2018A&A...611A..72K


Query : 2018A&A...611A..72K

2018A&A...611A..72K - Astronomy and Astrophysics, volume 611A, 72-72 (2018/3-1)

CHANG-ES. IX. Radio scale heights and scale lengths of a consistent sample of 13 spiral galaxies seen edge-on and their correlations.

KRAUSE M., IRWIN J., WIEGERT T., MISKOLCZI A., DAMAS-SEGOVIA A., BECK R., LI J.-T., HEALD G., MULLER P., STEIN Y., RAND R.J., HEESEN V., WALTERBOS R.A.M., DETTMAR R.-J., VARGAS C.J., ENGLISH J. and MURPHY E.J.

Abstract (from CDS):

Aim. The vertical halo scale height is a crucial parameter to understand the transport of cosmic-ray electrons (CRE) and their energy loss mechanisms in spiral galaxies. Until now, the radio scale height could only be determined for a few edge-on galaxies because of missing sensitivity at high resolution.
Methods. We developed a sophisticated method for the scale height determination of edge-on galaxies. With this we determined the scale heights and radial scale lengths for a sample of 13 galaxies from the CHANG-ES radio continuum survey in two frequency bands.
Results. The sample average values for the radio scale heights of the halo are 1.1±0.3kpc in C-band and 1.4±0.7kpc in L-band. From the frequency dependence analysis of the halo scale heights we found that the wind velocities (estimated using the adiabatic loss time) are above the escape velocity. We found that the halo scale heights increase linearly with the radio diameters. In order to exclude the diameter dependence, we defined a normalized scale height h~ which is quite similar for all sample galaxies at both frequency bands and does not depend on the star formation rate or the magnetic field strength. However, h~ shows a tight anticorrelation with the mass surface density.
Conclusions. The sample galaxies with smaller scale lengths are more spherical in the radio emission, while those with larger scale lengths are flatter. The radio scale height depends mainly on the radio diameter of the galaxy. The sample galaxies are consistent with an escape-dominated radio halo with convective cosmic ray propagation, indicating that galactic winds are a widespread phenomenon in spiral galaxies. While a higher star formation rate or star formation surface density does not lead to a higher wind velocity, we found for the first time observational evidence of a gravitational deceleration of CRE outflow, e.g. a lowering of the wind velocity from the galactic disk.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: spiral - galaxy: halo - galaxies: magnetic fields - galaxies: ISM - radio continuum: general - radio continuum: galaxies - radio continuum: galaxies

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 660 Sy2 01 43 02.350 +13 38 44.45   12.02 11.16     ~ 538 2
2 NGC 891 H2G 02 22 32.907 +42 20 53.95 11.08 10.81 9.93 7.86   ~ 1601 2
3 NGC 2613 EmG 08 33 22.841 -22 58 25.21   11.29 10.42 9.75 10.5 ~ 161 0
4 NGC 2683 AGN 08 52 41.3064829584 +33 25 18.597681516 11.57 10.68 9.79 9.38   ~ 419 1
5 NGC 2820 GiP 09 21 45.564 +64 15 28.87   13.1       ~ 154 0
6 NGC 2992 Sy2 09 45 42.045 -14 19 34.90 13.54 13.14 12.18 12.6 12.2 ~ 838 3
7 NGC 3003 GiG 09 48 35.580 +33 25 17.83   12.3       ~ 186 0
8 NGC 3044 G 09 53 40.884 +01 34 46.74   12.7   12.7 12.3 ~ 212 1
9 NGC 3079 Sy2 10 01 57.8789863992 +55 40 47.449758324 11.57 11.54 10.86     ~ 1331 3
10 NGC 3432 IG 10 52 31.132 +36 37 07.60   11.81 11.67 11.29   ~ 273 1
11 NGC 3448 IG 10 54 39.240 +54 18 18.82   12.2       ~ 200 1
12 NGC 3735 Sy2 11 35 57.2748856320 +70 32 07.951921080   12.4       ~ 176 2
13 NGC 3877 GiG 11 46 07.782 +47 29 40.20   11.8       ~ 303 0
14 NGC 4013 GiG 11 58 31.417 +43 56 49.28   12.4       ~ 400 1
15 NGC 4096 GiG 12 06 01.161 +47 28 42.09   11.61   10.86   ~ 236 0
16 NGC 4157 GiP 12 11 04.365 +50 29 04.85 12.48 12.15 11.35     ~ 331 2
17 NGC 4217 GiG 12 15 50.900 +47 05 30.44   12.4       ~ 275 2
18 NGC 4244 GiG 12 17 29.659 +37 48 25.60   10.71   9.99   ~ 536 1
19 NGC 4302 GiP 12 21 42.477 +14 35 51.94   13.4 11.61     ~ 308 0
20 NGC 4388 Sy2 12 25 46.820 +12 39 43.45 11.91 11.76 11.02     ~ 1275 2
21 NGC 4438 LIN 12 27 45.6705493536 +13 00 31.708096380 11.37 11.02 10.17     ~ 614 2
22 NGC 4565 LIN 12 36 20.804 +25 59 14.61   13.61 12.43     ~ 922 0
23 M 104 LIN 12 39 59.4302501832 -11 37 22.988264808 9.51 9.55 8.00 8.05   ~ 1339 3
24 NGC 4631 GiP 12 42 08.009 +32 32 29.44   9.78 9.19 9.10   ~ 1037 2
25 NGC 4666 GiP 12 45 08.676 -00 27 42.88   11.7   11.5 10.7 ~ 362 1
26 NGC 4845 AGN 12 58 01.242 +01 34 32.09   17.40 16.31     ~ 226 0
27 NGC 5084 LIN 13 20 16.923 -21 49 39.28   11.15 12.21 9.84 10.5 ~ 171 0
28 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 4120 4
29 NGC 5297 GiP 13 46 23.694 +43 52 19.34   12.3       ~ 156 0
30 NGC 5775 GiP 14 53 57.653 +03 32 40.10   13.0 11.34     ~ 419 2
31 NGC 5792 EmG 14 58 22.709 -01 05 27.89   11.8   11.8 11.1 ~ 170 0
32 UGC 10288 G 16 14 24.804 -00 12 27.14   13.5   13.4 12.9 ~ 107 0

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2022.10.07-05:56:13

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