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Observation Date (UT) Observation Lat

Canonical Name:HESS J1507-622
TeVCat Name:TeV J1506-623
Other Names:
Source Type:UNID
R.A.:15 06 52.8 (hh mm ss)
Dec.:-62 21 00.0 (dd mm ss)
Gal Long: 317.95 (deg)
Gal Lat: -3.49 (deg)
Distance:
Flux:0.01 (Crab Units)
Energy Threshold:500 GeV
Spectral Index:2.24
Extended:Yes
Size (X):0.15 (deg)
Size (Y):0.15 (deg)
Discovery Date:2009-12
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 J1507-622
Source Class: Unid
Identified Object: None
R.A. (J2000): 226.75 deg (15 06 59)
Dec. (J2000): -62.32 deg (-62 19 24)
Positional uncertainty: 0.039 deg
Spatial Model: Gaussian
Size: 0.175 +/- 0.017 deg
Spectral Model: power law
Integral Flux > 1 TeV: 2.60e-12 +/- 2.06e-13 cm-2 s-1
Pivot Energy, E0: 2.26 TeV
Diff. Flux at E0: 5.17e-13 +/- 4.11e-14 cm-2 s-1 TeV-1
Spectral Index: 2.22 +/- 0.07
HGPS Source Notes:
Three 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":
- 3FGL J1506.6−6219 (3FGL)
- CXOU J150706.0−621443 (EXTRA)
- 2FHL J1507.4−6213 (2FHL)
"EXTRA associations: For completeness, in addition to the associations obtained through the catalog-based, automatic procedure, we add a list of 20 extra associated objects that are plausible counterparts for some HGPS sources and are not covered by the limited set of catalogs we use."

Source position and its uncertainty:
From Acero et al. (2010):
- RA (J2000): 226.72deg +/- 0.05deg (15h 06m 52.8s)
- Dec (J2000): -62.35deg +/- 0.03deg (-62d 21' 00")
From Tibolla, O. et al. (2009):
- R.A.: 226.72 +/- 0.05
- Dec.: -62.35 +/- 0.03

Source Extent:
From Acero et al. (2011):
- radius: 0.15 +/- 0.02 deg
From Tibolla, O. et al. (2009):
- radius: 0.15 +/- 0.02 deg

Spectral Information:
From Acero et al. (2011):
- Spectral index: 2.24 +/- 0.16 (stat) +/- 0.20 (sys)

Source Classification:
From Eger et al. (2014):
- "... we report on results of follow-up observations of the potential
X-ray counterpart with Suzaku. We present detailed measurements of its
spectral parameters and find a high absorbing hydrogen column density,
compatible with the total amount of Galactic gas in this direction. In
comparisons to measurements and models of the Galactic
three-dimensional gas distribution we show that the potential X-ray
counterpart of HESS J1507-622 may be located at the far end of the
Galaxy. If the gamma-ray source is indeed physically connected to this
extended X-ray source, this in turn would place the object outside of
the usual distribution of Galactic VHE gamma-ray emitters."
From Domainko (2014):
- "The line of sight of HESS J1507-622 reaches a minimum distance to the
Galactic center at around a galactocentric distance of 5.3 kpc at
about 300 pc off the Galactic disc. This location coincides with the
scale length and width of stars with an age of 1.2 Gyr which could in
principle be an indication that HESS J1507-622 is connected to a
stellar population of similar age. For such a case the source appears
to be strongly particle dominated. In a leptonic scenario, if a
magnetic field in the source of 1 microG is assumed, equipartition
between magnetic field and particles would be realized at a distance
of >= 1 Mpc. This could indicate an extragalactic origin of this
object. However, an extragalactic origin is challenged by the
extension of the source."
- "The environment of HESS J1507-622 still remains elusive. For the case
where this source belongs to a new class of gamma-ray emitters, the
distribution of related objects (if existing) may help to settle the
respective environment and distance scale."
From Vorster et al. (2013):
- "... for this candidate PWN a scenario is favoured in the present
paper in which HESS J1507--622 has been compressed by the reverse
shock of the supernova remnant."
From Vorster et al. (2013):
- A spatially-independent model that can be used to calculate the
temporal evolution of the electron/ positron spectrum in a spherically
expanding pulsar wind nebula is presented. ...The parameters derived
from the model strengthens the idea that (this source) can be
identified as evolved pulsar wind nebulae.
From Acero et al. (2013):
- in the LAT energy range, this source is point-like with a relatively soft spectrum
From Domainko & Ohm (2012):
- "The SED constructed from the Fermi and H.E.S.S. data for this source
does not support a smooth power-law continuation from the VHE to the
HE gamma-ray range. With the available data it is not possible to
discriminate between a hadronic and a leptonic scenario for HESS
J1507–622. The location and compactness of the source indicate a
considerable physical offset from the Galactic plane for this
object. This challenges a pulsar wind nebula (PWN) origin for HESS
J1507–622 since the time of travel for a pulsar born in the Galactic
disk to reach such a location would exceed the IC cooling time of
electrons that are energetic enough to produce VHE
gamma-rays. However, an origin of this gamma-ray source connected to a
pulsar that was born off the Galactic plane in the explosion of a
hypervelocity star cannot be excluded."
From Tibolla et al. (2011):
- suggest that this source is an ancient PWN
From Acero et al. (2011):
- a leptonic scenario is favoured, while a hadronic one seems unlikely

Distance:
From Domainko (2014):
- "the energy density in particles is contrasted to the magnetic field
energy density and constraints on the distance based on equipartition
between these two components are calculated."
- it is concluded that the distance could be between 0.18 Mpc and 100 Mpc
- this would imply that the source lies outside the galaxy, a
challenging prospect for an extended source: "Such a scenario face the
challenge to explain the connected rather large extension of the
source."


Seen by: H.E.S.S.
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