| Canonical Name: | HESS J1809-193 |
| TeVCat Name: | TeV J1810-193 |
| Other Names: | 2HWC J1809-190
PSR J1809-1917
eHWC J1809-193
1LHAASO J1809-1918u |
| Source Type: | UNID |
| R.A.: | 18 10 31 (hh mm ss) |
| Dec.: | -19 18 00 (dd mm ss) |
| Gal Long: | 11.18 (deg) |
| Gal Lat: | -0.09 (deg) |
| Distance: | 3.7 kpc |
| Flux: | 0.14 (Crab Units) |
| Energy Threshold: | 250 GeV |
| Spectral Index: | 2.2 |
| Extended: | Yes |
| Size (X): | 0.53 (deg) |
| Size (Y): | 0.25 (deg) |
| Discovery Date: | 2007-09 |
| Discovered By: | H.E.S.S. |
| TeVCat SubCat: | Default Catalog |
Source Notes:
| H.E.S.S. Galactic Plane Survey (HGPS, 2018): |
| A selection of information for each of the 78 sources in the HGPS is provided in TeVCat. For full details, visit the HGPS website. |
| Name: | HESS J1809-193 |
| Source Class: | Unid |
| Identified Object: | None |
| R.A. (J2000): | 272.53 deg (18 10 07) |
| Dec. (J2000): | -19.33 deg (-19 19 46) |
| Positional uncertainty: | 0.128 deg |
| Spatial Model: | 3-Gaussian |
| Size: | 0.404 +/- 0.048 deg |
| Spectral Model: | power law |
| Integral Flux > 1 TeV: | 5.37e-12 +/- 4.49e-13 cm-2 s-1 |
| Pivot Energy, E0: | 1.05 TeV |
| Diff. Flux at E0: | 6.62e-12 +/- 4.66e-13 cm-2 s-1 TeV-1 |
| Spectral Index: | 2.38 +/- 0.07 |
| HGPS Source Notes: | |
| | |
Eight possible associations are listed in Table A.9. "This is a list of astronomical objects, extracted from catalogs of plausible counterparts, which are are found to be spatially coincident with the HGPS source":
- G11.0−0.0 (SNR)
- J1809−1917 (PSR)
- G11.1+0.1 (COMP)
- 3FGL J1810.1−1910 (3FGL)
- G11.4−0.1 (SNR)
- 3FGL J1811.3−1927c (3FGL)
- G11.2−0.3 (COMP)
- J1811−1925 (PSR)
160125: In light of the
Castelletti et al. (2016) results,
this object's classification was changed from PWN to UNID
Source Position:
From
Aharonian et al. (2007):
- R.A. (J2000): 18h 10m 31s +/- 12s
- Dec. (J2000): -19d 18m +/- 2m
From
Renaud et al. (2008):
- R.A. (J2000): 18h 09m 52s +/- 2'(stat)
- Dec. (J2000): -19d 23m 42s +/- 2'(stat)
From HESS
online catalog:
- R.A. (J2000): 18h 09m 21s
- Dec. (J2000): -19d 27m 00s
Source Extent:
From
Aharonian et al. (2007):
- 32' +/- 4' (= 0.53 +/- 0.07 deg)
- 15' +/- 2' (= 0.25 +/- 0.03 deg)
- angle: ~50 deg
From HESS
online catalog:
- radius: 32' = 0.53 deg
From
Renaud et al. (2008):
- radius: 0.25 +/- 0.02
Distance:
The quoted distance assumes the gamma-ray source is a PWN associated
with PSR J1809−1917. This association has not been clearly established.
Flux:
From
Aharonian et al. (2007)
- "Its integral flux between 1−10 TeV is about 14% of the flux of the
Crab nebula in the same energy range."
Source Association:
From
ChaoMing, Chong & Ruoyu (2023):
- "HESS J1809-193 is an extended TeV gamma-ray source and the origin
of its gamma-ray emission remains ambiguous. Pulsar wind nebula (PWN)
of PSR J1809-1917 laying inside the extended gamma-ray emission is a
possible candidate. Powered by the central pulsar, ultrarelativistic
electrons in PWN can produce radio to X-ray emission through
synchrotron and gamma-ray emission by inverse Compton (IC)
scattering."
