X-ray and UV Observations of the Luminous Narrow-line Seyfert 1 Galaxies RX J0439.7-4540 and PHL 1092

Details X-ray and UV Observations of the Luminous Narrow-line Seyfert 1 Galaxies RX J0439.7-4540 and PHL 1092 X-ray and UV Observations of the Luminous Narrow-line Seyfert 1 Galaxies RX J0439.7-4540 and PHL 1092

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...207.1807f&link_type=abstract

American Astronomical Society Meeting 207, #18.07; Bulletin of the American Astronomical Society, Vol. 37, p.1185

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Scientific paper

Narrow-line Seyfert 1 galaxies with high luminosities are likely to be among the highest specific accretion rate objects in the Universe. This is because if the width of the Hβ line is related to the dynamical mass, then the specific accretion rate ˙ {M}/˙ {M}Edd∝ v-2}L{1/2.
We present new and archival X-ray and UV observations of the two luminous NLS1s RX J0439.7-4540 and PHL 1092 (MV=-22.7 and -24.3 respectively). The X-ray spectra are very similar, consisting of a power law plus a prominent soft excess that can be modelled approximately by a black body. RX J0439.7-4540 experiences remarkable spectral variability between the ASCA observation made in 1997 and the XMM-Newton observation made in 2005: the flux decreased by a factor of >10, and the photon index flattened from Γ =2.32 ± 0.09 to Γ =1.56 ± 0.09.
Despite the similarity in X-ray properties, the UV spectra are spectacularly different. PHL 1092 shows weak, strongly blueshifted high-ionization lines, and strong low-ionization emission from \ion{Fe}{2}, similar to several other luminous NLS1s including PHL 1811. In contrast, RX J0439.7-4540 has rather strong high-ionization lines, and weak \ion{Fe}{2}, more typical of a bright broad-line quasar.
Results and discussion of these similarities and differences will be presented.
This research is supported by NASA XMM-Newton grant NNG05GD01G and StSCI grant HST-GO-09894.01-A.

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