HST observations of IP Pegasi in quiescence: The pre-eclipse spectrum

D. W. Hoard, Raymundo Baptista, Michael Eracleous, Keith Horne, K. A. Misselt, Allen W. Shafter, Paula Szkody, Janet H. Wood

Research output: Contribution to journalArticle

3 Citations (Scopus)

Abstract

We present time-resolved HST ultraviolet (UV) spectroscopy and ground-based optical photometry of the dwarf nova IP Pegasi in a quiescent state. The observations were obtained prior to an eclipse, when the bright spot caused by the impact of the accretion stream with the edge of the disc dominates the light output. The optical light curve is fairly strongly correlated with the UV spectrophotometric flux curve. An unusual emission-like feature near 1820 Å in the UV spectrum of IP Peg is likely to be a manifestation of the 'Fe II curtain'. Composite spectra constructed from the peaks and troughs of flickers in the light curve show substantial differences. The spectrum of the flickers (i.e., peaks minus troughs) is not adequately modelled by a simple blackbody, suggesting that a more sophisticated model is appropriate. We perform a cross-correlation analysis of the variability in spectrophotometric flux curves of the UV continuum and prominent UV emission lines (C II λ.1335, Si iv λ1400 and C IV λ1550). The continuum and lines are not correlated, suggesting that they are produced separately. The C II and Si IV lines are moderately correlated with each other, but neither line is correlated with C IV, suggesting that the latter forms in a different region from the former. We briefly discuss a qualitative model for the geometry of the emission regions in IP Peg that is consistent with the observed behaviour of the UV lines and continuum.

Original languageEnglish (US)
Pages (from-to)691-701
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Volume288
Issue number3
DOIs
StatePublished - Jan 1 1997

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eclipses
flicker
continuums
troughs
light curve
trough
curtains
ultraviolet emission
ultraviolet spectroscopy
ultraviolet spectra
curves
cross correlation
photometry
spectroscopy
accretion
geometry
composite materials
output

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Hoard, D. W., Baptista, R., Eracleous, M., Horne, K., Misselt, K. A., Shafter, A. W., ... Wood, J. H. (1997). HST observations of IP Pegasi in quiescence: The pre-eclipse spectrum. Monthly Notices of the Royal Astronomical Society, 288(3), 691-701. https://doi.org/10.1093/mnras/288.3.691
Hoard, D. W. ; Baptista, Raymundo ; Eracleous, Michael ; Horne, Keith ; Misselt, K. A. ; Shafter, Allen W. ; Szkody, Paula ; Wood, Janet H. / HST observations of IP Pegasi in quiescence : The pre-eclipse spectrum. In: Monthly Notices of the Royal Astronomical Society. 1997 ; Vol. 288, No. 3. pp. 691-701.
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abstract = "We present time-resolved HST ultraviolet (UV) spectroscopy and ground-based optical photometry of the dwarf nova IP Pegasi in a quiescent state. The observations were obtained prior to an eclipse, when the bright spot caused by the impact of the accretion stream with the edge of the disc dominates the light output. The optical light curve is fairly strongly correlated with the UV spectrophotometric flux curve. An unusual emission-like feature near 1820 {\AA} in the UV spectrum of IP Peg is likely to be a manifestation of the 'Fe II curtain'. Composite spectra constructed from the peaks and troughs of flickers in the light curve show substantial differences. The spectrum of the flickers (i.e., peaks minus troughs) is not adequately modelled by a simple blackbody, suggesting that a more sophisticated model is appropriate. We perform a cross-correlation analysis of the variability in spectrophotometric flux curves of the UV continuum and prominent UV emission lines (C II λ.1335, Si iv λ1400 and C IV λ1550). The continuum and lines are not correlated, suggesting that they are produced separately. The C II and Si IV lines are moderately correlated with each other, but neither line is correlated with C IV, suggesting that the latter forms in a different region from the former. We briefly discuss a qualitative model for the geometry of the emission regions in IP Peg that is consistent with the observed behaviour of the UV lines and continuum.",
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Hoard, DW, Baptista, R, Eracleous, M, Horne, K, Misselt, KA, Shafter, AW, Szkody, P & Wood, JH 1997, 'HST observations of IP Pegasi in quiescence: The pre-eclipse spectrum', Monthly Notices of the Royal Astronomical Society, vol. 288, no. 3, pp. 691-701. https://doi.org/10.1093/mnras/288.3.691

