PoS(ICRC2019)237 http://pos.sissa.it/ ∗ [email protected] [email protected] [email protected] [email protected] [email protected] Speaker. The importance of cosmic rays and magneticthe evolution fields of for the is demonstrated physics by of a the numbernew interstellar of observations recent medium of numerical and simulations. the We cosmic present raystructure electron in galactic transport halos as from well radio-continuum polarization astained studies the by of the magnetic edge-on CHANG-ES field disk (Continuum galaxies Halos strength in ob- and Nearbyobservations Galaxies are - an discussed EVLA in Survey) project. the The contextfrom the of star-forming transport disks models into for the halo. Cosmicstructure The Ray in observations Eelctrons galactic also halos. (CREs) allow to In derive addition, theof it magentic edge-on is field galaxies demonstrated with how LOFAR recent help low to frequency further observations constrain the problem. ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 36th International Cosmic Ray Conference -ICRC2019- July 24th - August 1st, 2019 Madison, WI, U.S.A. and the CHANG-ES Team Judith Irwin (PI), Dept. of Physics,Kingston, Engeneering Ontario, Physics, Canada, & K7L Astronomy, 3N6 Queen’s University, E-mail: Yelena Stein Centre de Données astronomiques de Strasbourg,l’Université, Observatoire 67000 de Strasbourg, Strasbourg France 11, rue de E-mail: Volker Heesen Universität Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, 21029E-mail: Hamburg, Germany Arpad Miskolczi Ruhr-Universität Bochum, Fakultät für Physik und(AIRUB), Astronomie, Universitätsstrasse Astronomisches 150, Institut 44801 Bochum, Germany E-mail: Ralf-Jürgen Dettmar Ruhr-Universität Bochum, Fakultät für Physik und(AIRUB), Astronomie, Universitätsstrasse Astronomisches 150, Institut 44801 Bochum, Germany E-mail: New constraints on galactic CRE transportradio from continuum observations PoS(ICRC2019)237 ], ]). 4 7 ]). The 8 Ralf-Jürgen Dettmar ]). For the mass range of typical disk 3 ]. As a results of this larger sample it 11 ], [ 2 ] follow the description for CR transport given 9 . Since dust emission in the ISM is a very good 1 WISE and Spitzer ]) in order to explain the observed dependence of the long-term global ] it is now possible to observe the emission from CREs at lower energies which are less 1 6 ]. It is demonstrated that advective and diffusive transport of cosmic ray electrons into the In a case study of the southern edge-on spiral galaxies NGC 7090 and NGC 7462 based on The polarized and frequency dependent radio-synchrotron radiation of CREs allows us to con- Various feedback mechanisms have been discussed in the context of formation scenar- 10 ]). In the following, observations of the synchrotron radiation of cosmic ray electrons (CREs) 5 Australia Telescope Compact Array (ATCA) data, [ clean synchrotron emission at variousemission frequencies by is then CREs to with be regardsuch used to as for diffusion magnetic studying or field advection. the strengths synchrotron and cosmic ray propagation processes halo can be distinguished by fittingprofiles a perpendicular 1-D to cosmic the ray galaxy transportin model disc. a to characteristic the The shape intensity transport of andmately modes the spectral exponential intensity of intensity profiles and advection and spectral and linearpredicts index diffusion spectral approximately profiles. result index Gaussian profiles Advection intensity while, predicts in profiles1 approxi- contrast, and below). diffusion parabolic This spectral was indexthe used profiles Westerbork for (see Synthesis the Fig. Radio analysis Telescope ofwas (WSRT) archival concluded in data that [ from the radio the halostransport Very Large of models. most Array For galaxies (VLA) these studied and galaxies so the far are bulk best velocity described of by the advective cosmic ray electrons correlates with by [ affected by energy losses. They representof an origin old in population the that star-forming has regions of traveled furthest the from mid-plane. the site 2. Cosmic ray electron transport into galactic halos strain the magnetic field strength andchrotron structure intensity in also galaxies. provides The information frequency dependence on of the the transport syn- processes for the CREs (e.g., [ galaxies several processes relatedexplosions, to stellar star winds, formation and are radiationimportance under pressure, of consideration: a magnetic number fields besides of andnamics supernova cosmic recent of ray papers the interstellar pressure discuss medium as the[ (ISM) an possible as additional well factor as for for the the global launching dy- of galactic winds (e.g., [ This, however, requires that thetribution observed emission of is the corrected thermal forConsiderable the radio-continuum progress frequency which has dependent is been con- madesatellite also in observations strongly this such correlated regard as with due to star-formation. the availability of infrared data from propagating in the magnetic fieldsmentation of at all galactic large halos radio are facilitiesand allows presented. thus for these a The new broader data recent wavelength provide coverage progress newinto at in constraints higher halos. for instru- sensitivity the long The standing significant problemLOFAR progress of [ CRE at propagation the lowest frequencies contributes to the discussion: with proxy for the star formation rate it can be used to correct for the thermal emission (e.g., [ ios (e.g., [ CRE transport from radio continuum observations 1. Introduction efficiency in dark matter halos of different mass (e.g., [ 3 . 19 0 = usion, ↵

