Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 710208.0, MPI für Astronomie / Publikationen_mpia
Absorption filaments toward the massive clump G0.253+0.016
Authors:Bally, J.; Rathborne, J. M.; Longmore, S. N.; Jackson, J. M.; Alves, J. F.; Bressert, E.; Contreras, Y.; Foster, J. B.; Garay, G.; Ginsburg, A.; Johnston, K. G.; Kruijssen, J. M. D.; Testi, L.; Walsh, A. J.
Date of Publication (YYYY-MM-DD):2014
Title of Journal:The Astrophysical Journal
Issue / Number:1
Start Page:id. 28 (19 pp)
Audience:Not Specified
Abstract / Description:ALMA HCO+ observations of the infrared dark cloud G0.253+0.016 located in the central molecular zone of the Galaxy are presented. The 89 GHz emission is area-filling, optically thick, and sub-thermally excited. Two types of filaments are seen in absorption against the HCO+ emission. Broad-line absorption filaments (BLAs) have widths of less than a few arcseconds (0.07-0.14 pc), lengths of 30-50 arcsec (1.2-1.8 pc), and absorption profiles extending over a velocity range larger than 20 km s--1. The BLAs are nearly parallel to the nearby G0.18 non-thermal filaments and may trace HCO+ molecules gyrating about highly ordered magnetic fields located in front of G0.253+0.016 or edge-on sheets formed behind supersonic shocks propagating orthogonal to our line of sight in the foreground. Narrow-line absorption filaments (NLAs) have line widths less than 20 km s--1. Some NLAs are also seen in absorption in other species with high optical depth, such as HCN, and occasionally in emission where the background is faint. The NLAs, which also trace low-density, sub-thermally excited HCO+ molecules, are mostly seen on the blueshifted side of the emission from G0.253+0.016. If associated with the surface of G0.253+0.016, the kinematics of the NLAs indicate that the cloud surface is expanding. The decompression of entrained, milli-Gauss magnetic fields may be responsible for the re-expansion of the surface layers of G0.253+0.016 as it recedes from the Galactic center following a close encounter with Sgr A.
Free Keywords:Galaxy: center; ISM: clouds; ISM: individual: G0.253+0.016; stars: formation
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X %R 10.1088/0004-637X/795/1/28
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.