THE FIRST FERMI LAT SUPERNOVA REMNANT CATALOG

The Fermi LAT is a pair-conversion γ-ray telescope that observes photons from 20 MeV to >300 GeV. Launched on 2008 June 11, the default observing mode is an all-sky survey optimized to provide relatively uniform coverage of the entire sky every three hours, including the Galactic plane where most known SNRs are located. Further details of the instrument can be found in Atwood et al. (2009).

In this work we focus on the 279 currently known Galactic SNRs. They are derived from the 274 SNRs noted in the catalog of Green (2009a, hereafter Green's catalog), plus five additional SNRs identified following its publication. All but 16 of these SNRs have been identified by their radio synchrotron emission, so their centroids and extensions are primarily determined from the radio. When the radio detection is not securely identified through the synchrotron emission, positional information is obtained from the optical, X-ray, or TeV observations that identified the SNR, as noted in Green's catalog. The catalog is thought to be complete down to a 1 GHz radio surface brightness limit of ≈10⁻²⁰ W m⁻² Hz⁻¹ sr⁻¹ (i.e., 1 MJy sr⁻¹). However, selection effects are known to bias radio surveys against the identification of radio faint and small angular size remnants (Green 2004; Brogan et al. 2006). We note that as this work neared completion, a revised catalog of 294 SNRs was published (Green 2014), representing only a small increase (<10%) over the previous catalog.

We briefly describe the five SNRs added to our catalog since the publication of Green's catalog. For the purposes of this work, these are implicitly included when we refer to Green's catalog and are also in the 2014 catalog unless otherwise noted.

• SNR G5.7−0.0: identified in the radio by Brogan et al. (2006), this remnant is known to be interacting with a nearby dense cloud due to the presence of OH(1720 MHz) masers (Hewitt & Yusef-Zadeh 2009). The TeV source HESS J1800−240C is coincident with the SNR, though it is unclear whether the γ-ray emission is attributable to SNR G5.7−0.0 or escaping CRs from SNR W28 (Aharonian et al. 2008d; Hanabata et al. 2014). This SNR was included in Green (2014) as a probable SNR, but was not included in the final list of 294 firmly identified SNRs.
• SNR G35.6−0.4: re-identified as an SNR by Green (2009b) but not included in Green's 2009 catalog, this is a middle-aged remnant with nearby MCs thought to lie at a distance of 3.6 ± 0.4 kpc (Zhu et al. 2013). The nearby TeV source HESS J1858+020 (Aharonian et al. 2008c) has been proposed as originating from CRs escaping from the SNR and illuminating nearby clouds (Paron & Giacani 2010).
• SNR G213.3−0.4: a very low radio surface brightness SNR initially designated as G213.0−0.6 by Reich et al. (2003), the SNR identification was later confirmed by optical line observations (Stupar & Parker 2012). The SNR lies near the ${\rm{H}}\;{\rm{II}}$ region S284, which is coincident with the γ-ray source 2FGL J0647.7+0032. No conclusive evidence for interaction between the SNR and S284 has been presented. The X-ray source 1RXS J065049.7−003220 lies near the center of the SNR.
• SNR G306.3−0.9: this X-ray source was first reported by Miller et al. (2011) with the designation Swift J132150.9−633350. This is a small-diameter SNR with a radius of 110''. X-ray observations indicate a young SNR of age 1300–4600 years in the Sedov phase and at a distance of 8 kpc (Reynolds et al. 2013). The SNR also shows 24 μm emission, indicating shocked or irradiated warm dust.
• SNR G308.4−1.4: this shell-type SNR was initially identified in radio surveys due to its steep radio spectral index α = −0.7 ± 0.2, and confirmed by its detection as an extended X-ray source (Reynolds et al. 2012). The eastern part of the remnant shows enhanced radio, infrared, and X-ray emission, which may signal that the shock-wave is expanding into a denser region to the east (Prinz & Becker 2012; De Horta et al. 2013). Chandra observations also revealed a bright X-ray point source near the geometrical center with a soft spectrum and putative periodicity that make it a candidate compact binary (Hui et al. 2012). Given a distance estimate of 6–12 kpc and an age of 5000–7500 years for the SNR (Prinz & Becker 2012), the point source and remnant may have originated from the same progenitor system.

This catalog was constructed using three years of LAT survey data from the Pass 7 (P7) "Source" class and the associated P7V6 instrument response functions (IRFs). This interval spans 36 months, from 2008 August 4 to 2011 August 4 (mission elapsed time 239557417−334108806). The Source event class is optimized for the analysis of persistent LAT sources, and balances effective area against suppression of background from residual misclassified charged particles. We selected only events within a maximum zenith angle of 100° and use the recommended filter string "DATA_QUAL==1 && LAT_CONFIG==1" in gtmktime.⁸⁵ The P7 data and associated products are comparable to those used in the other γ-ray catalogs employed in this work. We used the first three years of science data for which the associated IEM is suitable for measuring sources with >2° extension.⁸⁶ A detailed discussion of the instrument and event classes can be found in Atwood et al. (2009) and at the Fermi Science Support Center (see footnote 83).

