results. As mentioned in Sect. 5.5, the spectral properties of HESS J1852−000 are affected by systematic uncertainties larger than nominal.

The VHE emission is located along the eastern edge of SNR Kes 78 but extends well beyond the SNR. The SNR itself is characterized by an elongated and partial nonthermal shell seen in radio and X-rays (Zhou & Chen 2011; Bamba et al. 2016). It is interacting with adjacent molecular clouds, evidenced by the detection of a shock-excited OH(1720 MHz) maser on the shell (Koralesky et al. 1998) and studies of the CO molecular environment (Zhou & Chen 2011). The distance of the SNR is estimated to be ~5 kpc (Koralesky et al. 1998; Zhou & Chen 2011), although ~8.8 kpc has also been suggested (e.g., Xu & Zhang 2009). A hadronic origin of the VHE emission has been briefly discussed (Kosack et al. 2011), involving escaped cosmic rays from Kes 78 (e.g., Aharonian 1991; Gabici et al. 2007). However, the scenario remains unconfirmed in the absence of a more detailed study of the gas environment and its potential correlation with the complex VHE morphology.

The presence of two radio pulsars, PSR J1853−0004 and PSR J1853+0011, within the VHE emission region also suggests that the VHE γ-rays could originate in one of the PWN or could even be a result of superimposed emission from two PWNe. Although there are currently no known PWNe at other energies, the pulsars' spin-down luminosities $\dot{E} = 2.1 \times 10^{35}$ erg s⁻¹ and $2.1 \times 10^{34}$ erg s⁻¹, respectively, and distances $d = 6.6$ kpc and 7.5 kpc, are reasonable in the context of other pulsars thought to be powering VHE PWNe (H.E.S.S. Collaboration 2018e). The pulsars have so far only been detected in radio, although PSR J1853−0004 has been associated with the HE γ-ray source 3FGL J1853.2+0006, which is itself a source whose existence and properties are currently uncertain (subject to analysis Flags 3 and 4 in Acero et al. 2015).

In conclusion, it is not yet clear whether the VHE emission originates from a hadronic SNR and molecular cloud interaction, previously undetected PWNe associated with one or both of the spatially coincident pulsars, or some other yet unknown source.

### 5.6.17. Source candidates

Three VHE γ-ray source candidates (hotspots) were found above the TS = 30 detection threshold in one HGPS analysis (primary or cross-check), but these candidates had TS < 30 in the other analysis. These should be considered unconfirmed, or candidate, VHE sources to be confirmed by deeper VHE observations.

**HOTS J1111−611.** The VHE emission from the source candidate HOTS J1111−611 has a significance of TS = 22 (cross-check TS = 41). It is located at $(\ell, b) = (291.18^\circ \pm 0.03^\circ, -0.54^\circ \pm 0.03^\circ)$, has a measured integral flux $F(E > 1 \text{ TeV}) = 3.8 \times 10^{-13} \text{ cm}^{-2} \text{ s}^{-1}$, and a size $0.09^\circ \pm 0.03^\circ$. It is located near (~0.1°) the very energetic $\tau_c = 32.7$ kyr pulsar PSR J1112−6103 (Manchester et al. 2001) emitting in radio and HE γ-rays (3FGL J1111.9−6058, Abdo et al. 2013). The pulsar has a high spin-down luminosity $\dot{E} = 4.5 \times 10^{36}$ erg s⁻¹ and a distance of 12.2 kpc (Cordes & Lazio 2002). Moreover, a significant HE γ-ray source (2FHL J1112.1−6101e, Ackermann et al. 2016) above 50 GeV has been reported at 0.04° from the pulsar, which makes this HE source likely to be a PWN. The characteristics of this pulsar, the apparent efficiency $\epsilon_{E>1 \text{ TeV}} \sim 1\%$, and the presence of a HE component in its vicinity suggests that it could plausibly power a VHE PWN.

**HESS J1831−098.** The source candidate HESS J1831−098 is found to have TS = 59 in the main HGPS analysis but only TS = 17 in the cross-check analysis and is therefore considered a source candidate. HESS J1831−098 is located in a complex region with nearby diffuse components, which might explain the discrepancy observed for this source candidate. Preliminary VHE morphological and spectral properties on HESS J1831−098 were announced by Sheidaei (2011). This source candidate is coincident with the energetic pulsar PSR J1831−0952, which exhibits a spin-down luminosity of $1.1 \times 10^{36}$ erg s⁻¹ and a characteristic age of 128 kyr. According to Sheidaei (2011), a $\epsilon_{1-20 \text{ TeV}} \sim 1\%$ conversion efficiency from rotational energy to γ-rays would be required to power a PWN; this is similar to values observed in other VHE PWN.

**HOTS J1907+091.** The VHE emission from source candidate HOTS J1907+091 has a significance of only TS = 18 (cross-check TS = 43). It is located at $(\ell, b) = (42.88^\circ \pm 0.08^\circ, 0.69^\circ \pm 0.08^\circ)$, has a measured integral flux $F(E > 1 \text{ TeV}) = 4.3 \times 10^{-13} \text{ cm}^{-2} \text{ s}^{-1}$, and an extension of $0.17^\circ \pm 0.04^\circ$. Two potential counterparts are found to be spatially coincident with this source candidate: the magnetar SGR 1900+14 (Mazets et al. 1979) and the SNR G42.8+0.6 (Fuerst et al. 1987). The former has an age $\tau_c = 0.90$ kyr and a spin-down luminosity $\dot{E} = 2.6 \times 10^{34}$ erg s⁻¹. It is assumed to be at a distance $12.5 \pm 1.7$ kpc (Davies et al. 2009) based on an association of the magnetar with a massive star cluster (Wachter et al. 2008). SGR 1900+14 has similar properties to those of another magnetar, SGR 1806−20, that is associated with the VHE source HESS J1808−204 (H.E.S.S. Collaboration 2018a). It underwent a major burst of soft γ-ray emission in 1998 (Hurley et al. 1999; Frail et al. 1999) and, similar to SGR 1806−20, it might also be emitting VHE γ-rays. Little is known about SNR G42.8+0.6. The centroid of the VHE emission is marginally coincident with the magnetar, while the bulk of the emission overlaps the northeastern half of the SNR shell.

## 6. Summary and conclusions

The H.E.S.S. Collaboration has completed its Galactic plane survey, which is an observation and analysis program that spanned over a decade. This paper presents the final results of the survey. The four-telescope H.E.S.S. Phase I array was used for the observations, which features a 5° FoV that is well suited to scanning large regions of the sky like the Galactic plane. The Phase I array has a typical sensitivity to point-like γ-ray sources of 1% Crab Nebula integral flux ($\dot{E} > 1$ TeV) in less than 25 h.

The H.E.S.S. Collaboration added a fifth, larger telescope to the array in 2012 (H.E.S.S. Phase II) to extend its sensitivity to lower energies as well as its ability to rapidly reposition to observe transient phenomena. However, it also features a smaller FoV than the four Phase I telescopes, making it much less suited for scanning large regions. In addition, the HGPS had improved the uniformity of its exposure and achieved a target sensitivity of 2% Crab flux in the inner Galaxy. Primarily for these reasons, as well as the diminishing gains stemming from source significance scaling approximately as the square root of livetime, the H.E.S.S. Collaboration in 2013 decided not to continue the HGPS observation program.

First early results from the HGPS were published in 2005 (Aharonian et al. 2005a). The observations at the time amounted to just 120 h yet led to the detection of ten VHE γ-ray sources
in the inner Galaxy, eight of which were not previously known. Further results followed in 2006 (Aharonian et al. 2006a), using 230 h of data and discovering additional four γ-ray sources. Since then, we provided the community with periodic updates, which had steadily increasing exposure and additional source discoveries, by releasing new unidentified sources (Aharonian et al. 2008a) and via published conference proceedings (Hoppe 2008b; Chaves et al. 2008a; Chaves 2009; Gast et al. 2011; Deil 2012; Carrigan et al. 2013a,b).

The HGPS data set (Sect. 2) is now over a factor of ten larger than in 2006, comprising 2673 h of observations accumulated over the period 2004 to 2013. These data come from a variety of observations: observations from the initially published surveys, targeted observations of known sources, follow-up observations of newly discovered source candidates, observations to extend the HGPS spatial coverage, and fill-up observations to achieve a more uniform sensitivity across the Galactic plane (Fig. 4). The energy threshold of the HGPS varies with the longitude observed but is typically lower than 0.8 TeV for detections and maps (0.5 TeV for spectral analyses) and as low as 0.4 TeV (0.2 TeV) in many regions, especially the innermost Galaxy (Fig. 2).

Compared to the previous publication, the HGPS was also expanded to cover a much wider range of both longitude and latitude (Fig. 1). In the first Galactic quadrant, the HGPS now extends in longitude from the Galactic center to nearly $\ell = 65^\circ$, the northern limit of visibility from the southern-hemisphere H.E.S.S. site. In the fourth Galactic quadrant, the HGPS coverage is continuous and even extends beyond Vela to $\ell = 250^\circ$ in the third quadrant. In latitude, the coverage varies but is generally $b = \pm 3^\circ$ and as large as $b = \pm 5^\circ$ in some regions to explore areas of particular interest off the plane. The point-source sensitivity is better than 2% Crab along the Galactic plane ($b = 0^\circ$) over most of the longitudes covered by the HGPS (Figs. 4 and 11). However, the flux sensitivity varies significantly owing to the mix of observations comprising the HGPS. It is better than 1% Crab in numerous regions but at a more modest level of 2–10% Crab off-plane. The HGPS achieves the best sensitivity at the Galactic center, reaching 0.3% of the Crab flux.

To ensure robust results, the HGPS relies on results that agree between two independent software frameworks (chains; Sect. 2.3) used to calibrate raw Cherenkov data as well as reconstruct and analyze the γ-ray images and spectra. The primary software chain used the Hillas method for event reconstruction, and an event classification method using boosted decision trees. The secondary (cross-check) chain uses an alternative event reconstruction and classification based on EAS models, returning results that are in very good agreement globally although there are some variations on a source-by-source basis (discussed in Sect. 5.4). MC simulations provide the instrument response functions that describe the performance of the instrument. The mean angular resolution of H.E.S.S. (68% containment radius of the PSF) is ~0.08° and varies by approximately 10% across the survey region.

We have generated a number of sky maps (images; Sect. 3), which are public data products<fnref n="13" /> and also form the basis for the HGPS source catalog construction. To accumulate sufficient signal and search for γ-ray emission of different sizes, we generated three different sets of maps with events spatially correlated over radii of 0.1° (point-like), 0.2°, and 0.4°, respectively. To subtract background from hadronic CRs passing γ-ray selections in the FoV, we developed an adaptive version of the classic ring background method that is more flexible and can compensate

for large exclusion regions that minimize signal contaminating background regions (Sect. 3.3). The release maps are for statistical significance, flux, flux error, upper limit and sensitivity (see Appendix A.1).

To detect and characterize the VHE γ-ray sources, we developed a semi-automatic analysis pipeline to construct a source catalog (see Sect. 4). To disentangle individual γ-ray sources in complex regions of overlapping emission, we implemented morphological modeling based on two-dimensional maximum-likelihood estimation. We fit the γ-ray excess by two-dimensional symmetric Gaussian components, keeping components with $TS > 30$. To arrive at the HGPS catalog, Gaussian components that did not correspond to a clear emission peak in the main and cross-check analysis were rejected. Some components that strongly overlapped were merged into a single source for which position, extension, and flux were characterized by the moments of the multi-Gaussian emission model. In this process, it was necessary to model the underlying large-scale γ-ray emission along the Galactic plane to improve the modeling of the discrete sources (Sect. 4.6). We chose to use an empirical model derived with a sliding window method, 20° wide in longitude and Gaussian in latitude, whose Gaussian center, amplitude, and width were fit to the excess outside exclusion regions. We calculated source spectra using the reflected region background method when possible, fitting PL spectral models and determining the best-fit normalization and spectral index. Flux information is also available from the aforementioned maps albeit assuming a spectral index of $\Gamma = 2.3$.

The HGPS source catalog includes 78 sources of VHE γ-rays. Of these, 64 were detected with the HGPS pipeline analysis. For completeness, the catalog includes an additional 14 H.E.S.S. sources from regions excluded from the HGPS pipeline, for example, because of their complexity, such as the Galactic center region and sources with shell-like morphologies. H.E.S.S. has previously published the discovery of most of the HGPS sources, although in many cases the available observation time used for the HGPS analysis is considerably larger. Of the total 78 sources, 16 are new discoveries published here for the first time. Five of these new sources are firmly identified objects: HESS J1554–550 and HESS J1849–000 are PWNe (Sects. 5.6.5 and 5.6.15), and HESS J1119–614, HESS J1833–105, and HESS J1846–029 are composite SNRs (Sects. 5.6.1, 5.6.10, and 5.6.13). Three more of the new sources are spatially coincident with HE γ-ray pulsars, recently discovered in Fermi-LAT data, and are thus plausible PWN candidates.

