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ISM conditions in low z QSOs

Explore the ISM in low redshift QSOs through diagnostics tasks, PDR modeling, and emission line analysis to reveal star formation and AGN activity. Learn how to measure CO luminosity and constraints using available lines.

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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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