For each of the 279 SNRs we modeled emission within a 10° radius of the SNR's center. As a compromise between the number of photons collected, the spatial resolution, and the impact of the IEM, we chose 1 GeV as our minimum energy threshold. The limited statistics in source class above 100 GeV motivated using this as our upper energy limit.

To avoid times during which transient sources near SNRs were flaring, we removed periods with significant weekly variability detected by the Fermi All-sky Variability Analysis (FAVA) (Ackermann et al. 2013a). We conservatively defined a radius within which a flaring source may significantly affect the flux of a source at the center. We take this distance to be the radio radius of an SNR plus 28, corresponding to the overall 95% containment radius for the Fermi LAT point spread function (PSF) for a 1 GeV photon at normal incidence (Ackermann et al. 2012a). The time ranges of FAVA flares within this distance were removed in 23 RoIs, leaving $\geqslant 98.9\&percnt;$ of the total data in each RoI.

To characterize each candidate SNR we constructed a model of γ-ray emission in the RoI that includes all significant sources of emission as well as the residual background from CRs misclassified as γ-rays. We implemented an analysis method to create and optimize the 279 models for each of the 279 RoIs. For each RoI, we initially included all sources within the 10° RoI listed in the second Fermi LAT catalog (2FGL; Nolan et al. 2012), based on two years of source class data. To this we added pulsars from the LAT Second Pulsar Catalog (2PC; Abdo et al. 2013), based on three years of source class data, with 2PC taking precedence for sources that exist in both. For the diffuse emission we combined the standard IEM corresponding to our P7 data set, gal_2yearp7v6_v0.fits, with the standard model for isotropic emission, which accounts for extragalactic diffuse γ-ray emission and residual charged particles misclassified as γ-rays. Both the corresponding isotropic model, iso_p7v6source.txt, and the IEM are the same as used for the 2FGL catalog analysis.⁸⁷

Compared to 2FGL, we used an additional year of data and limited the energy range to 1–100 GeV. This can result in different detection significances and localizations than previously reported in 2FGL. To account for these effects, we recreated the RoIs' inner 3° radius regions, which encompass the radio extents of all known SNRs, observed to be $\leqslant 2\buildrel{\circ}\over{.}6$, and allows a margin for the LAT PSF. The 68% weighted average containment radius of the LAT PSF for events at 1 GeV is ∼07 (Ackermann et al. 2012a). We note that this implicitly assumes that an SNR's GeV extent should not be more than about an order of magnitude larger than its radio extension and also note that the selection biases stated in Green's catalog limit the range of known SNRs' radio extensions.

To build the inner 3° radius model for each RoI, we first removed all sources except identified active galactic nuclei (AGNs) and pulsars, whose positions on the sky are independently confirmed by precise timing measurements (Abdo et al. 2013). Retained AGNs were assigned their 2FGL positions and spectral model forms. Pulsars' positions and spectral forms were taken from 2PC. 2FGL sources identified or associated with SNRs were removed when they lied within the inner 3°.

We generated a map of source test statistic (TS) defined in Mattox et al. (1996) via pointlike on a square grid with 01 × 01 spacing that covers the entire RoI. pointlike employs a binned maximum likelihood method. The source TS is defined as twice the logarithm of the ratio between the likelihood ${{ \mathcal L }}_{1}$, here obtained by fitting the model to the data including a test source, and the likelihood ${{ \mathcal L }}_{0}$, obtained here by fitting without the source, i.e., $\mathrm{TS}=2\mathrm{log}({{ \mathcal L }}_{1}/{{ \mathcal L }}_{0})$. At the position of the maximum TS value, we added a new point source with a PL spectral model:

$$\begin{eqnarray}&&\displaystyle \frac{{dN}}{{dE}}=N\displaystyle \frac{(-{\rm{\Gamma }}+1){E}^{-{\rm{\Gamma }}}}{{E}_{{\rm{max}}}{}^{-{\rm{\Gamma }}+1}-{E}_{{\rm{min}}}{}^{-{\rm{\Gamma }}+1}},\end{eqnarray} \tag{ 1 }$$

where N is the integrated photon flux, Γ is the photon index, and E_min and E_max are the lower and upper limits of the energy range in the fit, set to 1 GeV and 100 GeV, respectively. We then performed a maximum likelihood fit of the RoI to determine N and Γ and localized the newly added source. The significance of a point source with a PL spectral model is determined by the ${\chi }_{n}^{2}$ distribution for n additional degrees of freedom for the additional point source, which is typically slightly less than $\sqrt{\mathrm{TS}}$.⁸⁸

To promote consistent convergence of the likelihood fit, we limited the number of free parameters in the model. For sources remaining after the removal step, described above, we freed the normalization parameters for the sources within 5° of the RoI center, including identified AGNs and pulsars. For 2FGL sources between 5° and 10°, we fixed all parameters. The spectrum of the IEM was scaled with a PL whose normalization and index were free, as done in 2FGL. For the isotropic emission model, we left the normalization fixed to the global fit value since the RoIs are too small to allow an independent fitting of the isotropic and Galactic IEM components. The isotropic component's contribution to the total flux is small compared to the IEM's at low Galactic latitudes.

