共查询到20条相似文献，搜索用时 62 毫秒
1.
Tigran Movsessian 《中国天文和天体物理学报》2006,6(4)
The ROSAT X-ray source 1RXS J114003.0 124112 was identified as a starburst galaxy at redshift 0.177 by He et al. The authors also noted that the source is almost two orders of magnitude brighter in X-ray than the X-ray-brightest starburst galaxy and it seems to be in a merging system, making this source an enigmatic system demanding further observations. Here we report a re-identification of 1RXS J114003.0 124112 using observations on the 2.6m telescope at Byurakan Astrophysical Observatory, Armenia and the SDSS data. The results indicate that the starburst activity is associated with the brighter object of the system, while the fainter object is a typical Seyfert 1 galaxy at a different redshift (0.282). Therefore, the two objects are not in a merging system, and the Seyfert 1 galaxy naturally accounts for the high X-ray flux. Three more objects reside in the vicinity, but they are all too faint to be responsible for the high X-ray flux. 相似文献
2.
Cindy R. Tam Victoria M. Kaspi Bryan M. Gaensler Eric V. Gotthelf 《Astrophysics and Space Science》2007,308(1-4):519-523
The population of clearly identified anomalous X-ray pulsars has recently grown to seven, however, one candidate anomalous
X-ray pulsar (AXP) still eludes re-confirmation. Here, we present a set of seven Chandra ACIS-S observations of the transient
pulsar AX J1845.0-0258, obtained during 2003. Our observations reveal a faint X-ray point source within the ASCA error circle
of AX J1845.0-0258’s discovery, which we designate CXOU J184454.6-025653 and tentatively identify as the quiescent AXP. Its
spectrum is well described by an absorbed single-component blackbody (kT∼2.0 keV) or power law (Γ∼1.0) that is steady in flux on timescales of at least months, but fainter than AX J1845.0-0258 was during its 1993 period
of X-ray enhancement by at least a factor of 13. Compared to the outburst spectrum of AX J1845.0-0258, CXOU J184454.6-025653
is considerably harder: if truly the counterpart, then its spectral behavior is contrary to that seen in the established transient
AXP XTE J1810-197, which softened from kT∼0.67 keV to ∼0.18 keV in quiescence. This unexpected result prompts us to examine the possibility that we have observed an
unrelated source, and we discuss the implications for AXPs, and magnetars in general.
相似文献
3.
The result of the search for, and the observations of radio emission from two groups of isolated neutron stars: AXP 1E 2259+586
and XDINS 1RXS J1308.6+212708 and 1RXS J214303.7+065419 are reported. The observations were carried out on two sensitive transit
radio telescopes at a few frequencies in the range 42–112 MHz. The flux densities, mean pulse profiles, as well as, the estimation
of the dispersion measures, distances and integrated radio luminosities of all objects are presented. Comparison with X-ray
data shows large differences in the mean pulse widths and luminosities.
相似文献
4.
Altan Baykal Ça&#;da&#; &#;nam M. Ali Alpar Jean in 'T Zand Tod Strohmayer 《Monthly notices of the Royal Astronomical Society》2001,327(4):1269-1272
Using X-ray data from the Rossi X-ray Timing Explorer , we report the pulse timing results of the accretion-powered, high-mass X-ray binary pulsar 4U 1907+09, covering a time-span of almost two years. We measured three new pulse periods in addition to the previously measured four pulse periods. We are able to connect pulse arrival times in phase for more than a year. The source has been spinning down almost at a constant rate, with a spin-down rate of for more than 15 yr. Residuals of pulse arrival times yield a very low level of random-walk noise, with a strength of ∼ on a time-scale of 383 d, which is 40 times lower than that of the high-mass X-ray binary pulsar Vela X-1. The noise strength is only a factor of 5 greater than that of the low-mass X-ray binary pulsar 4U 1626−67. The low level of the timing noise and the very stable spin-down rate of 4U 1907+09 make this source unique among the high-mass X-ray binary pulsars, providing another example, in addition to 4U 1626−67, of long-term quiet spin down from an accreting source. These examples show that the extended quiet spin-down episodes observed in the anomalous X-ray pulsars 1RXS J170849.0−400910 and 1E 2259+586 do not necessarily imply that these sources are not accreting pulsars. 相似文献
5.