The HGPS sources have diverse characteristics (Sect. 5). Apart from the shell-like sources, most source morphologies are generally well-modeled as symmetric two-dimensional Gaussians, but their sizes range from point-like ($\le 0.1^\circ$) to $0.6^\circ$ (Fig. 13). Their fluxes cover a wide range as well from 0.6% Crab to 103% Crab of which the majority are in the range 1–20% Crab (Fig. 13). The cumulative $\log N - \log S$ distribution above 10% Crab (containing 32 sources) is well described by a power law of slope $-1.3 \pm 0.2$ (Fig. 15), matching the expectation of a power law of slope $-1$ from a population of equal-luminosity sources homogeneously distributed in the Galactic disk. Below 10% Crab, the HGPS source catalog is incomplete and can only provide a lower limit on the true number of fainter VHE sources (70 above 1% Crab). Spectral indices range from hard ($\Gamma \approx 2.0$) to very soft ($\Gamma \approx 3.0$) in an approximately normal distribution centered at $2.4 \pm 0.3$ (Fig. 14). The VHE sources cluster narrowly along the Galactic plane (median $b = -0.20^\circ$, with a

<footnote n="13">¹³ https://www.mpi-hd.mpg.de/hfm/HESS/hgps</footnote>
spread of 0.51°), in good agreement with the distributions of SNRs, energetic pulsars, molecular gas, and HE γ-ray sources (Fig. 11). Their distribution in longitude (Fig. 12) shows a general correlation with molecular gas.

To study the origin of the VHE γ-rays, we performed a systematic search to associate the HGPS sources with known or suspected VHE source classes, based largely on spatial compatibility with objects in the SNR and PWN catalog SNRcat, the ATNF pulsar catalog, and the Fermi-LAT 3FGL and 2FHL catalogs (Sect. 5.1). By comparing the HGPS catalog to plausible MWL counterpart catalogs, we come to one of the main conclusions of the HGPS program: the majority (67, or 86%) of the HGPS sources are associated with at least one astronomical object that could potentially account for the production of γ-rays at TeV energies. The unassociated sources (11, 14%) are not necessarily dark, i.e., emitting exclusively in the VHE domain; it is also possible that their counterparts were missed by our association procedure. In short, most HGPS sources have either firm associations, plausible or potential counterparts in other wavelength regimes. Whether there remains a population of truly dark VHE sources in the HGPS can only be figured out with deeper MWL studies.

We then used additional, stricter criteria, such as shell-like morphology or variability, to establish firm identifications for 31 sources (Fig. 10). We found the largest identified VHE source class to be PWNe (12 sources, or 39% of identified sources), followed by shell-type SNRs (8, 26%); composite SNRs (8, 26%), where both the interior PWN and SNR shell may contribute to the emission; and high-energy binary systems (3, 10%). At present, only 40% of the HGPS sources can be firmly identified. This is typically due to difficulties resolving ambiguity among competing scenarios involving multiple associated objects in large part because of the large intrinsic sizes of VHE γ-ray sources.

The HGPS data set allows for population studies of sources. An early study of 15 globular clusters was published before the HGPS was completed (H.E.S.S. Collaboration 2013). Two further such studies, on the primary Galactic VHE source classes of PWNe and SNRs, are published as companion articles to this paper (H.E.S.S. Collaboration 2018e,l, respectively), together with more specific studies on a number of microquasars (H.E.S.S. Collaboration 2018g) and bow shocks of runaway stars (H.E.S.S. Collaboration 2018c). With the public release of the HGPS catalog along with sky maps, more comprehensive such population studies will become possible.

Further insights into the Galactic VHE source population and diffuse emission in the coming years can be expected. H.E.S.S., Fermi-LAT and HAWC are surveying the Milky Way; the analysis methods for the individual gamma-ray data sets, and joint analysis methods combining multiple data sets are improving; and new surveys at lower wavelengths (especially those detecting nonthermal emission in the radio and X-ray bands) will be come available soon. The next major leap forward will be achieved by the Galactic plane survey of the Cherenkov Telescope Observatory (CTA), which will consist of two arrays in the northern and southern hemisphere (The Cherenkov Telescope Array Consortium et al. 2017). The Galactic plane survey is a key science project of CTA, and is planned to cover the whole Galactic plane, over a wider energy band and with better angular resolution and sensitivity compared to HGPS (Dubus et al. 2013; The Cherenkov Telescope Array Consortium et al. 2017).

In conclusion, the additional exposure obtained since 2006, plus significant improvements in analysis and reconstruction methods, allowed us to probe much more of the Galaxy, whether

it be more distant sources, fainter nearby sources, or regions never before observed at TeV energies. The HGPS program clearly demonstrates that sources of VHE γ-ray emission are common in the Galaxy and are linked to diverse sites of high-energy particle acceleration.

**Acknowledgements.** This work made extensive use of gamma-cat<fnref n="14" />, SNR-cat<fnref n="15" /> (Ferrand & Safi-Harb 2012), ATNF<fnref n="16" /> (Manchester et al. 2005), SIMBAD<fnref n="17" /> (Wenger et al. 2000) and NASA's Astrophysics Data System Bibliographic Services. For data analysis, we made extensive use of the Python packages Gammapy<fnref n="18" /> (Donath et al. 2015; Deil et al. 2017), Astropy<fnref n="19" /> (Astropy Collaboration et al. 2013) and Sherpa<fnref n="20" /> (Freeman et al. 2001), as well as Numpy (Dubois et al. 1996), Scipy (Jones et al. 2001) and Matplotlib (Hunter 2007). The support of the Namibian authorities and the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, the University of Namibia, the Innsbruck University, the Austrian Science Fund (FWF), and the Austrian Federal Ministry for Science, Research and Economy, and by the University of Adelaide and the Australian Research Council. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation.

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<footnote n="1">¹ Centre for Space Research, North-West University, Potchefstroom 2520, South Africa</footnote>

<footnote n="2">² Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, 22761 Hamburg, Germany</footnote>

<footnote n="3">³ Max-Planck-Institut für Kernphysik, PO Box 103980, 69029 Heidelberg, Germany</footnote>

<footnote n="4">⁴ Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland</footnote>

<footnote n="5">⁵ National Academy of Sciences of the Republic of Armenia, Marshall Baghramian Avenue, 24, 0019 Yerevan, Republic of Armenia</footnote>

<footnote n="6">⁶ Yerevan Physics Institute, 2 Alikhanian Brothers St., 375036 Yerevan, Armenia</footnote>

<footnote n="7">⁷ Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, 12489 Berlin, Germany</footnote>

<footnote n="8">⁸ University of Namibia, Department of Physics, Private Bag 13301, Windhoek, Namibia</footnote>

<footnote n="9">⁹ GRAPPA, Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands</footnote>

<footnote n="10">¹⁰ Department of Physics and Electrical Engineering, Linnaeus University, 351 95 Växjö, Sweden</footnote>

<footnote n="11">¹¹ Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, 44780 Bochum, Germany</footnote>

<footnote n="12">¹² GRAPPA, Anton Pannekoek Institute for Astronomy and Institute of High-Energy Physics, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands</footnote>

<footnote n="13">¹³ Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, 6020 Innsbruck, Austria</footnote>

<footnote n="14">¹⁴ School of Physical Sciences, University of Adelaide, Adelaide 5005, Australia</footnote>
15 LUTH, Observatoire de Paris, PSL Research University, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France

16 Sorbonne Universités, UPMC Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, CNRS, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), 4 place Jussieu, 75252 Paris Cedex 5, France

17 Laboratoire Univers et Particules de Montpellier, Université Mont-
pellier, CNRS/IN2P3, CC 72, Place Eugène Bataillon, 34095 Mont-
pellier Cedex 5, France

18 IRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, France

19 Astronomical Observatory, The University of Warsaw, Al. Ujaz-
dowskie 4, 00-478 Warsaw, Poland

20 Aix Marseille Université, CNRS/IN2P3, CPPM, Marseille, France

21 Instytut Fizyki Jądrowej PAN, ul. Radzikowskiego 152, 31-342 Kraków, Poland

22 Funded by EU FP7 Marie Curie, grant agreement No. PIEF-GA-
2012-332350

23 School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg 2050, South Africa

24 Laboratoire d'Annecy-le-Vieux de Physique des Particules, Uni-
versité Savoie Mont-Blanc, CNRS/IN2P3, 74941 Annecy-le-Vieux,
France

25 Landessternwarte, Universität Heidelberg, Königstuhl,
69117 Heidelberg, Germany

26 Université Bordeaux, CNRS/IN2P3, Centre d'Études Nucléaires de Bordeaux Gradignan, 33175 Gradignan, France

27 Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, 10691 Stockholm, Sweden

28 Wallenberg Academy Fellow

29 Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany

30 Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, 91128 Palaiseau, France

31 APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France

32 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France

33 Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, UK

34 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland

35 Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, 14476 Potsdam, Germany

36 Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Cen-
tre for Astroparticle Physics, Erwin-Rommel-Str. 1, 91058 Erlangen,
Germany

37 DESY, 15738 Zeuthen, Germany

38 Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland

39 Centre for Astronomy, Faculty of Physics, Astronomy and Informat-
ics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun,
Poland

40 Department of Physics, University of the Free State, PO Box 339, Bloemfontein 9300, South Africa

41 Heisenberg Fellow (DFG), ITA Universität Heidelberg, Heidelberg, Germany

42 Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima-ku, Tokyo 171-8501, Japan

43 Japan Aerospace Exploration Agency (JAXA), Institute of Space and Astronautical Science (ISAS), 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 229-8510, Japan

44 Now at The School of Physics, The University of New South Wales, Sydney 2052, Australia

45 Now at Instituto de Física de São Carlos, Universidade de São Paulo, Av. Trabalhador São-carlense, 400 - CEP 13566-590 São Carlos SP, Brazil

46 Now at Technische Universität Kaiserslautern, 67663 Kaiserslautern, Germany

47 Now at I. Physikalisches Institut B, RWTH Aachen University, 52056 Aachen, Germany

48 Department of Physics and Astronomy, University of Manitoba, Winnipeg MB R3T 2N2, Canada
# Appendix A: Online material

In this section, we provide further information about the public data products released in electronic format. We also provide some guidance and caveats regarding the correct use of these products. The HGPS survey maps and source catalog presented in this paper are available for download at the CDS and at https://www.mpi-hd.mpg.de/hfm/HESS/hGPS

In addition to the figures and tables in this paper, there are a series of HGPS maps and tables available online:

- Figure A.1: HGPS flux map;

- Figures A.2–A.5: Four-panel HGPS significance maps with all VHE sources and MWL associations labeled;

- Table A.7: HGPS catalog source morphology summary;

- Table A.8: HGPS catalog source spectrum summary;

- Table A.9: HGPS catalog source associations.

## A.1. Sky maps

### Description

Survey maps are released in FITS format (Pence et al. 2010), using a Cartesian (CAR) projection in Galactic coordinates (Calabretta & Greisen 2002). The maps contain the whole HGPS region (–114° < l < 75° and –5° < b < +5°), with a binning of 0.02° per pixel corresponding to a total size of 9400 × 500 pixels. Maps are available for the following quantities:

- Statistical significance (described in Sect. 3.3);

- Flux (described in Sect. 3.4.2);

- $1\sigma$ flux error (described in Sect. 3.4.3);

- Flux upper limit (described in Sect. 3.4.3);

- Sensitivity (described in Sect. 3.4.4).

We provide all flux and flux-like quantities as integral photon fluxes above 1 TeV assuming a PL spectrum for the differential flux with an index $\Gamma = 2.3$. Each map is provided for two correlation radii, $R_c = 0.1°$ and $0.2°$.

A total of ten files are released (five quantities, each for two $R_c$), with file names `hgps_map_<quantity>_<radius>deg_v1.fits.gz`, e.g., the significance map with $R_c = 0.2°$ can be found in the file `hgps_map_significance_0.2deg_v1.fits.gz`.

### Usage notes and caveats

- Since none of the released flux-derived maps are computed for a point-like source hypothesis, information extracted from these maps should always be used in the context of full containment of the PSF. Otherwise, this could yield incorrect information, for example, a flux upper limit that is too low (optimistic). In particular, since the H.E.S.S. PSF has a size comparable to $0.1°$, the maps computed with this correlation radius do not fully contain the PSF. In this case, one only gets roughly 80% of the flux when reading a pixel value at a given position of a point-like source. Those maps should therefore be used with care when extracting a flux value (see also below).