After localizing them, the new sources were tested for spectral curvature. In each of the four energy bands between 1 and 100 GeV, centered at 1.8, 5.6, 17.8, and 56.2 GeV, we calculated the TS value for a PL with a spectral index fixed to 2 and then summed the TS values. We refer to this as ${\mathrm{TS}}_{\mathrm{band}\mathrm{fits}}$. A value for ${\mathrm{TS}}_{\mathrm{band}\mathrm{fits}}$ much greater than the TS calculated with a PL (TS_PL) suggests with a more rapid calculation that the PL model may not accurately describe the source. Analogously to 2FGL (Nolan et al. 2012), we allow for deviations of source spectra from a PL form by modeling sources with a log-normal model known colloquially as LogParabola or logP:

$$\begin{eqnarray}&&\displaystyle \frac{{dN}}{{dE}}={N}_{0}{\left(\displaystyle \frac{E}{{E}_{b}}\right)}^{-(\alpha +\beta \mathrm{log}(E/{E}_{b}))},\end{eqnarray} \tag{ 2 }$$

where N₀ is the normalization in units of photons/MeV, α and β define the curved spectrum, and E_b is fixed to 2 GeV.⁸⁹ If ${\mathrm{TS}}_{\mathrm{band}\mathrm{fits}}-{\mathrm{TS}}_{\mathrm{PL}}\geqslant 25$, we replaced the PL spectral model with a logP model and refit the RoI, including a new localization step for the source. We retained the logP model for the source if the global $\mathrm{log}{ \mathcal L }$ across the full band improved sufficiently: ${\mathrm{TS}}_{\mathrm{curve}}\equiv 2$ ($\mathrm{log}{ \mathcal L }$ ${}_{\mathrm{logP}}-$ $\mathrm{log}{ \mathcal L }$_PL) ≥16. Otherwise we returned the source to the PL model that provided the better global $\mathrm{log}{ \mathcal L }$. Across all RoIs, less than 2% of the newly added sources retained the logP model.

We continued to iteratively generate TS maps and add sources within the entire RoI until additional new sources did not significantly change the global likelihood of the fit. The threshold criterion was defined as obtaining $\mathrm{TS}\lt 16$ for three consecutively added new sources, denoted as ${N}_{\mathrm{TS}\lt 16}=3$. Despite iteratively adding a source at the location of the peak position in the TS map, the TS values of new sources may not decrease monotonically with each iteration for several reasons. First, source positions were localized after fitting the RoI and generating the TS map. Second, some added sources were fit with a more complex spectral model than a simple PL. Finally, when creating the TS map, we fixed the source's spectral index to 2, whereas when adding the actual source to the model, we allowed its index to vary.

The specific value of ${N}_{\mathrm{TS}\lt 16}=3$ was chosen to avoid missing sources with $\mathrm{TS}\ \geqslant \ 25$, the threshold commonly used for source detection in LAT data, and to optimize computation time. We tested the threshold by selecting eight representative SNRs from both complex and relatively simple regions of the sky, with both hard and soft spectral indices. We applied the above procedure to the test RoIs using a criterion of ${N}_{\mathrm{TS}\lt 16}=6$ and counted how many $\mathrm{TS}\ \geqslant \ 25$ sources would be excluded if a smaller ${N}_{\mathrm{TS}\lt 16}$ criterion was used. Reducing the threshold to ${N}_{\mathrm{TS}\lt 16}=3$ cut only one significant source in any of the regions. Since the maximum number of sources added in any test RoI was 38, the minimum was 14, and the total number of sources added across all test regions was 221, we chose to use ${N}_{\mathrm{TS}\lt 16}=3$ for the full sample. To allow for proper convergence of the likelihood fit, we reduced the number of free parameters prior to each new source addition. If the previously added source was between 3° and 5° of the center of the RoI, just its normalization was freed, and if it was greater than 5°, then all of its source parameters were fixed.

