A deficit of ultraluminous X-ray sources in luminous infrared galaxies

Luangtip, W.; Roberts, T. P.; Mineo, S.; Lehmer, Bret; Alexander, D. M.; Jackson, Floyd; Goulding, Andy D.; Fischer, J.

doi:10.1093/mnras/stu2086

Cited by 21 publications

(56 citation statements)

References 109 publications

(195 reference statements)

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“…In an earlier Chandra study, we found a deficiency of ultra-luminous X-ray point sources (ULXs; L X > 10 39 erg s −1 ) relative to L FIR for ultra-luminous infrared galaxies (ULIRGs) . This deficiency in ULXs in high SFR galaxies was later confirmed by Luangtip et al (2015). In the current study, we investigate whether there is a corresponding depression in the diffuse X-ray luminosity relative to the SFR at high L FIR , or if the global deficiency is due to point sources alone.…”

Section: Introductionmentioning

confidence: 70%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

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Using archived data from the Chandra X-ray telescope, we have extracted the diffuse Xray emission from 49 equal-mass interacting/merging galaxy pairs in a merger sequence, from widely separated pairs to merger remnants. After removal of contributions from unresolved point sources, we compared the diffuse thermal X-ray luminosity from hot gas (L X (gas)) with the global star formation rate (SFR). After correction for absorption within the target galaxy, we do not see strong trend of L X (gas)/SFR with SFR or merger stage for galaxies with SFR > 1 M ⊙ yr −1 . For these galaxies, the median L X (gas)/SFR is 5.5 × 10 39 ((erg s −1 )/M ⊙ yr −1 )), similar to that of normal spiral galaxies. These results suggest that stellar feedback in star forming galaxies reaches an approximately steady state condition, in which a relatively constant fraction of about 2% of the total energy output from supernovae and stellar winds is converted into X-ray flux. Three late-stage merger remnants with low SFRs and high K band luminosities (L K ) have enhanced L X (gas)/SFR; their UV/IR/optical colors suggest that they are post-starburst galaxies, perhaps in the process of becoming ellipticals. Systems with L K < 10 10 L ⊙ have lower L X (gas)/SFR ratios than the other galaxies in our sample, perhaps due to lower gravitational fields or lower metallicities. We see no relation between L X (gas)/SFR and Seyfert activity in this sample, suggesting that feedback from active galactic nuclei is not a major contributor to the hot gas in our sample galaxies.

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Section: Introductionmentioning

confidence: 70%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

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“…Gilfanov et al 2004, Luangtip et al 2014 continues to this day as new observations arise, and the balance has tipped recently in favour of stellar-mass BHs and NSs (M101 ULX-1, Liu et al 2013;NGC7793 P13, Motch et al 2014;M-82 X-2, Bachetti et al 2014) rather than IMBHs. It is actually interesting that the observations do not favour the "simpler" resolution of this issue: the main difficulty with ULXs is that they should not radiate above the Eddington limit (L Edd = 1.3 × 10 38 (MX /M ) erg s −1 ), and IMBHs with masses MX ∼10 2−4 M would remain comfortably below this limit.…”

Section: Discussionmentioning

confidence: 99%

Revisiting the dynamical case for a massive black hole in IC10 X-1

Laycock

Maccarone

Christodoulou

2015

Monthly Notices of the Royal Astronomical Society: Letters

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The relative phasing of the X-ray eclipse ephemeris and optical radial velocity (RV) curve for the X-ray binary IC10 X-1 suggests the He[λ4686] emission-line originates in a shadowed sector of the stellar wind that avoids ionization by X-rays from the compact object. The line attains maximum blueshift when the wind is directly toward us at mid X-ray eclipse, as is also seen in Cygnus X-3. If the RV curve is unrelated to stellar motion, evidence for a massive black hole evaporates because the mass function of the binary is unknown. The reported X-ray luminosity, spectrum, slow QPO, and broad eclipses caused by absorption/scattering in the WR wind are all consistent with either a low-stellar-mass BH or a NS. For a NS, the centre of mass lies inside the WR envelope whose motion is then far below the observed 370 km/s RV amplitude, while the velocity of the compact object is as high as 600 km/s. The resulting 0.4% doppler variation of X-ray spectral lines could be confirmed by missions in development. These arguments also apply to other putative BH binaries whose RV and eclipse curves are not yet phase-connected. Theories of BH formation and predicted rates of gravitational wave sources may need revision.

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“…As can be seen by comparing Figure 2 We estimate the flux of each 3σ-detected source assuming a power law with a photon index of Γ = 1.7 (Swartz et al 2004;Soria 2011). Their luminosities (Table 1) put them in the range of ultra-luminous X-ray sources (ULXs; commonly associated with star forming galaxies Swartz et al 2011;Luangtip Figure 2. (a) Extraction regions for both bright point-like sources W1-3, E1-5, and B1 associated with the southwestern galaxy UGC 12914, northeastern galaxy UGC 12915, and the bridge region, respectively; and the extended regions extracted (see Table 1).…”

Section: The Compact Sourcesmentioning

confidence: 99%

X-Ray Emission From the Taffy (Vv254) Galaxies and Bridge

Appleton

Lanz

Bitsakis

et al. 2015

ApJ

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We present the first X-ray observations of the Taffy galaxies (UGC 12914/5) with the Chandra observatory and detect soft X-ray emission in the region of the gas-rich, radio-continuum-emitting Taffy bridge. The results are compared to Herschel observations of dust and diffuse [C II] line-emitting gas. The diffuse component of the Taffy bridge has an X-ray luminosity of L X 0.5 8 keV, which accounts for 19% of the luminosity of the sum for the two galaxies. The total mass in hot gas is (0.8-1.3) × 10 8 M e , which is approximately 1% of the total (H I + H 2 ) gas mass in the bridge, and ∼11% of the mass of warm molecular hydrogen discovered by Spitzer. The soft X-ray and dense CO-emitting gas in the bridge have offset distributions, with the X-rays peaking along the northwestern side of the bridge in the region where stronger far-IR dust and diffuse [C II] gas is observed by Herschel. We detect nine Ultra Luminous X-ray sources in the system, the brightest of which is found in the bridge, associated with an extragalactic H II region. We suggest that the X-ray-emitting gas has been shockedheated to high temperatures and "splashed" into the bridge by the collision. The large amount of gas stripped from the galaxies into the bridge and its very long gas depletion timescale (>10 Gyr) may explain why this system, unlike most major mergers, is not a powerful IR emitter.

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A deficit of ultraluminous X-ray sources in luminous infrared galaxies

Cited by 21 publications

References 109 publications

Diffuse X-Ray-emitting Gas in Major Mergers

Diffuse X-Ray-emitting Gas in Major Mergers

Revisiting the dynamical case for a massive black hole in IC10 X-1

X-Ray Emission From the Taffy (Vv254) Galaxies and Bridge

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