Far-ultraviolet observations of NGC 4151 during the ORFEUS-SPAS II mission

B. R. Espey, G. A. Kriss, J. H. Krolik, W. Zheng, Zlatan Tsvetanov, A. F. Davidsen

Research output: Contribution to journalArticle

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Abstract

We observed the Seyfert 1 galaxy NGC 4151 on 11 occasions at 1-2 day intervals using the Berkeley spectrometer during the ORFEUS-SPAS II mission in 1996 November. The mean spectrum covers 912-1220 Å at ∼0.3 Å resolution with a total exposure of 15,658 s. The mean flux at 1000 Å was 4.7 × 10-13 ergs cm-2 s-1 Å-1. We identify the neutral hydrogen absorption with a number of components that correspond to the velocity distribution of H I seen in our own Galaxy as well as features identified in the C IV λ1549 absorption profile by Weymann et al. The main component of neutral hydrogen in NGC 4151 has a total column density of log NHI = 18.7 ± 1.5 cm-2 for a Doppler parameter b = 250 ± 50 km s-1, and it covers 84% ± 6% of the source. This is consistent with previous results obtained with the Hopkins Ultraviolet Telescope. Other intrinsic far-UV absorption features are not resolved, but the C III* λ1176 absorption line has a significantly higher blueshift relative to NGC 4151 than the C III λ977 resonance line. This implies that the highest velocity region of the outflowing gas has the highest density. Variations in the equivalent width of the C III* λ1176 absorption line anticorrelate with continuum variations on timescales of days. For an ionization timescale of less than 1 day, we set an upper limit of 25 pc on the distance of the absorbing gas from the central source. The O VI λ1034 and He II λ1085 emission lines also vary on timescales of 1-2 days, but their response to the continuum variations is complex. For some continuum variations they show no response, while for others the response is instantaneous to the limit of our sampling interval.

Original languageEnglish
JournalAstrophysical Journal
Volume500
Issue number1 PART II
Publication statusPublished - 1998
Externally publishedYes

Fingerprint

Shuttle pallet satellites
continuums
timescale
ultraviolet telescopes
hydrogen
galaxies
intervals
resonance lines
gases
gas
erg
ionization
spectrometer
velocity distribution
sampling
spectrometers
profiles

Keywords

  • Galaxies: active
  • Galaxies: individual (NGC 4151)
  • Galaxies: nuclei
  • Galaxies: Seyfert
  • Ultraviolet: galaxies

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Espey, B. R., Kriss, G. A., Krolik, J. H., Zheng, W., Tsvetanov, Z., & Davidsen, A. F. (1998). Far-ultraviolet observations of NGC 4151 during the ORFEUS-SPAS II mission. Astrophysical Journal, 500(1 PART II).

Far-ultraviolet observations of NGC 4151 during the ORFEUS-SPAS II mission. / Espey, B. R.; Kriss, G. A.; Krolik, J. H.; Zheng, W.; Tsvetanov, Zlatan; Davidsen, A. F.

In: Astrophysical Journal, Vol. 500, No. 1 PART II, 1998.

Research output: Contribution to journalArticle

Espey, BR, Kriss, GA, Krolik, JH, Zheng, W, Tsvetanov, Z & Davidsen, AF 1998, 'Far-ultraviolet observations of NGC 4151 during the ORFEUS-SPAS II mission', Astrophysical Journal, vol. 500, no. 1 PART II.
Espey BR, Kriss GA, Krolik JH, Zheng W, Tsvetanov Z, Davidsen AF. Far-ultraviolet observations of NGC 4151 during the ORFEUS-SPAS II mission. Astrophysical Journal. 1998;500(1 PART II).
Espey, B. R. ; Kriss, G. A. ; Krolik, J. H. ; Zheng, W. ; Tsvetanov, Zlatan ; Davidsen, A. F. / Far-ultraviolet observations of NGC 4151 during the ORFEUS-SPAS II mission. In: Astrophysical Journal. 1998 ; Vol. 500, No. 1 PART II.
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abstract = "We observed the Seyfert 1 galaxy NGC 4151 on 11 occasions at 1-2 day intervals using the Berkeley spectrometer during the ORFEUS-SPAS II mission in 1996 November. The mean spectrum covers 912-1220 {\AA} at ∼0.3 {\AA} resolution with a total exposure of 15,658 s. The mean flux at 1000 {\AA} was 4.7 × 10-13 ergs cm-2 s-1 {\AA}-1. We identify the neutral hydrogen absorption with a number of components that correspond to the velocity distribution of H I seen in our own Galaxy as well as features identified in the C IV λ1549 absorption profile by Weymann et al. The main component of neutral hydrogen in NGC 4151 has a total column density of log NHI = 18.7 ± 1.5 cm-2 for a Doppler parameter b = 250 ± 50 km s-1, and it covers 84{\%} ± 6{\%} of the source. This is consistent with previous results obtained with the Hopkins Ultraviolet Telescope. Other intrinsic far-UV absorption features are not resolved, but the C III* λ1176 absorption line has a significantly higher blueshift relative to NGC 4151 than the C III λ977 resonance line. This implies that the highest velocity region of the outflowing gas has the highest density. Variations in the equivalent width of the C III* λ1176 absorption line anticorrelate with continuum variations on timescales of days. For an ionization timescale of less than 1 day, we set an upper limit of 25 pc on the distance of the absorbing gas from the central source. The O VI λ1034 and He II λ1085 emission lines also vary on timescales of 1-2 days, but their response to the continuum variations is complex. For some continuum variations they show no response, while for others the response is instantaneous to the limit of our sampling interval.",
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AU - Espey, B. R.

