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Title:
Interaction between the north-eastern boundary of Sgr A East and giant molecular clouds
Authors:
Lee, Sungho; Pak, Soojong; Davis, Christopher J.; Herrnstein, Robeson M.; Geballe, T. R.; Ho, Paul T. P.; Wheeler, J. Craig
Affiliation:
AA(Astronomy Programme in SEES, Seoul National University, Shillim-Dong, Kwanak-Gu, Seoul 151-742, South Korea; Korea Astronomy Observatory, Whaam-Dong, Youseong-Gu, Taejeon 305-348, South Korea), AB(Astronomy Programme in SEES, Seoul National University, Shillim-Dong, Kwanak-Gu, Seoul 151-742, South Korea; Korea Astronomy Observatory, Whaam-Dong, Youseong-Gu, Taejeon 305-348, South Korea), AC(Joint Astronomy Centre, University Park, 660 North A`ohökü Place, Hilo, HI 96720, USA), AD(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AE(Gemini Observatory, 670 N. A`ohökü Place, Hilo, HI 96720, USA), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AG(Astronomy Department, University of Texas, Austin, TX 78712, USA)
Journal:
Monthly Notice of the Royal Astronomical Society, Volume 341, Issue 2, pp. 509-516. (MNRAS Homepage)
Publication Date:
05/2003
Origin:
MNRAS
MNRAS Keywords:
ISM: individual: Sgr A East, ISM: individual: M-0.02: 0.07, ISM: lines and bands, ISM: molecules, Galaxy: centre, infrared: ISM
Abstract Copyright:
(c) 2003 RAS
Bibliographic Code:
2003MNRAS.341..509L

Abstract

We have detected the v= 1 -> 0 S(1) (ル= 2.1218 レm) and v= 2 -> 1 S(1) (ル= 2.2477 レm) lines of H2 in the Galactic Centre, in a 90 ／ 27 arcsec2 region between the north-eastern boundary of the non-thermal source Sgr A East, and the giant molecular cloud (GMC) M-0.02 - 0.07. The detected H2v= 1 -> 0 S(1) emission has an intensity of 1.6-21 ／ 10-18 W m-2 arcsec-2 and is present over most of the region. Along with the high intensity, the large linewidths (FWHM = 40-70 km s-1) and the H2v= 2 -> 1 S(1) to v= 1 -> 0 S(1) line ratios (0.3-0.5) can be best explained by a combination of C-type shocks and fluorescence. The detection of shocked H2 is clear evidence that Sgr A East is driving material into the surrounding adjacent cool molecular gas. The H2 emission lines have two velocity components at ~+50 and ~0 km s-1, which are also present in the NH3(3, 3) emission mapped by McGary, Coil & Ho. This two-velocity structure can be explained if Sgr A East is driving C-type shocks into both the GMC M-0.02 - 0.07 and the northern ridge of McGary et al.
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