A far-infrared survey of the galactic center

Odenwald, Sten; Fazio, G. G.

doi:10.1086/162345

Cited by 64 publications

(50 citation statements)

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“…Line emission from both molecular CO and atomic C peak sharply in our Galaxy's central few hundred parsecs, and a somewhat smaller region is quite bright in radio and infrared continuum emission as well (Figure 1; Altenhoff et al 1978, Mezger & Pauls 1979, Odenwald & Fazio 1984, Dame et al 1987, Handa et al 1987, Cox & Laureijs 1989, Bennett et al 1994. This compact and luminous nuclear region, hereafter designated the central molecular zone or CMZ (to distinguish this largely molecular region from the more extensive "H I nuclear disk" in which it is ensconced), produces ∼ 5-10% of our Galaxy's infrared and Lyman continuum luminosities and accounts for roughly 10% of our Galaxy's molecular gas content (Mezger 1978, Mezger & Pauls 1979, Hauser et al 1984, Scoville & Sanders 1987, Cox & Laureijs 1989, Güsten 1989, Scoville & Good 1989, Bloemen et al 1990, Wright et al 1991, Bennett et al 1994.…”

Section: The Arenamentioning

confidence: 83%

“…The distributions of both ionized gas and diffuse infrared emission in the CMZ (Altenhoff et al 1978, Odenwald & Fazio 1984, Handa et al 1987, Cox & Laureijs 1989 are more symmetric than the CO distribution (Figure 1), suggesting that heating sources are more evenly distributed than are the discrete clouds. In particular, the dust temperature drops regularly as r −0.3 from its central peak to its asymptotic value of 23 K near a radius of 200 pc.…”

Section: The Central Molecular Zonementioning

confidence: 95%

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The Galactic Center Environment

Morris

Serabyn

1996

Annu. Rev. Astron. Astrophys.

899

905

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The central half kiloparsec region of our Galaxy harbors a variety of phenomena unique to the central environment. This review discusses the observed structure and activity of the interstellar medium in this region in terms of its inevitable inflow toward the center of the Galactic gravitational potential well. A number of dissipative processes lead to a strong concentration of gas into a "Central Molecular Zone" of about 200-pc radius, in which the molecular medium is characterized by large densities, large velocity dispersions, high temperatures, and apparently strong magnetic fields. The physical state of the gas and the resultant star formation processes occurring in this environment are therefore quite unlike those occurring in the large-scale disk. Gas not consumed by star formation either enters a hot X ray-emitting halo and is lost as a thermally driven galactic wind or continues moving inward, probably discontinuously, through the domain of the few parsec-sized circumnuclear disks and eventually into the central parsec. There, the central radio source SgrA * currently accepts only a tiny fraction of the inflowing material, likely as a result of a limit cycle wherein the continual inflow of matter provokes star formation, which in turn can temporarily halt the inflow via mass-outflow winds.

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Section: The Arenamentioning

confidence: 83%

Section: The Central Molecular Zonementioning

confidence: 95%

The Galactic Center Environment

Morris

Serabyn

1996

Annu. Rev. Astron. Astrophys.

899

905

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“…Figure 34 shows the 1.4 GHz continuum image of the main components of the Sgr C complex: the Sgr C H ii region, the NTF, and H ii regions known as FIR 4, Sources C and D (Liszt & Spiker 1995;Roy 2003;Odenwald & Fazio 1984). The NTF has been labeled "Part A" and "Part B" after Roy (2003).…”

Section: H I Absorption Toward the Sgr C Complexmentioning

confidence: 99%

A HIGH-RESOLUTION SURVEY OF H I ABSORPTION TOWARD THE CENTRAL 200 pc OF THE GALACTIC CENTER

Lang¹,

Goss²,

Cyganowski³

et al. 2010

ApJS

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We present an H i absorption survey of the central 250 pc of the Galaxy. Very Large Array observations were made at 21 cm in the DnC and CnB configurations and have a resolution of ∼15 (0.6 pc at the Galactic center (GC) distance) and a velocity resolution of ∼2.5 km s −1 . This study provides H i data with high spatial resolution, comparable with the many high-resolution observations which have been made of GC sources over the past 10 years. Here we present an overview of the H i absorption toward ∼40 well-known continuum sources and a detailed comparison of the ionized, atomic, and molecular components of the interstellar medium for the Sgr B, Radio Arc, and Sgr C regions. In these well-known regions, the atomic gas appears to be closely correlated in both velocity and distribution to the ionized and molecular gas, indicating that it resides in photodissociation regions related to the H ii regions in the GC. Toward the majority of the radio continuum sources, H i absorption by the 3 kpc arm is detected, constraining these sources to lie beyond a 5 kpc distance in the Galaxy.

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“…(iii) Finally, we consider an alternative source of the synchrotron electrons in the Sgr C NTF and the case of collision of the −100 km s −1 cloud with this already existing NTF. Liszt & Spiker (1995) proposed that the HII region FIR 4 (Odenwald & Fazio 1984) is associated with the Sgr C NTF, which acts as the source of relativistic electrons. Figure 7 in Liszt & Spiker (1995) shows a molecular cloud around this HII region.…”

Section: Kpcmentioning

confidence: 99%

Constraints on distances to Galactic Centre non-thermal filaments from HI absorption

Roy

2003

A&A

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Abstract. We have studied HI absorption towards three non-thermal filaments (NTFs) Sgr C, G359.54+0.18 and G359.79+0.17 using the Giant Metrewave Radio Telescope (GMRT). Our study, for the first time, constrains the distance of the Sgr C NTF and the HII region seen associated with the NTF in the sky plane, to within a few hundred parsecs from the Galactic Centre (GC). A molecular cloud with a velocity of −100 km s −1 appears to be associated with the central part of the Sgr C NTF. Our study also indicates that the Sgr C HII region is relatively farther away than the NTF along our line of sight, and thereby provides evidence against any possible interaction between the two objects. The NTF G359.54+0.18 shows weak HI absorption (4 σ detection) at a velocity of −140 km s −1 , which is the velocity of a known dense molecular cloud seen towards the NTF. This cloud is expected to be located within ∼200 pc of the GC and thereby provides a lower limit to the distance. The upper limit to the distance of this NTF from the Sun is 10.5 kpc. The distance to the NTF G359.79+0.17 is between 5.1 and 10.5 kpc from the Sun.

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A far-infrared survey of the galactic center

Cited by 64 publications

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The Galactic Center Environment

The Galactic Center Environment

A HIGH-RESOLUTION SURVEY OF H I ABSORPTION TOWARD THE CENTRAL 200 pc OF THE GALACTIC CENTER

Constraints on distances to Galactic Centre non-thermal filaments from HI absorption

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