| Canonical Name: | HESS J1616-508 |
| TeVCat Name: | TeV J1616-508 |
| Other Names: | |
| Source Type: | PWN |
| R.A.: | 16 16 24.0 (hh mm ss) |
| Dec.: | -50 54 00 (dd mm ss) |
| Gal Long: | 332.39 (deg) |
| Gal Lat: | -0.14 (deg) |
| Distance: | 6.5 kpc |
| Flux: | 0.19 (Crab Units) |
| Energy Threshold: | 200 GeV |
| Spectral Index: | |
| Extended: | Yes |
| Size (X): | 0.14 (deg) |
| Size (Y): | 0.14 (deg) |
| Discovery Date: | 2005-03 |
| Discovered By: | H.E.S.S. |
| TeVCat SubCat: | Default Catalog |
| 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 J1616-508 | |
| Source Class: | Unid | |
| Identified Object: | None | |
| R.A. (J2000): | 244.23 deg (16 16 54) | |
| Dec. (J2000): | -50.86 deg (-50 51 39) | |
| Positional uncertainty: | 0.077 deg | |
| Spatial Model: | 2-Gaussian | |
| Size: | 0.232 +/- 0.035 deg | |
| Spectral Model: | power law | |
| Integral Flux > 1 TeV: | 7.99e-12 +/- 5.49e-13 cm-2 s-1 | |
| Pivot Energy, E0: | 1.16 TeV | |
| Diff. Flux at E0: | 7.55e-12 +/- 4.35e-13 cm-2 s-1 TeV-1 | |
| Spectral Index: | 2.32 +/- 0.06 | |
| HGPS Source Notes: | ||
Six 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":
- J1617−5055 (PSR)
- G332.5−0.3 (PWN)
- 2FHL J1616.2−5054e (2FHL)
- 3FGL J1616.2−5054e (3FGL)
- G332.4−0.4 (SNR)
- G332.4+0.1 (SNR)
Source position and its uncertainty:
From Aharonian et al. (2006):
- l: 332.391 +/- 0.014 deg
- b: -0.138 +/- 0.013 deg
- R.A. (deg): 244.10 (Convert to HMS: 16 16 24.0)
- Dec. (deg): -50.90 (Convert to HMS: -50 54 00)
From HESS online catalog:
- R.A. (J2000): 16h 16m 24s
- Dec. (J2000): -50d 54m 00s
- l: 332.39
- b: -0.14
Source Extent:
From Aharonian et al. (2005):
- radius: 11' (= 0.183 deg)
- statistical error: 10-35%
From Aharonian et al. (2006):
- radius: 0.136 +/- 0.008 deg
Source Association:
From Lau et al. (2017):
- In this paper, the interstellar medium in the direction of HESS J1614-518
and HESS J1616-508 is studied in detail using "results from
a 7 mm-wavelength Mopra study, the Mopra Southern Galactic Plane CO
Survey, the Millimetre Astronomer's Legacy Team - 45 GHz survey and
[CI] data from the HEAT telescope"
- Several origin scenarios for the TeV gamma rays from these two HESS
sources are discussed but no "strong convincing evidence linking any
counterpart with HESS J1614−518 or HESS J1616−508" is found.
- "Several accelerator candidates towards HESS J1616-508 were
investigated in light of our ISM study. Neither of the two young SNRs
that flank the TeV source, Kes 32 and RCW 103, were found to be strong
candidates for association. We also found no convincing evidence to
link PSR J1617-5055 and its associated PWN to TeV gamma rays from
HESS J1616-508. Due to the somewhat conspicuous nature of the diffuse gas
seen in component 1 (-47 to -39 km s-1 ), we speculate on an
undetected accelerator at the centre of the TeV source interacting
with said gas. We find that a CR accelerator such as a young SNR would
readily be able explain the TeV gamma-ray flux from HESS J1616-508."
From Hare et al. (2017):
-"We report the results of three Chandra observations covering most of
the extent of the TeV γ-ray source HESS J1616–508 and a search for a
lower energy counterpart to this source. We detect 56 X-ray sources,
of which 37 have counterparts at lower frequencies, including a young
massive star cluster, but none of them appears to be a particularly
promising counterpart to the TeV source"
- "The brightest X-ray source, CXOU J161423.4–505738"... "is a likely
intermediate polar CV candidate. No counterparts of this source were
detected at other wavelengths. CVs are not known to produce extended
TeV emission, and the source is also largely offset (19' ) from HESS
J1616–508, making them unlikely to be associated."
- "We have also set an upper limit on the X-ray flux of PSR J1614–5048
in the 0.5-8 keV band" ... which ... "makes PSR J1614–5048 one of the
least X-ray efficient pulsars known." ..." We find no evidence
supporting the association between the pulsar and the TeV source."
- "We rule out a number of X-ray sources as possible counterparts to
the TeV emission and do not find a plausible counterpart among the
other sources."
- "Lastly, we discuss the possible relation of PSR J1617–5055 to HESS
J1616–508 in light of the new observations."
From Acero et al. (2013):
- Analysis of the LAT data from this source leads to its
classification as a PWN candidate
From Aharonian, Buckley, Kifune & Sinnis (2008):
- list this as a possible PWN.
From Tibolla et al. (2011):
- suggest that this source is an ancient PWN
Seen by: H.E.S.S.
- A study of the interstellar medium towards the unidentified dark TeV gamma-ray sources HESS J1614-518 and HESS J1616-508
Lau, J.C. et al., ArXiv e-prints p (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]
- Constraints on the Galactic Population of TEV Pulsar Wind Nebulae Using Fermi Large Area Telescope Observations
Acero, F. et al., ArXiv e-prints p (2013) [LINK]
- MALT-45: The Galactic plane in 7mm
Jordan, Christopher et al., Protostars and Planets VI Posters (2013) [LINK]
- New developments in the ancient PulsarWind Nebulae scenario
Tibolla, O. et al., ArXiv e-prints p (2011) [LINK]
- Ancient Pulsar Wind Nebulae in light of recent GeV and TeV observations
Tibolla, O. et al., ArXiv e-prints p (2011) [LINK]
- Young energetic PSR J1617-5055, its underluminous nebula and unidentified TeV source HESS J1616-508
Kargaltsev, O. et al., ArXiv e-prints 805 p (2008) [LINK]
- HESS J1616-508: likely to be powered by PSR J1617-5055
Landi, R. et al., MNRAS 380 p926-932 (2007) [LINK]
- The H.E.S.S. Survey of the Inner Galaxy in Very High Energy Gamma Rays
Aharonian, F. et al., ApJ 636 p777-797 (2006) [LINK]
- A New Population of Very High Energy Gamma-Ray Sources in the Milky Way
Aharonian, F. et al., Science 307 p1938-1942 (2005) [LINK]
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