2016A&A...595A..49Z


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.13CEST23:17:14

2016A&A...595A..49Z - Astronomy and Astrophysics, volume 595A, 49-49 (2016/11-1)

Colliding interstellar bubbles in the direction of l = 54°.

ZYCHOVA L. and EHLEROVA S.

Abstract (from CDS):

Context. Interstellar bubbles are structures in the interstellar medium with diameters of a few to tens of parsecs. Their progenitors are stellar winds, intense radiation of massive stars, or supernova explosions. Star formation and young stellar objects are commonly associated with these structures.
Aims. We compare infrared observations of bubbles N115, N116 and N117 with atomic, molecular and ionized gas in this region. While determining the dynamical properties of the bubbles, we also look into their ambient environment to understand their formation in a wider context.
Methods. To find bubbles in HI (Very Large Array Galactic Plane Survey) and CO data (Galactic Ring Survey), we used the images from the Galactic Legacy Infrared Mid-Plane Survey. We manually constructed masks based on the appearance of the bubbles in the IR images and applied them to the HI and CO data. We determined kinematic distance, size, expansion velocity, mass, original density of the maternal cloud, age, and energy input of the bubbles.
Results. We identified two systems of bubbles: the first, the background system, is formed by large structures G053.9+0.2 and SNR G054.4-0.3 and the infrared bubble N116+117. The second, the foreground system, includes the infrared bubble N115 and two large HI bubbles, which we discovered in the HI data. Both systems are independent, lying at different distances, but look similar. They are both formed by two large colliding bubbles with radii around 20-30pc and ages of a few million years. A younger and smaller (∼4pc, less than a million years) infrared bubble lies at the position of the collision.
Conclusions. We found that both infrared bubbles N115 and N116+117 are associated with the collisions of larger and older bubbles. We propose that such collisions increase the probability of further star formation, probably by squeezing the interstellar material, suggesting that they are an important mechanism for star formation.

Abstract Copyright: © ESO, 2016

Journal keyword(s): ISM: bubbles - ISM: clouds - HII regions - ISM: supernova remnants

Nomenclature: Tables 1-2: [ZE2016] A (Nos A-F).

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 [ZE2016] E bub 03 33 02 -00 25.1           ~ 1 0
2 [ZE2016] D bub 03 35 17 +00 18.1           ~ 1 0
3 [ZE2016] A bub 03 35 32 +00 10.8           ~ 1 0
4 [ZE2016] C bub 03 36 21 -00 05.2           ~ 1 0
5 SH 2-3 HII 17 12.4 -38 28           ~ 173 1
6 PSR B1925+18.8 Psr 19 27 24.97 +18 56 36.8           ~ 20 1
7 PSR B1926+18 Psr 19 29 16.78 +18 44 59.5           ~ 28 0
8 G3CC 69 Cl* 19 29 18.0 +17 56 41           ~ 2 0
9 G3CC 70 Cl* 19 29 32.3 +18 00 57           ~ 2 0
10 SNR G053.9+00.2 SNR 19 30 12 +18 42.8           ~ 9 0
11 Teutsch 42 OpC 19 30 13.1 +18 32 09           ~ 15 0
12 [BDS2003] 12 Cl* 19 30 23 +18 20.8           ~ 4 0
13 [CPA2006] N115 bub 19 30 24.5 +18 15 40           ~ 11 1
14 PSR J1930+1852 Psr 19 30 30.13 +18 52 14.1           ~ 84 1
15 SNR G054.1+00.3 SNR 19 30 31 +18 52.0           ~ 198 1
16 [BDS2003] 156 OpC 19 31 43 +18 41.9           ~ 6 0
17 [CPA2006] N117 bub 19 31 44.5 +18 43 15           ~ 9 0
18 [CPA2006] N116 bub 19 31 46.6 +18 41 40           ~ 5 0
19 SNR G054.4-00.3 SNR 19 33 22.5 +18 58 34           ~ 89 0
20 NAME the Wall reg ~ ~           ~ 13 0

    Equat.    Gal    SGal    Ecl

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