkpatrick, et al. 2014) and (Carilli & Walter 2013)

  8. Fit CO emission line

  9. N & G

  10. N & G

  11. N & G

  12. N & G W1355 W1005 W1422 W1634 W1659

  13. Thank you!

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