Complex variations in X-ray polarization in the X-ray pulsar LS V +44 17/RX J0440.9+4431

Doroshenko, V.; Poutanen, J.; Heyl, J.; S., Tsygankov, Sergey; Berdyugin, A.; Caiazzo, I.; Forsblom, S. V.; D., Gonz\ález-Caniulef,; Kravtsov, V.; Loktev, Vladislav; Lutovinov, A.; C., Malacaria,; Mereminskiy, I. A.; Molkov, S.; Mushtukov, A.; Nitindala, Anagha P.; Salganik, A.; Santangelo, A.; Suleimanov, V.; Turolla, R.; Veledina, A.; T.,; Agudo, I.; Antonelli, Lucia; Bachetti, M.; Baldini, L.; Baumgartner, W. H.; Bellazzini, R.; Bianchi, S.; Bongiorno, S. D.; Bonino, R.; Brez, A.; Bucciantini, N.; Capitanio, F.; Castellano, S.; Cavazzuti, E.; Chen, C.; Ciprini, S.; Costa, E.; Rosa, A. De; Monte, E. Del; Gesu, L. Di; Lalla, N. Di; Marco, A. Di; Donnarumma, I.; Dovčiak, M.; Ehlert, S. R.; Enoto, T.; Evangelista, Y.; Fabiani, S.; Ferrazzoli, R.; Garcia, J. A.; Gunji, S.; Hayashida, K.; Iwakiri, W.; Jorstad, S. G.; Kaaret, P.; Karas, V.; Kislat, F.; Kitaguchi, T.; Kolodziejczak, Jeffery J.; Krawczynski, H.; Monaca, F. La; Latronico, L.; Liodakis, I.; Maldera, S.; Manfreda, A.; Marin, F.; Marinucci, Andrea; Marscher, A. P.; Marshall, H. L.; Massaro, F.; Matt, G.; Mitsuishi, I.; Mizuno, T.; Muleri, F.; Negro, M.; Ng, Cherry; O'Dell, S. L.; Omodei, N.; Oppedisano, C.; Papitto, A.; Pavlov, G. G.; Peirson, A. L.; Perri, M.; Pesce-Rollins, M.; Petrucci, P.-O.; Pilia, M.; Possenti, A.; Puccetti, S.; Ramsey, B. D.; Rankin, J.; Ratheesh, A.; Roberts, O. J.; Romani, R. W.; Sgrò, C.; Slane, P.; Soffitta, P.; Spandre, G.; Swartz, D. A.; Tamagawa, T.; Tavecchio, F.; Taverna, R.; Tawara, Y.; F., Tent, A.; Thomas, N. E.; Tombesi, F.; Trois, A.; Vink, J.; Weisskopf, M. C.; Wu, K.; Xie, F.; Zane, S.

doi:10.1051/0004-6361/202347088

Cited by 7 publications

(2 citation statements)

References 36 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Such a "radio + high-frequency" strategic development could be extended to the PPA measurements in the near future, with the launch of dedicated X-ray polarimetry programs such as the missions of Imaging X-ray Polarimetry Explorer (Weisskopf et al 2022) and Enhanced X-ray Timing and Polarimetry (Zhang et al 2019). For these telescopes, precision  1 ( ) ~ can be achieved for measuring polarization angle of bright sources such as bright pulsars (Doroshenko et al 2023) and accretion flows around black holes (De Rosa et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Stochastic Wave Dark Matter with Fermi-LAT γ-Ray Pulsar Timing Array

Luu,

Liu,

Ren

et al. 2024

ApJL

View full text Add to dashboard Cite

Pulsar timing arrays (PTAs) can detect disturbances in the fabric of spacetime on a galactic scale by monitoring the arrival time of pulses from millisecond pulsars (MSPs). Recent advancements have enabled the use of γ-ray radiation emitted by MSPs, in addition to radio waves, for PTA experiments. Wave dark matter (DM), a prominent class of DM candidates, can be detected with PTAs due to its periodic perturbations of the spacetime metric. In response to this development, we perform in this Letter a first analysis of applying the γ-ray PTA to detect the ultralight axion-like wave DM, with the data of Fermi Large Area Telescope (Fermi-LAT). Despite its much smaller collecting area, the Fermi-LAT γ-ray PTA demonstrates a promising sensitivity potential. We show that the upper limits not far from those of the dedicated radio-PTA projects can be achieved. Moreover, we initiate a cross-correlation analysis using the data of two Fermi-LAT pulsars. The cross-correlation of phases, while carrying key information on the source of the spacetime perturbations, has been ignored in the existing data analyses for the wave DM detection with PTAs. Our analysis indicates that taking this information into account can improve the sensitivity to wave DM by ≳50% at masses below 10−23 eV.

