Abstract
ABSTRACT We present torus modelling for the X-ray spectra of a nearby narrow-line Seyfert 1 galaxy Mrk 1239 (z = 0.0199), based on archival Suzaku, NuSTAR, and Swift observations. Our model suggests very soft intrinsic power-law continuum emission of Γ ≈ 2.57 in 2019 and Γ ≈ 2.98 in 2007. By applying a correction factor to the unabsorbed X-ray luminosity, we find that Mrk 1239 is accreting near or around the Eddington limit. Our best-fitting spectral model also suggests a torus with a column density of log (NH,ave/ cm−2) = 25.0 ± 0.2 and a high covering factor of 0.90 in Mrk 1239, indicating that this source is most likely to be viewed almost face-on with i ≈ 26°. Our line of sight might cross the edge of the torus with NH,los = 2–5 × 1023 cm−2. The high Eddington ratio and the high line-of-sight column density makes Mrk 1239 one of the active galactic nuclei that are close to the limit where wind may form near the edge of the torus due to high radiation pressure.
Highlights
Mrk 1239 is a narrow-line Seyfert 1 galaxy (NLS1) that shows broad Balmer components of 1000 km s−1 and strong Fe [II] emission in the optical band (Osterbrock & Pogge 1985; Veron-Cetty, Veron & Goncalves 2001). Ryan et al (2007) estimated the mass of the supermassive black hole (BH) in the centre of Mrk 1239 to be 7.8 × M by using the size of the broad-line region based on the FWHM(Hβ)–Lλ5100 relation (Kaspi et al 2005) and 1.3 × M on the basis of the FWHM(Hβ)–LH β relation (Greene, Ho & Ulvestad 2006)
In addition to a low BH mass, Mrk 1239 shows interesting properties across multiple wavelengths: in the radio band, relatively stronger radio emission than typical NLS1s along with evidence of a kiloparsec-scale radio jet was found (Doi et al 2015), Mrk 1239 is identified as a radio-quiet source (e.g. 50 mJy at 20 cm, Ulvestad, Antonucci & Goodrich 1995)
Similar conclusions were found in Grupe et al (2004) where a multiwavelength SED was used for the calculation of the Eddington ratio: λEdd ≈ 2 assuming MBH = 5 × 106 M
Summary
Mrk 1239 is a narrow-line Seyfert 1 galaxy (NLS1) that shows broad Balmer components of 1000 km s−1 and strong Fe [II] emission in the optical band (Osterbrock & Pogge 1985; Veron-Cetty, Veron & Goncalves 2001). Ryan et al (2007) estimated the mass of the supermassive black hole (BH) in the centre of Mrk 1239 to be 7.8 × M by using the size of the broad-line region based on the FWHM(Hβ)–Lλ5100 relation (Kaspi et al 2005) and 1.3 × M on the basis of the FWHM(Hβ)–LH β relation (Greene, Ho & Ulvestad 2006). In addition to a low BH mass, Mrk 1239 shows interesting properties across multiple wavelengths: in the radio band, relatively stronger radio emission than typical NLS1s along with evidence of a kiloparsec-scale radio jet was found (Doi et al 2015), Mrk 1239 is identified as a radio-quiet source (e.g. 50 mJy at 20 cm, Ulvestad, Antonucci & Goodrich 1995) These features were previously seen only in radio-loud NLS1s A later study by Grupe, Mathur & Komossa (2004) suggested a similar conclusion of ≈ 3 by analysing the XMM–Newton observation of this source in the 0.3–10 keV band Such soft X-ray continuum emission indicates a high accretion rate in the central disc (e.g. Brightman et al 2013). Introduce our data reduction processes; in Section 3, we introduce a torus-based X-ray spectral model for Mrk 1239; in Section 4, we discuss and conclude our results
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