D. A. H. Buckley M. J. Coe J. B. Stevens K. van der Heyden L. Angelini N. White P. Giommi 《Monthly notices of the Royal Astronomical Society》2001,320(2):281-288
We report on two optical candidates for the counterpart to an X-ray source in the Small Magellanic Cloud , 1WGA J0053.8−7226, identified as a serendipitous X-ray source from the ROSAT Position Sensitive Proportional Counter (PSPC) archive, and also observed by the Einstein Imaging Proportional Counter . Its X-ray properties, namely the hard X-ray spectrum, flux variability and column density, indicate a hard, transient source, with a luminosity of ∼ XTE and ASCA observations have confirmed the source to be an X-ray pulsar, with a 46-s spin period. Our optical observations reveal two possible candidates within the error circle. Both exhibit strong H α and weaker H β emission. The optical colours indicate that both objects are Be-type stars. The Be nature of the stars implies that the counterpart is most likely a Be/X-ray binary system. Subsequent infrared (IR) photometry ( JHK ) of one of the objects shows that the source varies by at least 0.5 mag, while the measured nearly simultaneously with the UBVRI and spectroscopic observations indicate an IR excess of ∼0.3 mag. 相似文献
6.
D. I. Karasev A. A. Lutovinov M. G. Revnivtsev R. A. Krivonos 《Astronomy Letters》2012,38(10):629-637
We present the results of Chandra and XMM-Newton observations for six hard X-ray sources (IGR J12134-6015, IGR J18293-1213, IGR J18219-1347, IGR J17350-2045, IGR J18048-1455, XTE J1901+014) from the INTEGRAL all-sky survey. Based on these observations, we have improved significantly the localization accuracy of the objects and, therefore, have managed to identify their optical counterparts. Using data from the publicly available 2MASS and UKIDSS infrared sky surveys as well as data from the SOFI/NTT telescope (European Southern Observatory), we have determined the magnitudes of the optical counterparts, estimated their types and (in some cases) the distances to the program objects. A triplet of iron lines with energies of 6.4, 6.7, and 6.9 keV has been detected in the X-ray spectrum of IGR J18048-1455; together with the detection of pulsations with a period of ～1440 s from this source, this has allowed it to be classified as a cataclysmic variable, most likely an intermediate polar. In addition, broadband X-ray spectra of IGR J12134-6015 and IGR J17350-2045 in combination with infrared and radio observations suggest an extragalactic nature of these objects. The source IGR J18219-1347 presumably belongs to the class of high-mass X-ray binaries. 相似文献
7.
Victoria M. Kaspi 《Astrophysics and Space Science》2007,308(1-4):1-11
I review recent observational progress on Anomalous X-ray Pulsars, with an emphasis on timing, variability, and spectra. Highlighted
results include the recent timing and flux stabilization of the notoriously unstable AXP 1E 1048.1–5937, the remarkable glitches
seen in two AXPs, and the newly recognized variety of AXP variability types, including outbursts, bursts, flares, and pulse
profile changes. I also discuss recent discoveries regarding AXP spectra, including their surprising hard X-ray and far-infrared
emission, as well as the pulsed radio emission seen in one source. Much has been learned about these enigmatic objects over
the past few years, with the pace of discoveries remaining steady. However additional work on both observational and theoretical
fronts is needed before we have a comprehensive understanding of AXPs and their place in the zoo of manifestations of young
neutron stars.
相似文献
8.
Coe Buckley Charles Southwell & Stevens 《Monthly notices of the Royal Astronomical Society》1998,293(1):43-48
We report observations which identify the optical/IR counterpart to the ROSAT X-ray transient RX J0117.6−7330. The counterpart is suggested to be a B1–B2 star (luminosity class III–V) showing an IR excess and strong Balmer emission lines. The distance derived from reddening and systemic velocity measurements is consistent with the distance derived from X-ray measurements and puts the source in the Small Magellanic Cloud (SMC). 相似文献
9.
