Detection of CO(1−0) Emission at the Tips of the Tidal Tail in the Antennae Galaxies

The tip of the tidal tail, resulting from an encounter between galaxies, features gas concentrations and some star-forming regions, such as tidal dwarf galaxies (TDGs). This region provides a unique laboratory for examining the star formation process in a dynamical environment distinct from that of...

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Published inThe Astrophysical journal Vol. 962; no. 1; pp. 4 - 11
Main Authors Maeda, Fumiya, Egusa, Fumi, Tsujita, Akiyoshi, Inoue, Shuhei, Kohno, Kotaro, Komugi, Shinya, Ohta, Kouji, Asada, Yoshihisa, Fujimoto, Yusuke, Habe, Asao, Hatsukade, Bunyo, Inoue, Shin, Kaneko, Hiroyuki, Kobayashi, Masato I. N., Tosaki, Tomoka
Format Journal Article
LanguageEnglish
Published Philadelphia The American Astronomical Society 01.02.2024
IOP Publishing
Subjects
CO line emission
Disk galaxies
Dwarf galaxies
Emission
Galaxies
Galaxy interactions
Helium
Interstellar medium
Molecular gas
Molecular gases
Star & galaxy formation
Star formation
Stars
Tidal tails
Tips
Online AccessGet full text
ISSN0004-637X
1538-4357
DOI10.3847/1538-4357/ad1932

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Abstract The tip of the tidal tail, resulting from an encounter between galaxies, features gas concentrations and some star-forming regions, such as tidal dwarf galaxies (TDGs). This region provides a unique laboratory for examining the star formation process in a dynamical environment distinct from that of disk galaxies. Using the Nobeyama 45 m telescope, we conducted 12 CO(1−0) position-switching observations at the tips of the southern tidal tail in the Antennae galaxies. We detected CO emission not only from the two star-forming TDG candidates but also in regions with no significant star formation. Adopting a Galactic CO-to-H 2 conversion factor without helium correction, the H 2 gas surface density is ∼5–12 M ⊙ pc −2 . In most regions, the molecular-to-atomic gas ratio is around unity (0.6–1.9), but we find a region with a high ratio with a 3 σ lower limit of >7.2. The star formation efficiency (SFE) of molecular gas is notably low (<0.15 Gyr −1 ), indicating less active star formation than in both nearby disk galaxies (∼0.5–1.0 Gyr −1 ) and other TDGs previously observed. Including previous observations, the molecular gas SFEs vary widely among TDGs/tidal tails, from 10 −2 to 10 Gyr −1 , demonstrating significant variations in star formation activity. Potential factors contributing to the low SFE in the Antennae tail tips include extensive tides and/or the young age of the tail.
AbstractList The tip of the tidal tail, resulting from an encounter between galaxies, features gas concentrations and some star-forming regions, such as tidal dwarf galaxies (TDGs). This region provides a unique laboratory for examining the star formation process in a dynamical environment distinct from that of disk galaxies. Using the Nobeyama 45 m telescope, we conducted ^12 CO(1−0) position-switching observations at the tips of the southern tidal tail in the Antennae galaxies. We detected CO emission not only from the two star-forming TDG candidates but also in regions with no significant star formation. Adopting a Galactic CO-to-H _2 conversion factor without helium correction, the H _2 gas surface density is ∼5–12 M _⊙ pc ^−2 . In most regions, the molecular-to-atomic gas ratio is around unity (0.6–1.9), but we find a region with a high ratio with a 3 σ lower limit of >7.2. The star formation efficiency (SFE) of molecular gas is notably low (<0.15 Gyr ^−1 ), indicating less active star formation than in both nearby disk galaxies (∼0.5–1.0 Gyr ^−1 ) and other TDGs previously observed. Including previous observations, the molecular gas SFEs vary widely among TDGs/tidal tails, from 10 ^−2 to 10 Gyr ^−1 , demonstrating significant variations in star formation activity. Potential factors contributing to the low SFE in the Antennae tail tips include extensive tides and/or the young age of the tail.
The tip of the tidal tail, resulting from an encounter between galaxies, features gas concentrations and some star-forming regions, such as tidal dwarf galaxies (TDGs). This region provides a unique laboratory for examining the star formation process in a dynamical environment distinct from that of disk galaxies. Using the Nobeyama 45 m telescope, we conducted 12 CO(1−0) position-switching observations at the tips of the southern tidal tail in the Antennae galaxies. We detected CO emission not only from the two star-forming TDG candidates but also in regions with no significant star formation. Adopting a Galactic CO-to-H 2 conversion factor without helium correction, the H 2 gas surface density is ∼5–12 M ⊙ pc −2 . In most regions, the molecular-to-atomic gas ratio is around unity (0.6–1.9), but we find a region with a high ratio with a 3 σ lower limit of >7.2. The star formation efficiency (SFE) of molecular gas is notably low (<0.15 Gyr −1 ), indicating less active star formation than in both nearby disk galaxies (∼0.5–1.0 Gyr −1 ) and other TDGs previously observed. Including previous observations, the molecular gas SFEs vary widely among TDGs/tidal tails, from 10 −2 to 10 Gyr −1 , demonstrating significant variations in star formation activity. Potential factors contributing to the low SFE in the Antennae tail tips include extensive tides and/or the young age of the tail.
The tip of the tidal tail, resulting from an encounter between galaxies, features gas concentrations and some star-forming regions, such as tidal dwarf galaxies (TDGs). This region provides a unique laboratory for examining the star formation process in a dynamical environment distinct from that of disk galaxies. Using the Nobeyama 45 m telescope, we conducted 12CO(1−0) position-switching observations at the tips of the southern tidal tail in the Antennae galaxies. We detected CO emission not only from the two star-forming TDG candidates but also in regions with no significant star formation. Adopting a Galactic CO-to-H2 conversion factor without helium correction, the H2 gas surface density is ∼5–12 M⊙ pc−2. In most regions, the molecular-to-atomic gas ratio is around unity (0.6–1.9), but we find a region with a high ratio with a 3σ lower limit of >7.2. The star formation efficiency (SFE) of molecular gas is notably low (<0.15 Gyr−1), indicating less active star formation than in both nearby disk galaxies (∼0.5–1.0 Gyr−1) and other TDGs previously observed. Including previous observations, the molecular gas SFEs vary widely among TDGs/tidal tails, from 10−2 to 10 Gyr−1, demonstrating significant variations in star formation activity. Potential factors contributing to the low SFE in the Antennae tail tips include extensive tides and/or the young age of the tail.
Author Kobayashi, Masato I. N.
Inoue, Shuhei
Asada, Yoshihisa
Habe, Asao
Ohta, Kouji
Fujimoto, Yusuke
Kaneko, Hiroyuki
Hatsukade, Bunyo
Kohno, Kotaro
Egusa, Fumi
Maeda, Fumiya
Tsujita, Akiyoshi
Inoue, Shin
Komugi, Shinya
Tosaki, Tomoka
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  organization: University of Aizu Department of Computer Science and Engineering, Tsuruga Ikki-machi, Aizu-Wakamatsu, Fukushima 965-8580, Japan
– sequence: 10
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  surname: Habe
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  organization: Hokkaido University Department of Physics, Faculty of Science, Kita-10 Nishi-8, Kita-ku, Sapporo 060-0810, Japan
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  orcidid: 0000-0001-6469-8725
  surname: Hatsukade
  fullname: Hatsukade, Bunyo
  organization: Graduate Institute for Advanced Studies , SOKENDAI, Osawa, Mitaka, Tokyo 181-8588, Japan
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  orcidid: 0009-0004-6347-0613
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  surname: Tosaki
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  organization: Joetsu University of Education , 1, Yamayashiki-machi, Joetsu, Niigata 943–8512, Japan
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SubjectTerms CO line emission
Disk galaxies
Dwarf galaxies
Emission
Galaxies
Galaxy interactions
Helium
Interstellar medium
Molecular gas
Molecular gases
Star & galaxy formation
Star formation
Stars
Tidal tails
Tips
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Title Detection of CO(1−0) Emission at the Tips of the Tidal Tail in the Antennae Galaxies
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