Standard
X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator? / Mushtukov, A A; Tsygankov, S S; Poutanen, J; Doroshenko, V; Salganik, A; Costa, E; Marco, A Di; Heyl, J; Monaca, F La; Lutovinov, A A; Mereminsky, I A; Papitto, A; Semena, A N; Shtykovsky, A E; Suleimanov, V F; Forsblom, S V; González-Caniulef, D; Malacaria, C; Sunyaev, R A; Agudo, I; Antonelli, L A; 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-T; Ciprini, S; De Rosa, A; Del Monte, E; Gesu, L Di; Lalla, N 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, J J; Krawczynski, H; Latronico, L; Liodakis, I; Maldera, S; Manfreda, A; Marin, F; Marscher, A P; Marshall, H L; Massaro, F; Matt, G; Mitsuishi, I; Mizuno, T; Muleri, F; Negro, M; Ng, C-Y; O’Dell, S L; Omodei, N; Oppedisano, C; 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; Tennant, A F; Thomas, N E; Tombesi, F; Trois, A; Turolla, R; Vink, J; Weisskopf, M C; Wu, K; Xie, F; Zane, S.
In:
Monthly Notices of the Royal Astronomical Society, Vol. 524, No. 2, 29.06.2023, p. 2004-2014.
Research output: Contribution to journal › Article › peer-review
Harvard
Mushtukov, AA, Tsygankov, SS, Poutanen, J, Doroshenko, V
, Salganik, A, Costa, E, Marco, AD, Heyl, J, Monaca, FL, Lutovinov, AA, Mereminsky, IA, Papitto, A, Semena, AN, Shtykovsky, AE, Suleimanov, VF, Forsblom, SV, González-Caniulef, D, Malacaria, C, Sunyaev, RA, Agudo, I, Antonelli, LA, Bachetti, M, Baldini, L, Baumgartner, WH, Bellazzini, R, Bianchi, S, Bongiorno, SD, Bonino, R, Brez, A, Bucciantini, N, Capitanio, F, Castellano, S, Cavazzuti, E, Chen, C-T, Ciprini, S, De Rosa, A, Del Monte, E, Gesu, LD, Lalla, ND, Donnarumma, I, Dovčiak, M, Ehlert, SR, Enoto, T, Evangelista, Y, Fabiani, S, Ferrazzoli, R, Garcia, JA, Gunji, S, Hayashida, K, Iwakiri, W, Jorstad, SG, Kaaret, P, Karas, V, Kislat, F, Kitaguchi, T, Kolodziejczak, JJ, Krawczynski, H, Latronico, L, Liodakis, I, Maldera, S, Manfreda, A, Marin, F, Marscher, AP, Marshall, HL, Massaro, F, Matt, G, Mitsuishi, I, Mizuno, T, Muleri, F, Negro, M, Ng, C-Y, O’Dell, SL, Omodei, N, Oppedisano, C, Pavlov, GG, Peirson, AL, Perri, M, Pesce-Rollins, M, Petrucci, P-O, Pilia, M, Possenti, A, Puccetti, S, Ramsey, BD, Rankin, J, Ratheesh, A, Roberts, OJ, Romani, RW, Sgrò, C, Slane, P, Soffitta, P, Spandre, G, Swartz, DA, Tamagawa, T, Tavecchio, F, Taverna, R, Tawara, Y, Tennant, AF, Thomas, NE, Tombesi, F, Trois, A, Turolla, R, Vink, J, Weisskopf, MC, Wu, K, Xie, F & Zane, S 2023, '
X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?',
Monthly Notices of the Royal Astronomical Society, vol. 524, no. 2, pp. 2004-2014.
https://doi.org/10.1093/mnras/stad1961APA
Mushtukov, A. A., Tsygankov, S. S., Poutanen, J., Doroshenko, V.
