| Canonical Name: | MAGIC J1837-073 |
| TeVCat Name: | TeV J1837-072 |
| Other Names: | 3FGL J1837.6-0717 |
| Source Type: | UNID |
| R.A.: | 18 37 21.6 (hh mm ss) |
| Dec.: | -07 16 48 (dd mm ss) |
| Gal Long: | 24.85 (deg) |
| Gal Lat: | -0.21 (deg) |
| Distance: | |
| Flux: | (Crab Units) |
| Energy Threshold: | GeV |
| Spectral Index: | 2.29 |
| Extended: | Yes |
| Size (X): | 0.00 (deg) |
| Size (Y): | 0.00 (deg) |
| Discovery Date: | 2018-12 |
| Discovered By: | MAGIC |
| TeVCat SubCat: | Default Catalog |
Source Notes:
This discovery was announced in
MAGIC Collaboration (2018) in December 2018.
The field of view of SNR G24.7+0.6 was observed and three distinct sources were detected:
- the brightest source is identified with
HESS J1837-069
- an excess to the south of this source, MAGIC J1837-073 (discussed here), coincident with 3FGL J1837.6-0717
-
MAGIC J1835-069 that is perhaps associated with SNR G24.7+0.6
Source Position:
From
MAGIC Collaboration (2018):
- R.A. (J2000): 279.34 +/- 0.14 deg = 18h 37m 21.6s +/- 33.6s
- Dec. (J2000): -007.28 +/- 0.24 deg = -07d 16' 48'' +/- 864''
Source Extent:
From
MAGIC Collaboration (2018):
- "The comparison between a model describing the source as point like
and a model treating the source as a Gaussian results in a TS
difference of 23 or approx. 5 sigma, favouring the second model to
describe the total emission."
Spectral Information:
From
MAGIC Collaboration (2018):
- "The spectrum of this source extends to low energies."
- spectral index: 2.29 +/- 0.09
- flux at decorrelation energy: 1.7 +/- 0.1 x10e-12 TeV-1 cm-2 s-1
- decorrelation energy: 0.95 TeV
Source Association:
From
Banik & Bhadra (2021):
- "Recently the MAGIC telescope observed three TeV gamma-ray extended sources
in the galactic plane in the neighborhood of radio SNR G24.7+0.6. Among them,
the PWN
HESS J1837-069 was detected earlier by the HESS observatory during its
first galactic plane survey. The other two sources,
MAGIC J1835-069 and
MAGIC J1837-073 are detected for the first time at such high energies. Here
we shall show that the observed gamma-rays from the SNR G24.7+0.6 and the
HESS J1837-069 can be explained in terms of hadronic interactions of the
PWN/SNR accelerated cosmic rays with the ambient matter. We shall further
demonstrate that the observed gamma-rays from the
MAGIC J1837-073 can be
interpreted through hadronic interactions of runaway cosmic-rays from PWN
HESS J1837-069 with the molecular cloud at the location of
MAGIC J1837-073.
No such association has been found between
MAGIC J1835-069 and SNR G24.7+0.6
or PWN
HESS J1837-069. We have examined the maximum energy attainable by
cosmic-ray particles in the SNR G24.7+0.6/ PWN
HESS J1837-069 and the
possibility of their detection with future gamma-ray telescopes. The study
of TeV neutrino emissions from the stated sources suggests that the
HESS J1837-069 should be detected by IceCube Gen-2 neutrino telescope in a
few years of observation."
From
MAGIC Collaboration (2018):
- "Spatially coincident with the hotspot reported in
Marandon et al. (2008),
we named it MAGIC J1837–073 since no name was officially previously
attributed to it. This source is also coincident with 3FGL J1837.6–0717
reported in the Third Catalog of Fermi-LAT sources (
Acero et al. 2015)"
- "The origin of this emission remains unclear, although, under a
first approximation assumption of one single parent population, an
hadronic scenario is most likely to explain a single power-law
spectrum up to few tens of TeV. The region was subject of observations
with XMM -Newton (Katsuta et al. 2017) in a search for a multi-wavelength
counterpart of the GeV emission they detect (G25B). No PWN, SNR, or
pulsar with spin-down luminosity > 1x10e34 erg s-1 was found in the
region. However, the region is rich in molecular content at velocities
v = 45 - 65 km s-1. In the GeV regime, it has been postulated as
possible association with a bubble identified with the stellar cluster
candidate G25.18+0.26, but no sign of such connection can be derived
from the TeV data"
- "The spectrum of the source extends to 3 TeV with no sign of an
spectral break. Although the PWN scenario cannot be ruled out, this
detection is believed to be produced by cosmic rays interacting with a
stellar cluster. If the latter is confirmed, MAGIC J1837–073 will be
part of the scarcely populated group of similar objects like
Westerlund 1 and 2 or the Cygnus cocoon and may contribute to a better
understanding of whether these objects can account for the Galactic
cosmic ray flux."
Seen by: MAGIC
-
An interacting molecular cloud scenario for production of gamma-rays and neutrinos from MAGIC J1835-069, and MAGIC J1837-073
Banik, Prabir and Bhadra, Arunava, European Physical Journal C 81 p478 (2021) [LINK]
-
Discovery of TeV gamma-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC
MAGIC Collaboration et al., MNRAS 483 p4578-4585 (2019) [LINK]
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