Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-25T17:13:55.893Z Has data issue: false hasContentIssue false

TRAO 13CO Outer Galaxy Survey

Published online by Cambridge University Press:  21 March 2013

Youngung Lee
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea
Y. S. Kim
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea Chungnam National University, Daehakro 99, Yuseong-gu, Daejeon, Republic of Korea email: [email protected]
H. W. Kang
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea
J. H. Jung
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea
C. H. Lee
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea
I. S. Yim
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea
B. G. Kim
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea
H. G. Kim
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea
K. T. Kim
Affiliation:
Korea Astronomy and Space Science Institute, Daeduckdaero 776, Hwaam-dong, Yuseong-gu, Daejeon, Republic of Korea Chungnam National University, Daehakro 99, Yuseong-gu, Daejeon, Republic of Korea email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have observed the parts of the second quadrant of the Galactic Plane in 13CO(1-0) using the multibeam receiver system installed on the 14 m telescope at Taeduk Radio Astronomy Observatory (TRAO). The first target region A (L=108° to 112°.5) is the part of the 12CO Outer Galactic Plane Survey (OGS; Heyer et al. 1998), and it is for the exact Galactic plane with the latitude range of +1 and -1 degree. A total of 48,000 spectra (about 9 square degrees) were obtained on 50″ grid. Two following regions were also observed; Region B: L = 120° ∼ 121°.7, B = −1° ∼ +1° (38,000 spectra) Region C: L = 130° 132°, B = −1° ∼ +1° (42,000 spectra). Eventually all the regions of the OGS will be covered. The selected velocity resolution is 0.63 km s−1 and the covered velocity is 320 km s−1, from −210 to 110 km s−1. The typical system temperature is ranging from 400 to 800 K, and average sensitivity per channel is 0.17 K.

We developed a new reduction method, which effectively deals with a relatively noisy 3-dimensional database. After using simple linear baseline subtraction, we mainly used the IRAF twod.longslit.background task in 3D within some scripts, as well as IRAF tasks dealing with statistics, and a revised FCRAO reduction package, which is working within IRAF as external user's tasks. The collected 13CO database will be manipulated with pre-existing 12CO data to get several physical parameters. As it is located in the second quadrant, the kinematic distances of the individual clouds, which will be identified, can be estimated straightforwardly without any distance ambiguity. In this meeting we present the reduction method, integrated intensity maps, and spatial-velocity maps. We intend to clarify any difference of their characteristics between the clouds in the Outer Galaxy and Inner Galaxy using our data base.

The present TRAO receiver system has aged, and thus its performance level degraded. However, we have a plan to renovate our receiver system to a brand new one within the next two years. This will speed up the TOGS project. At present, it costs substantial amount of time to homogeneously reduce the spectra obtained with our present receiver system. To compensate this, we invested more integration time, and developed more advanced reduction methods (see above). A future multibeam array receiver system at the TRAO would be at least 16 beams with most recent mixers (Tsys ∼ 150 K at 110GHz), hopefully.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

Heyer, M. H., Brunt, C., Snell, R. L., Howe, J. E., Schloerb, F. P., & Carpenter, J. M. 1998, ApJS, 115, 241Google Scholar
Lee, Y., Stark, A. A., Kim, H. G., & Moon, D.-S. 2001, ApJS, 136, 137Google Scholar
Jackson, J. M., Rathborne, J. M., Shah, R. Y., Simon, R., Bania, T. M., Clemens, D. P., Chambers, E. T., Johnson, A. M. Dormody.; Lavoie, R., & Heyer, M. H. 2006, ApJS, 163, 145CrossRefGoogle Scholar