PoS(ICRC2019)237 µ shows a sim- is east of the values are on 0 B2 z h 3 3 3 3 3 3 3 < 4 4 4 4 4 r 7.94 kpc 2.65 kpc 5.29 kpc 7.94 kpc 5.29 kpc 2.65 kpc 3 3 3 3 3 + − + + − − r = 0 kpc 2 2 2 2 2 2 2 , with a tendency towards 1 r = r = r = r = r = r = = 28 kpc = 29 kpc = 19 kpc = 19 kpc = 34 kpc = 34 kpc = 8 kpc = 24 kpc = 27 kpc = 12 kpc = 6.6 kpc = 5.2 kpc = 4.9 kpc = 4.6 kpc = 5.2 kpc = 4.6 kpc = 6.8 kpc = 5.4 kpc = 6.6 kpc = 4.7 kpc = 9.9 kpc = 9.0 kpc 2 2 2 2 2 V V V V V V V V V V V V = 20.0 kpc 20.0 = kpc 9.6 = B2 B2 B2 B2 B2 B2 B2 B2 B2 B2 h h h h h h h h h h V V h h h h h h h h h h h h h h 1 1 1 1 1 1 1 km s 1 1 1 1 1 Ralf-Jürgen Dettmar 150 cient). Data points denote the vertical ⇡ 0 0 0 0 0 0 0 0 0 0 0 0 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 is west of the minor axis. Positive usion coe 0 ↵ -2 -2 -2 -2 -2 usion produces approximately Gaussian intensity Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Disc Galactic to Distance Disc (z) [kpc] Distance to Galactic > ]. First results for the complete ↵ r 13 -2 -2 -2 -2 -2 -2 -2 -3 -3 -3 -3 -3 . Di 13.85 kpc 6.92 kpc 6.92 kpc 13.85 kpc + − + − 0 r = r = r = 0 kpc r = r = = -4 -4 -4 -4 -4 µ -3 -3 -3 -3 -3 -3 -3 For NGC 891, advection is clearly favoured over di usion, the halo magnetic field scale height 0 0 0 0 0 0 0 0 0 0 0 0 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2 -1 -2