- The released maps are already spatially correlated (oversampled); therefore, pixel values should be read at the corresponding position of interest for a circular region of radius $R_c$. In the case of a region size between two of the provided $R_c$ values, interpolation could be used as a first approximation. The oversampling also implies that maps

should not be used for morphology studies (e.g., production of radial profiles or fitting).

- Some caution should be taken for values in the $0.2°$ correlation maps where a gradient in exposure is present, since the background is estimated at the center of the ROI and not averaged across it (see Sect. 3.2).

- The significance maps contain, at each position, the statistical significance of the $\gamma$-ray excess. This value is not corrected for trials and the large-scale emission component is not taken into account in its computation.

- We recommend assuming a systematic error of 30% on the flux values (see Sect. 4.12).

## A.2. Source catalog

### Description

The HGPS source catalog (construction described in Sect. 4) and a number of other tables are available as BINTABLE FITS extensions in the `hgps catalogue_v1.fits.gz` file.

An overview of the available tables (including links to the tables in this paper describing the columns in detail) is given in Table A.1. Here is some further information on the content of the tables:

- **HGPS_Sources**: The HGPS catalog, one source per row, identified via the `Source_Name` column, which is in the format `HESS JHHMM±DDd`.

- **HGPS_Gauss_Components**: The HGPS Gaussian component list, one component per row. Reference back to HGPS_Sources catalog via the `Source_Name` column (if the component is part of a source).

- **HGPS_Associations**: The HGPS association list, one association per row. Reference back to HGPS_Sources catalog via the `Source_Name` column. A given HGPS catalog source can appear zero, one, or multiple times in this table.

### Usage notes and caveats

For reasons of reproducibility, we decided to release the complete emission model on which the analysis is based. This includes the full list of Gaussian components and parameters of the large-scale emission model. When working with this data, beware of following usage notes and caveats:

- Some of the components are unstable and are not confirmed by the cross-check analysis. Use the source catalog, not the component list, for studies based on the HGPS.

- For the HGPS catalog, we did not perform detailed per-source systematic error estimates. In general, when using spectra from the HGPS catalog, we recommend assuming a systematic error of 30% on the absolute flux and 0.2 on the spectral index.

- In Fig. 9, there are a few sources where the integral flux estimate differs by more than 30% when using the two methods discussed in this paper. As discussed in Sect. 4.12, the estimate of a source spectrum is affected by the assumed source morphology, diffuse gamma and atmospheric hadronic background model and uncertainties in the instrument response functions. In particular, the integral flux estimate may be uncertain by more than 30% for sources with relatively low significance that are not spatially isolated from other sources. In those cases, one can assume the difference between Flux_Map and Flux_Spec_Int_1TeV to be a lower limit on the systematic error.
<figure><img src="image_34.png" /><figcaption>**Fig. A.1.** Integral flux above 1 TeV using a correlation radius $R_c = 0.1^\circ$ and assuming spectral index $\Gamma = 2.3$, in units of % Crab. The map is only filled where the point-source sensitivity for a 5$\sigma$ detection (c.f. Fig. 4) is better (lower) than 2.5% Crab.</figcaption></figure>
<figure><img src="image_35.png" /><figcaption>**Fig. A.2.** HGPS sources and associations in context (1 of 4). The background image shows $\sqrt{\text{TS}}$ of the VHE γ-ray excess in the Galactic plane assuming a point source morphology. All HGPS catalog sources are shown on top with transparent circles that correspond to the measured size of the source. Source names are labeled above the Galactic plane. Associations for the sources are shown with markers in white and corresponding labels. Pulsar (PSR) associations from the ATNF catalog are shown with triangles; SNRs as white circles with the radius representing the size, PWN and Composite (COMP) associations from the SNRcat catalog are marked with squares; associations with Fermi-LAT 3FGL and 2FHL sources are shown with diamonds; extra associations are shown with hexagonal markers. 3FGL sources are not labeled when they are identical to the pulsar. 2FHL sources are not labeled, when they are identical to the 3FGL source. The various object categories and the association criteria applied are detailed in Sect. 5.1.</figcaption></figure>
<figure><img src="image_36.png" /><figcaption>Fig. A.3. HGPS in a MWL context (2 of 4). Fig. A.2 continued.</figcaption></figure>
<figure><img src="image_37.png" /><figcaption>Fig. A.4. HGPS in a MWL context (3 of 4). Fig. A.2 continued.</figcaption></figure>
<figure><img src="image_38.png" /><figcaption>**Fig. A.5.** HGPS in a MWL context (4 of 4). Fig. A.2 continued.</figcaption></figure>
<figure><img src="image_39.png" /><figcaption>**Fig. A.6.** Illustration of cut-out regions (red), exclusion regions (blue) and modeling regions (ROIs; gray, numbered) in the HGPS map. The background image displays significance ($R_c = 0.1°$) in inverse grayscale.</figcaption></figure>
<table><caption>**Table A.1.** HGPS catalog FITS tables. See Sect. A.2.</caption><thead><tr><th>HDU Extension name</th><th>Description</th><th>Rows</th><th>Column description</th></tr></thead><tbody><tr><td>HGPS_Sources</td><td>HGPS source catalog</td><td>78</td><td>see Table A.2</td></tr><tr><td>HGPS_Gauss_Components</td><td>HGPS component list</td><td>98</td><td>see Table A.3</td></tr><tr><td>HGPS_Associations</td><td>HGPS association list</td><td>223</td><td>see Table A.4</td></tr><tr><td>HGPS_Identifications</td><td>HGPS identification list</td><td>31</td><td>see Table A.5</td></tr><tr><td>HGPS_Large_Scale_Component</td><td>HGPS large-scale emission model parameters</td><td>50</td><td>see Table A.6</td></tr><tr><td>SNRcat</td><td>Bundled version of SNRcat used for associations</td><td>282</td><td></td></tr></tbody></table>
<table><caption>**Table A.2.** HGPS FITS table columns for HGPS_Sources, the main source catalog.</caption><thead><tr><th>Column</th><th>Unit</th><th>Description</th></tr></thead><tbody><tr><td>Source_Name</td><td></td><td>Source name (HESS JHHmm±DDd identifier)</td></tr><tr><td>Analysis_Reference</td><td></td><td>Source analysis reference ("HGPS" for most sources, "EXTERN" if source in Table 1)</td></tr><tr><td>Source_Class</td><td></td><td>Source class (only filled for identified sources, see Table 3)</td></tr><tr><td>Identifiedرين</td><td></td><td>Identified object (only filled for identified sources, see Table 3)</td></tr><tr><td>Gamma_Cat_Source_ID</td><td></td><td>Source ID in the gamma-cat open TeV catalog</td></tr><tr><td>RAJ2000</td><td>deg</td><td>Right Ascension (J2000)</td></tr><tr><td>DEJ2000</td><td>deg</td><td>Declination (J2000)</td></tr><tr><td>GLON</td><td>deg</td><td>Galactic longitude</td></tr><tr><td>GLON_Err</td><td>deg</td><td>Statistical error (1 sigma) on GLON</td></tr><tr><td>GLAT</td><td>deg</td><td>Galactic latitude</td></tr><tr><td>GLAT_Err</td><td>deg</td><td>Statistical error (1 sigma) on GLAT</td></tr><tr><td>Pos_Err_68</td><td>deg</td><td>Position error (68% CL, including systematics, see Eq. (19))</td></tr><tr><td>Pos_Err_95</td><td>deg</td><td>Position error (95% CL, including systematics, see Eq. (19))</td></tr><tr><td>ROI Number</td><td></td><td>ROI number, see Fig. A.6 for details</td></tr><tr><td>Spatial_Model</td><td></td><td>Spatial model (one of "Gaussian", "X-Gaussian" or "Shell")</td></tr><tr><td>Components</td><td></td><td>List of Gaussian components the source is composed of</td></tr><tr><td>Sqrt_TS</td><td></td><td>Square root of the sum of the test statistics of the individual components (Eq. (11))</td></tr><tr><td>Size</td><td>deg</td><td>Source size (1 sigma for single-Gaussian sources, RMS equivalent for multi-Gaussian sources and outer radius for SNRs)</td></tr><tr><td>Size_Err</td><td>deg</td><td>Statistical error (1 sigma) on Size</td></tr><tr><td>Size UL</td><td>deg</td><td>Upper limit (95% CL) on Size (Eq. (18), NULL if source is extended)</td></tr><tr><td>R70</td><td>deg</td><td>70% containment radius, computed on the PSF-convolved excess model image</td></tr><tr><td>RSpec</td><td>deg</td><td>R<sub>spec</sub>, the radius of the spectral analysis circular region</td></tr><tr><td>Excess Model Total</td><td></td><td>Total excess from spatial model (this source only)</td></tr><tr><td>Excess_RSpec</td><td></td><td>Data excess in R_Spec (measured on maps)</td></tr><tr><td>Excess_RSpec Model</td><td></td><td>Model excess in R_Spec (this source, other sources, large scale emission component)</td></tr><tr><td>Background_RSpec</td><td></td><td>Background in R_Spec</td></tr><tr><td>Lifetime</td><td>hour</td><td>Lifetime for map</td></tr><tr><td>Energy_Threshold</td><td>TeV</td><td>Energy threshold for map (minimum)</td></tr><tr><td>Flux_Map</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Integral flux above 1 TeV from the morphology fit on the map (total)</td></tr><tr><td>Flux_Map_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Map_Total</td></tr><tr><td>Flux_Map_RSpec_Data</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Data flux in R_Spec (measured on maps)</td></tr><tr><td>Flux_Map_RSpec_Source</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Model flux in R_Spec (this source only)</td></tr><tr><td>Flux_Map_RSpec_Other</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Model flux in R_Spec (other sources only)</td></tr><tr><td>Flux_Map_RSpec_LS</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Model flux in R_Spec (large scale emission component only)</td></tr><tr><td>Flux_Map_RSpec_Total</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Model flux in R_Spec (this source, other sources, large scale emission component)</td></tr><tr><td>Containment_RSpec</td><td></td><td>Containment fraction (Eq. (23))</td></tr><tr><td>Contamination_RSpec</td><td></td><td>Contamination fraction (Eq. (22))</td></tr><tr><td>Flux_Correction_RSpec>To_Total</td><td></td><td>Total flux correction factor (Eq. (21))</td></tr><tr><td>Lifetime_Spec</td><td>hour</td><td>Lifetime for spectrum</td></tr><tr><td>Energy_Range_Spec_min</td><td>TeV</td><td>Minimum energy of counts spectrum</td></tr><tr><td>Energy_Range_Spec_max</td><td>TeV</td><td>Maximum energy of counts spectrum</td></tr><tr><td>Background_Spec</td><td></td><td>Background from spectral analysis</td></tr><tr><td>Excess_Spec</td><td></td><td>Excess from spectral analysis</td></tr><tr><td>Spectral Model</td><td></td><td>Spectral model, either "PL" or "ECPL" (Eq. (24)) and (Eq. (25))</td></tr><tr><td>TS_ECPL_over_PL</td><td></td><td>Test statistic difference of ECPL and PL model</td></tr><tr><td>Flux_Spec_Int_1TeV</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>PL or ECPL integral flux above 1 TeV, depending on Spectral Model</td></tr><tr><td>Flux_Spec_Int_1TeV_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_Int_1TeV</td></tr></tbody></table>

**Notes.** The column descriptions link back to sections and equations in the main text where needed.
<table><caption>**Table A.2.** continued.</caption><thead><tr><th>Column</th><th>Unit</th><th>Description</th></tr></thead><tbody><tr><td>Flux_Spec_Energy_1_10_TeV</td><td>erg cm<sup>-2</sup> s<sup>-1</sup></td><td>PL or ECPL energy flux in the 1–10 TeV range, depending on Spectral_Model</td></tr><tr><td>Flux_Spec_Energy_1_10_TeV_Err</td><td>erg cm<sup>-2</sup> s<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_Energy_1_10_TeV</td></tr><tr><td>Energy_Spec_PL_Pivot</td><td>TeV</td><td>Reference energy E<sub>0</sub>, see Eq. (24)</td></tr><tr><td>Flux_Spec_PL_Diff_Pivot</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Differential flux at pivot energy</td></tr><tr><td>Flux_Spec_PL_Diff_Pivot_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_PL_Diff_Pivot</td></tr><tr><td>Flux_Spec_PL_Diff_1TeV</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Differential flux at 1 TeV</td></tr><tr><td>Flux_Spec_PL_Diff_1TeV_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_PL_Diff_1TeV</td></tr><tr><td>Index_Spec_PL</td><td></td><td>Spectral index</td></tr><tr><td>Index_Spec_PL_Err</td><td></td><td>Statistical error (1 sigma) on Index_Spec_PL</td></tr><tr><td>Energy_Spec_ECPL_Pivot</td><td>TeV</td><td>Reference energy E<sub>0</sub> (Eq. (25))</td></tr><tr><td>Flux_Spec_ECPL_Diff_Pivot</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Differential flux at pivot energy</td></tr><tr><td>Flux_Spec_ECPL_Diff_Pivot_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_ECPL_Diff_Pivot</td></tr><tr><td>Flux_Spec_ECPL_Diff_1TeV</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Differential flux at 1 TeV</td></tr><tr><td>Flux_Spec_ECPL_Diff_1TeV_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_ECPL_Diff_1TeV</td></tr><tr><td>Index_Spec_ECPL</td><td></td><td>Spectral index</td></tr><tr><td>Index_Spec_ECPL_Err</td><td></td><td>Statistical error (1 sigma) on Index_Spec_ECPL</td></tr><tr><td>Lambda_Spec_ECPL</td><td>TeV<sup>-1</sup></td><td>Spectral cutoff fit parameter (inverse cutoff energy)</td></tr><tr><td>Lambda_Spec_ECPL_Err</td><td>TeV<sup>-1</sup></td><td>Statistical error (1 sigma) on Lambda_Spec_ECPL</td></tr><tr><td>Flux_Spec_PL_Int_1TeV</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Integral flux above 1 TeV</td></tr><tr><td>Flux_Spec_PL_Int_1TeV_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_PL_Int_1TeV</td></tr><tr><td>Flux_Spec_ECPL_Int_1TeV</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Integral flux above 1 TeV</td></tr><tr><td>Flux_Spec_ECPL_Int_1TeV_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Spec_ECPL_Int_1TeV</td></tr><tr><td>N_Flux_Points</td><td></td><td>Number of flux points</td></tr><tr><td>Flux_Points_Energy</td><td>TeV</td><td>Energy value</td></tr><tr><td>Flux_Points_EnergyMin</td><td>TeV</td><td>Lower bound of energy bin</td></tr><tr><td>Flux_Points_EnergyMax</td><td>TeV</td><td>Upper bound of energy bin</td></tr><tr><td>Flux_Points_Flux</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Differential flux at given energy</td></tr><tr><td>Flux_Points_Flux_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Lower error on Flux_Points_Flux</td></tr><tr><td>Flux_Points_Flux_Err_Hi</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Upper error on Flux_Points_Flux</td></tr><tr><td>Flux_Points_Flux UL</td><td>cm<sup>-2</sup> s<sup>-1</sup> TeV<sup>-1</sup></td><td>Upper limit on Flux_Points_Flux</td></tr><tr><td>Flux_Points_Flux_Is UL</td><td></td><td>Boolean flag when to use Flux_Points_Flux UL</td></tr></tbody></table>

<table><caption>**Table A.3.** HGPS FITS table columns for HGPS_Gauss_Components.</caption><thead><tr><th>Column</th><th>Unit</th><th>Description</th></tr></thead><tbody><tr><td>Component_ID</td><td></td><td>Gauss component identifier (HGPSC NNN)</td></tr><tr><td>Source_Name</td><td></td><td>Source name (HESS JHHmm±DDd identifier) the component belongs to</td></tr><tr><td>Component_Class</td><td></td><td>Component class (see Sect. 4.9)</td></tr><tr><td>GLON</td><td>deg</td><td>Galactic longitude</td></tr><tr><td>GLON_Err</td><td>deg</td><td>Statistical error (1 sigma) on GLON</td></tr><tr><td>GLAT</td><td>deg</td><td>Galactic latitude</td></tr><tr><td>GLAT_Err</td><td>deg</td><td>Statistical error (1 sigma) on GLAT</td></tr><tr><td>Sqrt_TS</td><td></td><td>Square root of the test statistics of the component (see Eq. (11))</td></tr><tr><td>Size</td><td>deg</td><td>Component size (1 σ Gaussian width)</td></tr><tr><td>Size_Err</td><td>deg</td><td>Statistical error (1 sigma) on Size</td></tr><tr><td>Flux_Map</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Integral flux above 1 TeV from the morphology fit on the map (total)</td></tr><tr><td>Flux_Map_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup></td><td>Statistical error (1 sigma) on Flux_Map</td></tr><tr><td>Excess</td><td></td><td>Total model excess contained in the component</td></tr></tbody></table>

**Notes.** See Sects. 4.8 and 4.10.
<table><caption>**Table A.4.** HGPS FITS table columns for HGPS_Associations.</caption><thead><tr><td>Column</td><td>Unit</td><td>Description</td></tr></thead><tbody><tr><td>Source_Name</td><td></td><td>Source name (HESS JHHmm±DDd identifier)</td></tr><tr><td>Association_Catalog</td><td></td><td>Association catalog name (see Table 2)</td></tr><tr><td>Association_Name</td><td></td><td>Association source name</td></tr><tr><td>Separation</td><td>deg</td><td>Angular separation to HGPS source position</td></tr></tbody></table>

Notes. See Sect. 5.1.

<table><caption>**Table A.5.** HGPS FITS table columns for HGPS_Identifications.</caption><thead><tr><td>Column</td><td>Unit</td><td>Description</td></tr></thead><tbody><tr><td>Source_Name</td><td></td><td>Source name (HESS JHHmm±DDd identifier)</td></tr><tr><td>Identified_Object</td><td></td><td>Identified object name</td></tr><tr><td>Class</td><td></td><td>Class of the identified object</td></tr><tr><td>Evidence</td><td></td><td>Evidence for the identification</td></tr><tr><td>Reference</td><td></td><td>Reference for the identification</td></tr><tr><td>Distance_Reference</td><td></td><td>Reference for the distance estimate</td></tr><tr><td>Distance</td><td>kpc</td><td>Distance of the identified object</td></tr><tr><td>Distance_min</td><td>kpc</td><td>Minimum distance of the identified object</td></tr><tr><td>Distance_max</td><td>kpc</td><td>Maximum distance of the identified object</td></tr></tbody></table>

Notes. See Sect. 5.1.3.

<table><caption>**Table A.6.** HGPS FITS table columns for HGPS_Large_Scale_Component.</caption><thead><tr><td>Column</td><td>Unit</td><td>Description</td></tr></thead><tbody><tr><td>GLON</td><td>deg</td><td>Galactic longitude of window center</td></tr><tr><td>GLAT</td><td>deg</td><td>Peak latitude</td></tr><tr><td>GLAT_Err</td><td>deg</td><td>Statistical error (1 sigma) on peak latitude</td></tr><tr><td>Surface_Brightness</td><td>cm<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup></td><td>Peak brightness</td></tr><tr><td>Surface_Brightness_Err</td><td>cm<sup>-2</sup> s<sup>-1</sup> sr<sup>-1</sup></td><td>Statistical error (1 sigma) on peak surface brightness</td></tr><tr><td>Width</td><td>deg</td><td>Gaussian width</td></tr><tr><td>Width_Err</td><td>deg</td><td>Statistical error (1 sigma) on Gaussian width</td></tr></tbody></table>