, Salganik, A., Costa, E., Marco, A. D., Heyl, J., Monaca, F. L., Lutovinov, A. A., Mereminsky, I. A., Papitto, A., Semena, A. N., Shtykovsky, A. E., Suleimanov, V. F., Forsblom, S. V., González-Caniulef, D., Malacaria, C., Sunyaev, R. A., ... Zane, S. (2023).
X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator? Monthly Notices of the Royal Astronomical Society,
524(2), 2004-2014.
https://doi.org/10.1093/mnras/stad1961Vancouver
Author
Mushtukov, A A ; Tsygankov, S S ; Poutanen, J ; Doroshenko, V
; Salganik, A ; Costa, E ; Marco, A Di ; Heyl, J ; Monaca, F La ; Lutovinov, A A ; Mereminsky, I A ; Papitto, A ; Semena, A N ; Shtykovsky, A E ; Suleimanov, V F ; Forsblom, S V ; González-Caniulef, D ; Malacaria, C ; Sunyaev, R A ; Agudo, I ; Antonelli, L A ; 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-T ; Ciprini, S ; De Rosa, A ; Del Monte, E ; Gesu, L Di ; Lalla, N 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, J J ; Krawczynski, H ; Latronico, L ; Liodakis, I ; Maldera, S ; Manfreda, A ; Marin, F ; Marscher, A P ; Marshall, H L ; Massaro, F ; Matt, G ; Mitsuishi, I ; Mizuno, T ; Muleri, F ; Negro, M ; Ng, C-Y ; O’Dell, S L ; Omodei, N ; Oppedisano, C ; 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 ; Tennant, A F ; Thomas, N E ; Tombesi, F ; Trois, A ; Turolla, R ; Vink, J ; Weisskopf, M C ; Wu, K ; Xie, F ; Zane, S. /
X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?. In:
Monthly Notices of the Royal Astronomical Society. 2023 ; Vol. 524, No. 2. pp. 2004-2014.
BibTeX
@article{4dcbdd4628984a6887165dbcce5a46cc,
title = "X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?",
abstract = "X Perseiis a persistent low-luminosity X-ray pulsar of period of ≈ 835 s in a Be binary system. The field strength at the neutron star surface is not known precisely, but indirect signs indicate a magnetic field above 1013 G, which makes the object one of the most magnetized known X-ray pulsars. Here we present the results of observations X Persei performed with the Imaging X-ray Polarimetry Explorer (IXPE). The X-ray polarization signal was found to be strongly dependent on the spin phase of the pulsar. The energy-averaged polarization degree in 3–8 keV band varied from several to ∼20 per cent over the pulse with a phase dependence resembling the pulse profile. The polarization angle shows significant variation and makes two complete revolutions during the pulse period resulting in nearly nil pulse-phase averaged polarization. Applying the rotating vector model to the IXPE data we obtain the estimates for the rotation axis inclination and its position angle on the sky as well as for the magnetic obliquity. The derived inclination is close to the orbital inclination reported earlier for X Persei. The polarimetric data imply a large angle between the rotation and magnetic dipole axes, which is similar to the result reported recently for the X-ray pulsar GRO J1008−57. After eliminating the effect of polarization angle rotation over the pulsar phase using the best-fitting rotating vector model, the strong dependence of the polarization degree with energy was discovered with its value increasing from 0 at ∼2 keV to 30 per cent at 8 keV.",