AU - Kriss, G. A.

AU - Krolik, J. H.

AU - Zheng, W.

AU - Tsvetanov, Zlatan

AU - Davidsen, A. F.

PY - 1998

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N2 - We observed the Seyfert 1 galaxy NGC 4151 on 11 occasions at 1-2 day intervals using the Berkeley spectrometer during the ORFEUS-SPAS II mission in 1996 November. The mean spectrum covers 912-1220 Å at ∼0.3 Å resolution with a total exposure of 15,658 s. The mean flux at 1000 Å was 4.7 × 10-13 ergs cm-2 s-1 Å-1. We identify the neutral hydrogen absorption with a number of components that correspond to the velocity distribution of H I seen in our own Galaxy as well as features identified in the C IV λ1549 absorption profile by Weymann et al. The main component of neutral hydrogen in NGC 4151 has a total column density of log NHI = 18.7 ± 1.5 cm-2 for a Doppler parameter b = 250 ± 50 km s-1, and it covers 84% ± 6% of the source. This is consistent with previous results obtained with the Hopkins Ultraviolet Telescope. Other intrinsic far-UV absorption features are not resolved, but the C III* λ1176 absorption line has a significantly higher blueshift relative to NGC 4151 than the C III λ977 resonance line. This implies that the highest velocity region of the outflowing gas has the highest density. Variations in the equivalent width of the C III* λ1176 absorption line anticorrelate with continuum variations on timescales of days. For an ionization timescale of less than 1 day, we set an upper limit of 25 pc on the distance of the absorbing gas from the central source. The O VI λ1034 and He II λ1085 emission lines also vary on timescales of 1-2 days, but their response to the continuum variations is complex. For some continuum variations they show no response, while for others the response is instantaneous to the limit of our sampling interval.

AB - We observed the Seyfert 1 galaxy NGC 4151 on 11 occasions at 1-2 day intervals using the Berkeley spectrometer during the ORFEUS-SPAS II mission in 1996 November. The mean spectrum covers 912-1220 Å at ∼0.3 Å resolution with a total exposure of 15,658 s. The mean flux at 1000 Å was 4.7 × 10-13 ergs cm-2 s-1 Å-1. We identify the neutral hydrogen absorption with a number of components that correspond to the velocity distribution of H I seen in our own Galaxy as well as features identified in the C IV λ1549 absorption profile by Weymann et al. The main component of neutral hydrogen in NGC 4151 has a total column density of log NHI = 18.7 ± 1.5 cm-2 for a Doppler parameter b = 250 ± 50 km s-1, and it covers 84% ± 6% of the source. This is consistent with previous results obtained with the Hopkins Ultraviolet Telescope. Other intrinsic far-UV absorption features are not resolved, but the C III* λ1176 absorption line has a significantly higher blueshift relative to NGC 4151 than the C III λ977 resonance line. This implies that the highest velocity region of the outflowing gas has the highest density. Variations in the equivalent width of the C III* λ1176 absorption line anticorrelate with continuum variations on timescales of days. For an ionization timescale of less than 1 day, we set an upper limit of 25 pc on the distance of the absorbing gas from the central source. The O VI λ1034 and He II λ1085 emission lines also vary on timescales of 1-2 days, but their response to the continuum variations is complex. For some continuum variations they show no response, while for others the response is instantaneous to the limit of our sampling interval.

KW - Galaxies: active

KW - Galaxies: individual (NGC 4151)

KW - Galaxies: nuclei

KW - Galaxies: Seyfert

KW - Ultraviolet: galaxies

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