show abstract

Section: Introductionmentioning

confidence: 99%

Stochastic Wave Dark Matter with Fermi-LAT γ-Ray Pulsar Timing Array

Luu,

Liu,

Ren

et al. 2024

ApJL

View full text Add to dashboard Cite

show abstract

“…The geometrical parameters of NS rotation in the observer's reference frame (i.e., inclination of rotating NS and magnetic obliquity, i.e., the angle between the spin axis and magnetic axis) are purely known. However, there is some progress in determination XRP geometry on the base of data obtained with X-ray polarimeters (see, e.g., Doroshenko et al 2022Doroshenko et al , 2023Tsygankov et al 2022Tsygankov et al , 2023Mushtukov et al 2023;Suleimanov et al 2023;Malacaria et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Apparent luminosity and pulsed fraction affected by gravitational lensing of accretion columns in bright X-ray pulsars

Markozov,

Mushtukov

2023

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The luminosity of X-ray pulsars is their key parameter determining the geometry and physical conditions of the accretion flow both on the spatial scales of a binary system and on much smaller scales of emitting regions located close to the stellar surface. Traditionally, the luminosity of X-ray pulsars is estimated out of the X-ray energy flux averaged over the pulsed period and the estimated distance to the source. Due to the anisotropy of X-ray emission, the luminosity estimated on the base of the observed pulse profile can differ from the actual one. Super-critical X-ray pulsars with accretion columns are of particular interest because the X-ray flux from columns is a matter of strong gravitational lensing by a neutron star. Using toy model of an accretion column, we simulate beam patterns in super-critical X-ray pulsars, construct theoretical pulse profiles for different geometries and mutual orientations of pulsars and distant observers and show that despite strong light bending, the typical deviation of the apparent luminosity from the actual one is $\sim 20~{{\%}}$ only, and in $\sim 90~{{\%}}$ of cases, the apparent luminosity 0.8L ≲ Lapp ≲ 1.25L. However, the shape of the pulse profiles is strongly affected by the geometry of the emitting region. We show that the appearance and growth of accretion columns tend to be accompanied by an increase of observed pulsed fraction, which is in agreement with the recent observations of bright X-ray transients.

show abstract

X-ray polarimetry of the accreting pulsar GX 301−2

Suleimanov,

Forsblom,

Tsygankov

et al. 2023

A&A

View full text Add to dashboard Cite

The phase- and energy-resolved polarization measurements of accreting X-ray pulsars (XRPs) allow us to test different theoretical models of their emission, and they also provide an avenue to determine the emission region geometry. We present the results of the observations of the XRP GX 301−2 performed with the Imaging X-ray Polarimetry Explorer (IXPE). A persistent XRP, GX 301−2 has one of the longest spin periods known: ∼680 s. A massive hyper-giant companion star Wray 977 supplies mass to the neutron star via powerful stellar winds. We did not detect significant polarization in the phase-averaged data when using spectro-polarimetric analysis, with the upper limit on the polarization degree (PD) of 2.3% (99% confidence level). Using the phase-resolved spectro-polarimetric analysis, we obtained a significant detection of polarization (above 99% confidence level) in two out of nine phase bins and a marginal detection in three bins, with a PD ranging between ∼3% and ∼10% and a polarization angle varying in a very wide range from ∼0° to ∼160°. Using the rotating vector model, we obtained constraints on the pulsar geometry using both phase-binned and unbinned analyses, finding excellent agreement. Finally, we discuss possible reasons for a low observed polarization in GX 301−2.

show abstract

Complex variations in X-ray polarization in the X-ray pulsar LS V +44 17/RX J0440.9+4431

Cited by 7 publications

References 36 publications

Stochastic Wave Dark Matter with Fermi-LAT γ-Ray Pulsar Timing Array

Stochastic Wave Dark Matter with Fermi-LAT γ-Ray Pulsar Timing Array

Apparent luminosity and pulsed fraction affected by gravitational lensing of accretion columns in bright X-ray pulsars

X-ray polarimetry of the accreting pulsar GX 301−2

Contact Info

Product

Resources

About