| Full text | |
| Author(s): |
Akhter, Shaila
[1, 2]
;
Cunningham, Maria R.
[2]
;
Harvey-Smith, Lisa
[2, 3]
;
Nawaz, Mohammad Ali
[4, 5]
;
Jones, Paul A.
[2]
;
Walsh, Andrew
[6]
;
de Gouveia Dal Pino, Elisabete M.
[7]
Total Authors: 7
|
| Affiliation: | [1] CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710 - Australia
[2] Univ New South Wales, Sch Phys, Sydney, NSW 2052 - Australia
[3] Western Sydney Univ, Sch Comp Engn & Math, Locked Bag 1797, Penrith, NSW 2751 - Australia
[4] Univ Sao Paulo, Escola Artes Ciencias & Humanidades, Rua Arlindo Bettio 1000, BR-03828000 Sao Paulo, SP - Brazil
[5] North South Univ, Dept Math & Phys, Dhaka 1229 - Bangladesh
[6] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845 - Australia
[7] Univ Sao Paulo IAG USP, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo - Brazil
Total Affiliations: 7
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 502, n. 4, p. 5896-5920, APR 2021. |
| Web of Science Citations: | 0 |
| Abstract | |
We used NH(1,1) data from the HO Southern Galactic Plane Survey (HOPS) between -60 degrees < l < -2.7 degrees and 3.9 degrees < l < 30 degrees and vertical bar b vertical bar < 0.5 degrees to identify dense molecular regions/clumps of the Milky Way Galaxy that are likely to form high-mass stars. We identified similar to 500 such clumps and in this paper we report on 14 of these clumps near the Central Molecular Zone that show broad emission spectral lines (with observed velocity widths between 19.8 and 47.6 kms(-1) corresponding to intrinsic velocity widths between 7.1 and 25.2 kms(-1)). We find that these clumps are grouped into three clusters of dense molecular cores centred at l approximate to 5.4 degrees, -5.4 degrees, and -10 degrees. We name them `Cluster-1', `Cluster-2' (also known as `Bania's Clump 1'), and `Cluster-3'. We find that the same clumps exhibit broad emission spectra for other molecular lines - NH3(2,2), (3,3), and HC3N(3 - 2). The antisymmetry of Cluster-1 and Cluster-2 in the l - b plane, and the large velocity dispersion of each clump in these two clusters suggest that clusters 1 and 2 may be associated with the Galactic bar potential x-1 orbits. Our assessments show that the clumps of these three clusters host hot gases and their emission-line broadening are associated with shock heating. We find that Cluster-3 is likely to be undergoing high-mass star formation, as suggested by the presence of emission from H2O maser and radio recombination line (H69 alpha) from HOPS. (AU) | |
| FAPESP's process: | 13/10559-5 - Investigation of high energy and plasma astrophysics phenomena: theory, numerical simulations, observations, and instrument development for the Cherenkov Telescope Array (CTA) |
| Grantee: | Elisabete Maria de Gouveia Dal Pino |
| Support Opportunities: | Special Projects |
| FAPESP's process: | 15/25126-2 - Interaction of jets with the intracluster medium: The role of jet precession |
| Grantee: | Mohammad Ali Nawaz |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |