Abstract
We observed CO J = 1-0 and HCN J = 1-0 line emission toward a high-velocity, compact molecular cloud, CO 0.02-0.02, near the center of our Galaxy, using the Nobeyama Millimeter Array (NMA). A CO velocity-integrated map with a resolution of 4.″3 × 2.″4 shows two oval clumps with sizes of 0.8 pc. These clumps are seperated by 1.2 pc, being located at the eastern and southwestern peripheries of the CO 0.02-0.02 cloud. The overall distribution of HCN emission coincides with that taken with the Nobeyama 45 m telescope. The HCN velocity-integrated map with a resolution of 6.″ × 3.″4 shows two prominent peaks in the cloud center. Both NMA maps at VLSR ∼ 110km s-1 show an arc-shaped edge in the southeast, which may correspond to the edge of the "emission cavity" found in the CO J = 3-2 integrated-intesity map. We also noticed a faint radio continuum "arc" that encircles the bulk of the CO 0.02-0.02 cloud. These results support the notion that CO 0.02-0.02 has been accelerated, heated, and compressed in a series of supernova shocks that occurred within the last (3-5) × 104 yr. We suggest that a massive compact cluster with an age of 10-30 Myr is responsible for the formation of the CO 0.02-0.02 cloud.
| Original language | English |
|---|---|
| Pages (from-to) | 429-434 |
| Number of pages | 6 |
| Journal | Publications of the Astronomical Society of Japan |
| Volume | 60 |
| Issue number | 3 |
| Publication status | Published - 2008 |
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Keywords
- Galaxies: nuclei
- Galaxy: center
- ISM: clouds
- ISM: molecules
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
Aperture synthesis imaging of a high-velocity compact cloud near the galactic center. / Oka, Tomoharu; Hasegawa, Tetsuo; White, Glenn J.; Sato, Fumio; Tsuboi, Masato; Miyazaki, Atsushi.
In: Publications of the Astronomical Society of Japan, Vol. 60, No. 3, 2008, p. 429-434.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Aperture synthesis imaging of a high-velocity compact cloud near the galactic center
AU - Oka, Tomoharu
AU - Hasegawa, Tetsuo
AU - White, Glenn J.
AU - Sato, Fumio
AU - Tsuboi, Masato
AU - Miyazaki, Atsushi
PY - 2008
Y1 - 2008
N2 - We observed CO J = 1-0 and HCN J = 1-0 line emission toward a high-velocity, compact molecular cloud, CO 0.02-0.02, near the center of our Galaxy, using the Nobeyama Millimeter Array (NMA). A CO velocity-integrated map with a resolution of 4.″3 × 2.″4 shows two oval clumps with sizes of 0.8 pc. These clumps are seperated by 1.2 pc, being located at the eastern and southwestern peripheries of the CO 0.02-0.02 cloud. The overall distribution of HCN emission coincides with that taken with the Nobeyama 45 m telescope. The HCN velocity-integrated map with a resolution of 6.″ × 3.″4 shows two prominent peaks in the cloud center. Both NMA maps at VLSR ∼ 110km s-1 show an arc-shaped edge in the southeast, which may correspond to the edge of the "emission cavity" found in the CO J = 3-2 integrated-intesity map. We also noticed a faint radio continuum "arc" that encircles the bulk of the CO 0.02-0.02 cloud. These results support the notion that CO 0.02-0.02 has been accelerated, heated, and compressed in a series of supernova shocks that occurred within the last (3-5) × 104 yr. We suggest that a massive compact cluster with an age of 10-30 Myr is responsible for the formation of the CO 0.02-0.02 cloud.
AB - We observed CO J = 1-0 and HCN J = 1-0 line emission toward a high-velocity, compact molecular cloud, CO 0.02-0.02, near the center of our Galaxy, using the Nobeyama Millimeter Array (NMA). A CO velocity-integrated map with a resolution of 4.″3 × 2.″4 shows two oval clumps with sizes of 0.8 pc. These clumps are seperated by 1.2 pc, being located at the eastern and southwestern peripheries of the CO 0.02-0.02 cloud. The overall distribution of HCN emission coincides with that taken with the Nobeyama 45 m telescope. The HCN velocity-integrated map with a resolution of 6.″ × 3.″4 shows two prominent peaks in the cloud center. Both NMA maps at VLSR ∼ 110km s-1 show an arc-shaped edge in the southeast, which may correspond to the edge of the "emission cavity" found in the CO J = 3-2 integrated-intesity map. We also noticed a faint radio continuum "arc" that encircles the bulk of the CO 0.02-0.02 cloud. These results support the notion that CO 0.02-0.02 has been accelerated, heated, and compressed in a series of supernova shocks that occurred within the last (3-5) × 104 yr. We suggest that a massive compact cluster with an age of 10-30 Myr is responsible for the formation of the CO 0.02-0.02 cloud.
KW - Galaxies: nuclei
KW - Galaxy: center
KW - ISM: clouds
KW - ISM: molecules
UR - http://www.scopus.com/inward/record.url?scp=48249103133&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=48249103133&partnerID=8YFLogxK
M3 - Article
VL - 60
SP - 429
EP - 434
JO - Publication of the Astronomical Society of Japan
JF - Publication of the Astronomical Society of Japan
SN - 0004-6264
IS - 3
ER -