2022A&A...661A.136G


Query : 2022A&A...661A.136G

2022A&A...661A.136G - Astronomy and Astrophysics, volume 661A, 136-136 (2022/5-1)

The molecular gas resolved by ALMA in the low-metallicity merging dwarf galaxy Haro 11.

GAO Y., GU Q., SHI Y., ZHOU L., BAO M., YU X., ZHANG Z.-Y., WANG T., MADDEN S.C., HAYES M., LU S. and XU K.

Abstract (from CDS):


Context. The physical mechanisms driving starbursts and quenching in less massive (M* ≤ 1010 M) galaxies are unclear. The merger is one of the inescapable processes referred to as both starburst and quenching in massive galaxies. However, the effects of the merger on star formation in dwarf galaxies and their evolution are still uncertain.
Aims. We aim to explore how star formation in dwarf galaxies is both triggered and quenched by studying metal-poor gas-rich dwarf mergers based on multi-band observations at a spatial resolution of ∼460 pc.
Methods. We use archival data of Atacama Large Millimetre Array (Band 3 and 8) and Very Large Telescope/Multi Unit Spectroscopic Explorer to map CO(J = 1-0), [CI](3P1-3P0), and Hα emission in one of the most extreme merging starburst dwarf galaxies, Haro 11.
Results. We find the molecular gas is assembled around the central two star-forming regions (knots B and C). The molecular and ionized gas and stellar components show complex kinematics, indicating that the gas is probably at a combined stage of collision of clouds and feedback from star formation. The peak location and distribution of [CI](1-0) closely coincide with the CO(1-0) emission, meaning that it might trace the same molecular gas as CO in such a dwarf merger starburst galaxy. The enhancement of line ratios (∼0.5) of [CI]/CO around knot C is probably generated by the dissociation of CO molecules by cosmic rays and far-ultraviolet photons. Globally, Haro 11 and its star-forming regions share similar star formation efficiency (SFE) to the high-z starburst galaxies or the clumps in nearby ultraluminous infrared galaxies.
Conclusions. Given the high SFE, the high specific star formation rate, small stellar mass, low metallicity, and deficient HI gas, Haro 11 could be an analog of a high-z dwarf starburst and the potential progenitor of the nearby less massive elliptical galaxies. The significantly smaller turbulent pressure and viral parameter is probably triggering the intense starbursts. We predict that Haro 11 will quench at M* ≤ 8.5 x 109 M.

Abstract Copyright: © ESO 2022

Journal keyword(s): galaxies: ISM - galaxies: starburst - galaxies: individual: Haro 11 - galaxies: interactions

Status at CDS : Examining the need for a new acronym.

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 [VFT93] 0034-3349B HXB 00 36 52.454 -33 33 16.77           ~ 22 0
2 ESO 350-38 Sy2 00 36 52.489 -33 33 17.23   14.31 14.41 13.49   ~ 391 0
3 [VFT93] 0034-3349A G 00 36 52.543 -33 33 16.57   11.93   11.28   ~ 16 0
4 [VFT93] 0034-3349C HXB 00 36 52.660 -33 33 17.07           ~ 23 0
5 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3368 2
6 M 33 GiG 01 33 50.8965749232 +30 39 36.630403128 6.17 6.27 5.72     ~ 5882 1
7 ESO 495-21 bCG 08 36 15.190 -26 24 33.66 12.04 11.93 11.45 11.09 12.3 ~ 576 3
8 Mrk 116 PaG 09 34 02.1 +55 14 25           ~ 1111 1
9 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1697 0
10 MCG+01-32-056 GiG 12 25 52.500 +05 48 36.32   15.2       ~ 77 0

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