An X-ray halo in the “hot-spot” galaxy NGC 2903

Tschöke, D.; Hensler, G.; Junkes, N.

doi:10.1051/0004-6361:20030952

Cited by 17 publications

(33 citation statements)

References 34 publications

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“…A H II ionized region at a distance of 2.12 was detected by Tschöeke et al (2003) and Popping et al (2010). In the SIMBAD database, we did not find any counterpart or entry to XMM-NGC2903 X2, XMM-NGC2903 X5, nor to XMM-NGC2903 X6, within a 10 radius query.…”

Section: X-ray Point Sources In the Ngc 2903mentioning

confidence: 70%

“…Although we obtained the respective PSLAs by means of the psechain task for each source, we considered an absolute error of 2 , which also accounts for the pointing uncertainties of XMM-Newton, according to the latest calibration report 2 . We cross-correlated the sources with the catalogues of Tschöeke et al (2003) and Popping et al (2010) for the locations of H II regions and SF knots, the work by Sonbas et al (2009) with new detections of supernova remnants (SNRs), and also the catalogue of Alonso-Herrero et al (2001) with the locations of nuclear star clusters. We also cross-identified the location of the X-ray sources with the ULX catalogues of Liu & Bregman (2005) and the ROSAT high resolution survey of galaxies of Roberts & Warwick (2000).…”

Section: X-ray Point Sources In the Ngc 2903mentioning

confidence: 99%

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XMM-Newtonobservations of the hot spot galaxy NGC 2903

Pérez-Ramírez

Caballero‐García

Ebrero

et al. 2010

A&A

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We report on the first deeper X-ray broad-band observation of the hot spot galaxy NGC 2903 obtained with XMM-Newton. X-ray imaging and spectra of the spiral barred galaxy NGC 2903 were obtained from XMM-Newton archival data to study its X-ray population and the conditions of the hot gas in its central region. We investigate the spectral properties of the discrete point-source population and give estimates of their X-ray spectral parameters. By analysing the RGS spectra, we derive temperature and abundances for the hot gas located in its central region. A total of six X-ray point sources (four of them ULX candidates) were detected in the energy range of 0.3-10.0 keV located within the galaxy D 25 optical disk. Three of these sources are detected for the first time, and one of them, XMM-NGC2903 X2 with a luminosity of higher than 10 39 erg s −1 . After fitting three different models, we were able to estimate their luminosities, which are compatible with those of binaries with a compact object in the form of black holes (BHs) rather than neutron stars (NSs). We extracted the combined first-order RGS1 and RGS2 spectra of its central region, which display several emission lines.The spectrum is dominated by a strong O viii Lyα emission line along with Ne x Lyα and several Fe xvii features. The O vii complex is also significantly detected, although only the forbidden and resonance lines could be resolved. Both O vii f and r lines seem to be of similar strength, which is consistent with the presence of the collisionally ionized gas that is typical of starburst galaxies. We fitted the spectrum to a model for a plasma in collisional ionization equilibrium (CIE) and the continuum was modelled with a power law, resulting in a plasma temperature of T = 0.31 ± 0.01 keV and an emission measure EM ≡ n H n e V = 6.4 +0.5 −0.4 × 10 61 cm −3 . We also estimated abundances that are consistent with solar values.

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Section: X-ray Point Sources In the Ngc 2903mentioning

confidence: 70%

Section: X-ray Point Sources In the Ngc 2903mentioning

confidence: 99%

XMM-Newtonobservations of the hot spot galaxy NGC 2903

Pérez-Ramírez

Caballero‐García

Ebrero

et al. 2010

A&A

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“…However, a slight increase in the polarization degree, thus a higher degree of magnetic field ordering, in the eastern disk, as well as the higher pitch angle of the magnetic field, may represent some external influence. In particular, the X-ray observations of Tschöke et al (2000) trace central activity that may be triggered by tidal interactions within the cluster environment. Likely evidence of this could be a radio emission extension to the northeast.…”

