2025ApJ...986..230M

Query : 2025ApJ...986..230M

2025ApJ...986..230M - Astrophys. J., 986, 230 (2025/June-3)

A Two-week IXPE Monitoring Campaign on Mrk 421.

MAKSYM W.P., LIODAKIS I., SAADE M.L., KIM D.E., MIDDEI R., DI GESU L., KIEHLMANN S., MATZEU G., AGUDO I., MARSCHER A.P., EHLERT S.R., JORSTAD S.G., KAARET P., MARSHALL H.L., PACCIANI L., PERRI M., PUCCETTI S., KOUCH P.M., LINDFORS E., ACEITUNO F.J., BONNOLI G., CASANOVA V., ESCUDERO J., GOMEZ J.L., AGIS-GONZALEZ B., HUSILLOS C., MORCUENDE D., OTERO-SANTOS J., SOTA A., PIIROLA V., IMAZAWA R., SASADA M., FUKAZAWA Y., KAWABATA K.S., UEMURA M., MIZUNO T., NAKAOKA T., AKITAYA H., McCALL C., JERMAK H.E., STEELE I.A., BORMAN G.A., GRISHINA T.S., HAGEN-THORN V.A., KOPATSKAYA E.N., LARIONOVA E.G., MOROZOVA D.A., SAVCHENKO S.S., SHISHKINA E.V., TROITSKIY I.S., TROITSKAYA Y.V., VASILYEV A.A., ZHOVTAN A.V., MYSERLIS I., GURWELL M., KEATING G., RAO R., PAULEY C., ANGELAKIS E., KRAUS A., BERDYUGIN A.V., KAGITANI M., KRAVTSOV V., POUTANEN J., SAKANOI T., KANG S., LEE S.-S., KIM S.-H., CHEONG W.Y., JEONG H.-W., SONG C., BLINOV D., SHABLOVINSKAYA E., 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., COSTA E., DE ROSA A., DEL MONTE E., DI LALLA N., DI MARCO A., DONNARUMMA I., DOROSHENKO V., DOVCIAK M., ENOTO T., EVANGELISTA Y., FABIANI S., FERRAZZOLI R., GARCIA J.A., GUNJI S., HAYASHIDA K., HEYL J., IWAKIRI W., KARAS V., KISLAT F., KITAGUCHI T., KOLODZIEJCZAK J.J., KRAWCZYNSKI H., LA MONACA F., LATRONICO L., MALDERA S., MANFREDA A., MARIN F., MARINUCCI A., MASSARO F., MATT G., MITSUISHI I., MULERI F., NEGRO M., NG C.-Y., O'DELL S.L., OMODEI N., OPPEDISANO C., PAPITTO A., PAVLOV G.G., PEIRSON A.L., PESCE-ROLLINS M., PETRUCCI P.-O., PILIA M., POSSENTI A., 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):

X-ray polarization is a unique new probe of the particle acceleration in astrophysical jets made possible through the Imaging X-ray Polarimetry Explorer. Here we report on the first dense X-ray polarization monitoring campaign on the blazar Mrk 421. Our observations were accompanied by an even denser radio and optical polarization campaign. We find significant short-timescale variability in both X-ray polarization degree and angle, including an ∼90° angle rotation about the jet axis. We attribute this to random variations of the magnetic field, consistent with the presence of turbulence but also unlikely to be explained by turbulence alone. At the same time, the degree of lower-energy polarization is significantly lower and shows no more than mild variability. Our campaign provides further evidence for a scenario in which energy-stratified shock-acceleration of relativistic electrons, combined with a turbulent magnetic field, is responsible for optical to X-ray synchrotron emission in blazar jets.

Abstract Copyright: © 2025. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Blazars - Jets - X-ray astronomy - Shocks - Markarian galaxies - Time domain astronomy - Polarimetry - Radio jets

Simbad objects: 6

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Number of rows : 6
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 Z 184-50 BLL 11 04 27.3140835504 +38 12 31.798495872   13.50 12.90 8.31   ~ 2841 1
3 PG 1553+113 BLL 15 55 43.0440048528 +11 11 24.365649948 14.91 14.72 14.57 13.99   ~ 672 1
4 Z 225-7 BLL 16 53 52.21668403 +39 45 36.6088754 14.09 14.15 13.29 8.26   ~ 2304 2
5 QSO B1959+650 BLL 19 59 59.8520303688 +65 08 54.652536492     12.8 11.21   ~ 699 2
6 PKS J2158-3013 BLL 21 58 52.0652249880 -30 13 32.118447792   13.36 13.09 12.62   ~ 1829 1

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