Broad-band properties of the hard X-ray cataclysmic variables IGR J00234+6141 and 1RXS J213344.1+510725

Anzolin, G.; Martino, D. de; Falanga, M.; Mukai, K.; Bonnet‐Bidaud, J. M.; Mouchet, M.; Terada, Y.; Ishida, M.

doi:10.1051/0004-6361/200911816

Cited by 31 publications

(44 citation statements)

References 56 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Further to this Anzolin et al (2009) report XMM observations which clearly show spin modulated X-ray variability below 2 keV, but not above it. No hard X-ray detections of the white dwarf spin period have been reported.…”

Section: Igr J00234+6141mentioning

confidence: 59%

RXTE andXMMobservations of intermediate polar candidates

Butters

Norton

Mukai

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We aim to determine the credentials of nine candidate intermediate polars in order to confirm whether or not they are magnetic cataclysmic variables. Methods. Frequency analysis of RXTE and XMM data was used to search for temporal variations that could be associated with the spin period of the magnetic white dwarf. X-ray spectral analysis was carried out to characterize the emission and absorption properties of each target.Results. The hard X-ray light curve of V2069 Cyg shows a pulse period of 743.2 s, and its spectrum is fit by an absorbed bremsstrahlung model with an iron line, confirming this to be a genuine intermediate polar. The hard X-ray light curve of the previously confirmed intermediate polar IGR J00234+6141 is shown to be consistent with the previous low-energy X-ray detection of a 563.5 s pulse period. The likely polar IGR J14536-5522 shows no coherent modulation at the previously identified period of 3.1 h, but does exhibit a clear signal at periods likely to be harmonically related to it. Whilst our RXTE observations of RX J0153.3+7447, Swift J061223.0+701243.9, V436 Car, and DD Cir are largely too faint to give any definitive results, the observations of IGR J16167-4957 and V2487 Oph show some characteristics of intermediate polars, and these objects remain good candidates. Conclusions. We confirmed one new hard X-ray selected intermediate polar from our sample, V2069 Cyg.

show abstract

Section: Igr J00234+6141mentioning

confidence: 59%

RXTE andXMMobservations of intermediate polar candidates

Butters

Norton

Mukai

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…The soft-X-ray excess is mostly prominent in the X-ray spectra of polars; however, the growing number of IPs (e.g., PQ Gem, NY Lup, GK Per, V405 Aur, and V2400 Oph) also shows the soft X-ray component. In many systems, this soft-X-ray excess was explained by the black-body component with a temperature less than 100 eV (e.g., Mason et al 1992;Haberl et al 1994;de Martino et al 2004;Evans & Hellier 2007;Anzolin et al 2008Anzolin et al , 2009). However, in an IP IGR J17195−4100 the soft-X-ray excess was well fitted by a low-temperature apec component in X-ray spectra (Girish & Singh 2012).…”

Section: ×10mentioning

confidence: 99%

Paloma: A Magnetic Cv Between Polars and Intermediate Polars

Joshi

Pandey

Singh

et al. 2016

ApJ

View full text Add to dashboard Cite

We present analyses of archival X-ray data obtained from the XMM-Newton satellite and optical photometric data obtained from 1 m class telescopes of ARIES, Nainital of a magnetic cataclysmic variable (MCV) Paloma. Two persistent periods at 156 ± 1 minutes and 130 ± 1 minutes are present in the X-ray data, which we interpret as the orbital and spin periods, respectively. These periods are similar to those obtained from the previous as well as new optical photometric observations. The soft-X-ray excess seen in the X-ray spectrum of Paloma and the averaged X-ray spectra are well fitted by two-temperature plasma models with temperatures of 0.10 +0.02 −0.01 and 13.0 +0.5 −0.5 keV with an Fe Kα line and an absorbing column density of 4.6 × 10 22 cm -2 . This material partially covers 60 ± 2 % of the X-ray source. We also present the orbital and spin-phase-resolved spectroscopy of Paloma in the 0.3 − 10.0 keV energy band and find that the X-ray spectral parameters show orbital and spin-phase dependencies. New results obtained from optical and X-ray studies of Paloma indicate that it belongs to a class of a few magnetic CVs that seem to have the characteristics of both the polars and the intermediate polars.

