2023ApJ...945...52F

Query : 2023ApJ...945...52F

2023ApJ...945...52F - Astrophys. J., 945, 52 (2023/March-1)

X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho's Supernova Remnant.

FERRAZZOLI R., SLANE P., PROKHOROV D., ZHOU P., VINK J., BUCCIANTINI N., COSTA E., DI LALLA N., DI MARCO A., SOFFITTA P., WEISSKOPF M.C., ASAKURA K., BALDINI L., HEYL J., KAARET P.E., MARIN F., MIZUNO T., NG C.-Y., PESCE-ROLLINS M., SILVESTRI S., SGRO C., SWARTZ D.A., TAMAGAWA T., YANG Y.-J., AGUDO I., ANTONELLI L.A., BACHETTI M., BAUMGARTNER W.H., BELLAZZINI R., BIANCHI S., BONGIORNO S.D., BONINO R., BREZ A., CAPITANIO F., CASTELLANO S., CAVAZZUTI E., CHEN C.-T., CIPRINI S., DE ROSA A., DEL MONTE E., DI GESU L., DONNARUMMA I., DOROSHENKO V., DOVCIAK M., EHLERT S.R., ENOTO T., EVANGELISTA Y., FABIANI S., GARCIA J.A., GUNJI S., HAYASHIDA K., IWAKIRI W., JORSTAD S.G., KISLAT F., KARAS V., KITAGUCHI T., KOLODZIEJCZAK J.J., KRAWCZYNSKI H., LA MONACA F., LATRONICO L., LIODAKIS I., MALDERA S., MANFREDA A., MARINUCCI A., MARSCHER A.P., MARSHALL H.L., MATT G., MITSUISHI I., MULERI F., NEGRO M., O'DELL S.L., OMODEI N., OPPEDISANO C., PAPITTO A., PAVLOV G.G., PEIRSON A.L., PERRI M., PETRUCCI P.-O., PILIA M., POSSENTI A., POUTANEN J., PUCCETTI S., RAMSEY B.D., RANKIN J., RATHEESH A., ROBERTS O., ROMANI R.W., SPANDRE G., TAVECCHIO F., TAVERNA R., TAWARA Y., TENNANT A.F., THOMAS N.E., TOMBESI F., TROIS A., TSYGANKOV S.S., TUROLLA R., WU K., XIE F. and ZANE S.

Abstract (from CDS):

Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho's supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% ± 2% averaged over the whole remnant, and 12% ± 2% at the rim, higher than the value of polarization of 7%-8% observed in the radio band. In the west region, the degree of polarization is 23% ± 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 ± 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities.

Journal keyword(s): Supernova remnants - Polarimetry - X-ray astronomy

Simbad objects: 7

Full paper

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Number of rows : 7

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	SN 1572A	SN*	00 25 21.5	+64 08 27						B8	1254	1
2	Z 184-50	BLL	11 04 27.3140835504	+38 12 31.798495872		13.50	12.90	8.31		~	2841	1
3	3C 279	Bla	12 56 11.16657958	-05 47 21.5251510		18.01	17.75	15.87		~	3205	2
4	NAME Circinus Galaxy	Sy2	14 13 09.906	-65 20 20.47		10.89	9.84	10.6	10.0	~	1331	1
5	Z 225-7	BLL	16 53 52.21668403	+39 45 36.6088754	14.09	14.15	13.29	8.26		~	2304	2
6	NAME BL Lac	BLL	22 02 43.2913536816	+42 16 39.979416792		15.66	14.72			~	2397	1
7	NAME Cas A	SNR	23 23 26.0	+58 48 41			14.30			~	3033	1

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