2024ApJ...963..133S

Query : 2024ApJ...963..133S

2024ApJ...963..133S - Astrophys. J., 963, 133 (2024/March-2)

X-Ray Polarimetry of the Dipping Accreting Neutron Star 4U 1624-49.

SAADE M.L., KAARET P., GNARINI A., POUTANEN J., URSINI F., BIANCHI S., BOBRIKOVA A., LA MONACA F., DI MARCO A., CAPITANIO F., VELEDINA A., AGUDO I., ANTONELLI L.A., BACHETTI M., BALDINI L., BAUMGARTNER W.H., BELLAZZINI R., BONGIORNO S.D., BONINO R., BREZ A., BUCCIANTINI N., CASTELLANO S., CAVAZZUTI E., CHEN C.-T., CIPRINI S., COSTA E., DE ROSA A., DEL MONTE E., DI GESU L., DI LALLA N., DONNARUMMA I., DOROSHENKO V., DOVCIAK M., EHLERT S.R., ENOTO T., EVANGELISTA Y., FABIANI S., FERRAZZOLI R., GARCIA J.A., GUNJI S., HAYASHIDA K., HEYL J., IWAKIRI W., JORSTAD S.G., KARAS V., KISLAT F., KITAGUCHI T., KOLODZIEJCZAK J.J., KRAWCZYNSKI H., LATRONICO L., LIODAKIS I., MALDERA S., MANFREDA A., MARIN F., MARINUCCI A., 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., 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., SGRO 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., TSYGANKOV S.S., TUROLLA R., VINK J., WEISSKOPF M.C., WU K., XIE F. and ZANE S.

Abstract (from CDS):

We present the first X-ray polarimetric study of the dipping accreting neutron star 4U 1624-49 with the Imaging X-ray Polarimetry Explorer. We report a detection of polarization in the nondip time intervals with a confidence level of 99.99%. We find an average polarization degree (PD) of 3.1% ± 0.7% and a polarization angle of 81° ± 6° east of north in the 2-8 keV band. We report an upper limit on the PD of 22% during the X-ray dips with 95% confidence. The PD increases with energy, reaching from 3.0% ± 0.9% in the 4-6 keV band to 6% ± 2% in the 6-8 keV band. This indicates the polarization likely arises from Comptonization. The high PD observed is unlikely to be produced by Comptonization in the boundary layer or spreading layer alone. It can be produced by the addition of an extended geometrically thin slab corona covering part of the accretion disk, as assumed in previous models of dippers, and/or a reflection component from the accretion disk.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): X-ray binary stars - Neutron stars - X-ray astronomy - Polarimetry

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 4U 1323-62 LXB 13 26 37.0 -62 08 09           ~ 192 0
2 V* BR Cir HXB 15 20 40.8532547060 -57 10 00.206639033   21.4 21.4     B5-A0I 849 1
3 V* V818 Sco LXB 16 19 55.0692669024 -15 38 25.017666540 11.60 12.40 11.1     Oev 1730 0
4 4U 1624-49 LXB 16 28 02.825 -49 11 54.61           ~ 250 0
5 X Nor X-1 LXB 16 34 01.610 -47 23 34.80           ~ 579 0
6 [KRL2007b] 214 LXB 17 00 58.46 -46 11 08.6           ~ 296 0
7 V* V2216 Oph LXB 17 31 44.17 -16 57 40.9 16.40 17.10 16.8     ~ 329 1
8 X Sgr X-1 LXB 17 47 56.3 -26 33 47           ~ 402 0
9 4U 1758-25 LXB 18 01 09.7308060816 -25 04 44.120221284     11.08     ~ 705 1
10 X Sgr X-4 LXB 18 23 40.57 -30 21 40.6   19.06 18.81     ~ 1056 1
11 V* V4634 Sgr LXB 18 29 28.8 -23 47 48 18.90 19.40 19     ~ 399 0
12 V* V1341 Cyg LXB 21 44 41.1544345272 +38 19 17.066570988 15.00 15.13 14.68 15.00   A9III 1229 1

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