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Understanding Dust Extinction in the Milky Way: Effects of Inclination, ICM, and High-Velocity Clouds

This study explores the multifaceted nature of dust extinction in the Milky Way Galaxy, focusing on internal extinction in spiral galaxies, extinction caused by the Intergalactic Medium (ICM) and Super-Galactic Plane, and the role of high-velocity clouds (HVCs). The effects of inclination on brightness are analyzed, and various scientific projects are proposed to deepen our understanding of how dust impacts observations of UV light from distant objects. The research builds on past studies and aims to provide insights into the luminosity function and dust concentration in galactic structures.

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Understanding Dust Extinction in the Milky Way: Effects of Inclination, ICM, and High-Velocity Clouds

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  1. Dust extinction and the SDSS 조정연 (J. Cho) (충남대)

  2. 1. Internal Extinction (effect of inclination) 2. Extinction by the ICM/Super-Galactic Plane 3. Extinction by HVCs (high velocity clouds) cluster HVC Milky Way Galaxy

  3. Topic 1: Internal Extinction in Spirals (effect of inclination)

  4. Sombrero

  5. NGC5866

  6. Tully et al 1998 K: ~2.2mm R: ~700nm I: ~ 900nm Mag. after Galactic & k-corrections What causes the scatter? * Note: Insignificant absorption at K-band

  7. Answer: Inclination! b a

  8. Mag. after Galactic, k-, & inclination correction

  9. Possible projects: • Repeat Tully et al 1998? Shao et al 2006? • Study the effect of concentration • Study the effect of inclination for bulge and disk separately • Study the effect of inclination for blue- and red-bulge • separately

  10. Luminosity function Driver et al 07

  11. Park & Choi (2005) spirals Calculate similar plots for bulge and disk separately?

  12. Topic 2: Extinction by ICM/SGP Dust in galaxy clusters - IR emission detected (Stickel et al 1998; Cox et al 1998; Bregmann 1990)) * Mdust ~ 108-9 Msun - Extinction of UV objects behind Coma observed (Boyle et al 1998; Dwek et al 1990)

  13. Stickel et al 1998

  14. Nollenberg et al 2003

  15. Possible projects • Color change by clusters • Change of number count?

  16. Topic 3: Extinction by HVCs 1) High velocity clouds (HVCs) + Compact HVCs (CHVCs) * |VLSR| > 90 km/sec 2) Intermediate velocity clouds (IVCs) * 90 > |VLSR| > 30 km/sec

  17. 1) HVCs: - Muller et al (1963) : 1st detection in H21cm - |VLSR| > 90 km/sec - low metallicity (~0.1 solar for Complex C; ~0.3 for the Magellanic Stream) - catalog: Wakker & van Woerden (1991) - failed CO detection: Wakker et al (1997) C Magellanic Stream Mivillie-Deschenes (2006)

  18. Richter (2006)

  19. HVC

  20. Wakker et al 1997: failed to detect CO

  21. Compact HVCs • -Angular size: < 2o • Braun & Burton (1999): 66 CHVCs • -de Heij et al (2002): 67 CHVCs • Putman et al (2002): 179 CHVCs •  de Heij et al (2002b): 216 CHVCs • -origin? • Blitz et al (1999): far away (~1Mpc) massive (~107 Msun) • dark matter clouds? • *problem: Recent measurements indicate • that distance ~ 10 kpc • Infall of low metallicity gas from intergalactic space? • Galactic fountain? • Observation of chemical composition is crucial • * Do they have star formation? Do they have molecules?

  22. 2o ~1Mpc Blitz (1999) : Massive satellites Falling primordial gas Galactic fountain

  23. HVCs in M31

  24. Are there dust grains?

  25. They do contain dust grains  clumpy structures? Complex C Mivillie-Deschenes et al (2005)

  26. 2) IVCs - 90>|VLSR| > 30 km/sec - metallicity : 0.5 ~ 1 solar - catalog: Kuntz & Danly (1996) also Wakker (2001) - a few CO observations

  27. Weiss et al (1999): CO observation CO CO CO See also Mebold et al 1985 Heiles, Reach, & Koo 1988 Desert, Bazell & Blitz 1990

  28. IVCs do have H2

  29. Systematic studies of dust in IVCs will be useful This is HI map

  30. Conclusion • Possible projects • Effect of inclination • Dust in the ICM • Dust in HVCs/IVCs

  31. Extinction by galaxy?

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