X-ray and optical-to-infrared follow-up observations of the transient X-ray burster SAX J1810.8–2609
J. Greiner A. J. Castro-Tirado TH. Boller H. W. Duerbeck S. Covino G. L. Israel M. J. D. Linden-Vørnle X. Otazu-Porter 《Monthly notices of the Royal Astronomical Society》1999,308(3):L17-L21
We have performed a ROSAT follow-up observation of the X-ray transient SAX J1810.8–2609 on 1998 March 24 and detected a bright X-ray source (named RX J1810.7–2609) which was not detected during the ROSAT all-sky survey in September 1990. Optical-to-infrared follow-up observations of the 10" radius ROSAT HRI X-ray error box revealed one variable object ( R =19.5±0.5 on March 13, R >21.5 on 1998 August 27) which we tentatively propose as the optical/IR counterpart of RX J1810.7–2609≡SAX J1810.8–2609. 相似文献
10.
We present the latest results from a multi-epoch timing and spectral study of the Transient Anomalous X-ray Pulsar XTE J1810–197.
We have acquired seven observations of this pulsar with the Newton X-ray Multi-mirror Mission (XMM-Newton) over the course
of two and a half years, to follow the spectral evolution as the source fades from outburst. The spectrum is arguably best
characterized by a two-temperature blackbody whose luminosities are decreasing exponentially with τ
1=870 d and τ
2=280 d, respectively. The temperatures of these components are currently cooling at a rate of 22% per year from a nearly constant
value recorded at earlier epochs of kT
1=0.25 keV and kT
2=0.67 keV, respectively. The new data show that the temperature T
1 and luminosity of that component have nearly returned to their historic quiescent levels and that its pulsed fraction, which
has steadily decreased with time, is now consistent with the previous lack of detected pulsations in quiescence. We also summarize
the detections of radio emission from XTE J1810–197, the first confirmed for any AXP. We consider possible models for the
emission geometry and mechanisms of XTE J1810–197.
XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This
research is supported by XMM-Newton grant NNG05GJ61G and NASA ADP grant ADP04-0059-0024. 相似文献
11.
The X-ray source IGR J16318-4848 was the first source discovered by INTEGRAL on January 29, 2003. The high energy spectrum
exhibits such a high column density that the source is undetectable in X-rays below 2 keV. On February 23–25, 2003 we triggered
a Target of Opportunity (ToO) Program using the EMMI and SOFI instruments on the New Technology Telescope of the European
Southern Observatory (La Silla) to get optical and near-infrared (NIR) observations. We discovered the optical counterpart,
and confirmed the already proposed candidate in the NIR. NIR spectroscopy revealed a large amount of emission lines, including
forbidden iron lines and P-Cygni profiles, showing a strong similarity with CI Cam, another strongly absorbed source. Together
with the spectral energy distribution (SED), these data point to a high luminosity, high temperature source, with an intrinsic
absorption greater than the interstellar absorption, but two orders of magnitude below the X-ray absorption. All these observations
show that IGR J16318-4848 is a high mass X-ray binary (HMXB) at a distance between 0.9 and 6.2 kpc, the mass donor being an
early-type star, probably a sgB[e] star, surrounded by a dense and absorbing circumstellar material. This would make the second
HMXB with a sgB[e] star as the mass donor after CI Cam.
Other sources, discovered by INTEGRAL near IGR J16318-4848 in the direction of the Norma arm, present the same characteristics,
at least in X-rays. Such sources may represent a different evolutionary state of X-ray binaries previously undetected with
the lower energy space telescopes; if it is so, a new class of strongly absorbed X-ray binaries is being unveiled by INTEGRAL.
Out of the 15 sources present in this region, only one might be associated with an unidentified EGRET source: IGR J16393-4643.
