Teng, S.H. and Rigby, J.R. and Stern, D. and Ptak, A. and Alexander, D.M. and Bauer, F.E. and Boggs, S.E. and Brandt, W.N. and Christensen, F.E. and Comastri, A. and Craig, W.W. and Farrah, D. and Gandhi, P. and Hailey, C.J. and Harrison, F.A. and Hickox, R.C. and Koss, M. and Luo, B. and Treister, E. and Zhang, W.W. (2015) 'A NuSTAR survey of nearby ultraluminous infrared galaxies.', Astrophysical journal., 814 (1). p. 56.
We present a Nuclear Spectroscopic Telescope Array (NuSTAR), Chandra, and XMM-Newton survey of nine of the nearest ultraluminous infrared galaxies (ULIRGs). The unprecedented sensitivity of NuSTAR at energies above 10 keV enables spectral modeling with far better precision than was previously possible. Six of the nine sources observed were detected sufficiently well by NuSTAR to model in detail their broadband X-ray spectra, and recover the levels of obscuration and intrinsic X-ray luminosities. Only one source (IRAS 13120–5453) has a spectrum consistent with a Compton-thick active galactic nucleus (AGN), but we cannot rule out that a second source (Arp 220) harbors an extremely highly obscured AGN as well. Variability in column density (reduction by a factor of a few compared to older observations) is seen in IRAS 05189–2524 and Mrk 273, altering the classification of these borderline sources from Compton-thick to Compton-thin. The ULIRGs in our sample have surprisingly low observed fluxes in high-energy (>10 keV) X-rays, especially compared to their bolometric luminosities. They have lower ratios of unabsorbed 2–10 keV to bolometric luminosity, and unabsorbed 2–10 keV to mid-IR [O iv] line luminosity than do Seyfert 1 galaxies. We identify IRAS 08572+3915 as another candidate intrinsically X-ray weak source, similar to Mrk 231. We speculate that the X-ray weakness of IRAS 08572+3915 is related to its powerful outflow observed at other wavelengths.
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|Publisher Web site:||http://dx.doi.org/10.1088/0004-637X/814/1/56|
|Publisher statement:||© 2015. The American Astronomical Society.|
|Date accepted:||No date available|
|Date deposited:||15 July 2016|
|Date of first online publication:||17 November 2015|
|Date first made open access:||No date available|
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