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The physical properties of S0 galaxy PGC 26218: the origin of starburst and star formation | | Xue Ge
; Qiu-Sheng Gu
; Rubén García-Benito
; Meng-Yuan Xiao
; Zong-Nan Li
; | | Date: |
16 Jan 2020 | | Abstract: | We present 2D-spectroscopic observations from Centro Astron’omico Hispano
Alem’an (CAHA) 3.5 m telescope and the millimetre observation from NOrthern
Extended Millimeter Array (NOEMA) of the nearby S0 galaxy PGC 26218, which
shows central star-formation activity and post-starburst outside in the disk.
We estimate the star formation rate (SFR = $0.28pm0.01$ $M_{odot}
m
yr^{-1}$) and molecular gas mass ($
m log $$M_{
m H_{2}}=7.60pm0.15
M_{odot}$) of PGC 26218 based on the extinction-corrected H$alpha$ emission
line and the CO-$
m H_{2}$ conversion factor ($alpha_{
m CO}$) of the Milky
Way, respectively. We find that PGC 26218 follows the star forming main
sequence (SFMS) and the Kennicutt-Schmidt law. Comparing the kinematics of
CO($J$=1-0), stars and H$alpha$, we find that the rotational axis of
CO($J$=1-0) is 45$^{circ}$ different from that of H$alpha$. In addition, the
profile of the CO($J$=1-0) emission line shows asymmetry and has an inflow
component of $sim$ 46 $
m km s^{-1}$. With the decomposition of the optical
image, we confirm that PGC 26218 shows multiple nuclear structures. The
projected offset between the most luminous optical center and the center of
CO($J$=1-0) is $5.2arcsec$ ($sim$ 0.6 kpc) and the latter overlaps with one
of the optical cores. These results support that PGC 26218 may have experienced
a gas-rich minor merger, extending its star formation and locating it in the
SFMS. | | Source: | arXiv, 2001.5679 | | Services: | Forum | Review | PDF | Favorites | |
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