- "To check whether this PWN is the counterpart of HESS J1809-193, we
analyzed Chandra X-ray radial intensity profile and the spectral
index profile of this PWN."
- "We then adopt a one-zone isotropic diffusion model to fit the keV
and the TeV data. We find diffuse nonthermal X-ray emission extending
beyond PWN, which is likely an X-ray halo radiated by escaping
electron/positron pairs from the PWN. A relatively strong magnetic
field of 21 microG is required to explain the spatial evolution of
the X-ray spectrum (i.e., the significant softening of the spectrum
with increasing distance from the pulsar), which, however, would
suppress the IC radiation of pairs."
- "Our result implies that a hadronic component may be needed to
explain HESS J1809-193."
From
Klingler et al. (2018):
- "PSR J1809-1917 is a young (age = 51 kyr) energetic (E-dot = 1.8 x10e36 erg s−1 )
radio pulsar powering a pulsar wind nebula (PWN). We report on the
results of three Chandra X-ray Observatory observations which show
that the PWN consists of a small (approx. 20'') bright compact nebula
(CN) and faint extended emission seen up to 20 from the pulsar."
- "The more extended emission and CN share the same symmetry axis,
which is also aligned with the direction toward the TeV gamma-ray
source HESS J1809-193, supporting their association."
From
Araya (2018):
- A detailed study of the GeV emission of the region around this
source and
HESS J1813-178 was undertaken.
- The author postulates that HESS J1809-193 could be a proton pevatron.
- "The GeV emission has an extended morphology in the region of the
TeV emission and the overall spectrum can be accounted for by a cosmic
ray population having a simple power-law spectrum with energies
extending up to 1 PeV. However, the spectrum at tens of TeV should be
observed more deeply in the future to confirm its hadronic nature, and
other scenarios involving combinations of leptonic and hadronic
emission from several of the known supernova remnants in the region
cannot be ruled out. "
"The nearby TeV source
HESS J1813-178, thought to be a PWN, is also
studied in detail at GeV energies and we find a region of significant
emission which is much more extended than the TeV emission and whose
spectrum is softer than expected from a PWN but similar to those seen
in several star forming regions that are believed to accelerate
protons. There is marginal evidence for a GeV point source at the
location of the X-ray PWN, beside the extended emission."
From
Abeysekara et al. (2017):
- "2HWC J1809-190 may be associated with HESS J1809-193 (centered
approx. 0.3 deg away."
From
Castelletti et al. (2016):
- "No radio counterpart to the observed X-ray emission supposed to be a
pulsar wind nebula powered by PSR J1809-1917 is seen in the new JVLA
image. We discovered a system of molecular clouds on the edge of the
supernova remnant (SNR) G11.0-0.0 shock front, which is positionally
coincident with the brightest part of the TeV source HESS
J1809-193. We determine, on the basis of kinematic and morphological
evidences, a physical link of the SNR with the clouds ..."
"We propose as the most likely origin of the very high-energy
gamma-ray radiation from HESS J1809-193 a hadronic mechanism through
collisions of ions accelerated at the SNR G11.0-0.0 shock with the
molecular matter in the vicinity of the remnant."
From
Rangelov et al. (2014)
- "We investigate whether there is any connection between the possible
TeV extension of HESS J1809-193 and the sources seen at lower
energies. We find that another X-ray binary candidate, Suzaku
J1811-1900, and a radio supernova remnant, SNR G11.4-0.1, can hardly
be responsible for the putative TeV emission. Our multiwavelength
classification of fainter X-ray point sources also does not produce a
plausible candidate. We conclude that the northeast extension of HESS
J1809-193, if confirmed by deeper observations, can be considered as a
dark accelerator - a TeV source without visible counterpart at lower
energies."