Therefore these obscured INTEGRAL sources do not seem to be powerful high energy (E > 100 MeV) emitters.
Based on observations collected at the European Southern Observatory, Chile (proposal ESO N∘ 70.D-0340). 相似文献
12.
A UBVR monitoring of the X-ray source 1RXS J220111+281849 was performed during August 2–21, 1999. Seven moderately intense ultraviolet flares with 1–3m amplitudes were detected. The object exhibits both rapid and slow flares. An unusual superintense flare with an $11\mathop .\limits^m 0$ amplitude in U was detected on August 18, 1999. Light curves of the flares are presented, and their physical parameters are briefly analyzed. 相似文献
13.
S. Naik P. C. Agrawal B. Paul A. R. Rao S. Seetha K. Kasturirangan 《Journal of Astrophysics and Astronomy》2000,21(1-2):29-38
The outburst of X-ray transient source XTE J2012+381 was detected by the RXTE All-Sky Monitor on 1998 May 24th. Following
the outburst, X-ray observations of the source were made in the 2–18 keV energy band with the Pointed Proportional Counters
of the Indian X-ray Astronomy Experiment (IXAE) on-board the Indian satellite IRS-P3 during 1998 June 2nd–10th. The X-ray
flux of the source in the main outburst decreased exponentially during the period of observation. No large amplitude short-term
variability in the intensity is detected from the source. The power density spectrum obtained from the timing analysis of
the data shows no indication of any quasi-periodic oscillations in 0.002–0.5 Hz band. The hardness ratio i.e. the ratio of
counts in 6–18 keV to 2–6 keV band, indicates that the X-ray spectrum is soft with spectral index >2. From the similarities
of the X-ray properties with those of other black hole transients, we conclude that the X-ray transient XTE J2012+381 is likely
to be a black hole. 相似文献
14.
M. N. Pavlinsky S. A. Grebenev A. A. Lutovinov R. A. Sunyaev A. V. Finoguenov 《Astronomy Letters》2001,27(5):297-303
ART-P/Granat observations of the X-ray burster SLX 1732-304 in the globular cluster Terzan 1 are presented. The X-ray (3–20 keV) fluxes from the source differed by more than a factor of 4 during the observing sessions on September 8 (F x ? 6.95 × 10?10 erg cm?2 s?1) and October 6, 1990 (F x ? 1.64 × 10?10 erg cm?2 s?1). The intensity variations of SLX 1732-304 were apparently accompanied by variations in its hardness: whereas the source in its high state had the spectrum with a distinct exponential cutoff typical of bright low-mass X-ray binaries, its low-state spectrum could be satisfactorily described by a simple power law with a photon index α?1.7. During the ART-P observation on September 8, a type I X-ray burst was detected from SLX 1732-304. 相似文献
15.
I. A. Mereminskiy E. V. Filippova R. A. Krivonos S. A. Grebenev R. A. Burenin R. A. Sunyaev 《Astronomy Letters》2017,43(3):167-174
During the scanning observations of the Galactic center region in late August–September 2016 we detected a new (third) outburst of the historical X-ray nova GRS 1739-278, a presumed black hole in a low-mass X-ray binary. This was reported in the Astronomer’s Telegrams (Mereminskiy et al. 2016). In this paper we present the results of INTEGRAL and Swift observations of the outburst development. According to these observations, the flux from the source in the hard X-ray band (20–60 keV) rose from ~11 (September 3) to ~30 mCrab (September 14), was at the attained level for ~8 days, and then returned to ~15 mCrab. The spectrum of the source taken at its peak brightness in the energy range 0.5–150 keV could be fitted by a single power law with a photon index of 1.86 ± 0.07 distorted only by photoabsorption corresponding to the hydrogen column density log10 (N H) = 22.37 under the assumption of a solar abundance. This means that the source at this time was in the low/hard state. Infrared observations with the RTT-150 telescope near the X-ray brightness peak of the source revealed no emission down to \(22_ \cdot ^m 0\) (in the r’ band) and \(20_ \cdot ^m 9\) (in the i’ band). At the time of writing the paper we do not yet know whether this outburst ended or only its initial stage was observed. If it ended, then based on the light curve and spectra, we can state that it was a “failed” outburst, i.e., the amount of accreted matter in this episode was insufficient to reach the high or very high state with a soft blackbody component in the spectrum characteristic of developed outbursts. 相似文献
16.