author = "Mushtukov, {A A} and Tsygankov, {S S} and J Poutanen and V Doroshenko and A Salganik and E Costa and Marco, {A Di} and J Heyl and Monaca, {F La} and Lutovinov, {A A} and Mereminsky, {I A} and A Papitto and Semena, {A N} and Shtykovsky, {A E} and Suleimanov, {V F} and Forsblom, {S V} and D Gonz{\'a}lez-Caniulef and C Malacaria and Sunyaev, {R A} and I Agudo and Antonelli, {L A} and M Bachetti and L Baldini and Baumgartner, {W H} and R Bellazzini and S Bianchi and Bongiorno, {S D} and R Bonino and A Brez and N Bucciantini and F Capitanio and S Castellano and E Cavazzuti and C-T Chen and S Ciprini and A De Rosa and {Del Monte}, E and Gesu, {L Di} and Lalla, {N Di} and I Donnarumma and M Dov{\v c}iak and Ehlert, {S R} and T Enoto and Y Evangelista and S Fabiani and R Ferrazzoli and Garcia, {J A} and S Gunji and K Hayashida and W Iwakiri and Jorstad, {S G} and P Kaaret and V Karas and F Kislat and T Kitaguchi and Kolodziejczak, {J J} and H Krawczynski and L Latronico and I Liodakis and S Maldera and A Manfreda and F Marin and Marscher, {A P} and Marshall, {H L} and F Massaro and G Matt and I Mitsuishi and T Mizuno and F Muleri and M Negro and C-Y Ng and O{\textquoteright}Dell, {S L} and N Omodei and C Oppedisano and Pavlov, {G G} and Peirson, {A L} and M Perri and M Pesce-Rollins and P-O Petrucci and M Pilia and A Possenti and S Puccetti and Ramsey, {B D} and J Rankin and A Ratheesh and Roberts, {O J} and Romani, {R W} and C Sgr{\`o} and P Slane and P Soffitta and G Spandre and Swartz, {D A} and T Tamagawa and F Tavecchio and R Taverna and Y Tawara and Tennant, {A F} and Thomas, {N E} and F Tombesi and A Trois and R Turolla and J Vink and Weisskopf, {M C} and K Wu and F Xie and S Zane",
year = "2023",
month = jun,
day = "29",
doi = "10.1093/mnras/stad1961",
language = "English",
volume = "524",
pages = "2004--2014",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Wiley-Blackwell",
number = "2",
}
RIS
TY - JOUR
T1 - X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?
AU - Mushtukov, A A
AU - Tsygankov, S S
AU - Poutanen, J
AU - Doroshenko, V
AU - Salganik, A
AU - Costa, E
AU - Marco, A Di
AU - Heyl, J
AU - Monaca, F La
AU - Lutovinov, A A
AU - Mereminsky, I A
AU - Papitto, A
AU - Semena, A N
AU - Shtykovsky, A E
AU - Suleimanov, V F
AU - Forsblom, S V
AU - González-Caniulef, D
AU - Malacaria, C
AU - Sunyaev, R A
AU - Agudo, I
AU - Antonelli, L A
AU - Bachetti, M
AU - Baldini, L
AU - Baumgartner, W H
AU - Bellazzini, R
AU - Bianchi, S
AU - Bongiorno, S D
AU - Bonino, R
AU - Brez, A
AU - Bucciantini, N
AU - Capitanio, F
AU - Castellano, S
AU - Cavazzuti, E
AU - Chen, C-T
AU - Ciprini, S
AU - De Rosa, A
AU - Del Monte, E
AU - Gesu, L Di
AU - Lalla, N Di
AU - Donnarumma, I
AU - Dovčiak, M
AU - Ehlert, S R
AU - Enoto, T
AU - Evangelista, Y
AU - Fabiani, S
AU - Ferrazzoli, R
AU - Garcia, J A
AU - Gunji, S
AU - Hayashida, K
AU - Iwakiri, W
AU - Jorstad, S G
AU - Kaaret, P
AU - Karas, V
AU - Kislat, F
AU - Kitaguchi, T
AU - Kolodziejczak, J J
AU - Krawczynski, H
AU - Latronico, L
AU - Liodakis, I
AU - Maldera, S
AU - Manfreda, A
AU - Marin, F
AU - Marscher, A P
AU - Marshall, H L
AU - Massaro, F
AU - Matt, G
AU - Mitsuishi, I
AU - Mizuno, T
AU - Muleri, F
AU - Negro, M
AU - Ng, C-Y
AU - O’Dell, S L
AU - Omodei, N
AU - Oppedisano, C
AU - Pavlov, G G
AU - Peirson, A L
AU - Perri, M
AU - Pesce-Rollins, M
AU - Petrucci, P-O
AU - Pilia, M
AU - Possenti, A
AU - Puccetti, S
AU - Ramsey, B D
AU - Rankin, J
AU - Ratheesh, A
AU - Roberts, O J
AU - Romani, R W
AU - Sgrò, C
AU - Slane, P
AU - Soffitta, P
AU - Spandre, G
AU - Swartz, D A
AU - Tamagawa, T
AU - Tavecchio, F
AU - Taverna, R
AU - Tawara, Y
AU - Tennant, A F
AU - Thomas, N E
AU - Tombesi, F
AU - Trois, A