From
Aharonian et al. (2007)
- "In the case of HESS J1809−193 the multi-wavelength picture is much
more complicated. Though the bulk of the emission can be explained by
a PWN powered by PSR J1809−1917, several supernova remnants as well as
another PWN may contribute to the observed VHE emission. Deeper
observations in both gamma-ray and X-ray wavebands are needed to
conclusively distinguish the origin of the signal."
Emission above 56 GeV:
From
HAWC Collaboration (2019):
- This source overlaps with eHWC J1809-193 one of nine sources in the
first catalog of gamma-ray sources emitting above 56 TeV presented by
the HAWC Collaboration
- The properties given in the eHWC catalog are the following:
... Source name: eHWC J1809-193
... R.A. (deg): 272.46 +/- 0.13
... Dec. (deg): -19.34 +/- 0.14
... Extension > 56 TeV (deg): 0.34 +/- 0.13
... F (10e-14 ph cm-2 s-1): 2.4+0.6 -0.5
... sqrt(TS) > 56 TeV: 6.97
... Nearest 2HWC source: J1809-190
... Distance to 2HWC source (deg): 0.30
... sqrt(TS) > 100 TeV: 4.82
A PeVatron:
From
Cao et al. (2024):
- This source is listed as being a UHE source in Table 2. This means
that it has a detection above 100 TeV at a significance level
corresponding to a test statistic of greater than 20.
Seen by: H.E.S.S., HAWC, LHAASO
-
The First LHAASO Catalog of Gamma-Ray Sources
Cao, Zhen et al., ApJS 271 p25 (2024) [LINK]
-
Revisiting the Chandra Observation on the Region of PSR J1809-1917: Indication of an X-ray Halo and Implication for the Origin of HESS J1809-193
Li, ChaoMing et al., arXiv e-prints parXiv:2303.14946 (2023) [LINK]
-
Formation pathway for lonely stripped-envelope supernova progenitors: implications for Cassiopeia A
Hirai, Ryosuke et al., MNRAS 499 p1154-1171 (2020) [LINK]
-
Connecting the ISM to TeV PWNe and PWN candidates
Voisin, F.J. et al., pasa 36 pe014 (2019) [LINK]
-
Multiple Galactic Sources with Emission Above 56 TeV Detected by HAWC
HAWC Collaboration et al., arXiv e-prints parXiv:1909.08609 (2019) [LINK]
-
GeV emission in the region of HESS J1809-193 and HESS J1813-178: is HESS J1809-193 a proton pevatron?
Araya, M., ArXiv e-prints p (2018) [LINK]
-
The Variable Pulsar Wind Nebula of PSR J1809-1917
Klingler, N. et al., ArXiv e-prints p (2018) [LINK]
-
The 2HWC HAWC Observatory Gamma-Ray Catalog
Abeysekara, A.U. et al., ApJ 843 p40 (2017) [LINK]
-
Dense molecular gas at 12 mm towards Galactic TeV gamma-ray sources
de Wilt, P. et al., MNRAS 468 p2093-2113 (2017) [LINK]
-
Unveiling the origin of HESS J1809-193
Castelletti, G. et al., ArXiv e-prints p (2016) [LINK]
-
Multiwavelength study of the northeastern outskirts of the extended TeV source HESS J1809-193
Rangelov, B. et al., ArXiv e-prints p (2014) [LINK]
-
Pulsar Wind Nebulae from X-rays to VHE gamma-rays
Kargaltsev, O. et al., 466 p167 (2013) [LINK]
-
X-Ray Studies of HESS J1809-193 with Suzaku
Anada, T. et al., ArXiv e-prints p (2009) [LINK]
-
Pulsar Wind Nebula candidates recently discovered by H.E.S.S.
Renaud, M. et al., 1085 p285-288 (2008) [LINK]
-
Discovery of two candidate pulsar wind nebulae in very-high-energy gamma rays
Aharonian, F. et al., A&A 472 p489-495 (2007) [LINK]
Want a reference added? Send a bibtex entry to
the TeVCat Team