Notes. See Sect. 4.6.
<table><caption>**Table A.7.** HGPS source catalog – summary of map-based measurements.</caption><thead><tr><th rowspan="2">Name</th><th rowspan="2">Spatial model</th><th>GLON</th><th>GLAT</th><th>R<sub>95</sub></th><th>Size</th><th>F(&gt;1 TeV)</th><th>F(&gt;1 TeV)</th><th>√TS</th></tr><tr><th>deg</th><th>deg</th><th>deg</th><th>deg</th><th>10<sup>-12</sup>cm<sup>-2</sup>s<sup>-1</sup></th><th>% Crab</th><th></th></tr></thead><tbody><tr><td>HESS J0835-455</td><td>3-Gaussian</td><td>263.96</td><td>-3.05</td><td>0.09</td><td>0.58 ± 0.052</td><td>15.36 ± 0.53</td><td>67.7 ± 2.4</td><td>39.4</td></tr><tr><td>HESS J0852-463*</td><td>Shell</td><td>266.29</td><td>-1.24</td><td>–</td><td>1.00</td><td>23.39 ± 2.35</td><td>103.2 ± 10.3</td><td>–</td></tr><tr><td>HESS J1018-589 A</td><td>Gaussian</td><td>284.35</td><td>-1.67</td><td>0.03</td><td>0.00 ± 0.012</td><td>0.30 ± 0.05</td><td>1.3 ± 0.2</td><td>8.7</td></tr><tr><td>HESS J1018-589 B</td><td>Gaussian</td><td>284.22</td><td>-1.77</td><td>0.12</td><td>0.15 ± 0.026</td><td>0.83 ± 0.17</td><td>3.7 ± 0.8</td><td>7.6</td></tr><tr><td>HESS J1023-575</td><td>Gaussian</td><td>284.19</td><td>-0.40</td><td>0.05</td><td>0.17 ± 0.009</td><td>2.56 ± 0.17</td><td>11.3 ± 0.8</td><td>21.4</td></tr><tr><td>HESS J1026-582</td><td>Gaussian</td><td>284.85</td><td>-0.52</td><td>0.12</td><td>0.13 ± 0.039</td><td>0.69 ± 0.19</td><td>3.0 ± 0.9</td><td>7.3</td></tr><tr><td>HESS J1119-614</td><td>Gaussian</td><td>292.13</td><td>-0.53</td><td>0.06</td><td>0.10 ± 0.014</td><td>0.87 ± 0.13</td><td>3.8 ± 0.6</td><td>10.2</td></tr><tr><td>HESS J1302-638</td><td>Gaussian</td><td>304.18</td><td>-1.00</td><td>0.02</td><td>0.01 ± 0.009</td><td>0.40 ± 0.05</td><td>1.7 ± 0.2</td><td>16.6</td></tr><tr><td>HESS J1303-631</td><td>2-Gaussian</td><td>304.24</td><td>-0.35</td><td>0.04</td><td>0.18 ± 0.015</td><td>5.26 ± 0.27</td><td>23.2 ± 1.2</td><td>54.5</td></tr><tr><td>HESS J1356-645</td><td>Gaussian</td><td>309.79</td><td>-2.50</td><td>0.08</td><td>0.23 ± 0.020</td><td>5.53 ± 0.53</td><td>24.4 ± 2.3</td><td>17.3</td></tr><tr><td>HESS J1418-609</td><td>Gaussian</td><td>313.24</td><td>0.14</td><td>0.04</td><td>0.11 ± 0.011</td><td>3.01 ± 0.31</td><td>13.3 ± 1.4</td><td>21.9</td></tr><tr><td>HESS J1420-607</td><td>Gaussian</td><td>313.58</td><td>0.27</td><td>0.03</td><td>0.08 ± 0.006</td><td>3.28 ± 0.24</td><td>14.5 ± 1.1</td><td>27.6</td></tr><tr><td>HESS J1427-608</td><td>Gaussian</td><td>314.42</td><td>-0.16</td><td>0.04</td><td>0.05 ± 0.009</td><td>0.74 ± 0.10</td><td>3.3 ± 0.5</td><td>10.5</td></tr><tr><td>HESS J1442-624*</td><td>Shell</td><td>315.43</td><td>-2.29</td><td>–</td><td>0.30 ± 0.020</td><td>2.44 ± 0.67</td><td>10.8 ± 3.0</td><td>–</td></tr><tr><td>HESS J1457-593</td><td>Gaussian</td><td>318.35</td><td>-0.42</td><td>0.15</td><td>0.33 ± 0.045</td><td>2.50 ± 0.40</td><td>11.0 ± 1.8</td><td>12.5</td></tr><tr><td>HESS J1458-608</td><td>Gaussian</td><td>317.95</td><td>-1.70</td><td>0.17</td><td>0.37 ± 0.031</td><td>2.44 ± 0.30</td><td>10.8 ± 1.3</td><td>11.5</td></tr><tr><td>HESS J1503-582</td><td>Gaussian</td><td>319.57</td><td>0.29</td><td>0.14</td><td>0.28 ± 0.033</td><td>1.89 ± 0.28</td><td>8.3 ± 1.2</td><td>10.8</td></tr><tr><td>HESS J1507-622</td><td>Gaussian</td><td>319.79</td><td>-3.48</td><td>0.06</td><td>0.18 ± 0.017</td><td>2.99 ± 0.31</td><td>13.2 ± 1.4</td><td>17.0</td></tr><tr><td>HESS J1514-591</td><td>3-Gaussian</td><td>320.32</td><td>-1.19</td><td>0.03</td><td>0.14 ± 0.026</td><td>6.43 ± 0.21</td><td>28.4 ± 0.9</td><td>42.0</td></tr><tr><td>HESS J1534-571*</td><td>Shell</td><td>323.70</td><td>-1.02</td><td>–</td><td>0.40 ± 0.040</td><td>1.98 ± 0.23</td><td>8.7 ± 1.0</td><td>–</td></tr><tr><td>HESS J1554-550</td><td>Gaussian</td><td>327.16</td><td>-1.08</td><td>0.03</td><td>0.02 ± 0.009</td><td>0.36 ± 0.06</td><td>1.6 ± 0.3</td><td>9.1</td></tr><tr><td>HESS J1614-518*</td><td>Shell</td><td>331.47</td><td>-0.60</td><td>–</td><td>0.42 ± 0.010</td><td>5.87 ± 0.42</td><td>25.9 ± 1.9</td><td>–</td></tr><tr><td>HESS J1616-508</td><td>2-Gaussian</td><td>332.48</td><td>-0.17</td><td>0.12</td><td>0.23 ± 0.035</td><td>8.48 ± 0.44</td><td>37.4 ± 1.9</td><td>34.3</td></tr><tr><td>HESS J1626-490</td><td>Gaussian</td><td>334.82</td><td>-0.12</td><td>0.14</td><td>0.20 ± 0.035</td><td>1.65 ± 0.33</td><td>7.3 ± 1.5</td><td>8.4</td></tr><tr><td>HESS J1632-478</td><td>Gaussian</td><td>336.39</td><td>0.26</td><td>0.08</td><td>0.18 ± 0.020</td><td>2.93 ± 0.51</td><td>12.9 ± 2.3</td><td>14.8</td></tr><tr><td>HESS J1634-472</td><td>Gaussian</td><td>337.12</td><td>0.26</td><td>0.06</td><td>0.17 ± 0.013</td><td>2.90 ± 0.37</td><td>12.8 ± 1.6</td><td>17.8</td></tr><tr><td>HESS J1640-465</td><td>2-Gaussian</td><td>338.28</td><td>-0.04</td><td>0.05</td><td>0.11 ± 0.034</td><td>3.33 ± 0.19</td><td>14.7 ± 0.8</td><td>41.1</td></tr><tr><td>HESS J1641-463</td><td>Gaussian</td><td>338.52</td><td>0.08</td><td>0.05</td><td>0.04 ± 0.013</td><td>0.27 ± 0.06</td><td>1.2 ± 0.3</td><td>6.9</td></tr><tr><td>HESS J1646-458</td><td>Gaussian</td><td>339.33</td><td>-0.78</td><td>0.15</td><td>0.50 ± 0.030</td><td>5.48 ± 0.46</td><td>24.2 ± 2.0</td><td>18.6</td></tr><tr><td>HESS J1702-420</td><td>Gaussian</td><td>344.23</td><td>-0.19</td><td>0.08</td><td>0.20 ± 0.025</td><td>3.91 ± 0.65</td><td>17.3 ± 2.9</td><td>15.0</td></tr><tr><td>HESS J1708-410</td><td>Gaussian</td><td>345.67</td><td>-0.44</td><td>0.03</td><td>0.06 ± 0.006</td><td>0.88 ± 0.09</td><td>3.9 ± 0.4</td><td>17.0</td></tr><tr><td>HESS J1708-443</td><td>Gaussian</td><td>343.07</td><td>-2.32</td><td>0.14</td><td>0.28 ± 0.031</td><td>2.28 ± 0.32</td><td>10.1 ± 1.4</td><td>11.0</td></tr><tr><td>HESS J1713-381</td><td>Gaussian</td><td>348.62</td><td>0.38</td><td>0.05</td><td>0.09 ± 0.017</td><td>0.65 ± 0.13</td><td>2.9 ± 0.6</td><td>11.6</td></tr><tr><td>HESS J1713-397*</td><td>Shell</td><td>347.31</td><td>-0.46</td><td>–</td><td>0.50</td><td>16.88 ± 0.82</td><td>74.4 ± 3.6</td><td>–</td></tr><tr><td>HESS J1714-385</td><td>Gaussian</td><td>348.42</td><td>0.14</td><td>0.04</td><td>0.03 ± 0.011</td><td>0.25 ± 0.05</td><td>1.1 ± 0.2</td><td>8.6</td></tr><tr><td>HESS J1718-374*</td><td>Point-Like</td><td>349.72</td><td>0.17</td><td>–</td><td>–</td><td>0.12 ± 0.04</td><td>0.6 ± 0.2</td><td>–</td></tr><tr><td>HESS J1718-385</td><td>Gaussian</td><td>348.88</td><td>-0.48</td><td>0.06</td><td>0.12 ± 0.015</td><td>0.80 ± 0.14</td><td>3.5 ± 0.6</td><td>11.6</td></tr><tr><td>HESS J1729-345</td><td>Gaussian</td><td>353.39</td><td>-0.02</td><td>0.13</td><td>0.19 ± 0.031</td><td>0.86 ± 0.17</td><td>3.8 ± 0.8</td><td>8.4</td></tr><tr><td>HESS J1731-347*</td><td>Shell</td><td>353.54</td><td>-0.67</td><td>–</td><td>0.27 ± 0.020</td><td>2.01 ± 0.15</td><td>8.8 ± 0.6</td><td>–</td></tr><tr><td>HESS J1741-302*</td><td>Point-Like</td><td>358.28</td><td>0.05</td><td>–</td><td>–</td><td>0.16 ± 0.04</td><td>0.7 ± 0.2</td><td>–</td></tr><tr><td>HESS J1745-290*</td><td>Point-Like</td><td>359.94</td><td>-0.04</td><td>–</td><td>–</td><td>1.70 ± 0.08</td><td>7.5 ± 0.3</td><td>–</td></tr><tr><td>HESS J1745-303</td><td>Gaussian</td><td>358.64</td><td>-0.56</td><td>0.11</td><td>0.18 ± 0.020</td><td>0.94 ± 0.21</td><td>4.1 ± 0.9</td><td>13.7</td></tr><tr><td>HESS J1746-285*</td><td>Point-Like</td><td>0.14</td><td>-0.11</td><td>–</td><td>–</td><td>0.15 ± 0.05</td><td>0.7 ± 0.2</td><td>–</td></tr><tr><td>HESS J1746-308</td><td>Gaussian</td><td>358.45</td><td>-1.11</td><td>0.15</td><td>0.16 ± 0.036</td><td>0.68 ± 0.22</td><td>3.0 ± 1.0</td><td>8.7</td></tr><tr><td>HESS J1747-248</td><td>Gaussian</td><td>3.78</td><td>1.71</td><td>0.06</td><td>0.06 ± 0.012</td><td>0.29 ± 0.05</td><td>1.3 ± 0.2</td><td>8.1</td></tr><tr><td>HESS J1747-281*</td><td>Point-Like</td><td>0.87</td><td>0.08</td><td>–</td><td>–</td><td>0.60 ± 0.13</td><td>2.6 ± 0.6</td><td>–</td></tr><tr><td>HESS J1800-240</td><td>Gaussian</td><td>5.96</td><td>-0.42</td><td>0.13</td><td>0.32 ± 0.039</td><td>2.44 ± 0.35</td><td>10.8 ± 1.5</td><td>12.6</td></tr><tr><td>HESS J1801-233*</td><td>Gaussian</td><td>6.66</td><td>-0.27</td><td>–</td><td>0.17 ± 0.030</td><td>0.45 ± 0.10</td><td>2.0 ± 0.4</td><td>–</td></tr><tr><td>HESS J1804-216</td><td>2-Gaussian</td><td>8.38</td><td>-0.09</td><td>0.15</td><td>0.24 ± 0.034</td><td>5.88 ± 0.27</td><td>25.9 ± 1.2</td><td>34.2</td></tr><tr><td>HESS J1808-204</td><td>Gaussian</td><td>10.01</td><td>-0.24</td><td>0.07</td><td>0.06 ± 0.014</td><td>0.19 ± 0.04</td><td>0.8 ± 0.2</td><td>6.4</td></tr><tr><td>HESS J1809-193</td><td>3-Gaussian</td><td>11.11</td><td>-0.02</td><td>0.21</td><td>0.40 ± 0.048</td><td>5.27 ± 0.29</td><td>23.2 ± 1.3</td><td>26.6</td></tr></tbody></table>

**Notes.** This is a small excerpt of the information available in the FITS catalog. The data shown here correspond to the following catalog columns (described in Table A.2): *Source_Name*, *Spatial_Model*, *GLON*, *GLAT*, *Pos_Err_95*, *Size*, *Size_Err*, *Size UL*, *Flux_Map*, *Flux_Map_Err*, and *Sqrt_TS*. The values for sources indicated with an asterisk are taken from external references; see Table 1 for details.
<table><caption>Table A.7. continued.</caption><thead><tr><th rowspan="2">Name</th><th rowspan="2">Spatial model</th><th>GLON</th><th>GLAT</th><th>R<sub>95</sub></th><th>Size</th><th>F(&gt;1 TeV)</th><th>F(&gt;1 TeV)</th><th>√TS</th></tr><tr><th>deg</th><th>deg</th><th>deg</th><th>deg</th><th>10<sup>-12</sup> cm<sup>-2</sup> s<sup>-1</sup></th><th>% Crab</th></tr></thead><tbody><tr><td>HESS J1813-126</td><td>Gaussian</td><td>17.31</td><td>2.49</td><td>0.19</td><td>0.21 ± 0.032</td><td>1.08 ± 0.24</td><td>4.8 ± 1.1</td><td>6.1</td></tr><tr><td>HESS J1813-178</td><td>Gaussian</td><td>12.82</td><td>-0.03</td><td>0.02</td><td>0.05 ± 0.004</td><td>1.98 ± 0.15</td><td>8.7 ± 0.7</td><td>26.4</td></tr><tr><td>HESS J1818-154</td><td>Gaussian</td><td>15.41</td><td>0.16</td><td>0.04</td><td>0.00 ± 0.046</td><td>0.17 ± 0.04</td><td>0.7 ± 0.2</td><td>5.6</td></tr><tr><td>HESS J1825-137</td><td>3-Gaussian</td><td>17.53</td><td>-0.62</td><td>0.20</td><td>0.46 ± 0.032</td><td>18.41 ± 0.56</td><td>81.2 ± 2.5</td><td>76.5</td></tr><tr><td>HESS J1826-130</td><td>Gaussian</td><td>18.48</td><td>-0.39</td><td>0.10</td><td>0.15 ± 0.021</td><td>0.86 ± 0.17</td><td>3.8 ± 0.7</td><td>9.4</td></tr><tr><td>HESS J1826-148</td><td>Gaussian</td><td>16.88</td><td>-1.29</td><td>0.02</td><td>0.01 ± 0.004</td><td>1.28 ± 0.04</td><td>5.7 ± 0.2</td><td>58.1</td></tr><tr><td>HESS J1828-099</td><td>Gaussian</td><td>21.49</td><td>0.38</td><td>0.05</td><td>0.05 ± 0.011</td><td>0.43 ± 0.07</td><td>1.9 ± 0.3</td><td>8.9</td></tr><tr><td>HESS J1832-085</td><td>Gaussian</td><td>23.21</td><td>0.29</td><td>0.05</td><td>0.02 ± 0.012</td><td>0.21 ± 0.05</td><td>0.9 ± 0.2</td><td>5.9</td></tr><tr><td>HESS J1832-093</td><td>Gaussian</td><td>22.48</td><td>-0.16</td><td>0.03</td><td>0.00 ± 0.012</td><td>0.17 ± 0.03</td><td>0.8 ± 0.1</td><td>6.8</td></tr><tr><td>HESS J1833-105</td><td>Gaussian</td><td>21.50</td><td>-0.90</td><td>0.03</td><td>0.02 ± 0.017</td><td>0.39 ± 0.07</td><td>1.7 ± 0.3</td><td>11.4</td></tr><tr><td>HESS J1834-087</td><td>2-Gaussian</td><td>23.26</td><td>-0.33</td><td>0.06</td><td>0.21 ± 0.037</td><td>3.34 ± 0.24</td><td>14.7 ± 1.1</td><td>21.0</td></tr><tr><td>HESS J1837-069</td><td>3-Gaussian</td><td>25.15</td><td>-0.09</td><td>0.05</td><td>0.36 ± 0.031</td><td>12.05 ± 0.45</td><td>53.1 ± 2.0</td><td>41.5</td></tr><tr><td>HESS J1841-055</td><td>2-Gaussian</td><td>26.71</td><td>-0.23</td><td>0.17</td><td>0.41 ± 0.033</td><td>10.16 ± 0.42</td><td>44.8 ± 1.9</td><td>33.9</td></tr><tr><td>HESS J1843-033</td><td>2-Gaussian</td><td>28.90</td><td>0.07</td><td>0.20</td><td>0.24 ± 0.063</td><td>2.88 ± 0.30</td><td>12.7 ± 1.3</td><td>16.0</td></tr><tr><td>HESS J1844-030</td><td>Gaussian</td><td>29.41</td><td>0.09</td><td>0.04</td><td>0.02 ± 0.013</td><td>0.26 ± 0.05</td><td>1.1 ± 0.2</td><td>7.3</td></tr><tr><td>HESS J1846-029</td><td>Gaussian</td><td>29.71</td><td>-0.24</td><td>0.03</td><td>0.01 ± 0.013</td><td>0.45 ± 0.05</td><td>2.0 ± 0.2</td><td>13.8</td></tr><tr><td>HESS J1848-018</td><td>Gaussian</td><td>30.92</td><td>-0.21</td><td>0.12</td><td>0.25 ± 0.032</td><td>1.74 ± 0.35</td><td>7.7 ± 1.6</td><td>12.0</td></tr><tr><td>HESS J1849-000</td><td>Gaussian</td><td>32.61</td><td>0.53</td><td>0.06</td><td>0.09 ± 0.015</td><td>0.53 ± 0.09</td><td>2.3 ± 0.4</td><td>9.1</td></tr><tr><td>HESS J1852-000</td><td>Gaussian</td><td>33.11</td><td>-0.13</td><td>0.18</td><td>0.28 ± 0.042</td><td>1.30 ± 0.25</td><td>5.7 ± 1.1</td><td>9.0</td></tr><tr><td>HESS J1857+026</td><td>2-Gaussian</td><td>36.06</td><td>-0.06</td><td>0.10</td><td>0.26 ± 0.056</td><td>3.77 ± 0.40</td><td>16.6 ± 1.8</td><td>16.8</td></tr><tr><td>HESS J1858+020</td><td>Gaussian</td><td>35.54</td><td>-0.58</td><td>0.07</td><td>0.08 ± 0.016</td><td>0.53 ± 0.11</td><td>2.3 ± 0.5</td><td>8.4</td></tr><tr><td>HESS J1908+063</td><td>Gaussian</td><td>40.55</td><td>-0.84</td><td>0.13</td><td>0.49 ± 0.027</td><td>6.53 ± 0.50</td><td>28.8 ± 2.2</td><td>19.0</td></tr><tr><td>HESS J1911+090*</td><td>Point-Like</td><td>43.26</td><td>-0.19</td><td>-</td><td>-</td><td>0.15 ± 0.03</td><td>0.6 ± 0.1</td><td>-</td></tr><tr><td>HESS J1912+101*</td><td>Shell</td><td>44.46</td><td>-0.13</td><td>-</td><td>0.49 ± 0.040</td><td>2.49 ± 0.35</td><td>11.0 ± 1.5</td><td>-</td></tr><tr><td>HESS J1923+141</td><td>Gaussian</td><td>49.08</td><td>-0.40</td><td>0.10</td><td>0.12 ± 0.019</td><td>0.78 ± 0.15</td><td>3.5 ± 0.7</td><td>7.3</td></tr><tr><td>HESS J1930+188</td><td>Gaussian</td><td>54.06</td><td>0.27</td><td>0.05</td><td>0.02 ± 0.025</td><td>0.29 ± 0.09</td><td>1.3 ± 0.4</td><td>5.8</td></tr><tr><td>HESS J1943+213</td><td>Gaussian</td><td>57.78</td><td>-1.30</td><td>0.05</td><td>0.03 ± 0.022</td><td>0.32 ± 0.10</td><td>1.4 ± 0.4</td><td>5.9</td></tr></tbody></table>
<table><caption>**Table A.8.** HGPS source catalog – summary of spectral measurements.</caption><thead><tr><th rowspan="2">Name</th><th rowspan="2">R<sub>spec</sub></th><th rowspan="2">E<sub>min</sub></th><th rowspan="2">F(&gt;1 TeV)</th><th rowspan="2">Γ</th><th rowspan="2">λ</th><th colspan="2">Contain.</th><th colspan="2">CF</th></tr><tr><th>TeV<sup>-1</sup></th><th>%</th><th>%</th></tr><tr><th></th><th>deg</th><th>TeV</th><th>10<sup>-12</sup> cm<sup>-2</sup> s<sup>-1</sup></th><th></th><th></th><th></th><th></th><th></th><th></th></tr></thead><tbody><tr><td>HESS J0835-455</td><td>0.50</td><td>0.3</td><td>17.43 ± 1.40</td><td>1.35 ± 0.08</td><td>0.08 ± 0.01</td><td>37</td><td>0</td><td>271.4</td><td></td></tr><tr><td>HESS J0852-463*</td><td>1.00</td><td>0.3</td><td>23.39 ± 2.35</td><td>1.81 ± 0.08</td><td>0.15 ± 0.03</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1018-589 A</td><td>0.15</td><td>0.4</td><td>0.21 ± 0.03</td><td>2.24 ± 0.13</td><td>–</td><td>92</td><td>42</td><td>63.5</td><td></td></tr><tr><td>HESS J1018-589 B</td><td>0.25</td><td>0.5</td><td>0.70 ± 0.09</td><td>2.20 ± 0.09</td><td>–</td><td>70</td><td>32</td><td>96.8</td><td></td></tr><tr><td>HESS J1023-575</td><td>0.27</td><td>0.4</td><td>2.41 ± 0.13</td><td>2.36 ± 0.05</td><td>–</td><td>70</td><td>5</td><td>135.5</td><td></td></tr><tr><td>HESS J1026-582</td><td>0.22</td><td>0.5</td><td>0.66 ± 0.09</td><td>1.81 ± 0.10</td><td>–</td><td>70</td><td>11</td><td>126.9</td><td></td></tr><tr><td>HESS J1119-614</td><td>0.18</td><td>0.4</td><td>0.92 ± 0.09</td><td>2.64 ± 0.12</td><td>–</td><td>70</td><td>4</td><td>137.9</td><td></td></tr><tr><td>HESS J1302-638</td><td>0.15</td><td>0.4</td><td>0.39 ± 0.03</td><td>2.59 ± 0.09</td><td>–</td><td>90</td><td>40</td><td>67.4</td><td></td></tr><tr><td>HESS J1303-631</td><td>0.29</td><td>0.4</td><td>5.21 ± 0.35</td><td>2.04 ± 0.06</td><td>0.07 ± 0.01</td><td>70</td><td>5</td><td>136.2</td><td></td></tr><tr><td>HESS J1356-645</td><td>0.37</td><td>0.5</td><td>4.39 ± 0.39</td><td>2.20 ± 0.08</td><td>–</td><td>70</td><td>0</td><td>142.8</td><td></td></tr><tr><td>HESS J1418-609</td><td>0.19</td><td>0.4</td><td>2.69 ± 0.15</td><td>2.26 ± 0.05</td><td>–</td><td>70</td><td>6</td><td>134.7</td><td></td></tr><tr><td>HESS J1420-607</td><td>0.15</td><td>0.4</td><td>2.77 ± 0.15</td><td>2.20 ± 0.05</td><td>–</td><td>70</td><td>4</td><td>138.5</td><td></td></tr><tr><td>HESS J1427-608</td><td>0.15</td><td>0.4</td><td>0.48 ± 0.09</td><td>2.85 ± 0.22</td><td>–</td><td>84</td><td>5</td><td>113.3</td><td></td></tr><tr><td>HESS J1442-624*</td><td>0.41</td><td>0.4</td><td>2.44 ± 0.67</td><td>1.59 ± 0.22</td><td>0.29 ± 0.10</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1457-593</td><td>0.50</td><td>0.5</td><td>4.31 ± 0.56</td><td>2.52 ± 0.14</td><td>–</td><td>67</td><td>10</td><td>135.1</td><td></td></tr><tr><td>HESS J1458-608</td><td>0.50</td><td>0.5</td><td>1.40 ± 0.35</td><td>1.81 ± 0.14</td><td>–</td><td>58</td><td>1</td><td>170.2</td><td></td></tr><tr><td>HESS J1503-582</td><td>0.45</td><td>0.4</td><td>3.07 ± 0.24</td><td>2.68 ± 0.08</td><td>–</td><td>70</td><td>8</td><td>131.1</td><td></td></tr><tr><td>HESS J1507-622</td><td>0.29</td><td>0.5</td><td>2.60 ± 0.21</td><td>2.22 ± 0.07</td><td>–</td><td>70</td><td>0</td><td>142.9</td><td></td></tr><tr><td>HESS J1514-591</td><td>0.22</td><td>0.4</td><td>5.72 ± 0.42</td><td>2.05 ± 0.06</td><td>0.05 ± 0.01</td><td>70</td><td>0</td><td>142.8</td><td></td></tr><tr><td>HESS J1534-571*</td><td>0.47</td><td>0.4</td><td>1.98 ± 0.23</td><td>2.51 ± 0.09</td><td>–</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1554-550</td><td>0.15</td><td>0.4</td><td>0.29 ± 0.06</td><td>2.19 ± 0.17</td><td>–</td><td>92</td><td>0</td><td>108.6</td><td></td></tr><tr><td>HESS J1614-518*</td><td>0.49</td><td>0.3</td><td>5.87 ± 0.42</td><td>2.42 ± 0.06</td><td>–</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1616-508</td><td>0.36</td><td>0.3</td><td>7.99 ± 0.55</td><td>2.32 ± 0.06</td><td>–</td><td>70</td><td>2</td><td>139.9</td><td></td></tr><tr><td>HESS J1626-490</td><td>0.32</td><td>0.3</td><td>2.13 ± 0.26</td><td>2.47 ± 0.11</td><td>–</td><td>70</td><td>11</td><td>126.9</td><td></td></tr><tr><td>HESS J1632-478</td><td>0.30</td><td>0.3</td><td>2.32 ± 0.16</td><td>2.52 ± 0.06</td><td>–</td><td>70</td><td>34</td><td>93.9</td><td></td></tr><tr><td>HESS J1634-472</td><td>0.28</td><td>0.3</td><td>2.87 ± 0.15</td><td>2.31 ± 0.05</td><td>–</td><td>70</td><td>31</td><td>98.8</td><td></td></tr><tr><td>HESS J1640-465</td><td>0.16</td><td>0.3</td><td>2.84 ± 0.73</td><td>2.12 ± 0.13</td><td>0.24 ± 0.09</td><td>70</td><td>4</td><td>137.6</td><td></td></tr><tr><td>HESS J1641-463</td><td>0.15</td><td>0.3</td><td>0.22 ± 0.03</td><td>2.47 ± 0.11</td><td>–</td><td>90</td><td>58</td><td>47.4</td><td></td></tr><tr><td>HESS J1646-458</td><td>0.50</td><td>0.3</td><td>5.81 ± 0.73</td><td>2.54 ± 0.13</td><td>–</td><td>39</td><td>2</td><td>254.4</td><td></td></tr><tr><td>HESS J1702-420</td><td>0.32</td><td>0.2</td><td>4.45 ± 0.36</td><td>2.09 ± 0.07</td><td>–</td><td>70</td><td>14</td><td>122.9</td><td></td></tr><tr><td>HESS J1708-410</td><td>0.15</td><td>0.2</td><td>0.65 ± 0.05</td><td>2.54 ± 0.07</td><td>–</td><td>81</td><td>9</td><td>112.8</td><td></td></tr><tr><td>HESS J1708-443</td><td>0.44</td><td>0.2</td><td>3.32 ± 0.37</td><td>2.17 ± 0.08</td><td>–</td><td>70</td><td>0</td><td>142.9</td><td></td></tr><tr><td>HESS J1713-381</td><td>0.16</td><td>0.2</td><td>0.52 ± 0.07</td><td>2.74 ± 0.12</td><td>–</td><td>70</td><td>15</td><td>121.4</td><td></td></tr><tr><td>HESS J1713-397*</td><td>0.60</td><td>0.2</td><td>16.88 ± 0.82</td><td>2.06 ± 0.02</td><td>0.08 ± 0.01</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1714-385</td><td>0.15</td><td>0.2</td><td>0.21 ± 0.03</td><td>2.52 ± 0.12</td><td>–</td><td>91</td><td>47</td><td>57.9</td><td></td></tr><tr><td>HESS J1718-374*</td><td>0.10</td><td>0.2</td><td>0.12 ± 0.04</td><td>2.80 ± 0.27</td><td>–</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1718-385</td><td>0.20</td><td>0.2</td><td>0.62 ± 0.14</td><td>0.98 ± 0.22</td><td>0.09 ± 0.03</td><td>70</td><td>23</td><td>110.4</td><td></td></tr><tr><td>HESS J1729-345</td><td>0.30</td><td>0.2</td><td>0.82 ± 0.09</td><td>2.43 ± 0.09</td><td>–</td><td>70</td><td>25</td><td>108.0</td><td></td></tr><tr><td>HESS J1731-347*</td><td>0.30</td><td>0.2</td><td>2.01 ± 0.15</td><td>2.32 ± 0.06</td><td>–</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1741-302*</td><td>0.10</td><td>0.4</td><td>0.16 ± 0.04</td><td>2.30 ± 0.20</td><td>–</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1745-290*</td><td>0.10</td><td>–</td><td>1.70 ± 0.08</td><td>2.14 ± 0.02</td><td>0.09 ± 0.02</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1745-303</td><td>0.29</td><td>0.2</td><td>1.09 ± 0.08</td><td>2.57 ± 0.06</td><td>–</td><td>70</td><td>30</td><td>99.6</td><td></td></tr><tr><td>HESS J1746-285*</td><td>0.09</td><td>0.3</td><td>0.15 ± 0.05</td><td>2.17 ± 0.24</td><td>–</td><td>–</td><td>–</td><td>–</td><td></td></tr><tr><td>HESS J1746-308</td><td>0.26</td><td>0.2</td><td>0.30 ± 0.09</td><td>3.27 ± 0.22</td><td>–</td><td>70</td><td>23</td><td>110.2</td><td></td></tr><tr><td>HESS J1747-248</td><td>0.15</td><td>0.2</td><td>0.27 ± 0.04</td><td>2.36 ± 0.14</td><td>–</td><td>83</td><td>0</td><td>120.5</td><td></td></tr></tbody></table>

**Notes.** This is a small excerpt of the information available in the FITS catalog. The data shown here correspond to the following catalog columns (described in Table A.2): *Source_Name*, *RSpec*, *Energy_Range_Spec_Lo*, *Flux_Spec_Int_1TeV* (Flux_Map for extern sources), *Index_Spec_PL*, *Index_Spec_PL_Err* (for PL spectrum sources), *Index_Spec_ECPL*, *Index_Spec_ECPL_Err*, *Lambda_Spec_ECPL*, *Lambda_Spec_ECPL_Err* (for ECPL spectrum sources), *Containment_RSpec*, *Contamination_RSpec* and *Flux_Correction_RSpec>To_Total*. The values for sources indicated with an asterisk are taken from external references, see Table 1 for details.
<table><caption>Table A.8. continued.</caption><thead><tr><th rowspan="2">Name</th><th rowspan="2">R<sub>spec</sub></th><th rowspan="2">E<sub>min</sub></th><th rowspan="2">F(&gt;1 TeV)</th><th rowspan="2">Γ</th><th rowspan="2">λ</th><th>Contain.</th><th>Contam.</th><th>CF</th></tr><tr><th>deg</th><th>TeV</th><th>10<sup>-12</sup> cm<sup>-2</sup> s<sup>-1</sup></th><th>TeV<sup>-1</sup></th><th>%</th><th>%</th></tr></thead><tbody><tr><td>HESS J1747-281*</td><td>0.10</td><td>0.3</td><td>0.60 ± 0.13</td><td>2.40 ± 0.11</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>HESS J1800-240</td><td>0.50</td><td>0.2</td><td>2.90 ± 0.31</td><td>2.47 ± 0.09</td><td>–</td><td>70</td><td>17</td><td>118.9</td></tr><tr><td>HESS J1801-233*</td><td>0.20</td><td>0.3</td><td>0.45 ± 0.10</td><td>2.66 ± 0.27</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>HESS J1804-216</td><td>0.38</td><td>0.2</td><td>5.12 ± 0.23</td><td>2.69 ± 0.04</td><td>–</td><td>70</td><td>8</td><td>131.6</td></tr><tr><td>HESS J1808-204</td><td>0.15</td><td>0.2</td><td>0.19 ± 0.03</td><td>2.19 ± 0.14</td><td>–</td><td>85</td><td>27</td><td>86.1</td></tr><tr><td>HESS J1809-193</td><td>0.50</td><td>0.2</td><td>5.37 ± 0.45</td><td>2.38 ± 0.07</td><td>–</td><td>54</td><td>16</td><td>154.2</td></tr><tr><td>HESS J1813-126</td><td>0.34</td><td>0.2</td><td>1.04 ± 0.21</td><td>1.99 ± 0.14</td><td>–</td><td>70</td><td>0</td><td>143.6</td></tr><tr><td>HESS J1813-178</td><td>0.15</td><td>0.2</td><td>2.12 ± 0.40</td><td>1.64 ± 0.12</td><td>0.14 ± 0.04</td><td>89</td><td>14</td><td>96.6</td></tr><tr><td>HESS J1818-154</td><td>0.15</td><td>0.2</td><td>0.23 ± 0.05</td><td>2.21 ± 0.15</td><td>–</td><td>95</td><td>29</td><td>74.6</td></tr><tr><td>HESS J1825-137</td><td>0.50</td><td>0.2</td><td>19.15 ± 1.85</td><td>2.15 ± 0.06</td><td>0.07 ± 0.02</td><td>47</td><td>3</td><td>203.6</td></tr><tr><td>HESS J1826-130</td><td>0.25</td><td>0.2</td><td>1.14 ± 0.16</td><td>2.04 ± 0.10</td><td>–</td><td>70</td><td>41</td><td>84.4</td></tr><tr><td>HESS J1826-148</td><td>0.15</td><td>0.2</td><td>0.84 ± 0.08</td><td>2.32 ± 0.07</td><td>–</td><td>95</td><td>10</td><td>94.5</td></tr><tr><td>HESS J1828-099</td><td>0.15</td><td>0.2</td><td>0.38 ± 0.05</td><td>2.25 ± 0.12</td><td>–</td><td>89</td><td>11</td><td>100.3</td></tr><tr><td>HESS J1832-085</td><td>0.15</td><td>0.2</td><td>0.23 ± 0.04</td><td>2.38 ± 0.14</td><td>–</td><td>94</td><td>27</td><td>77.7</td></tr><tr><td>HESS J1832-093</td><td>0.15</td><td>0.2</td><td>0.16 ± 0.04</td><td>2.54 ± 0.22</td><td>–</td><td>95</td><td>25</td><td>78.9</td></tr><tr><td>HESS J1833-105</td><td>0.15</td><td>0.2</td><td>0.26 ± 0.06</td><td>2.42 ± 0.19</td><td>–</td><td>94</td><td>2</td><td>104.6</td></tr><tr><td>HESS J1834-087</td><td>0.34</td><td>0.2</td><td>2.47 ± 0.22</td><td>2.61 ± 0.07</td><td>–</td><td>70</td><td>8</td><td>131.2</td></tr><tr><td>HESS J1837-069</td><td>0.50</td><td>0.2</td><td>11.55 ± 0.49</td><td>2.54 ± 0.04</td><td>–</td><td>63</td><td>8</td><td>145.6</td></tr><tr><td>HESS J1841-055</td><td>0.50</td><td>0.2</td><td>11.58 ± 1.36</td><td>2.21 ± 0.07</td><td>0.09 ± 0.03</td><td>51</td><td>10</td><td>178.3</td></tr><tr><td>HESS J1843-033</td><td>0.38</td><td>0.2</td><td>3.04 ± 0.20</td><td>2.15 ± 0.05</td><td>–</td><td>70</td><td>15</td><td>121.0</td></tr><tr><td>HESS J1844-030</td><td>0.15</td><td>0.2</td><td>0.28 ± 0.04</td><td>2.48 ± 0.12</td><td>–</td><td>94</td><td>28</td><td>77.0</td></tr><tr><td>HESS J1846-029</td><td>0.15</td><td>0.2</td><td>0.48 ± 0.05</td><td>2.41 ± 0.09</td><td>–</td><td>94</td><td>10</td><td>95.8</td></tr><tr><td>HESS J1848-018</td><td>0.39</td><td>0.3</td><td>1.11 ± 0.15</td><td>2.57 ± 0.11</td><td>–</td><td>70</td><td>26</td><td>105.9</td></tr><tr><td>HESS J1849-000</td><td>0.16</td><td>0.3</td><td>0.58 ± 0.07</td><td>1.97 ± 0.09</td><td>–</td><td>70</td><td>9</td><td>129.9</td></tr><tr><td>HESS J1852-000</td><td>0.44</td><td>0.3</td><td>1.21 ± 0.15</td><td>2.17 ± 0.10</td><td>–</td><td>70</td><td>25</td><td>106.8</td></tr><tr><td>HESS J1857+026</td><td>0.41</td><td>0.3</td><td>4.00 ± 0.29</td><td>2.57 ± 0.06</td><td>–</td><td>70</td><td>11</td><td>127.6</td></tr><tr><td>HESS J1858+020</td><td>0.15</td><td>0.3</td><td>0.47 ± 0.06</td><td>2.39 ± 0.12</td><td>–</td><td>72</td><td>14</td><td>120.6</td></tr><tr><td>HESS J1908+063</td><td>0.50</td><td>0.3</td><td>8.35 ± 0.57</td><td>2.26 ± 0.06</td><td>–</td><td>41</td><td>2</td><td>240.9</td></tr><tr><td>HESS J1911+090*</td><td>0.10</td><td>0.3</td><td>0.15 ± 0.03</td><td>3.14 ± 0.24</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>HESS J1912+101*</td><td>0.56</td><td>0.7</td><td>2.49 ± 0.35</td><td>2.56 ± 0.09</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>HESS J1923+141</td><td>0.21</td><td>0.4</td><td>0.69 ± 0.11</td><td>2.55 ± 0.17</td><td>–</td><td>70</td><td>3</td><td>138.7</td></tr><tr><td>HESS J1930+188</td><td>0.15</td><td>0.5</td><td>0.32 ± 0.07</td><td>2.59 ± 0.26</td><td>–</td><td>92</td><td>8</td><td>100.3</td></tr><tr><td>HESS J1943+213</td><td>0.15</td><td>0.6</td><td>0.39 ± 0.08</td><td>2.83 ± 0.22</td><td>–</td><td>91</td><td>1</td><td>109.0</td></tr></tbody></table>
<table><caption>**Table A.9.** HGPS source associations (see Sect. 5.1).</caption><thead><tr><th>H.E.S.S. source</th><th>Association</th></tr></thead><tbody><tr><td>HESS J0835-455</td><td>G263.9-3.3 (COMP)<br>2FHL J0835.3-4511 (2FHL)<br>3FGL J0835.3-4510 (3FGL)<br>B0833-45 (PSR)</td></tr><tr><td>HESS J0852-463</td><td>G266.2-1.2 (SNR)<br>2FHL J0852.8-4631e (2FHL)<br>3FGL J0852.7-4631e (3FGL)<br>J0855-4644 (PSR)<br>G267.0-1.0 (PWN)</td></tr><tr><td>HESS J1018-589 A</td><td>3FGL J1018.9-5856 (3FGL)<br>G284.3-1.8 (SNR)</td></tr><tr><td>HESS J1018-589 B</td><td>G284.3-1.8 (SNR)<br>3FGL J1018.9-5856 (3FGL)<br>J1016-5857 (PSR)<br>G284.0-1.8 (PWN)<br>3FGL J1016.3-5858 (3FGL)</td></tr><tr><td>HESS J1023-575</td><td>3FGL J1023.1-5745 (3FGL)<br>J1023-5746 (PSR)<br>Westerlund 2 (EXTRA)<br>2FHL J1022.0-5750 (2FHL)<br>3FGL J1024.3-5757 (3FGL)</td></tr><tr><td>HESS J1026-582</td><td>G285.1-0.5 (PWN)<br>J1028-5819 (PSR)</td></tr><tr><td>HESS J1119-614</td><td>3FGL J1119.1-6127 (3FGL)<br>J1119-6127 (PSR)<br>G292.2-0.5 (COMP)</td></tr><tr><td>HESS J1302-638</td><td>B1259-63 (PSR)</td></tr><tr><td>HESS J1303-631</td><td>2FHL J1303.4-6312e (2FHL)<br>3FGL J1303.0-6312e (3FGL)<br>J1301-6305 (PSR)<br>J1301-6310 (PSR)<br>G304.1-0.2 (PWN)</td></tr><tr><td>HESS J1356-645</td><td>3FGL J1356.6-6428 (3FGL)<br>G309.8-2.6 (PWN)<br>J1357-6429 (PSR)<br>2FHL J1355.1-6420e (2FHL)</td></tr><tr><td>HESS J1418-609</td><td>3FGL J1418.6-6058 (3FGL)<br>G313.3+0.1 (PWN)<br>J1418-6058 (PSR)</td></tr><tr><td>HESS J1420-607</td><td>G313.6+0.3 (PWN)<br>J1420-6048 (PSR)<br>3FGL J1420.0-6048 (3FGL)<br>2FHL J1419.3-6047e (2FHL)</td></tr><tr><td>HESS J1427-608</td><td>Suzaku J1427-6051 (EXTRA)</td></tr><tr><td>HESS J1442-624</td><td>G315.4-2.3 (SNR)<br>2FHL J1443.2-6221e (2FHL)</td></tr><tr><td>HESS J1457-593</td><td>–</td></tr></tbody></table>

