Hostname: page-component-cd9895bd7-gbm5v Total loading time: 0 Render date: 2024-12-12T09:43:44.460Z Has data issue: false hasContentIssue false
  • English
  • Français

Survey of Correlated FIR, HI, CO, and Radio-Continuum Emission Features in the Multi-Phase Milky Way

Published online by Cambridge University Press:  25 May 2016

W.F. Wall  and
W.H. Waller
W.F. Wall
Affiliation:
INAOE, México NASA/GSFC, USA StarStuff Incorporated
W.H. Waller
Affiliation:
StarStuff Incorporated Hughes STX, NASA/GSFC USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The interstellar medium (ISM) is rich with structure on varying size scales, reflecting its diverse energetics and dynamics. A step toward understanding this structure is to enhance the visibility of the structure on finer size scales. We present maps of a section of the Galactic plane filtered with the Median Normalized Spatial Filter (MNSF, a median smoothed map is divided into the original map), which emphasizes higher latitude emission relative to that of the plane itself (see also Waller et al., this volume, p. 194). The maps also illustrate the spatial correlations between the interstellar dust and the various gas phases: ionized, atomic, and molecular. The dust is represented by the IR emission maps of the IRAS survey, the ionized gas by the radio continuum maps at 1.4 GHz (Reich 1978, northern sky) and 2.3 GHz (Jonas & Baart 1995, southern sky), the atomic gas by surveys of the HI 21 cm line emission (Heiles & Habing 1974, Weaver & Williams 1973, Cleary et al. 1979, Kerr et al. 1986), and the molecular gas by surveys of the CO J = 1 → 0 line emission (Dame et al. 1987).

Type
Part 3. The Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 179: New Horizons from Multi-Wavelength Sky Surveys , 1998 , pp. 191 - 193
Copyright
Copyright © Kluwer 1998 

References

Cleary, M. N., Heiles, C., & Haslam, C. G. T. 1979, Astron. Astrophys. Suppl., 36, 95.Google Scholar
Dame, T. M., Ungerechts, H., Cohen, R. S., de Geus, E. J., Grenier, I. A., May, J., Murphy, D. C., Nyman, L.-Å., & Thaddeus, P. 1987, Astrophys. J., 322, 706.Google Scholar
Heiles, C. & Habing, H. J. 1974, Astron. Astrophys. Suppl., 14, 1.Google Scholar
Jonas, J.L. & Baart, E. E. 1995, Astrophys. Sp. Sc., 230, 351.CrossRefGoogle Scholar
Kerr, F. J., Bowers, P. F., Jackson, P. D., & Kerr, M. 1986, Astron. Astrophys. Suppl., 66, 373.Google Scholar
Reich, W. 1978, Astron. Astrophys., 64, 407.Google Scholar
Weaver, H. & Williams, W. 1973, Astron. Astrophys. Suppl., 8, 1.Google Scholar