Complex gaseous structure in the nucleus of NGC 5252

Zlatan Tsvetanov, Jon A. Morse, Andrew S. Wilson, Gerald Cecil

Research output: Contribution to journalArticle

20 Citations (Scopus)

Abstract

We present several Hubble Space Telescope (HST) WFPC2 emission-line and continuum images of NGC 5252, a Seyfert 2 S0 galaxy with a large-scale " ionization bi-cone." In the Hα + [N II] image, the nucleus is bracketed at ∼0″.3 radii by two bright emission-line clumps along P.A. = 35° (∼20° from the major axis of the large-scale stellar disk). These three knots dominate the emission in the innermost ∼ 1″ (∼450 pc at 92 Mpc distance). Two major and several smaller spiral filaments, wound tightly counterclockwise, extend ∼ 3″ to the northwest and ∼4″.5 to the southeast of the nucleus. Several of these filaments extend from the two clumps near the nucleus, possibly indicating that the three collinear knots comprise a bar. Our Fabry-Perot velocity map shows that the spiral pattern is rotating, in a disk inclined significantly to both the galaxy stellar disk and the radio jets. The nuclear radio jets appear to have no obvious association with the Hα + [N II] filaments and clumps. Although most of the line flux is emitted within the inward extrapolation of the largescale ionization bi-cone, some of the Hα + [N II] filaments extend beyond the cone boundaries. A remarkable D-shaped pattern of obscuring dust is visible on the northwest side of the galaxy major axis. Most of the spiral filaments in the Hα + [N II] image also appear in the obscuration map. The extinction by the filaments requires a column density of NH ≈ 5 7times; 1020 cm-2. If the filaments are uniformly filled, both the gas responsible for the extinction and the ionized gas responsible for the emission have number densities of a few cm-3.

Original languageEnglish
Pages (from-to)172-177
Number of pages6
JournalAstrophysical Journal
Volume458
Issue number1 PART I
Publication statusPublished - 1996
Externally publishedYes

Fingerprint

filaments
nuclei
clumps
ionization
extinction
cones
radio
galaxies
gas
dust
occultation
ionized gases
Hubble Space Telescope
extrapolation
continuums
radii
gases

Keywords

  • Galaxies
  • Individual (NGC 5252) - Galaxies
  • ISM - Galaxies
  • Nuclei - Galaxies
  • Peculiar -galaxies
  • Seyfert

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Space and Planetary Science

Cite this

Tsvetanov, Z., Morse, J. A., Wilson, A. S., & Cecil, G. (1996). Complex gaseous structure in the nucleus of NGC 5252. Astrophysical Journal, 458(1 PART I), 172-177.

Complex gaseous structure in the nucleus of NGC 5252. / Tsvetanov, Zlatan; Morse, Jon A.; Wilson, Andrew S.; Cecil, Gerald.

In: Astrophysical Journal, Vol. 458, No. 1 PART I, 1996, p. 172-177.

Research output: Contribution to journalArticle

Tsvetanov, Z, Morse, JA, Wilson, AS & Cecil, G 1996, 'Complex gaseous structure in the nucleus of NGC 5252', Astrophysical Journal, vol. 458, no. 1 PART I, pp. 172-177.
Tsvetanov Z, Morse JA, Wilson AS, Cecil G. Complex gaseous structure in the nucleus of NGC 5252. Astrophysical Journal. 1996;458(1 PART I):172-177.
Tsvetanov, Zlatan ; Morse, Jon A. ; Wilson, Andrew S. ; Cecil, Gerald. / Complex gaseous structure in the nucleus of NGC 5252. In: Astrophysical Journal. 1996 ; Vol. 458, No. 1 PART I. pp. 172-177.
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AB - We present several Hubble Space Telescope (HST) WFPC2 emission-line and continuum images of NGC 5252, a Seyfert 2 S0 galaxy with a large-scale " ionization bi-cone." In the Hα + [N II] image, the nucleus is bracketed at ∼0″.3 radii by two bright emission-line clumps along P.A. = 35° (∼20° from the major axis of the large-scale stellar disk). These three knots dominate the emission in the innermost ∼ 1″ (∼450 pc at 92 Mpc distance). Two major and several smaller spiral filaments, wound tightly counterclockwise, extend ∼ 3″ to the northwest and ∼4″.5 to the southeast of the nucleus. Several of these filaments extend from the two clumps near the nucleus, possibly indicating that the three collinear knots comprise a bar. Our Fabry-Perot velocity map shows that the spiral pattern is rotating, in a disk inclined significantly to both the galaxy stellar disk and the radio jets. The nuclear radio jets appear to have no obvious association with the Hα + [N II] filaments and clumps. Although most of the line flux is emitted within the inward extrapolation of the largescale ionization bi-cone, some of the Hα + [N II] filaments extend beyond the cone boundaries. A remarkable D-shaped pattern of obscuring dust is visible on the northwest side of the galaxy major axis. Most of the spiral filaments in the Hα + [N II] image also appear in the obscuration map. The extinction by the filaments requires a column density of NH ≈ 5 7times; 1020 cm-2. If the filaments are uniformly filled, both the gas responsible for the extinction and the ionized gas responsible for the emission have number densities of a few cm-3.

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