• The Bulletin of The Korean Astronomical Society
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• v.35 no.2
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• pp.34.2-34.2
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• 2010

The 3C84 (NGC 1275), one of Seyfert 2 galaxy, is an interesting object with its peculiar sub-mas structure. We found that the inner jet (r < 2.5mas) of 3C84 seemed to even changed its position angle and flux over one and a half years based on the result of global 86GHz VLBI survey (Lee et al. 2008). In order to confirm the 'precession' of jet, we observed the object in 4 epochs May07, Oct.07, May08 and Oct.08 with the GMVA (Global mm-VLBI Array) at 3mm (86.25GHz) and the each observation time is about 14 hours. Here we present observation and preliminary result of Oct.07 and May08 epochs.

• Journal of The Korean Astronomical Society
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• v.41 no.2
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• pp.17-22
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• 2008

We present an analysis of the soft X-ray emission of MRK 841 to investigate its long-term variation. The light variation of MRK 841 for three different energy bands of soft, medium, and hard values were studied. The maximum variability with a factor of 5 for about two years was confirmed at all three different bands. The light curves exhibit a gradual variation of brightness. In addition to a gradual variation, the short- term or micro variation was also confirmed with a factor of about two for all three different bands. The light variation of each band did not exhibit a correlation between them, but the flare event is strongest in the soft band. The hardness ratio for hard and soft bands shows irregular variation but there was no correlation between them. It was confirmed that there is a gradual decrease of the photon index. Results of our analysis are discussed within the framework of the accretion disk phenomenon.

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.531-533
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• 2015

We have investigated the long term variability of the intensities of the broad-line region emission lines in the UV spectra of Seyfert I galaxy NGC 5548 from 1973-1996. We have obtained the following results: 1) a high level correlation between the intensities of emission lines as well as between intensities of emission lines and continuum fluxes was discovered. With increasing wavelength the correlation in both cases becomes weaker, 2) the relationship between the intensity of emission lines and the flux radiation in the continuum can be expressed by a power law function with coefficients of ${\alpha}{\approx}0.8-1.1$ for different lines. When the difference between the wavelengths of spectral lines and the continuum is increased, the value of the power function decreases, and 3) it was found that the magnitude of the variability of the line intensities are weaker than the range of variability of the continuum fluxes. The magnitude of the variability of the line intensities and the continuum fluxes increase at longer wavelengths.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.56.2-56.2
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• 2011

NGC 5728은 Seyfert 2 은하로 활동성 은하핵을 가지고 있다. 우리는 기존에 연구된 NGC5728에 관한 자료 중 중심핵 주변의 ring구조의 형성 원인과 과정을 알아보기 위해 시뮬레이션을 하고자 한다. 이 연구를 위해 CFHT 3.6-m의 OASIS로 은하의 중심부 $12{\times}10arcsec2$ 영역을 관측한 자료를 이용하였다. NGC 5728의 중심핵 주변의 구조는 [OIII]5007 영상에서는 두개의 중심핵이 나타나며, $H{\alpha}$ 영상에서는 NW방향에 ring구조가 뚜렷하게 나타난다. 이러한 ring구조의 반경은 ～5.4arcsec, 기울기 ${\sim}50^{\circ}$으로 은하면과 거의 나란하게 위치해 있는 것으로 예상되며 시계방향으로 회전하고 있음이 알려졌다. 관측 자료는 ring의 NW방향은 다가오고 SE방향은 멀어지고 있음이 보여지며 이러한 ring의 형성 원인이 무엇인지에 대하여 조사하였고 ring의 기울기와 은하면의 기울기의 구조적 위치를 추가적으로 알아보고자 한다. 시뮬레이션 프로그램으로는 GADGET-2를 이용하였으며 IDL로 시뮬레이션 결과를 볼 수 있도록 하였다. 현재 관찰된 ring구조가 나타날 수 있도록 여러 조건하에서 연구를 수행중이다.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.49.1-49.1
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• 2011

Utilizing single-epoch spectra and the empirical relation between the size of the broad-line region and AGN continuum luminosity, the so-called single-epoch method has been widely used for estimating AGN black hole masses. However, the systematic uncertainties and the potential biases of this method are not well examined. Taking the full advantage of the high-quality homogeneous spectra from the Lick AGN Monitoring Project (LAMP), we investigate in detail the uncertainties of single-epoch mass estimates by comparing with the reverberation-mapping results. We find that the uncertainty due to AGN variability is less than 0.1 dex, while there is a systematic offset between single-epoch masses and reverberation masses. Particularly, narrow-line Seyfert 1 galaxies show that the Hbeta line widths measured from single-epoch (or mean) spectra are systematically larger than those from rms spectra, indicating a potential bias of single-epoch masses. We will present the detailed measurement method, the test of virial assumption, and the systematic uncertainties.