↵ 10 10 10 10 10 10 10

10 10 10 10 10

10 10 10 10 10 10 10 10 10 10 10 10 10 10

10 10 10 10 10 10 10 10 10 10

nt nt nt nt nt nt nt

nt nt nt nt nt Normalized Intensity (I Intensity Normalized Normalized Intensity (I Intensity Normalized (I Intensity Normalized ) (I Intensity Normalized ) ) (I Intensity Normalized ) (I Intensity Normalized ) (I Intensity Normalized ) ) Normalized Intensity (I Intensity Normalized Normalized Intensity (I Intensity Normalized ) (I Intensity Normalized ) (I Intensity Normalized ) ) ) Normalized Intensity (I Intensity Normalized for comparison we additionally modelled thisand galaxy with profiles whereas advection leads tosince exponential the ones. synchrotron Therefore, emission of NGC 4565 is described equally mainly because the data aretral more index consistent with profiles the producedspeeds linear consistently spec- by around advection. Wehigh find upper advection error limitsdi at large radii.ilar For behaviour to both the advection synchrotron scale and heights, however with a remaining models are presented inlist Appendix the D, key where parameters we fordependence also with all galactocentric models. radius, In we orderof present these to radial parameters illustrate profiles for the a subset of models in Fig. 10. well by Gaussian and exponential profiles, we used the former for ]. 12 2 ) = 3 3 3 3 3 3 3 V as 4 4 4 4 4 h µ 1) -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 -1 (or ] claiming that edge-on galaxies do not possess radio- values are on the north side and negative ones on the south side of the mid-plane. + at each 3 3 3 3 3 . Hence, s s s s s s z 2 2 2 2 2 2 2 2 2 2 2 2 2 µ 15 B2 is east of the minor axis and min h , 0 2 ↵ 5GHz 2 2 2 2 2 . ] in combination with a first data release of the D-array data 1 < , = 140 km s = 180 km s = 120 km s = 150 km s = 150 km s = 170 km s = 150 km s = 150 km s = 210 km = 150 km s = 160 km s = 130 km s = 140 km s = 110 km s = 110 km s = 150 km ( 0 0 0 0 0 0 0 0 0 0 0 0 0 0 r 1 1 1 1 1 1 1 14 V V V V V V V V V V V V V V nth  I = 4.5e28 cm = 4.5e28 cm = 5.5e28 cm = 5.5e28 cm = 8.0e28 cm = 4.0e28 cm ), and 1 1 1 1 1 0 0 0 0 0 0 0 2 ↵ D D D D D D NGC 4565: diffusion model NGC 4565: diffusion NGC 891: advection model advection NGC 891: D 0 0 0 0 0 0 0 0 0 0 0 0 (or . As discussed above, the intensity and spectral index profiles distinguish and 1 usion models. V 1) ↵ -1 -1 -1 -1 -1 -1 -1 -1 -1 s s s s + 2 2 2 2 -1 -1 -1 -1 -1 -1 -1 min -2 -2 -2 -2 -2 , Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Distance to Galactic Disc (z) [kpc] Disc Galactic to Distance 2 I Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) [kpc] Distance to Galactic Disc (z) Distance to Galactic Disc (z) [kpc] ( -2 -2 -2 -2 -2 -2 -2 P. Schmidt: An in-depth view of the cosmic-ray transport in NGC 891 and NGC 4565 P. Schmidt: An in-depth view of the cosmic-ray transport in NGC 891 and NGC 4565 = 4.5e28 cm = 4.5e28 cm = 2.5e28 cm = 3.5e28 cm -3 -3 -3 -3 -3  0 0 0 0 is west of the minor axis. Positive D D D D I 2 Comparison of advection models in NGC 891 and diffusion models in NGC 4565. In the left 0 usion models of NGC 891 the best fits were > -4 -4 -4 -4 -4 -3 -3 -3 -3 -3 -3 -3 ] is shown in Fig. ↵ r -1 -1 -1 -1 -1 -1 -1 -2 -3 -1 -2 -3 -2 -3 -1 -2 -3 -1 -1 -2 -3 -1 This modelling of the synchrotron emission is now to be applied to observations from the Karl -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -1.2 -1.4 -1.6 -1.8 -2.2 -2.4 -2.6 -2.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -2.2 -2.4 -2.6 -2.8 -1.2 -1.4 -1.6 -1.8 -2.2 -2.4 -2.6 -2.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -2.2 -2.4 -2.6 -2.8 -0.6 -0.8 -0.6 -0.8 -1.2 -1.4 -1.6 -1.8 -2.2 -2.4 -2.6 -2.8 -0.6 -0.8 12

and the non-thermal intensity

nt nt nt nt nt nt

nt usion models for NGC 4565 (assuming no energy dependence for the di

an Evla Survey” (CHANG-ES) project. The CHANG-ES sample consists of 35 edge-on spiral α α α α α α α

) ( Index Spectral ) ( Index Spectral ) ( Index Spectral ) ( Index Spectral ) ( Index Spectral ) ( Index Spectral ) ( Index Spectral nt nt nt nt nt

