• Title/Summary/Keyword: outflows

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Detection of AGN outflows in micro-arcsec scales

  • Oh, Junghwan;Trippe, Sascha;Krichbaum, Thomas;Sohn, Bong Won;Bremer, Michael
    • The Bulletin of The Korean Astronomical Society
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    • v.38 no.2
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    • pp.43.1-43.1
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    • 2013

  • We report the preliminary results of our GMVA(Global mm VLBI Array) observation at the frequency of 86 GHz. Observation were made in the dual polarization mode (LCP and RCP), to produce the polarimetric maps with the maximum angular resolution which the array is capable of. We aim to link the source-integrated AGN polarization properties with the polarized spatial source structure, by mapping the polarized "fine structure" of the target AGN. We selected 2 targets, 0954+658 and 0716+714, which (1) have been observed multiple times by the PdBI polarimetric monitoring program; (2) have sufficient integrated fluxes ($S_{90GHz}$ > 1 Jy) ; (3) are close enough to resolve the source structure < 1 pc with given angular resolution ; and (4) are located at high northern declination for good UV coverages. As preliminary results, we present LL and RR polarized images of each target with the maximum angular resolution of ${\sim}60{\mu}as$. Extended structures, probably the jet outflows, are discovered in both sources.

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OBSERVATIONS OF CO J = 2 $\to$ 1 AND 3 $\to$ 2 LINES TOWARD EXTREMELY HIGH VELOCITY OUTFLOWS

  • CHOI MINHO
    • Journal of The Korean Astronomical Society
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    • v.29 no.spc1
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    • pp.195-196
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    • 1996

  • We observed CO J = 2 $\to$ 1 and J = 3 $\to$ 2 lines toward several star formation regions with extremely high velocity (EHV) outflows: W3 IRS5, W28 A2, GL2591, S140, and Cepheus A. The full width of the wings are 90-235 km $s^{-1}$. Some wings show clear break of slope in the line profile implying that the nature of the EHV outflow is different from that of the high velocity outflow. We suggest that the EHV CO wing emission is tracing CO molecules in the stellar wind or jet which drives the high velocity outflow.

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Determining the star formation rate of type 2 AGNs with multi-wavelength SED from UV to radio

  • Lee, Jeong Ae;Woo, Jong-Hak
    • The Bulletin of The Korean Astronomical Society
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    • v.43 no.1
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    • pp.61.1-61.1
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    • 2018

  • Outflows are common among local AGNs. Woo et al. (2017) suggested that AGN feedback through outflows is delayed by a dynamical time scale before the suppression of SFR is observationally detected. However, these SFR have large uncertainties because they were estimated by Artificial Neural Network (ANN) method (Ellison et al. 2016). We measured the SFR of 21 far-IR matched sources (z < 0.1) with total IR luminosity from multi-wavelength SED fitting from UV to radio. 15 out of 21 sources were observed with JCMT SCUBA-2 450 and 850um and 4 and 2 sources were matched with archival data of JCMT SCUBA-2 and Herschel SPIRE, respectively. We compared the true SFR by SED fitting with ANN-based one. In addition, we confirmed that sub-mm data are important to determine the SFR with total IR luminosity from SED fitting. Finally, we discuss the significance of true SFR and further the AGN-SF link.

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