Galactic Sources Detected in the NuSTAR Serendipitous Survey

Tomsick, John A.; Lansbury, G. B.; Rahoui, Farid; Clavel, M.; Fornasini, Francesca M.; Hong, Jaesub; Aird, James; Alexander, D. M.; Bodaghee, A.; Chiu, Jeng Jiann; Grindlay, Jonathan E.; Hailey, Charles J.; Harrison, Fiona A.; Krivonos, R.; Mori, Kaya; Stern, Daniel

doi:10.3847/1538-4365/aa7517

Cited by 9 publications

(13 citation statements)

References 67 publications

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“…Then, we find a bright object, CXO J092418.2−314217, in a Swift/XRT soft X-ray image. According to a study by Tomsick et al (2017), it can be classified as the LMXB or the CV, and here we representatively adopt the LMXB. (C) One of the brightest galaxies is selected for the most plausible counterpart.…”

Section: Discussionmentioning

confidence: 99%

The 7-year MAXI/GSC X-Ray Source Catalog in the High Galactic Latitude Sky (3MAXI)

Kawamuro

Ueda

Shidatsu

et al. 2018

ApJS

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We present the third MAXI/GSC catalog in the high Galactic-latitude sky (|b| > 10 • ) based on the 7complementary to that in the low Galactic-latitude sky (|b| < 10 • ; Hori et al. 2018). We compile 682 sources detected at significances of s D,4−10 keV ≥ 6.5 in the 4-10 keV band. A two-dimensional image fit based on the Poisson likelihood algorithm (Cstatistics) is adopted for the detections and constraints on their fluxes and positions. The 4-10 keV sensitivity reaches ≈ 0.48 mCrab, or ≈ 5.9 × 10 −12 erg cm −2 s −1 , over the half of the survey area. Compared with the 37-month catalog (Hiroi et al. 2013), which adopted a threshold of s D,4−10 keV ≥ 7, the source number increases by a factor of ∼1.4. The fluxes in the 3-4 keV and 10-20 keV bands are further estimated, and hardness ratios (HRs) are calculated using the 3-4 keV, 4-10 keV, 3-10 keV, and 10-20 keV band fluxes. We also make the 4-10 keV lightcurves in one year bins for all the sources and characterize their variabilities with an index based on a likelihood function and the excess variance. Possible counterparts are found from five major X-ray survey catalogs by Swift , Uhuru, RXTE , XMM-Newton, and ROSAT , and an X-ray galaxy-cluster catalog (MCXC). Our catalog provides the fluxes, positions, detection significances, HRs, one-year bin lightcurves, variability indices, and counterpart candidates.

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Section: Discussionmentioning

confidence: 99%

The 7-year MAXI/GSC X-Ray Source Catalog in the High Galactic Latitude Sky (3MAXI)

Kawamuro

Ueda

Shidatsu

et al. 2018

ApJS

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“…Blue circles represent observations from our 2015 decay, with the blue solid lines connecting the data points to illustrate the evolution with time (following the direction of the blue arrow). Red triangles show spectral fits from pre-outburst observations compiled from Reynolds et al (2014) and Rana et al (2016), the red diamond represents a Chandra observation from 2015 November (Tomsick et al 2015), and black squares represent the average photon indices of 10 quiescent BHXBs binned by Eddington ratio, from Plotkin et al (2013). The X-ray spectral softening occurs over a narrow range in Eddington ratio (from than the value for the mechanism that produces the source of seed photons, on account of SSC depending on the product of the photon field density and the particle density (e.g., Falcke & Biermann 1995).…”

Section: Comments On Jet Synchrotron X-ray Emissionmentioning

confidence: 99%

“…et al (2014) and Tomsick et al (2015) in upcoming figures, we convert their reported 0.3-10 keV fluxes to 0.5-10 keV.…”

Section: Quiescent X-ray Spectramentioning

confidence: 99%

“…We also include a Chandra observation of V404 Cygni obtained by Tomsick et al (2015) on 2015 November 27 (obsID 17245; PI Tomsick; note that this was 26 days before V404 Cygni flared again on 2015 December 23; Beardmore et al 2015b). This post-outburst observation shows X-ray properties similar to preoutburst, including .…”

Section: Quiescent X-ray Spectramentioning

confidence: 99%

“…(Hynes et al 2004(Hynes et al , 2009Corbel et al 2008), and one from the VLA/NuSTAR in 2013 (Rana et al 2016). We also adopt X-ray spectral parameters from the literature based on three additional X-ray observations taken pre-outburst from Chandra, XMMNewton, and Suzaku (Reynolds et al 2014) and one Chandra observation taken after the outburst in 2015 November (Tomsick et al 2015; see Section 3.4.3). .…”

Section: Comparison Observations From the Literaturementioning

confidence: 99%

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The 2015 Decay of the Black Hole X-Ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition Into Quiescence

Plotkin

Miller-Jones

Gallo

et al. 2017

ApJ

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We present simultaneous X-ray and radio observations of the black hole X-ray binary V404 Cygni at the end of its 2015 outburst. From 2015 July 11-August 5, we monitored V404 Cygni with Chandra, Swift, and NuSTAR in the X-ray, and with the Karl G. Jansky Very Large Array and the Very Long Baseline Array in the radio, spanning a range of luminosities that were poorly covered during its previous outburst in 1989 (our 2015 campaign covers10 erg s 33 X 34 1 ). During our 2015 campaign, the X-ray spectrum evolved rapidly from a hard photon index of). We argue that V404 Cygni reaching G » 2 marks the beginning of the quiescent spectral state, which occurs at a factor of ≈3-4 higher X-ray luminosity than the average pre-outburst luminosity of »´-8 10 erg s 32 1. V404 Cygni falls along the same radio/X-ray luminosity correlation that it followed during its previous outburst in 1989, implying a robust disk-jet coupling. We exclude the possibility that a synchrotron-cooled jet dominates the X-ray emission in quiescence, leaving synchrotron self-Compton from either a hot accretion flow or from a radiatively cooled jet as the most likely sources of X-ray radiation, and/or particle acceleration along the jet becoming less efficient in quiescence. Finally, we present the first indications of correlated radio and X-ray variability on minute timescales in quiescence, tentatively measuring the radio emission to lag the X-ray by  15 4 minute, suggestive of X-ray variations propagating down a jet with alength of<3.0 au.

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