Hot gas and the gaseous structure of the galaxy
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| Natura: | Artículo científico |
| Lingua: | en |
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Universidad Nacional Autónoma de México
2000
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| _version_ | 1876441636943167488 |
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| author | Donald P. Cox |
| author_facet | Donald P. Cox |
| contents | Hot gas and the gaseous structure of the galaxy Donald P. Cox Física, Astronomía y Matemáticas RAYS: ISM ISM: GENERAL ISM: BUBBLES GALAXY: GENERAL GALAXY: STRUCTURE Major advances have been made in the past decade in our knowledge of the hotinterstellar gas of our Milky Way galaxy. The Di use X-ray Spectrometer obtainedspectra in the 0.15{0.28 keV range from the Galactic plane (i.e., from the LocalBubble) that show emission lines and blends. These spectra conrm that the soft Xraybackground in this energy range is thermal in origin, at temperature roughly 106K, but the spectra are not well t by standard plasma emission models. Data fromthe ROSAT satellite, both from the all-sky survey and from pointed observations,have provided constraints on the distances to some of the hot gas emitting regions inthe Local Bubble, the local ISM, and the Galactic halo. These data conrm that thelocal bubble is 100 pc in size, and they indicate the existence of two independenthot gas components in the Galactic halo: a patchy, localized lower temperaturehalo component near 106 K, and a smoother higher temperature halo component atseveral 106 K, with a spatial structure reective of the overall structure of the galaxy.The ASCA satellite has observed emission from hot plasmas at temperatures above107 K from the Galactic ridge, from two di erent galactic center components, andfrom the Galactic bulge. More recently, the Wisconsin/Goddard micro-calorimetersounding rocket payload has observed the spectrum of the di use emission from(l; b) (90; 60) with a 1 sr eld of view over the 0.1{1 keV spectral range with 8 eV resolution. Lines from O VII and O VIII are clearly seen, but there are onlyupper limits to the expected Fe XVII lines. 2000 artículo científico 0185-1101 https://www.redalyc.org/articulo.oa?id=57100906 en http://www.redalyc.org/revista.oa?id=571 Revista Mexicana de Astronomía y Astrofísica application/pdf Universidad Nacional Autónoma de México Revista Mexicana de Astronomía y Astrofísica (México) Vol.9 |
| format | Artículo científico |
| id | redalyc_57100906 |
| institution | Redalyc |
| language | en |
| publishDate | 2000 |
| publisher | Universidad Nacional Autónoma de México |
| spellingShingle | Hot gas and the gaseous structure of the galaxy Donald P. Cox Física, Astronomía y Matemáticas RAYS: ISM ISM: GENERAL ISM: BUBBLES GALAXY: GENERAL GALAXY: STRUCTURE Hot gas and the gaseous structure of the galaxy Donald P. Cox Física, Astronomía y Matemáticas RAYS: ISM ISM: GENERAL ISM: BUBBLES GALAXY: GENERAL GALAXY: STRUCTURE Major advances have been made in the past decade in our knowledge of the hotinterstellar gas of our Milky Way galaxy. The Di use X-ray Spectrometer obtainedspectra in the 0.15{0.28 keV range from the Galactic plane (i.e., from the LocalBubble) that show emission lines and blends. These spectra conrm that the soft Xraybackground in this energy range is thermal in origin, at temperature roughly 106K, but the spectra are not well t by standard plasma emission models. Data fromthe ROSAT satellite, both from the all-sky survey and from pointed observations,have provided constraints on the distances to some of the hot gas emitting regions inthe Local Bubble, the local ISM, and the Galactic halo. These data conrm that thelocal bubble is 100 pc in size, and they indicate the existence of two independenthot gas components in the Galactic halo: a patchy, localized lower temperaturehalo component near 106 K, and a smoother higher temperature halo component atseveral 106 K, with a spatial structure reective of the overall structure of the galaxy.The ASCA satellite has observed emission from hot plasmas at temperatures above107 K from the Galactic ridge, from two di erent galactic center components, andfrom the Galactic bulge. More recently, the Wisconsin/Goddard micro-calorimetersounding rocket payload has observed the spectrum of the di use emission from(l; b) (90; 60) with a 1 sr eld of view over the 0.1{1 keV spectral range with 8 eV resolution. Lines from O VII and O VIII are clearly seen, but there are onlyupper limits to the expected Fe XVII lines. 2000 artículo científico 0185-1101 https://www.redalyc.org/articulo.oa?id=57100906 en http://www.redalyc.org/revista.oa?id=571 Revista Mexicana de Astronomía y Astrofísica application/pdf Universidad Nacional Autónoma de México Revista Mexicana de Astronomía y Astrofísica (México) Vol.9 |
| title | Hot gas and the gaseous structure of the galaxy |
| topic | Física, Astronomía y Matemáticas RAYS: ISM ISM: GENERAL ISM: BUBBLES GALAXY: GENERAL GALAXY: STRUCTURE |
| url | https://www.redalyc.org/articulo.oa?id=57100906 |