α α α α α Spectral Index ( Index Spectral ) Spectral Index ( Index Spectral ) ( Index Spectral ) Spectral Index ( Index Spectral ) Spectral Index ( Index Spectral ) ↵ usion and the latter for modelling advection. For galaxies in the local universein selected the by B-, angular C- size and and D-array-configurations total flux. in C-products. The and This targets paper L-band were also [ observed provides anthe image sample. of The an conclusion averaged that radio-continuum the halohalo average or is edge-on thick galaxy disk different exhibits for from ancontinuum extended the radio-continuum thick finding disks by or halos [ Milky that Way. would The make CHANG-ES the data emissionan now look example allow similar the for to a comparative that study detailed observedby analysis of in [ of the the the prototypical CRE edge-on transportadvection galaxies and from NGC 891 as diffusion and dominated transport. NGC 4565 Some more general properties of the CHANG-ES 3. First results from CHANG-ES G. Jansky Very Large Array− (VLA) in the context of the “Continuum HAlos in Nearby Galaxies the escape velocity of the galaxies as expected for galactic winds. Figure 1: panels, data points denote theobtained vertical from profile the of CHANG-ES the observations.non-thermal non-thermal intensity spectral In models index the at between right 1.5 1.5best-fitting panels, GHz and cosmic-ray the for 6 data transport NGC GHz show models. 891 as exponentialand and and Advection linear NGC Gaussian spectral predicts 4565, index approximately respectively. profiles;and exponential Solid parabolic in intensity lines spectral contrast, profiles show index diffusion the profiles. predicts Adopted from approximately [ Gaussian intensity profiles sample have been presented by [ CRE transport from radio continuum observations Accelerated advection models for NGC 891. Data points denote the vertical profile of the non-thermal spectral index between 1.5 ↵ Di 6GHz 5 . 1 , and 6 GHz (left panels)each and profile the is exponential given model in ofthe the the north right-hand-side non-thermal side plot; intensity and profile negative at ones 1.5 on GHz the (right south panels). side The of radial the position mid-plane. of Solid lines show the best-fitting advection models. at 1.5 GHz (right panels).minor The axis radial and position of eachSolid profile lines along show the the major best-fitting axis di is given in the right-hand-side plot; profile of the non-thermal spectral index between 1.5 and 6 GHz (left panels) and the Gaussian model of the non-thermal intensity profile nth

While for the di ↵

, NGC 4565 could also be fitted with lower values of Figure 12:

Figure 13: 5

. 18

0 gions (e.g. Tabatabaei et al. 2013) and possibly in superbubbles achieved using the commonly assumed energy exponent of

(Heesen et al. 2015). fusion models, in Figs. 12 and 13 for our preferred solutions. The

dex major-axis position, along with our best-fitting advection and dif- 8.2.3. Results

each model, we adopted the range of their upper and lower error margins. modelling di

values for which both We present the vertical profiles of the non-thermal spectral in- PoS(ICRC2019)237 ]. 21 ] and an 16 ] is now pro- 20 ]. The extent of Ralf-Jürgen Dettmar 18 ]. 17 ]). The reprocessing by A. 21 ], [ 20 Jy/beam at 6 arcsec resolution. µ 70 ∼ ]. The LOFAR LoTSS survey [ 19 3 ] in galaxies with a relatively low star-formation rate. 24 shows a map of NGC 4217 observed as part of the LoTSS Data Release 1 [ 2 The edge-on galaxy NGC 4217 with a dumbbell-shaped radio-continuum halo is observed by ] for a more detailed discussion). The low-frequency observations of the above mentioned 23 Radio-continuum halos of star-forming disk galaxies frequently exhibit a large scale X-shaped The dumbbell-shape radio halo (or thick disk) results from the combined effect of a radial de- ], [ 22 magnetic field as, e.g., described for the prototypical case of NGC 5775 in [ Miskolczi resulted in the reproduced map with a noise level of 4. Low frequency observations with LOFAR the synchrotron emission itself ishalo. proof Since for the the low presence energyresponding of cosmic low rays a frequency are magnetic emission expected field allow to us reachingnow be to far provides transported probe into observations furthest, the with the studies magnetic of unprecedented fieldas, far the sensitivity e.g., into cor- and demonstrated the resolution by halo. at the LOFAR such study of low NGC frequencies 891 [ target NGC 4565 with LOFAR presented indominated a transport recent [ paper support the interpretation of a diffusion cline of the magnetic field strength and[ the energy losses of the CREs transported into the halo (see Figure 2: sample such as typicaloverview scale of the heights CHANG-ES of project and the of radio-continuum its first disks results are is presented provided in by [ [ viding a very good basepotential, for Fig. in-depth studies of many more edge-on galaxies. To demonstrate this LOFAR at 145 MHz as part of the Data Release 1 of the LoTSS survey ([ CRE transport from radio continuum observations PoS(ICRC2019)237 ], the 25 Left panel: -2 -3 1 0 -1 10 10 10 10 10 . In all panels, the 1 Ralf-Jürgen Dettmar =1.09 =1.41 − 2 2 =1.39 χ 1.5GHz Sim χ Sim 2 14 χ 0.144GHz Sim Jy beam . As described by [ µ 3 12 and increasing by a factor of two. 1 − 10 . In this case advection with a linearly 4 2 mJybeam . 8 1 = 4 σ 4–8-GHz (C band, D array) image in contours starting at 6 Distance from disk [kpc] disk from Distance 4 Right panel: . 1 − 2 and increasing by a factor of two. Some CLEANing artefacts are visible in the form 0 1