HST observations of IP Pegasi in quiescence : The pre-eclipse spectrum. / Hoard, D. W.; Baptista, Raymundo; Eracleous, Michael; Horne, Keith; Misselt, K. A.; Shafter, Allen W.; Szkody, Paula; Wood, Janet H.

In: Monthly Notices of the Royal Astronomical Society, Vol. 288, No. 3, 01.01.1997, p. 691-701.

Research output: Contribution to journalArticle

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T1 - HST observations of IP Pegasi in quiescence

T2 - The pre-eclipse spectrum

AU - Hoard, D. W.

AU - Baptista, Raymundo

AU - Eracleous, Michael

AU - Horne, Keith

AU - Misselt, K. A.

AU - Shafter, Allen W.

AU - Szkody, Paula

AU - Wood, Janet H.

PY - 1997/1/1

Y1 - 1997/1/1

N2 - We present time-resolved HST ultraviolet (UV) spectroscopy and ground-based optical photometry of the dwarf nova IP Pegasi in a quiescent state. The observations were obtained prior to an eclipse, when the bright spot caused by the impact of the accretion stream with the edge of the disc dominates the light output. The optical light curve is fairly strongly correlated with the UV spectrophotometric flux curve. An unusual emission-like feature near 1820 Å in the UV spectrum of IP Peg is likely to be a manifestation of the 'Fe II curtain'. Composite spectra constructed from the peaks and troughs of flickers in the light curve show substantial differences. The spectrum of the flickers (i.e., peaks minus troughs) is not adequately modelled by a simple blackbody, suggesting that a more sophisticated model is appropriate. We perform a cross-correlation analysis of the variability in spectrophotometric flux curves of the UV continuum and prominent UV emission lines (C II λ.1335, Si iv λ1400 and C IV λ1550). The continuum and lines are not correlated, suggesting that they are produced separately. The C II and Si IV lines are moderately correlated with each other, but neither line is correlated with C IV, suggesting that the latter forms in a different region from the former. We briefly discuss a qualitative model for the geometry of the emission regions in IP Peg that is consistent with the observed behaviour of the UV lines and continuum.

AB - We present time-resolved HST ultraviolet (UV) spectroscopy and ground-based optical photometry of the dwarf nova IP Pegasi in a quiescent state. The observations were obtained prior to an eclipse, when the bright spot caused by the impact of the accretion stream with the edge of the disc dominates the light output. The optical light curve is fairly strongly correlated with the UV spectrophotometric flux curve. An unusual emission-like feature near 1820 Å in the UV spectrum of IP Peg is likely to be a manifestation of the 'Fe II curtain'. Composite spectra constructed from the peaks and troughs of flickers in the light curve show substantial differences. The spectrum of the flickers (i.e., peaks minus troughs) is not adequately modelled by a simple blackbody, suggesting that a more sophisticated model is appropriate. We perform a cross-correlation analysis of the variability in spectrophotometric flux curves of the UV continuum and prominent UV emission lines (C II λ.1335, Si iv λ1400 and C IV λ1550). The continuum and lines are not correlated, suggesting that they are produced separately. The C II and Si IV lines are moderately correlated with each other, but neither line is correlated with C IV, suggesting that the latter forms in a different region from the former. We briefly discuss a qualitative model for the geometry of the emission regions in IP Peg that is consistent with the observed behaviour of the UV lines and continuum.

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