Section: Distributions In the Disk Planementioning

confidence: 99%

The magnetic fields of large Virgo cluster spirals. II

Weżgowiec

Urbanik

Beck

et al. 2012

A&A

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Context. The Virgo cluster of galaxies provides excellent conditions for studying interactions of galaxies with the cluster environment. Both the high-velocity tidal interactions and effects of ram pressure stripping by the intracluster gas can be investigated in detail. Aims. We extend our systematic search for possible anomalies in the magnetic field structures of Virgo cluster spirals in order to characterize a variety of effects and attribute them to different disturbing agents. Methods. Six angularly large Virgo cluster spiral galaxies (NGC 4192, NGC 4302, NGC 4303, NGC 4321, NGC 4388, and NGC 4535) were targets of a sensitive total power and polarization study using the 100-m radio telescope in Effelsberg at 4.85 GHz and 8.35 GHz (except for NGC 4388 observed only at 4.85 GHz, and NGC 4535 observed only at 8.35 GHz). The presented twofrequency studies allow Faraday rotation analysis. Results. Magnetic field structures distorted to various extent are found in all galaxies. Three galaxies (NGC 4302, NGC 4303, and NGC 4321) show some signs of possible tidal interactions, while NGC 4388 and NGC 4535 have very likely experienced strong ram-pressure and shearing effects, respectively, visible as distortions and asymmetries of polarized intensity distributions. As in our previous study, even strongly perturbed galaxies closely follow the radio-far-infrared correlation. In NGC 4303 and NGC 4321, we observe symmetric spiral patterns of the magnetic field and in NGC 4535 an asymmetric pattern. Conclusions. The cluster environment clearly affects the evolution of its member galaxies via various effects. Magnetic fields allow us to trace even weak interactions that are difficult to detect with other observations. Our results show that the degree of distortions of a galaxy is not a simple function of the distance to the cluster center but reflects also the history of its interactions. The angle Θ between the velocity vector u and the rotation vector Ω of a galaxy may be a general parameter that describes the level of distortions of galactic magnetic fields. Information about the motions of galaxies in the sky plane and their three-dimensional distribution, as well as information about the intracluster medium can also be obtained from the Faraday rotation analysis.

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“…Geometry of system Tschöcke et al (1999), from inspection of the HST image of NGC 4410A, considered that this galaxy was in an almost faceon orientation (low angle of inclination). However, the evidence from the axis ratio in our ellipse-fitting suggests that it is at an angle of ≈45…”

Section: The Optical Bridgesmentioning

confidence: 99%

“…• 17 40 , J2000.0) has been classified as a Sab pec asymmetric double-lobed radio-galaxy (Hummel et al 1986;Tschöcke et al 1999;Smith 2000), with the radio emission interpreted as a distorted radio jet. This galaxy forms a galaxy pair and, most probably, a future merger (Smith 2000;Donahue et al 2002;Smith et al 2003) with the E?…”

Section: Introductionmentioning

confidence: 99%

BVRIphotometric analysis for the galaxy group NGC 4410

Grana

Kemp

Katsiyannis

et al. 2008

A&A

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We present a BVRI CCD (Charge Coupled Device) surface photometry analysis of the galaxy group NGC 4410, which contains four galaxies in interaction. Along with our photometric study, we show residual images (after subtracting isophotal models) and unsharp masked images to uncover any hidden structures in this system of galaxies; we have also performed a two-dimensional bulge-disk decomposition for NGC 4410C and D, and a major axis sector profile for NGC 4410A. We have calculated BVRI surface brightnesses and colors within regions such as galaxy centers, bridges, tails and optical knots in the NGC 4410 system, generating B− V color maps and color profiles. The information obtained was used to discover the predominant stellar populations. The colors of the galaxies imply ages of ∼2 × 10 9 to ∼2 × 10 10 years for models using a range of metallicities. The bluer knots and H II regions have colors implying ages of a minimum of 5× 10 8 years, but possibly as high as 3× 10 9 years for stellar populations formed in the interaction. These results lead us to conclude that there is a moderate star formation rate and a tranquil evolving state of the system with a long timescale for interaction, much longer than the typical dynamical timescales of 10 8 years. Although we note that NGC 4410D has a blue nucleus (possible nuclear starburst?), bulge, bar, and short spiral arms, and may be interacting with a H I gas cloud. Some observed structures in NGC 4410A are coincident with previously studied H II regions, a tidal arm and optical/radio knots found in this galaxy. An optical knot E coincident with a radio knot may be an optical synchrotron emission or an H II region. The galaxy NGC 4410B appears to be a boxy giant elliptical with a possible dusty disk embedded (similar to Cen A?) and NGC 4410C is confirmed as a lenticular galaxy.

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An X-ray halo in the “hot-spot” galaxy NGC 2903

Cited by 17 publications

References 34 publications

XMM-Newtonobservations of the hot spot galaxy NGC 2903

XMM-Newtonobservations of the hot spot galaxy NGC 2903

The magnetic fields of large Virgo cluster spirals. II

BVRIphotometric analysis for the galaxy group NGC 4410

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