− index 1 0 -1 -2 -3

10 10 10 10 10 Normalized intensity Normalized Resulting profiles of the advective cosmic-ray propagation model using a linearly accelerating Jybeam Radio images in contours superimposed on a three-colour optical image from SDSS. µ 66 = σ intensity and spectral index profilescreasing resulting advection from speed this is combination considered are as better shown modelled in if Fig. an in- For several of the CHANG-ESm galaxies wavelength under now study covered the by broad LOFARthe and wavelength case JVLA range of observations between NGC requires 3556 cm to the and expand significantLOFAR the larger is extend model. shown of For in the radio-halo comparison seen to at lower the frequencies JVLA with observations in Fig. of symmetric features on the south side of the galaxy. The rms noise is 22 Figure 4: wind speed. The blue dotsMHz represent measurements normalised and measured the intensities; middle theradio shows top spectral the panel index shows VLA profile. the 1.5 LOFARintensity GHz In 144 profiles measurements. all is panels, logarithmic, The whereas the bottom the red panel spectral lines shows index represent is the the shown in simulated linear quantity. scale. The scale for the LOFAR 144-MHz image in contours rangingThe from rms 3 noise is 0.43 mJy beam synthesised beam of 21" FWHM is shown as a filled white circle in the bottom left corner. Figure 3: CRE transport from radio continuum observations PoS(ICRC2019)237 Ralf-Jürgen Dettmar ] 26 provides the best fit to the measurements 1 − 5 ]. The significance of this poloidal halo component of the 28 shows the magnetic field structure of the CHANG-ES target NGC 4666 as dis- 5 ], gives a more complex picture which links the multi-component profile to the star- ] in more detail. Besides the prominent halo magnetic field this galaxy is noteworthy 27 26 NGC 4666 optical SDSS image produced from the u, g, r filters with apparent magnetic field Yet another recently published case study for a galaxy from the CHANG-ES sample, namely Further progress in describing the transport of CRs into galactic halos will certainly also de- orientations shown in white with a beam of 10"x10". (adopted from [ NGC 4013 [ formation history of the galaxy. Figure 5: since the CHANG-ES data indicate aof the possible disk. reversal of the magnetic field direction in the plane 5. Magnetic fields in galactic halos pend on better models of thedistribution magnetic of field configuration. the The radio-continuum observedpoloidal emission dumbbell-shape halo intensity component suggests of the the large wide-spreadnetic scale field existence magnetic models field of as which provided, requires a e.g., a by X-shaped [ new generation of mag- cussed by [ at the three frequencies used (1.5 GHz, 6 GHz, and 144 MHz). magnetic field is supported by atechnique first at analyses the of JVLA the allows CHANG-ES toan sample. apply example, The RM-synthesis Fig. wide-band reconstruction receiver of the polarized intensity. As CRE transport from radio continuum observations increasing wind speed starting at a velocity of 123 km s PoS(ICRC2019)237 , , ApJL Ralf-Jürgen Dettmar , MNRAS (2016), , Galaxies (2019) 7, 42 , A&A (2000), 364, L36 , AJ (2015), 150, 81 , A&A (2013), 556 , A2 , A&A (2018), 611, A72 6 , ApJ (2013), 772, 112 , A&A Review (2015), 24, 4 , ApJ (2018), 853, 128 , Cambridge University Press , arXiv [1907.03789] LOFAR: The LOw-Frequency ARray The LOFAR Two-metre Sky Survey. I. Survey description and preliminary