Journal of the Korean earth science society (한국지구과학회지)

The Korean Earth Science Society (한국지구과학회)
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Radial Velocity and FWHM Spatial Distribution of [OIII] and H𝛽 Lines of the Type II Seyfert Galaxy Mrk 1

제2형 세이퍼트 은하 Mrk 1의 [O III]와 H𝛽선의 시선 속도와 FWHM 공간 분포 연구

  • Hyung, Siek (Department of Earth-science Education, Chungbuk National University) ;
  • Lee, Seong-Jae (Department of Earth-science Education, Chungbuk National University) ;
  • Cho, Ji Eun (Department of Earth-science Education, Chungbuk National University)
  • 형식 (충북대학교 지구과학교육과) ;
  • 이성재 (충북대학교 지구과학교육과) ;
  • 조지은 (충북대학교 지구과학교육과)
  • Received : 2021.11.10
  • Accepted : 2022.06.08
  • Published : 2022.06.30
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Abstract

We investigated the kinematic activity of the Type II Seyfert galaxy Mrk 1 based on H𝛽 and [O III] 5007 extracted from the MR 1 grism spectra observed with the OASIS attached to the CFHT 3.6 m telescope. The [O III] forbidden Gaussian line profiles exhibited asymmetric features with an excess of the blue component: (1) strongest at a distance of about 960 pc from the galaxy center, and (2) a wider line width of about ~900 km s-1 in the NS direction of the center. The velocity distributions in the spectral images showed blue or approaching flow motion in the NE zone, while receding in the SW zone, implying the counter-clockwise rotation. The radial velocity data showed that the center of the AGN region appears to be blocked by gas-dust approaching toward the Earth.

우리는 CFHT에 부착된 OASIS 분광기, MR 1 그리즘으로 관측한 방출선 중, H𝛽와 [O III] 5007 방출선을 분석하여, 제 2형 세이퍼트 은하 Mrk 1의 운동학적 특성을 파악하였다. [O III] 금지선의 가우시안 선 윤곽 분석을 통해 초과하는 청색 이동 성분의 방출 영역이 비대칭적으로 보이는데, (1) 은하 중심부 약 960 pc거리에서 플럭스는 최대를 보이고, (2) 은하 중심부에서 NS 방향으로 ~900 km s-1인 큰 선폭 지역이 있음을 확인하였다. 두 원소의 분광 영상에서 보이는 시선 속도의 특징은 NE 방향에서 접근하는 가스의 흐름이, SW 방향으로 적색 이동, 즉 멀어지는 가스의 흐름이 나타나 반시계 방향 은하의 회전 경향성을 보여준다. 시선 속도 자료로부터 은하 중심은 우리를 향해 접근하는 먼지 가스가 가리고 있음을 파악하였다.

Keywords

Acknowledgement

이 논문은 한국 연구재단 지역 대학 우수과학자지원 사업 연구비 지원(NRF 2020R1I1A3063742; NRF2017R1D1A3B03029309)에 의해 연구되었다. OASIS자료의 분석에 도움을 준 서울대 손동훈 박사와 프랑스 리옹 천체물리학 연구 센터의 Pierre Ferruit박사에게 감사를 표한다.

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