<table><caption>**Table A.9.** continued.</caption><thead><tr><th>H.E.S.S. source</th><th>Association</th></tr></thead><tbody><tr><td>HESS J1458-608</td><td>J1459-6053 (PSR)<br>3FGL J1459.4-6053 (3FGL)<br>3FGL J1456.7-6046 (3FGL)</td></tr><tr><td>HESS J1503-582</td><td>3FGL J1503.5-5801 (3FGL)<br>2FHL J1505.1-5808 (2FHL)</td></tr><tr><td>HESS J1507-622</td><td>3FGL J1506.6-6219 (3FGL)<br>CXOU J150706.0-621443 (EXTRA)<br>2FHL J1507.4-6213 (2FHL)</td></tr><tr><td>HESS J1514-591</td><td>B1509-58 (PSR)<br>3FGL J1513.9-5908 (3FGL)<br>G320.4-1.2 (COMP)<br>3FGL J1514.0-5915e (3FGL)<br>2FHL J1514.0-5915e (2FHL)</td></tr><tr><td>HESS J1534-571</td><td>G323.7-1.0 (SNR)</td></tr><tr><td>HESS J1554-550</td><td>G327.1-1.1 (COMP)</td></tr><tr><td>HESS J1614-518</td><td>Suzaku J1614-5141 (EXTRA)<br>2FHL J1615.3-5146e (2FHL)<br>3FGL J1615.3-5146e (3FGL)</td></tr><tr><td>HESS J1616-508</td><td>J1617-5055 (PSR)<br>G332.5-0.3 (PWN)<br>2FHL J1616.2-5054e (2FHL)<br>3FGL J1616.2-5054e (3FGL)<br>G332.4-0.4 (SNR)<br>G332.4+0.1 (SNR)</td></tr><tr><td>HESS J1626-490</td><td>3FGL J1626.2-4911 (3FGL)</td></tr><tr><td>HESS J1632-478</td><td>G336.4+0.2 (PWN)<br>2FHL J1633.5-4746e (2FHL)<br>3FGL J1633.0-4746e (3FGL)<br>J1632-4757 (PSR)</td></tr><tr><td>HESS J1634-472</td><td>G337.2+0.1 (COMP)<br>3FGL J1636.2-4709c (3FGL)</td></tr><tr><td>HESS J1640-465</td><td>2FHL J1640.6-4632 (2FHL)<br>3FGL J1640.4-4634c (3FGL)<br>J1640-4631 (PSR)<br>G338.3-0.0 (COMP)</td></tr><tr><td>HESS J1641-463</td><td>G338.5+0.1 (SNR)<br>3FGL J1641.1-4619c (3FGL)</td></tr><tr><td>HESS J1646-458</td><td>3FGL J1648.3-4611 (3FGL)<br>J1648-4611 (PSR)<br>3FGL J1650.3-4600 (3FGL)</td></tr><tr><td>HESS J1702-420</td><td>–</td></tr><tr><td>HESS J1708-410</td><td>–</td></tr><tr><td>HESS J1708-443</td><td>G343.1-2.3 (COMP)<br>B1706-44 (PSR)<br>3FGL J1709.7-4429 (3FGL)</td></tr><tr><td>HESS J1713-381</td><td>G348.7+0.3 (SNR)<br>CXOU J171405.7-381031 (EXTRA)<br>J1714-3810 (PSR)</td></tr></tbody></table>
<table><caption>Table A.9. continued.</caption><thead><tr><th>H.E.S.S. source</th><th>Association</th></tr></thead><tbody><tr><td>HESS J1713-397</td><td>2FHL J1713.5-3945e (2FHL)<br>3FGL J1713.5-3945e (3FGL)<br>G347.3-0.5 (SNR)<br>2FHL J1714.1-4012 (2FHL)</td></tr><tr><td>HESS J1714-385</td><td>3FGL J1714.5-3832 (3FGL)<br>G348.5+0.1 (COMP)</td></tr><tr><td>HESS J1718-374</td><td>G349.7+0.2 (SNR)<br>3FGL J1718.0-3726 (3FGL)</td></tr><tr><td>HESS J1718-385</td><td>3FGL J1718.1-3825 (3FGL)<br>G348.9-0.4 (PWN)<br>J1718-3825 (PSR)</td></tr><tr><td>HESS J1729-345</td><td>-</td></tr><tr><td>HESS J1731-347</td><td>G353.6-0.7 (SNR)</td></tr><tr><td>HESS J1741-302</td><td>-</td></tr><tr><td>HESS J1745-290</td><td>Sgr A* (EXTRA)<br>J1745-2900 (PSR)<br>G359.9-0.0 (PWN)<br>2FHL J1745.7-2900 (2FHL)<br>3FGL J1745.6-2859c (3FGL)<br>G0.0+0.0 (COMP)<br>3FGL J1745.3-2903c (3FGL)</td></tr><tr><td>HESS J1745-303</td><td>3FGL J1745.1-3011 (3FGL)<br>2FHL J1745.1-3035 (2FHL)</td></tr><tr><td>HESS J1746-285</td><td>3FGL J1746.3-2851c (3FGL)<br>G0.1-0.1 (COMP)<br>J1746-2850 (PSR)</td></tr><tr><td>HESS J1746-308</td><td>G358.5-0.9 (SNR)<br>B1742-30 (PSR)</td></tr><tr><td>HESS J1747-248</td><td>3FGL J1748.0-2447 (3FGL)<br>Terzan 5 (EXTRA)</td></tr><tr><td>HESS J1747-281</td><td>J1747-2809 (PSR)<br>G0.9+0.1 (COMP)</td></tr><tr><td>HESS J1800-240</td><td>3FGL J1800.8-2402 (3FGL)<br>2FHL J1801.7-2358 (2FHL)<br>3FGL J1758.8-2402 (3FGL)<br>G5.7-0.1 (SNR)</td></tr><tr><td>HESS J1801-233</td><td>2FHL J1801.3-2326e (2FHL)<br>3FGL J1801.3-2326e (3FGL)<br>W28 (EXTRA)</td></tr><tr><td>HESS J1804-216</td><td>G8.3-0.0 (SNR)<br>B1800-21 (PSR)<br>3FGL J1805.6-2136e (3FGL)<br>2FHL J1805.6-2136e (2FHL)<br>G8.7-0.1 (COMP)<br>J1803-2149 (PSR)<br>3FGL J1803.1-2147 (3FGL)</td></tr><tr><td>HESS J1808-204</td><td>J1808-2024 (PSR)<br>SGR 1806-20 (EXTRA)<br>1806-20 star cluster (EXTRA)</td></tr></tbody></table>

<table><caption>Table A.9. continued.</caption><thead><tr><th>H.E.S.S. source</th><th>Association</th></tr></thead><tbody><tr><td>HESS J1809-193</td><td>G11.0-0.0 (SNR)<br>J1809-1917 (PSR)<br>G11.1+0.1 (COMP)<br>3FGL J1810.1-1910 (3FGL)<br>G11.4-0.1 (SNR)<br>3FGL J1811.3-1927c (3FGL)<br>G11.2-0.3 (COMP)<br>J1811-1925 (PSR)</td></tr><tr><td>HESS J1813-126</td><td>J1813-1246 (PSR)<br>3FGL J1813.4-1246 (3FGL)</td></tr><tr><td>HESS J1813-178</td><td>J1813-1749 (PSR)<br>G12.8-0.0 (COMP)<br>G12.7-0.0 (SNR)</td></tr><tr><td>HESS J1818-154</td><td>G15.4+0.1 (COMP)</td></tr><tr><td>HESS J1825-137</td><td>3FGL J1824.5-1351e (3FGL)<br>2FHL J1824.5-1350e (2FHL)<br>G18.0-0.7 (PWN)<br>B1823-13 (PSR)</td></tr><tr><td>HESS J1826-130</td><td>G18.5-0.4 (PWN)<br>J1826-1256 (PSR)<br>3FGL J1826.1-1256 (3FGL)<br>G18.6-0.2 (SNR)</td></tr><tr><td>HESS J1826-148</td><td>LS 5039 (EXTRA)<br>3FGL J1826.2-1450 (3FGL)<br>2FHL J1826.3-1450 (2FHL)</td></tr><tr><td>HESS J1828-099</td><td>-</td></tr><tr><td>HESS J1832-085</td><td>-</td></tr><tr><td>HESS J1832-093</td><td>XMMU J183245-0921539 (EXTRA)</td></tr><tr><td>HESS J1833-105</td><td>G21.5-0.9 (COMP)<br>J1833-1034 (PSR)<br>3FGL J1833.5-1033 (3FGL)</td></tr><tr><td>HESS J1834-087</td><td>J1834-0845 (PSR)<br>G23.3-0.3 (COMP)<br>2FHL J1834.5-0846e (2FHL)<br>3FGL J1834.5-0841 (3FGL)</td></tr><tr><td>HESS J1837-069</td><td>J1838-0655 (PSR)<br>2FHL J1836.5-0655e (2FHL)<br>3FGL J1836.5-0655e (3FGL)<br>2FHL J1837.4-0717 (2FHL)<br>3FGL J1837.6-0717 (3FGL)<br>G25.2+0.3 (PWN)<br>3FGL J1838.9-0646 (3FGL)</td></tr><tr><td>HESS J1841-055</td><td>2FHL J1840.9-0532e (2FHL)<br>3FGL J1840.9-0532e (3FGL)<br>G26.6-0.1 (PWN)<br>J1841-0524 (PSR)<br>3FGL J1839.3-0552 (3FGL)<br>J1838-0537 (PSR)<br>3FGL J1838.9-0537 (3FGL)</td></tr></tbody></table>
<table><caption>Table A.9. continued.</caption><thead><tr><th>H.E.S.S. source</th><th>Association</th></tr></thead><tbody><tr><td>HESS J1843-033</td><td>3FGL J1843.7-0322 (3FGL)<br>3FGL J1844.3-0344 (3FGL)<br>G28.6-0.1 (SNR)</td></tr><tr><td>HESS J1844-030</td><td>PMN J1844-0306 (EXTRA)<br>G29.4+0.1 (COMP)</td></tr><tr><td>HESS J1846-029</td><td>J1846-0258 (PSR)<br>G29.7-0.3 (COMP)</td></tr><tr><td>HESS J1848-018</td><td>3FGL J1848.4-0141 (3FGL)<br>W43 (EXTRA)</td></tr><tr><td>HESS J1849-000</td><td>G32.6+0.5 (PWN)<br>J1849-0001 (PSR)</td></tr><tr><td>HESS J1852-000</td><td>3FGL J1853.2+0006 (3FGL)<br>G32.8-0.1 (SNR)<br>J1853+0011 (PSR)<br>J1853-0004 (PSR)<br>G33.2-0.6 (SNR)</td></tr><tr><td>HESS J1857+026</td><td>J1856+0245 (PSR)<br>MAGIC J1857.2+0263 (EXTRA)<br>MAGIC J1857.6+0297 (EXTRA)<br>2FHL J1856.8+0256 (2FHL)</td></tr><tr><td>HESS J1858+020</td><td>3FGL J1857.9+0210 (3FGL)</td></tr><tr><td>HESS J1908+063</td><td>ARGO J1907+0627 (EXTRA)<br>MGRO J1908+06 (EXTRA)<br>G40.5-0.5 (SNR)<br>3FGL J1907.9+0602 (3FGL)<br>J1907+0602 (PSR)</td></tr><tr><td>HESS J1911+090</td><td>G43.3-0.2 (SNR)<br>2FHL J1911.0+0905 (2FHL)<br>3FGL J1910.9+0906 (3FGL)</td></tr><tr><td>HESS J1912+101</td><td>J1913+1011 (PSR)</td></tr><tr><td>HESS J1923+141</td><td>3FGL J1923.2+1408e (3FGL)<br>2FHL J1923.2+1408e (2FHL)</td></tr><tr><td>HESS J1930+188</td><td>G54.1+0.3 (COMP)<br>J1930+1852 (PSR)<br>VER J1930+188 (EXTRA)</td></tr><tr><td>HESS J1943+213</td><td>IGR J19443+2117 (EXTRA)<br>2FHL J1944.1+2117 (2FHL)</td></tr></tbody></table>