• The Bulletin of The Korean Astronomical Society
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• v.40 no.1
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• pp.73.1-73.1
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• 2015

Isolated galaxies in low-density regions are significant in the sense that they are least affected by the hierarchical pattern of galaxy growth and interactions with perturbers at least for the last few Gyr. To form a comprehensive picture of the star formation history of isolated galaxies, we construct a catalog of isolated galaxies and their comparison sample in relatively denser environments. The galaxies are drawn from SDSS DR7 in the redshift range of 0.025 < z < 0.044. We performed visual inspection and classified their morphology following the Hubble classification scheme. We have investigated the color-magnitude diagram and found elliptical and unbarred spiral galaxies in isolated systems are relatively fainter and bluer than those in denser regions. For the spectroscopic study, we make use of the OSSY catalog (Oh et al. 2011). Our analysis on the absorption-line properties based on the comparison with stellar population models suggests that isolated elliptical galaxies are likely to be younger and metal poorer, while isolated Sc-type galaxies seem to have older luminosity-weighted ages, than their high-density counterpart. In addition, according to the BPT diagnostics, early-type galaxies among isolated galaxies are rather evenly classified into star forming, composite, Seyfert and LINER, whereas their comparisons are mainly populated in the LINER region. On the other hand, late-type galaxies do not show any prominent difference. We discuss the evolutionary histories of isolated galaxies in the context of the standard ${\Lambda}CDM$ cosmology.

• Publications of The Korean Astronomical Society
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• v.27 no.4
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• pp.257-258
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• 2012

With AKARI, we carried out near-infrared spectroscopy of the nearby barred spiral galaxy, NGC 1097, categorized as Seyfert 1 with a circumnuclear starburst ring. Our observations mapped the galactic center region. As a result, we obtain the spatial distributions of the polycyclic aromatic hydrocarbon $3.3{\mu}m$ and the aliphatic hydrocarbon $3.4-3.6{\mu}m$ emission. The former is detected from all the observed regions and the latter is enhanced near the bar connecting the ring with the nucleus. In addition, we detect absorption features due to $H_2O$ ice and CO/SiO at the ring and the galactic center, while we detect the hydrogen recombination line $Br{\alpha}$ only from the ring. Hence the observed spectra change dramatically within the central 1 kpc region.

• The Bulletin of The Korean Astronomical Society
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• v.42 no.2
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• pp.77.1-77.1
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• 2017

We present the preliminary results from our intensive monitoring campaign for measuring continuum and line variability of a low-mass Seyfert galaxy, NGC 4395, which host a smallest known AGN black hole in the reverberation mapping studies. We performed consecutive photometric observations during 5 nights in April 2017. Various telescopes in the world, including BOAO 1.8-m, NYSC 1-m, MDM 2.4-m, 1.3-m, etc, were dedicated for this campaign. Preliminary results show that the tentative time lag can be determined, which is approximately order of 1-2 hours.

• Journal of The Korean Astronomical Society
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• v.36 no.2
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• pp.73-73
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• 2003

Proof correction to the equation in the third paragraph of the DISCUSSION AND CONCLUSION has not been carried faithfully to the published version of the paper. The corrected equation should read ${\approx}10^{-3}\;M_8^4/^3(N_{\ast}/10^6\;pc^{-3})({\sigma}/300 km\;s^{-l})^{-l}(r/r_t)\;yr^{-1}$, where Ms is the mass of the SMBH in units of $10^8\;M_{\bigodot}$, $\sigma$ is the virial velocity of the stars, $r_t$ is the tidal radius of the SMBH. This estimates the frequency that a star would pass within a sphere with the radius r from the SMBH, rather than the frequency of the tidal disruption event. Therefore, it increases with the mass of the SMBH. However, the loss cone effect should also be taken into account, which reduces the actual event rate. Here, we adopted a factor of one hundred to consider the deficiency from the isotrophic rate. The authors sincerely regret this error.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.1
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• pp.36.3-37
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• 2018

We present a new catalog of hard X-ray sources detected in the first 105 months of observations with the Burst Alert Telescope (BAT) on board the Neil Gehrels Swift observatory. The 105 month Swift-BAT survey is a uniform hard X-ray all-sky survey performed in the 14-195 keV band. The Swift-BAT 105 month catalog provides 1632 (422 new detections) hard X-ray sources in the 14 - 195 keV band above the 4.8 sigma significance level. Adding to the previously known hard X-ray sources, 34% (144/422) of the new detections are identified as Seyfert AGN in nearby galaxies (z < 0.2). The majority of the remaining identified sources are X-ray binaries (7%, 31) and blazars/BL Lac objects (10%, 43). As part of this new edition of the Swift-BAT catalog, we release eight-channel spectra and monthly sampled light curves for each object in the online journal and at the Swift-BAT 105 month Web site.