To avoid having newly added sources overlap with pulsars, we deleted new sources from the RoI if they were within 02 of a γ-ray pulsar and refit the pulsar in the 1–100 GeV range following the 2PC conventions. 2PC modeled pulsar spectra as PL with an exponential cutoff (PLEC),

$$\begin{eqnarray}&&\displaystyle \frac{{dN}}{{dE}}={N}_{0}{\left(\displaystyle \frac{E}{{E}_{0}}\right)}^{-{\rm{\Gamma }}}\mathrm{exp}{\left(-\displaystyle \frac{E}{{E}_{c}}\right)}^{b},\end{eqnarray} \tag{ 3 }$$

where N₀ is the normalization factor, Γ is the photon spectral index, E_c is the cutoff energy, and b determines to the sharpness of the cutoff. 2PC assessed the validity of fixing b to 1 in Equation (3) (PLEC1) by repeating the analysis using a PL model, as well as the more general exponentially cutoff PL form, allowing the parameter b in Equation (3) to vary. For the pulsar spectra in this analysis, we compared the maximum likelihood values for spectral models with and without a cutoff and with and without the value of b being free, via ${\mathrm{TS}}_{\mathrm{cut}}\equiv 2$ ($\mathrm{log}{{ \mathcal L }}_{\mathrm{PLEC}1}-$ $\mathrm{log}{{ \mathcal L }}_{\mathrm{PL}})$ and ${\mathrm{TS}}_{b}\equiv 2($ $\mathrm{log}{{ \mathcal L }}_{\mathrm{PLEC}}\;-$ $\mathrm{log}{{ \mathcal L }}_{\mathrm{PLEC}1})$ to determine which to use. If ${\mathrm{TS}}_{\mathrm{cut}}\lt 9$ is reported for the pulsar in 2PC then a PL model is used. If TS${}_{\mathrm{cut}}\geqslant 9$, we then check to see if the cutoff energy fit in 2PC lies within the restricted energy range of 1–100 GeV used in this work. For pulsars with cutoffs $\geqslant 1\;{\rm{GeV}}$, we then use the PLEC model, and free the cutoff if TS${}_{{\text{}}b}\geqslant 9$. For those pulsars with cutoffs less than 1 GeV the spectral parameters are fixed to the 2PC values.

To complete the construction of our point source RoI model, we took the output of the previous steps and removed all sources with TS < 16. This final model was then used as the starting model for analyzing candidate SNR emission. We conservatively allow sources with TS down to 16 (∼4σ) in order to account for the effects of at least the brightest sub-threshold sources on the parameter fits for the other sources in the model. Furthermore, while the SNR analysis method described in the next Section (2.3) is allowed to remove sources, it cannot add them. Thus we start from a set of sources designed to allow the final model to capture all significant emission within the central region. To corroborate our method of systematically adding sources to a region, we compare our RoI source models with those found by the 2FGL approach in Appendix A.

For each SNR, we characterize the morphology and spectrum of any γ-ray emission that may be coincident with the radio position reported in Green's catalog. This was achieved by testing multiple hypotheses for the spatial distribution of γ-ray emission: a point source and two different algorithms for an extended disk. The best fit was selected based on the global likelihoods of the fitted hypotheses and their numbers of degrees of freedom. The hypothesis with the best global likelihood was then evaluated using a classification algorithm described in Section 3.1 to determine whether the radio SNR could be associated with the detected γ-ray emission.

Spatial coincidence is a necessary but not sufficient criterion to identify a γ-ray source with a known SNR. The detection of spatially extended γ-ray emission increases confidence in an identification, especially if GeV and radio sizes are similar, as has been observed on an individual basis for several extended SNRs (e.g., Lande et al. 2012). The LAT has sufficient spatial resolution to detect many Galactic SNRs as extended. Figure 1 shows the distribution of radio diameters from Green's catalog. Vertical dashed lines show the minimum detectable extension for sources with flux and index typical of those observed in this catalog, based on simulations using the P7V6 IRFs (Lande et al. 2012). The minimum detectable extension depends not only on the source's flux and spectrum, but also on the flux of the background, which was estimated by scaling the average isotropic background level by factors of 10 and 100 to be comparable to the Galactic plane. As Figure 1 illustrates, roughly one-third of the known Galactic SNRs may be resolved by the LAT if they are sufficiently bright GeV sources.

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In order to determine the best representation for each SNR, we analyzed each SNR-centered RoI using multiple hypotheses for the spatial and spectral form. We used pointlike (Kerr 2010) to compare PL and logP spectral forms, to compare point source versus extended source hypotheses, and to analyze the robustness of sources near the extended source.

For each hypothesis, we started with the input model described in Sections 2.1 and 2.2. We removed sources falling within the SNR's radio disk unless they had been identified as an AGN or pulsar, as described in Section 2.2. We then proceeded to evaluate the following point and extended source hypotheses. For the point source hypothesis, a point source with a PL index initialized to 2.5 was placed at the radio centroid of the SNR. The positions, spectral index, and spectral normalization of the point source were then fit. As for the initial input model described in Section 2.2, we tested the source for spectral curvature. To test the extended source hypothesis, we employed two separate procedures. Both employed a uniform disk model initially placed at the center of the RoI with a radius equal to that observed in the radio. In the first procedure, called the "disk" hypothesis, we fit both the position and extension of the disk, as well as tested for spectral curvature. A second procedure, which results in a model we call the "neardisk" hypothesis, additionally examines the significance of sources nearby the disk, removing those that are not considered independently significant and refitting the disk position and radius. This procedure is described in Section 2.3.1.

Having evaluated these hypotheses, we compared the global likelihood values of the final extended hypothesis and of the point source hypothesis to determine which model had the largest maximum likelihood. If the source is significant in the best hypothesis, the model parameters are reported in Tables 1 and 2. If no hypothesis had a significant γ-ray source that was coincident with the radio SNR, we calculated the upper limit on the flux from a region consistent with the radio SNR, described in Section 2.3.2, and report the results in Table 3.

Table 1.  LAT SNR Catalog: Results of Spatial Analysis

SNR Name	TS	R.A. (J2000)	decl. (J2000)	l	b	TSext	Radius	Alt IEMs	Location	Extension
		(deg) ± stat ± sys	(deg) ± stat ± sys	(deg)	(deg)		(deg) ± stat ± sys	Effect	Overlap	Overlap
Classified Candidates:
G006.4−00.1	1622	270.36 ± 0.01 ± 0.02	−23.44 ± 0.01 ± 0.01	6.54	−0.26	168	0.37 ± 0.02${}_{-0.00}^{+0.00}$	0, 0, 0	1.00	0.61
G008.7−00.1	788	271.36 ± 0.02 ± 0.03	−21.59 ± 0.02 ± 0.01	8.60	−0.16	123	0.37 ± 0.02${}_{-0.03}^{+0.03}$	0, 0, 0	1.00	0.71
G020.0−00.2	32	277.11 ± 0.09 ± 0.22	−11.50 ± 0.05 ± 0.07	20.09	−0.20	...	...	0, 4, 0	0.93	1.00
G023.3−00.3	208	278.57 ± 0.03 ± 0.07	−8.75 ± 0.03 ± 0.04	23.20	−0.20	25	0.33 ± 0.04${}_{-0.00}^{+0.00}$	0, 7, 0	1.00	0.46
G024.7+00.6	89	278.60 ± 0.03 ± 0.11	−7.17 ± 0.03 ± 0.03	24.61	0.50	25	0.25 ± 0.04${}_{-0.12}^{+0.21}$	0, 4, 0	1.00	0.47
G034.7−00.4	832	284.05 ± 0.01 ± 0.01	1.34 ± 0.02 ± 0.00	34.66	−0.45	61	0.31 ± 0.02${}_{-0.01}^{+0.01}$	0, 0, 0	1.00	0.71
G043.3−00.2	787	287.75 ± 0.01 ± 0.00	9.09 ± 0.01 ± 0.00	43.25	−0.17	...	...	0, 1, 0	0.55	1.00
G045.7−00.4	45	288.94 ± 0.03 ± 0.10	11.08 ± 0.03 ± 0.11	45.55	−0.28	...	...	0, 3, 0	0.53	0.49
G049.2−00.7	1309	290.81 ± 0.01 ± 0.02	14.14 ± 0.01 ± 0.00	49.11	−0.46	74	0.25 ± 0.02${}_{-0.01}^{+0.01}$	0, 0, 0	1.00	0.62
G074.0−08.5	417	312.77 ± 0.06 ± 0.15	30.90 ± 0.06 ± 0.04	74.18	−8.43	313	1.74 ± 0.04${}_{-0.10}^{+0.11}$	0, 0, 0	1.00	0.82
G078.2+02.1	228	305.26 ± 0.03 ± 2.11	40.41 ± 0.03 ± 0.67	78.15	2.14	86	0.69 ± 0.03${}_{-0.51}^{+1.92}$	0, 0, 0	1.00	0.53
G089.0+04.7	193	311.15 ± 0.06 ± 0.11	50.42 ± 0.06 ± 0.30	88.67	4.75	58	0.97 ± 0.06${}_{-0.42}^{+0.74}$	0, 5, 0	1.00	0.77
G109.1−01.0	45	345.41 ± 0.03 ± 0.02	58.83 ± 0.04 ± 0.00	109.13	−1.06	...	...	0, 1, 0	1.00	0.73
G111.7−02.1	584	350.85 ± 0.01 ± 0.00	58.83 ± 0.01 ± 0.00	111.74	−2.12	...	...	0, 0, 0	0.72	1.00
G180.0−01.7	77	84.55 ± 0.10 ± 0.44	27.86 ± 0.10 ± 0.12	180.05	−1.95	37	1.50 ± 0.06${}_{-0.11}^{+0.12}$	0, 0, 0	1.00	0.92
G189.1+03.0	5807	94.28 ± 0.01 ± 0.01	22.57 ± 0.01 ± 0.00	189.04	3.01	527	0.33 ± 0.01${}_{-0.00}^{+0.00}$	0, 0, 0	1.00	0.76
G205.5+00.5	130	98.91 ± 0.11 ± 0.35	5.87 ± 0.11 ± 0.64	205.91	−0.82	89	2.28 ± 0.08${}_{-0.14}^{+0.15}$	0, 0, 0	1.00	0.54
G260.4−03.4	432	125.68 ± 0.02 ± 0.01	−42.90 ± 0.02 ± 0.01	260.37	−3.30	50	0.33 ± 0.02${}_{-0.01}^{+0.01}$	0, 0, 0	1.00	0.50
G266.2−01.2	411	133.00 ± 0.05 ± 0.13	−46.36 ± 0.05 ± 0.03	266.28	−1.24	316	1.19 ± 0.04${}_{-0.08}^{+0.09}$	0, 0, 0	1.00	0.71
G291.0−00.1	551	168.01 ± 0.01 ± 0.01	−60.67 ± 0.01 ± 0.01	291.05	−0.12	...	...	0, 1, 0	1.00	1.00
G292.0+01.8	381	171.16 ± 0.02 ± 0.01	−59.23 ± 0.02 ± 0.01	292.02	1.79	...	...	0, 4, 0	1.00	1.00
G296.5+10.0	27	182.13 ± 0.11 ± 0.00	−52.73 ± 0.11 ± 0.00	296.37	9.60	21	0.76 ± 0.08	0, 8, 0	1.00	0.57
G298.6−00.0	159	183.52 ± 0.02 ± 0.02	−62.63 ± 0.03 ± 0.00	298.65	−0.07	...	...	0, 5, 0	0.89	1.00
G321.9−00.3	223	230.46 ± 0.02 ± 0.00	−57.61 ± 0.02 ± 0.01	322.01	−0.42	...	...	0, 3, 0	1.00	0.47
G326.3−01.8	341	238.20 ± 0.02 ± 0.01	−56.19 ± 0.02 ± 0.01	326.26	−1.76	19	0.21 ± 0.03${}_{-0.02}^{+0.02}$	0, 2, 0	1.00	0.43
G347.3−00.5	134	258.39 ± 0.04 ± 0.14	−39.77 ± 0.04 ± 0.07	347.33	−0.48	81	0.53 ± 0.03${}_{-0.14}^{+0.20}$	0, 0, 0	1.00	0.86
G348.5+00.1	175	258.64 ± 0.02 ± 0.01	−38.50 ± 0.01 ± 0.00	348.47	0.11	...	...	0, 3, 0	0.82	0.94
G349.7+00.2	59	259.52 ± 0.03 ± 0.01	−37.45 ± 0.02 ± 0.00	349.73	0.15	...	...	0, 1, 0	1.00	1.00
G355.4+00.7	39	262.91 ± 0.03 ± 0.09	−32.58 ± 0.03 ± 0.15	355.31	0.59	...	...	0, 2, 0	0.80	0.48
G357.7−00.1	60	265.12 ± 0.03 ± 0.05	−30.94 ± 0.03 ± 0.10	357.71	−0.10	...	...	0, 5, 0	1.00	1.00
Classified Candidates Identified as Not SNRs:a
G005.4−01.2	28	270.49 ± 0.05 ± 0.22	−24.84 ± 0.05 ± 0.91	5.37	−1.06	...	...	0, 4, 0	1.00	0.48
G184.6−05.8	868	83.63 ± 0.00 ± 0.00	22.02 ± 0.00 ± 0.00	184.55	−5.79	...	...	0, 0, 0	1.00	1.00
G284.3−01.8	923	154.73 ± 0.01 ± 0.01	−58.93 ± 0.01 ± 0.01	284.34	−1.68	...	...	0, 1, 0	1.00	0.66
G320.4−01.2	92	228.60 ± 0.02 ± 0.00	−59.18 ± 0.02 ± 0.00	320.35	−1.23	...	...	0, 0, 0	1.00	0.48
Marginally Classified Candidates:
G011.4−00.1	48	272.79 ± 0.03 ± 0.05	−19.10 ± 0.03 ± 0.03	11.43	−0.12	...	...	0, 1, 0	0.33	1.00
G017.4−00.1	110	275.81 ± 0.02 ± 0.01	−13.71 ± 0.02 ± 0.06	17.55	−0.12	...	...	0, 2, 0	0.16	1.00
G018.9−01.1	59	277.23 ± 0.04 ± 0.03	−12.86 ± 0.04 ± 0.03	18.95	−0.94	...	...	0, 2, 0	0.63	0.26
G032.4+00.1b	31	282.48 ± 0.04 ± 0.02	−0.37 ± 0.04 ± 0.02	32.43	0.17	...	...	2, 1, 0	0.85	1.00
G073.9+00.9b	30	303.49 ± 0.04 ± 0.11	36.18 ± 0.04 ± 0.09	73.86	0.92	...	...	8, 3, 6	1.00	0.70
G074.9+01.2	341	303.93 ± 0.01 ± 0.00	37.16 ± 0.02 ± 0.01	74.87	1.17	...	...	0, 0, 0	0.19	1.00
G132.7+01.3	226	35.48 ± 0.06 ± 0.26	62.34 ± 0.06 ± 0.02	133.22	1.29	48	1.09 ± 0.06${}_{-0.07}^{+0.07}$	0, 0, 0	0.64	0.32
G179.0+02.6	145	88.54 ± 0.03 ± 0.00	31.09 ± 0.03 ± 0.01	179.10	2.69	...	...	0, 0, 0	1.00	0.12
G292.2−00.5	233	169.59 ± 0.03 ± 0.23	−61.47 ± 0.03 ± 0.04	292.06	−0.57	22	0.26 ± 0.04${}_{-0.13}^{+0.24}$	0, 4, 0	0.72	0.29
G304.6+00.1	35	196.61 ± 0.03 ± 0.01	−62.78 ± 0.03 ± 0.01	304.65	0.04	...	...	0, 3, 0	0.21	1.00
G316.3−00.0	84	220.67 ± 0.03 ± 0.14	−59.89 ± 0.04 ± 0.00	316.47	0.02	...	...	0, 5, 0	0.37	0.48
G332.0+00.2	83	243.50 ± 0.02 ± 0.71	−50.93 ± 0.02 ± 0.34	332.09	0.09	...	...	0, 8, 0	0.17	0.89
G337.8−00.1	108	249.63 ± 0.02 ± 0.00	−46.95 ± 0.02 ± 0.01	337.75	−0.02	...	...	0, 3, 0	0.15	1.00
G356.3−00.3	64	264.34 ± 0.05 ± 0.17	−32.20 ± 0.04 ± 0.14	356.29	−0.22	...	...	0, 7, 0	0.39	0.98
Other Detected Candidate Sources:
G000.0+00.0	1168	266.45 ± 0.01 ± 0.01	−28.99 ± 0.01 ± 0.01	359.97	−0.06	30	0.16 ± 0.02${}_{-0.01}^{+0.01}$	0, 1, 0	0.53	0.01
G000.3+00.0	48	266.61 ± 0.02 ± 0.18	−28.78 ± 0.03 ± 0.16	0.23	−0.07	...	...	0, 5, 0	0.00	0.75
G004.5+06.8b	48	264.48 ± 0.16 ± 0.17	−23.88 ± 0.16 ± 0.26	3.39	4.13	44	3.00 ± 0.04${}_{-0.17}^{+0.18}$	1, 1, 1	0.00	0.00
G005.2−02.6b	28	271.70 ± 0.09 ± 0.00	−24.83 ± 0.07 ± 0.00	5.92	−2.02	...	...	8, 3, 9	0.00	0.00
G006.1+00.5	190	270.08 ± 0.05 ± 0.50	−23.76 ± 0.05 ± 0.93	6.13	−0.21	17	0.64 ± 0.04${}_{-1.00}^{+1.00}$	0, 4, 3	0.00	0.00
