Walton, D. J.12; Fuerst, F.12; Harrison, F.12; Stern, D.12; Bachetti, M.4; Barret, D.4; Bauer, F.5; Boggs, S. E.13; Christensen, Finn Erland1; Craig, W. W.14; Fabian, A. C.15; Grefenstette, B. W.12; Hailey, C. J.16; Madsen, K. K.12; Miller, J. M.17; Ptak, A.18; Rana, V.12; Webb, N. A.4; Zhang, W. W.18
1 National Space Institute, Technical University of Denmark2 Astrophysics, National Space Institute, Technical University of Denmark3 California Institute of Technology4 Université de Toulouse5 Space Sci Inst, Boulder, CO 80301 USA6 University of California at Berkeley7 Lawrence Livermore National Laboratory8 University of Cambridge9 Columbia University10 University of Michigan11 NASA Goddard Space Flight Center12 California Institute of Technology13 University of California at Berkeley14 Lawrence Livermore National Laboratory15 University of Cambridge16 Columbia University17 University of Michigan18 NASA Goddard Space Flight Center
Following a serendipitous detection with the Nuclear Spectroscopic Telescope Array (NuSTAR), we present a multi-epoch spectral and temporal analysis of an extreme ultraluminous X-ray source (ULX) located in the outskirts of the Circinus galaxy, hereafter Circinus ULX5, including coordinated XMM-Newton+NuSTAR follow-up observations. The NuSTAR data presented here represent one of the first instances of a ULX reliably detected at hard (E > 10 keV) X-rays. Circinus ULX5 is variable on long time scales by at least a factor of similar to 5 in flux, and was caught in a historically bright state during our 2013 observations (0.3-30.0 keV luminosity of 1.6 x 10(40) erg s(-1)). During this epoch, the source displayed a curved 3-10 keV spectrum, broadly similar to other bright ULXs. Although pure thermal models result in a high energy excess in the NuSTAR data, this excess is too weak to be modeled with the disk reflection interpretation previously proposed to explain the 3-10 keV curvature in other ULXs. In addition to flux variability, clear spectral variability is also observed. While in many cases the interpretation of spectral components in ULXs is uncertain, the spectral and temporal properties of all the high quality data sets currently available strongly support a simple disk-corona model reminiscent of that invoked for Galactic binaries, with the accretion disk becoming more prominent as the luminosity increases. However, although the disk temperature and luminosity are well correlated across all time scales currently probed, the observed luminosity follows L proportional to T1.70+/-0.17, flatter than expected for simple blackbody radiation. The spectral variability displayed here is highly reminiscent of that observed from known Galactic black hole binaries (BHBs) at high luminosities. This comparison implies a black hole mass of similar to 90 M-circle dot for Circinus ULX5. However, given the diverse behavior observed from Galactic BHB accretion disks, this mass estimate is still uncertain. Finally, the limits placed on any undetected iron absorption features with the 2013 data set imply that we are not viewing the central regions of Circinus ULX5 through any extreme super-Eddington outflow.
Astrophysical Journal, 2013, Vol 779, Issue 2
ASTRONOMY; MASS BLACK-HOLES; ACTIVE GALACTIC NUCLEI; HOLMBERG IX X-1; SPECTRAL STATE TRANSITIONS; SPITZER-SPACE-TELESCOPE; PHOTON IMAGING CAMERA; COOL ACCRETION DISKS; NGC 1313 X-1; XMM-NEWTON; ESO 243-49