data Investigation of the cosmic ray population and magnetic field strength in the The Average Star Formation Histories of Galaxies in Dark Matter Halos from z The thermal and non-thermal gaseous halo of NGC 5775 Launching Cosmic-Ray-driven Outflows from the Magnetized Interstellar Medium CHANG-ES X: Spatially Resolved Separation of Thermal Contribution from Radio Galactic star formation and accretion histories from matching galaxies to dark CHANG-ES XVI: An in-depth view of the cosmic-ray transport in the edge-on spiral Galactic Winds Driven by Isotropic and Anisotropic Cosmic-Ray Diffusion in Disk CHANG-ES. IX. Radio scale heights and scale lengths of a consistent sample of 13 CHANG-ES. IV. Radio Continuum Emission of 35 Edge-on Galaxies Observed with , A&A (2018), 615, A98 Radio haloes in nearby galaxies modelled with 1D cosmic ray transport using Advective and diffusive cosmic ray transport in galactic haloes Axial Ratio of Edge-On Spiral Galaxies as a Test for Bright Radio Halos CHANG-ES XVIII: The CHANG-ES Survey and Selected Results Continuum Halos in Nearby Galaxies: An EVLA Survey (CHANG-ES). I. Introduction , MNRAS (2013), 428, 3121 , MNRAS (2018), 476, 158 , AJ (2012), 144, 43 High Energy Astrophysics Magnetic fields in spiral galaxies , ApJL (2016), 824, L30 Unleashing Positive Feedback: Linking the Rates of Star Formation, Supermassive Black Hole , A&A (2017), 598, A104 , ApJ (2013), 770, 57 spiral galaxies seen edge-on and their correlations (2015), 799, L10 the Karl G. Jansky Very Large Array in D Configuration-Data Release 1 458, 332 SPINNAKER to the Survey halo of NGC 891 galaxies NGC 891 and NGC 4565 release Galaxies Continuum Emission in Edge-on Galaxies matter haloes ApJL (2016), 816, L19 = 0-8 Accretion, and Outflows in Distant Galaxies [1] J. Silk, [7] R. Beck, [8] C. J. Vargas et al., [9] V. Heesen et al., [6] M. P. van Haarlem et al., [2] P. S. Behroozi et al., [4] P. Girichidis et al., [5] R. Pakmor et al., [3] B. P. Moster et al., [16] M. Krause et al., [18] R. Tüllmann et al., [17] J. Irwin et al., CRE transport from radio continuum observations Acknowledgements Research at RUB is supported by BMBF Verbundforschung 05A17PC1. References [10] M. Longair, [11] V. Heesen et al., [13] J. Irwin et al., [14] T. Wiegert et al., [15] J. Singal et al., [19] D. D. Mulcahy et al., [12] P. Schmidt et al., [20] T. W. Shimwell et al., PoS(ICRC2019)237 , , A&A Ralf-Jürgen Dettmar , A&A accepted, arXiv [1906.10650] 7 , A&A (2019), 623, A33 , A&A (2009a), 494, 563 Analytical models of X-shape magnetic fields in galactic halos , A&A (2009b), 506, 1123 CHANG-ES XII. A LOFAR and VLA view of the edge-on star-forming galaxy Cosmic rays and the magnetic field in the nearby NGC 253. I.Cosmic The rays and the magnetic field in the nearby starburst galaxy NGC 253. II.Warped diffusive The radio halo around the quiescent spiral edge-on galaxy NGC 4565 priv. comm CHANG-ES XIII: Transport processes and the magnetic fields of NGC 4666: CHANG-ES XIX: Galaxy NGC 4013 – a diffusion-dominated radio halo with , A&A (2019), 622, A9 (2014), 561, A100 NGC 3556 plane-parallel disk and vertical halo magnetic fields distribution and transport of cosmic rays magnetic field structure arXiv [1907.07076] indication of a reversing disk magnetic field [23] V. Heesen et al., [26] Y. Stein et al., [27] Y. Stein et al., [28] K. Ferrière and P. Terral, [24] V. Heesen et al., [25] A. Miskolczi et al., CRE transport from radio continuum observations [21] T. W. Shimwell, [22] V. Heesen et al.,