AU - Turolla, R
AU - Vink, J
AU - Weisskopf, M C
AU - Wu, K
AU - Xie, F
AU - Zane, S
PY - 2023/6/29
Y1 - 2023/6/29
N2 - X Perseiis a persistent low-luminosity X-ray pulsar of period of ≈ 835 s in a Be binary system. The field strength at the neutron star surface is not known precisely, but indirect signs indicate a magnetic field above 1013 G, which makes the object one of the most magnetized known X-ray pulsars. Here we present the results of observations X Persei performed with the Imaging X-ray Polarimetry Explorer (IXPE). The X-ray polarization signal was found to be strongly dependent on the spin phase of the pulsar. The energy-averaged polarization degree in 3–8 keV band varied from several to ∼20 per cent over the pulse with a phase dependence resembling the pulse profile. The polarization angle shows significant variation and makes two complete revolutions during the pulse period resulting in nearly nil pulse-phase averaged polarization. Applying the rotating vector model to the IXPE data we obtain the estimates for the rotation axis inclination and its position angle on the sky as well as for the magnetic obliquity. The derived inclination is close to the orbital inclination reported earlier for X Persei. The polarimetric data imply a large angle between the rotation and magnetic dipole axes, which is similar to the result reported recently for the X-ray pulsar GRO J1008−57. After eliminating the effect of polarization angle rotation over the pulsar phase using the best-fitting rotating vector model, the strong dependence of the polarization degree with energy was discovered with its value increasing from 0 at ∼2 keV to 30 per cent at 8 keV.
AB - X Perseiis a persistent low-luminosity X-ray pulsar of period of ≈ 835 s in a Be binary system. The field strength at the neutron star surface is not known precisely, but indirect signs indicate a magnetic field above 1013 G, which makes the object one of the most magnetized known X-ray pulsars. Here we present the results of observations X Persei performed with the Imaging X-ray Polarimetry Explorer (IXPE). The X-ray polarization signal was found to be strongly dependent on the spin phase of the pulsar. The energy-averaged polarization degree in 3–8 keV band varied from several to ∼20 per cent over the pulse with a phase dependence resembling the pulse profile. The polarization angle shows significant variation and makes two complete revolutions during the pulse period resulting in nearly nil pulse-phase averaged polarization. Applying the rotating vector model to the IXPE data we obtain the estimates for the rotation axis inclination and its position angle on the sky as well as for the magnetic obliquity. The derived inclination is close to the orbital inclination reported earlier for X Persei. The polarimetric data imply a large angle between the rotation and magnetic dipole axes, which is similar to the result reported recently for the X-ray pulsar GRO J1008−57. After eliminating the effect of polarization angle rotation over the pulsar phase using the best-fitting rotating vector model, the strong dependence of the polarization degree with energy was discovered with its value increasing from 0 at ∼2 keV to 30 per cent at 8 keV.
UR - https://www.mendeley.com/catalogue/84014772-9770-3520-ab9f-726f287f7cf6/
U2 - 10.1093/mnras/stad1961
DO - 10.1093/mnras/stad1961
M3 - Article
VL - 524
SP - 2004
EP - 2014
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -
