2019A&A...621A.138K


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.26CEST23:51:52

2019A&A...621A.138K - Astronomy and Astrophysics, volume 621A, 138-138 (2019/1-1)

Magnetic field estimates from the X-ray synchrotron emitting rims of the 30 Dor C superbubble and the implications for the nature of 30 Dor C's TeV emission.

KAVANAGH P.J., VINK J., SASAKI M., CHU Y.-H., FILIPOVIC M.D., OHM S., HABERL F., MANOJLOVIC P. and MAGGI P.

Abstract (from CDS):


Context. The 30 Dor C superbubble is unique for its synchrotron X-ray shell, as well as being the first superbubble to be detected in TeV γ-rays, though which is the dominant TeV emission mechanism, leptonic or hadronic, is still unclear.
Aims. We aim to use new Chandra observations of 30 Dor C to resolve the synchrotron shell in unprecedented detail and to estimate the magnetic (B) field in the postshock region, a key discriminator between TeV γ-ray emission mechanisms.
Methods. We extracted radial profiles in the 1.5-8keV range from various sectors around the synchrotron shell and fitted these with a projected and point spread function convolved postshock volumetric emissivity model to determine the filament widths. We then calculated the postshock magnetic field strength from these widths.
Results. We find that most of the sectors were well fitted with our postshock model and the determined B-field values were low, all with best fits ≤20µG. Upper limits on the confidence intervals of three sectors reached ≥30µG though these were poorly constrained. The generally low B-field values suggests a leptonic-dominated origin for the TeV γ-rays. Our postshock model did not provide adequate fits to two sectors. We find that one sector simply did not provide a clean enough radial profile, while the other could be fitted with a modified postshock model where the projected profile falls off abruptly below ∼0.8 times the shell radius, yielding a postshock B-field of 4.8(3.7-11.8)µG which is again consistent with the leptonic TeV γ-ray mechanism. Alternatively, the observed profiles in these sectors could result from synchrotron enhancements around a shock-cloud interaction as suggested in previous works.
Conclusions. The average postshock B-field determined around the X-ray synchrotron shell of 30 Dor C suggests the leptonic scenario as the dominant emission mechanism for the TeV γ-rays.

Abstract Copyright: © ESO 2019

Journal keyword(s): ISM: supernova remnants - ISM: bubbles - Magellanic Clouds - X-rays: ISM - ISM: magnetic fields

Nomenclature: Table 1: [KVS2019] NN (Nos 1-10).

Status at CDS:  

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5612 1
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14744 1
3 SN 1987A SN* 05 35 28.020 -69 16 11.07   4.75 4.81     SNIIpec 4450 2
4 [JGB98] 30 Dor-25 MoC 05 35 42.0 -69 09 38           ~ 3 0
5 [KVS2019] 1 X 05 35 42.40 -69 11 52.3           ~ 1 0
6 [KVS2019] 2 X 05 35 42.80 -69 12 06.9           ~ 1 0
7 [KVS2019] 3 X 05 35 48.30 -69 09 33.9           ~ 1 0
8 HESS J0535-691 gam 05 35 55.0 -69 11 10           ~ 1 0
9 [KVS2019] 4 X 05 35 57.00 -69 09 13.6           ~ 1 0
10 [KVS2019] 5 X 05 35 59.70 -69 11 51.1           ~ 1 0
11 [KVS2019] 6 X 05 35 59.90 -69 11 21.6           ~ 1 0
12 [KVS2019] 7 X 05 36 00.60 -69 09 26.7           ~ 1 0
13 [KVS2019] 8 X 05 36 06.40 -69 11 47.3           ~ 1 0
14 NAME 30 Dor C Rad 05 36 07.70 -69 11 52.6           ~ 62 1
15 NGC 2044 As* 05 36 11 -69 11.8   10.69 10.59     ~ 81 0
16 [KVS2019] 9 X 05 36 25.00 -69 10 05.0           ~ 1 0
17 [KVS2019] 10 X 05 36 33.20 -69 11 40.6           ~ 1 0
18 LHA 120-N 70 HII 05 43 17.5 -67 50 48           ~ 78 0
19 ESO 134-11 HII 14 40 29 -62 38.7           ~ 507 1
20 SNR G347.3-00.5 SNR 17 12 27 -39 41.2           ~ 603 1
21 NAME Cas A SNR 23 23 24.000 +58 48 54.00           ~ 2396 1

    Equat.    Gal    SGal    Ecl

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2020.05.26-23:51:52

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