2023ApJ...957...23R

Query : 2023ApJ...957...23R

2023ApJ...957...23R - Astrophys. J., 957, 23 (2023/November-1)

The Polarized Cosmic Hand: IXPE Observations of PSR B1509-58/MSH 15-52.

ROMANI R.W., WONG J., DI LALLA N., OMODEI N., XIE F., NG C.-Y., FERRAZZOLI R., DI MARCO A., BUCCIANTINI N., PILIA M., SLANE P., WEISSKOPF M.C., JOHNSTON S., BURGAY M., WEI D., YANG Y.-J., ZHANG S., ANTONELLI L.A., BACHETTI M., BALDINI L., BAUMGARTNER W.H., BELLAZZINI R., BIANCHI S., BONGIORNO S.D., BONINO R., BREZ A., CAPITANIO F., CASTELLANO S., CAVAZZUTI E., CHEN C.-T., CIBRARIO N., CIPRINI S., COSTA E., 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., HEYL J., IWAKIRI W., LIODAKIS I., KAARET P., KARAS V., KIM D.E., KITAGUCHI T., KOLODZIEJCZAK J.J., KRAWCZYNSKI H., LA MONACA F., LATRONICO L., MADEJSKI G., MALDERA S., MANFREDA A., MARIN F., MARINUCCI A., MARSCHER A.P., MARSHALL H.L., MASSARO F., MATT G., MIDDEI R., MITSUISHI I., MIZUNO T., MULERI F., NEGRO M., O'DELL S.L., OPPEDISANO C., PACCIANI L., PAPITTO A., PAVLOV G.G., PERRI M., PESCE-ROLLINS M., PETRUCCI P.-O., POSSENTI A., POUTANEN J., PUCCETTI S., RAMSEY B.D., RANKIN J., RATHEESH A., ROBERTS O.J., SGRO C., 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., TUROLLA R., VINK J., WU K. and ZANE S.

Abstract (from CDS):

We describe IXPE polarization observations of the pulsar wind nebula (PWN) MSH 15-52, the “Cosmic Hand.” We find X-ray polarization across the PWN, with B-field vectors generally aligned with filamentary X-ray structures. High-significance polarization is seen in arcs surrounding the pulsar and toward the end of the “jet,” with polarization degree PD > 70%, thus approaching the maximum allowed synchrotron value. In contrast, the base of the jet has lower polarization, indicating a complex magnetic field at significant angle to the jet axis. We also detect significant polarization from PSR B1509-58 itself. Although only the central pulse phase bin of the pulse has high individual significance, flanking bins provide lower-significance detections and, in conjunction with the X-ray image and radio polarization, can be used to constrain rotating vector model solutions for the pulsar geometry.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Pulsar wind nebulae - Rotation powered pulsars - Polarimetry

Simbad objects: 11

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Number of rows : 11
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 RX J0232.8+2017 BLL 02 32 48.6148874688 +20 17 17.486717388     18.00 13.96   ~ 387 1
2 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
3 PSR B0540-69 Psr 05 40 11.2000490438 -69 19 54.198559829           ~ 976 3
4 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
5 MCG-05-23-016 Sy2 09 47 40.1332188528 -30 56 55.960779696   14.10 13.69 12.44   ~ 611 0
6 IC 4329A Sy1 13 49 19.2601801224 -30 18 34.213815504   13.81 13.66 12.18 12.35 ~ 876 1
7 3A 1510-590 Psr 15 13 17.000 -59 04 54.00           ~ 434 3
8 SNR G320.4-01.0 SNR 15 13 35 -59 00.2           ~ 87 0
9 PSR B1509-58 Psr 15 13 47.6 -59 07 54     13.06     ~ 879 1
10 PG 1553+113 BLL 15 55 43.0440048528 +11 11 24.365649948 14.91 14.72 14.57 13.99   ~ 672 1
11 NAME Galactic Ridge ? ~ ~           ~ 543 1

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