show abstract

“…So far 64 CVs are identified in the latest catalogue releases (Bird et al 2010;Cusumano et al 2010), 43 of them are mCVs. The IPs represent ∼80% of this hard X-ray sample (including both already known, Barlow et al 2006) and recently discovered members (Bonnet-Bidaud et al 2007;de Martino et al 2008;Anzolin et al 2009;Butters et al 2008;Bonnet-Bidaud et al 2009;Pretorius 2009;Scaringi et al 2011), though one misidentification was found (de Martino et al 2010). Hence, while in the pre-INTEGRAL and Swift times IPs amounted to only ∼20 members, this number has more than doubled nowadays.…”

Section: Introductionmentioning

confidence: 98%

“…An intense soft (kT ∼ 20−50 eV) component is a characteristic signature of the X-ray spectra of the Polars, mostly balancing the cyclotron flux (Beuermann 2004). On the other hand IPs have typically stronger hard X-ray fluxes than the Polars and only recently a soft highly absorbed optically thick component has been detected (de Martino et al 2004;Evans & Hellier 2007;Anzolin et al 2008Anzolin et al , 2009.…”

Section: Introductionmentioning

confidence: 99%

Characterization of new hard X-ray cataclysmic variables

Bernardini

Martino

Falanga

et al. 2012

A&A

Self Cite

View full text Add to dashboard Cite

Aims. We aim at characterizing a sample of nine new hard X-ray selected cataclysmic variable (CVs), to unambiguously identify them as magnetic systems of the intermediate polar (IP) type. Methods. We performed detailed timing and spectral analysis by using X-ray, and simultaneous UV and optical data collected by XMM-Newton, complemented with hard X-ray data provided by INTEGRAL and Swift. The pulse arrival time were used to estimate the orbital periods. The broad band X-ray spectra were fitted using composite models consisting of different absorbing columns and emission components. Results. Strong X-ray pulses at the white dwarf (WD) spin period are detected and found to decrease with energy. Most sources are spin-dominated systems in the X-rays, though four are beat dominated at optical wavelengths. We estimated the orbital period in all system (except for IGR J16500-3307), providing the first estimate for IGR J08390-4833, IGR J18308-1232, and IGR J18173-2509. All X-ray spectra are multi-temperature. V2069 Cyg and RX J0636+3535 posses a soft X-ray optically thick component at kT ∼ 80 eV. An intense K α Fe line at 6.4 keV is detected in all sources. An absorption edge at 0.76 keV from OVII is detected in IGR J08390-4833. The WD masses and lower limits to the accretion rates are also estimated. Conclusions. We found all sources to be IPs. IGR J08390-4833, V2069 Cyg, and IGR J16500-3307 are pure disc accretors, while IGR J18308-1232, IGR J1509-6649, IGR J17195-4100, and RX J0636+3535 display a disc-overflow accretion mode. All sources show a temperature gradient in the post-shock regions and a highly absorbed emission from material located in the pre-shock flow which is also responsible for the X-ray pulsations. Reflection at the WD surface is likely the origin of the fluorescent iron line. There is an increasing evidence for the presence of a warm absorber in IPs, a feature that needs future exploration. The addition of two systems to the subgroup of soft X-ray IPs confirms a relatively large (∼30%) incidence.

show abstract

Broad-band properties of the hard X-ray cataclysmic variables IGR J00234+6141 and 1RXS J213344.1+510725

Cited by 31 publications

References 56 publications

RXTE andXMMobservations of intermediate polar candidates

RXTE andXMMobservations of intermediate polar candidates

Paloma: A Magnetic Cv Between Polars and Intermediate Polars

Characterization of new hard X-ray cataclysmic variables

Contact Info

Product

Resources

About