TY - JOUR
T1 - CO(J = 1–0) Mapping Survey of 64 Galaxies in the Fornax Cluster with the ALMA Morita Array
AU - Morokuma-Matsui, Kana
AU - Bekki, Kenji
AU - Wang, Jing
AU - Serra, Paolo
AU - Koyama, Yusei
AU - Morokuma, Tomoki
AU - Egusa, Fumi
AU - For, Bi-Qing
AU - Nakanishi, Kouichiro
AU - Koribalski, Bärbel S.
AU - Okamoto, Takashi
AU - Kodama, Tadayuki
AU - Lee, Bumhyun
AU - Maccagni, Filippo M.
AU - Miura, Rie E.
AU - Espada, Daniel
AU - Takeuchi, Tsutomu T.
AU - Yang, Dong
AU - Lee, Minju M.
AU - Ueda, Masaki
AU - Matsushita, Kyoko
PY - 2022
Y1 - 2022
N2 - We conduct a 12C16O(J = 1−0) (hereafter CO)
mapping survey of 64 galaxies in the Fornax cluster using the Atacama
Large Millimeter/submillimeter Array Morita array in cycle 5. CO
emission is detected from 23 out of the 64 galaxies. Our sample includes
dwarf, spiral, and elliptical galaxies with stellar masses of Mstar ∼ 106.3−11.6 M⊙. The achieved beam size and sensitivity are 15'' × 8'' and ∼12 mJy beam−1 at the velocity resolution of ∼10 km s−1, respectively. We study the cold gas (molecular and atomic gas) properties of 38 subsamples with Mstar > 109 M⊙ combined with literature H i
data. We find that (1) the low star formation (SF) activity in the
Fornax galaxies is caused by the decrease in the cold gas mass fraction
with respect to stellar mass (hereafter, gas fraction) rather than the
decrease of the SF efficiency from the cold gas; (2) the atomic gas
fraction is more heavily reduced than the molecular gas fraction of such
galaxies with low SF activity. A comparison between the cold gas
properties of the Fornax galaxies and their environmental properties
suggests that the atomic gas is stripped tidally and by the ram
pressure, which leads to the molecular gas depletion with an aid of the
strangulation and consequently SF quenching. Preprocesses in the group
environment would also play a role in reducing cold gas reservoirs in
some Fornax galaxies.
AB - We conduct a 12C16O(J = 1−0) (hereafter CO)
mapping survey of 64 galaxies in the Fornax cluster using the Atacama
Large Millimeter/submillimeter Array Morita array in cycle 5. CO
emission is detected from 23 out of the 64 galaxies. Our sample includes
dwarf, spiral, and elliptical galaxies with stellar masses of Mstar ∼ 106.3−11.6 M⊙. The achieved beam size and sensitivity are 15'' × 8'' and ∼12 mJy beam−1 at the velocity resolution of ∼10 km s−1, respectively. We study the cold gas (molecular and atomic gas) properties of 38 subsamples with Mstar > 109 M⊙ combined with literature H i
data. We find that (1) the low star formation (SF) activity in the
Fornax galaxies is caused by the decrease in the cold gas mass fraction
with respect to stellar mass (hereafter, gas fraction) rather than the
decrease of the SF efficiency from the cold gas; (2) the atomic gas
fraction is more heavily reduced than the molecular gas fraction of such
galaxies with low SF activity. A comparison between the cold gas
properties of the Fornax galaxies and their environmental properties
suggests that the atomic gas is stripped tidally and by the ram
pressure, which leads to the molecular gas depletion with an aid of the
strangulation and consequently SF quenching. Preprocesses in the group
environment would also play a role in reducing cold gas reservoirs in
some Fornax galaxies.
KW - Galaxy environments
KW - Galaxy clusters
KW - Molecular gas
U2 - 10.3847/1538-4365/ac983b
DO - 10.3847/1538-4365/ac983b
M3 - Journal article
SN - 0067-0049
VL - 263
JO - The Astrophysical Journal Supplement Series
JF - The Astrophysical Journal Supplement Series
IS - 2
M1 - 40
ER -