A Multiwavelength Study of the X‐Ray Sources in NGC 5018

Ghosh, K. K.; Swartz, Douglas A.; Tennant, Allyn F.; Wu, Kinwah; Saripalli, L.

doi:10.1086/428939

Cited by 12 publications

(12 citation statements)

References 47 publications

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“…They found that the diffuse X-ray emission is spatially coincident with strong Hα emission, suggesting that it is powered by star formation. Ghosh et al (2005) obtained a good fit for the spectrum of the diffuse light with a MEKAL plus power law model with Galactic absorption. For the MEKAL component they found kT = 0.41 ± 0.04 keV.…”

Section: Mrk 231 (Iras 12540+5708)mentioning

confidence: 91%

“…It is listed as E3: in the RC3 and in NED, but was classified as an SAB0-by Buta et al (2010) based on Spitzer 3.6 µm images. In short wavelength Spitzer images (Kim et al 2012) and in optical images (Ghosh et al 2005), a tail-like structure extends to the northwest. NGC 5018 was identified as a very latestage major merger remnant by Schweizer et al (1990) and Buson et al (2004).…”

Section: Mrk 231 (Iras 12540+5708)mentioning

confidence: 99%

“…The Chandra X-ray data for NGC 5018 were previously analyzed by Ghosh et al (2005). They note that the nucleus hosts an X-ray point source which may be a low luminosity AGN (intrinsic L X ≤ 3.5 × 10 39 erg s −1 ).…”

Section: Mrk 231 (Iras 12540+5708)mentioning

confidence: 99%

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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: Mrk 231 (Iras 12540+5708)mentioning

confidence: 91%

Section: Mrk 231 (Iras 12540+5708)mentioning

confidence: 99%

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Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

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“…Similarly, optical photometric and spectroscopic studies have revealed that stars, star clusters, ionized nebulae, etc. are possible optical counterparts of ULXs (Ghosh et al 2001(Ghosh et al , 2005Ptak et al 2006;Ramsey et al 2006). Optical spectroscopic studies on the local environments of some ULXs have detected different emission lines, which suggest that both shock and photo-ionization excitations are the dominant physical processes around these objects (Abolmasov 2007a,b;Mucciarelli et al 2005Mucciarelli et al , 2007Zepf et al 2007).…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength Study of the Bright X-Ray Source Population in the Interacting Galaxies NGC 5774/NGC 5775

Ghosh

Saripalli

Gandhi

et al. 2009

The Astronomical Journal

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A few nearby interacting galaxies are known that host elevated number of ultraluminous X-ray sources. Here we report the results of a multiwavelength study of the X-ray source population in the field of the interacting pair of galaxies NGC 5774/5775. A total of 49 discrete sources are detected, including 12 ultraluminous X-ray source candidates with luminosities above 10 39 ergs s −1 in the 0.5 -8.0 keV X-ray band. X-ray source positions are mapped onto optical and radio images to search for potential counterparts. Twelve sources in the field have optical counterparts. Optical colors are used to differentiate these sources, which are mostly located outside the optical extent of the interacting galaxies, as potential globular clusters (2), one compact blue dwarf galaxy and quasars (5). We obtained optical spectra of two of the latter, which confirm that they are background quasars. We expect 3 background sources in the field of these two galaxies. These results are used to determine the true X-ray population of these two interacting galaxies, which are connected with two bridges. Two high mass X-ray binaries are detected on these two bridges suggesting their formation through the interaction-induced starformation episode.NGC 5774 is an extremely low starforming galaxy with five X-ray sources plus three ultraluminous X-ray source candidates. Observed X-ray population of this galaxy does not scale with the starformation rate alone but it may scale jointly with the mass of the galaxy and the starformation rate.

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“…We used the METRIC program 1 to determine the relative positional errors (∼0. ′′ 27) between the PC1 and WF3 images (Ghosh et al 2005). The resultant astrometric accuracy is less than 0.…”

Section: Hubble Wfpc2 Observationsmentioning

confidence: 92%

Detection of X-Ray Elongated Emission From an Ultraluminous X-Ray Source in the Interacting Pair of Galaxies NGC 5953/5954

Rosado¹,

Ghosh²,

Fuentes-Carrera³

2008

The Astronomical Journal

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We present radio through X-ray results of a bright (> 10 40 ergs s −1 in the 0.5 to 8.0 keV band) ultraluminous X-ray source (ULX), CXOU J153434.9+151149, in the starburst, interacting pair of galaxies NGC 5953/5954. Chandra image of this ULX shows that it is elongated. From HST/WFPC2/F606W data we have detected a counterpart of the ULX system with M F 606W ∼ -7.1±0.7 mag. This optical counterpart may be either an O-type supergiant star or a young star cluster. From our Fabry-Perot interferometric observations, we have detected Hα and [NII] (λ6584Å) diffuse emission, with velocity gradients up to 60 km s −1 at the astrometric corrected Chandra position of the ULX. Different scenarios have been invoked as to explain the possible nature of CXOU J153434.9+151149.Based on the observed X-ray morphology of the ULX, we determine that the inclination angle to the elongated emission will be ∼53 o . Beaming with this geometry from a stellar-mass black hole system will be inadequate to explain the observed X-ray luminosity of this ULX. Finally, we suggest that mild-beaming from a binary black hole with mass more than 50M ⊙ associated with a young star cluster, is the most favorable scenario that describes the multiwavelength properties of this ULX. Future observations are highly essential to determine the nature of this rare object.

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A Multiwavelength Study of the X‐Ray Sources in NGC 5018

Cited by 12 publications

References 47 publications

Diffuse X-Ray-emitting Gas in Major Mergers

Diffuse X-Ray-emitting Gas in Major Mergers

Multiwavelength Study of the Bright X-Ray Source Population in the Interacting Galaxies NGC 5774/NGC 5775

Detection of X-Ray Elongated Emission From an Ultraluminous X-Ray Source in the Interacting Pair of Galaxies NGC 5953/5954

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