We present observations and an analysis of the X-ray source 1RXS J0832.6–2525 which shows it to be a low field magnetic white dwarf with an unusual high mass. This is the second magnetic white dwarf for which a determination of a spectroscopic mass has been possible, and both stars belong to the growing class of ultramassive white dwarfs ( M ≥ 1.1 M⊙). 相似文献
17.
The ROSAT source 1RXS J181333.7+453118 is a Seyfert Sy1 galaxy with a red shift of z=0.093. A ROSAT spectrum and a spectrum over wavelengths of λ4500-7250? taken with the 2.6-m telescope at the Byurakan Astrophysical
Observatory are shown. The x-ray spectrum has characteristics similar to an AGN with a soft x-ray excess. 相似文献
18.
Ü. Ertan M. A. Alpar M. H. Erkut K. Y. Ekşi Ş. Çalışkan 《Astrophysics and Space Science》2007,308(1-4):73-77
The anomalous X-ray pulsar 4U 0142+61 was recently detected in the mid infrared bands with the SPITZER Observatory (Wang, Chakrabarty and Kaplan: Nature 440, 772 (2006)). This observation is the first instance for a disk around an AXP. From a reanalysis of optical and infrared data, we show that the observations indicate that the disk is likely to be an active disk rather than a passive dust disk beyond the light cylinder, as proposed in the discovering paper. Furthermore, we show that the irradiated accretion disk model can also account for all the optical and infrared observations of the anomalous X-ray pulsars in the persistent state. 相似文献
19.
Sempere MJ Cernicharo J Lefloch B González-Alfonso E Leeks S 《The Astrophysical journal》2000,535(2):L123-L127
We report the discovery of quasi-periodic oscillations (QPOs) at roughly 187 and 150 Hz in the X-ray intensity of X-ray nova XTE J1859+226. The source was observed during a recent outburst with the Rossi X-Ray Timing Explorer. Besides these high-frequency QPOs, we have also detected QPOs (and sometimes their harmonics) at 6-7 Hz and significant broadband variability at low frequencies. These properties, as well as the observed hard X-ray spectrum, make XTE J1859+226 a black hole candidate (BHC). The detection of QPOs at two distinct frequencies greater, similar100 Hz in two observations separated by about 4 hr provide additional insights into the high-frequency QPO phenomenon in BHCs. The importance lies in the proposed interpretations, which invariably involve the effects of strong gravity near a black hole. We compare our results to those of other BHCs and discuss the impact of the observational data on the models in a global context. 相似文献
20.
A. Giunta E. Bozzo F. Bernardini G. Israel L. Stella M. Falanga S. Campana A. Bazzano A. J. Dean M. Mendez 《Monthly notices of the Royal Astronomical Society》2009,399(2):744-749
IGR J18483−0311 was discovered with INTEGRAL in 2003 and later classified as a supergiant fast X-ray transient. It was observed in outburst many times, but its quiescent state is still poorly known. Here, we present the results of XMM–Newton , Swift and Chandra observations of IGR J18483−0311. These data improved the X-ray position of the source, and provided new information on the timing and spectral properties of IGR J18483−0311 in quiescence. We report the detection of pulsations in the quiescent X-ray emission of this source, and give for the first time a measurement of the spin-period derivative of this source. In IGR J18483−0311, the measured spin-period derivative of −(1.3 ± 0.3) × 10−9 s s−1 likely results from light travel time effects in the binary. We compare the most recent observational results of IGR J18483−0311 and SAX J1818.6−1703, the two supergiant fast X-ray transients for which a similar orbital period has been measured. 相似文献