G008.3−00.0	354	271.27 ± 0.03 ± 0.04	−21.67 ± 0.03 ± 0.07	8.49	−0.12	19	0.33 ± 0.03${}_{-0.06}^{+0.07}$	0, 4, 0	0.00	0.01
G010.5−00.0	47	272.11 ± 0.03 ± 0.03	−19.86 ± 0.04 ± 0.02	10.45	0.07	...	...	0, 0, 0	0.00	0.68
G012.5+00.2	159	273.61 ± 0.04 ± 0.23	−17.69 ± 0.04 ± 0.29	13.04	−0.13	18	0.41 ± 0.07${}_{-1.00}^{+1.00}$	0, 2, 2	0.00	0.00
G015.4+00.1	97	275.87 ± 0.14 ± 0.95	−14.07 ± 0.14 ± 1.50	17.25	−0.33	90	2.35 ± 0.05${}_{-0.30}^{+0.34}$	0, 0, 0	0.00	0.00
G016.4−00.5	96	275.88 ± 0.13 ± 0.35	−14.18 ± 0.13 ± 0.82	17.17	−0.39	56	2.39 ± 0.06${}_{-0.47}^{+0.59}$	0, 1, 1	0.00	0.00
G016.7+00.1	132	275.54 ± 0.06 ± 0.28	−13.76 ± 0.06 ± 0.29	17.38	0.10	24	1.13 ± 0.09${}_{-0.17}^{+0.20}$	0, 0, 0	0.00	0.00
G017.0−00.0	92	275.94 ± 0.04 ± 0.63	−14.20 ± 0.04 ± 0.99	17.18	−0.45	34	2.30 ± 0.03${}_{-0.77}^{+1.16}$	0, 0, 0	0.00	0.00
G017.8−02.6b	49	277.67 ± 0.06 ± 0.11	−14.64 ± 0.06 ± 0.02	17.56	−2.14	16	0.60 ± 0.05${}_{-1.00}^{+1.00}$	4, 7, 0	0.00	0.08
G018.1−00.1b	68	276.04 ± 0.04 ± 0.23	−13.48 ± 0.04 ± 0.32	17.86	−0.20	34	1.65 ± 0.05${}_{-0.26}^{+0.30}$	1, 1, 0	0.00	0.00
G022.7−00.2b	204	278.56 ± 0.03 ± 0.07	−8.75 ± 0.03 ± 0.01	23.19	−0.20	22	0.33 ± 0.04${}_{-0.08}^{+0.11}$	2, 3, 3	0.00	0.00
G023.6+00.3b	211	278.56 ± 0.04 ± 0.10	−8.74 ± 0.04 ± 0.05	23.20	−0.19	33	0.33 ± 0.04${}_{-0.08}^{+0.11}$	2, 3, 1	0.00	0.00
G024.7−00.6	238	279.23 ± 0.05 ± 0.02	−6.95 ± 0.05 ± 0.03	25.10	0.04	43	0.73 ± 0.04${}_{-0.02}^{+0.02}$	0, 0, 0	0.00	0.01
G027.4+00.0	279	280.13 ± 0.03 ± 0.17	−5.19 ± 0.03 ± 0.11	27.07	0.05	19	0.70 ± 0.03${}_{-0.17}^{+0.22}$	0, 3, 0	0.00	0.00
G027.8+00.6	163	280.08 ± 0.06 ± 0.08	−5.08 ± 0.06 ± 0.41	27.14	0.15	22	0.82 ± 0.04${}_{-0.17}^{+0.21}$	0, 4, 0	0.00	0.11
G028.6−00.1	124	281.10 ± 0.03 ± 0.02	−3.73 ± 0.02 ± 0.03	28.81	−0.13	...	...	0, 2, 0	0.00	0.51
G028.8+01.5	79	279.35 ± 0.18 ± 0.78	−2.81 ± 0.18 ± 0.96	28.83	1.84	38	2.72 ± 0.10${}_{-0.51}^{+0.63}$	0, 2, 0	0.99	0.09
G029.6+00.1	98	281.11 ± 0.05 ± 0.21	−3.15 ± 0.05 ± 0.24	29.33	0.12	28	0.42 ± 0.07${}_{-0.20}^{+0.29}$	0, 3, 0	0.00	0.01
G030.7+01.0b	64	281.51 ± 0.18 ± 0.94	−0.73 ± 0.18 ± 0.66	31.67	0.86	20	2.25 ± 0.10${}_{-1.08}^{+2.08}$	3, 5, 3	0.00	0.01
G031.5−00.6	39	282.62 ± 0.08 ± 0.19	−0.40 ± 0.08 ± 0.77	32.46	0.03	...	...	0, 6, 0	0.00	0.00
G031.9+00.0	273	282.40 ± 0.02 ± 0.04	−0.92 ± 0.02 ± 0.17	31.90	−0.01	16	0.63 ± 0.05${}_{-1.00}^{+1.00}$	0, 3, 0	1.00	0.01
G032.8−00.1	33	282.67 ± 0.06 ± 0.30	−0.41 ± 0.05 ± 0.83	32.48	−0.02	...	...	0, 6, 0	0.00	0.00
G033.2−00.6	88	282.77 ± 0.08 ± 0.87	−0.03 ± 0.08 ± 1.33	32.86	0.06	28	1.05 ± 0.09${}_{-0.36}^{+0.55}$	0, 3, 2	0.00	0.02
G035.6−00.4	180	284.44 ± 0.02 ± 0.10	2.20 ± 0.02 ± 0.19	35.61	−0.40	...	...	0, 3, 0	0.00	0.86
G036.6−00.7	334	284.64 ± 0.08 ± 0.06	3.73 ± 0.08 ± 0.02	37.06	0.12	33	0.66 ± 0.05${}_{-0.05}^{+0.06}$	0, 0, 0	0.00	0.00
G192.8−01.1	26	92.49 ± 0.06 ± 0.07	17.21 ± 0.09 ± 0.12	192.94	−1.04	...	...	0, 2, 0	1.00	0.09
G213.3−00.4	45	101.93 ± 0.04 ± 0.03	0.54 ± 0.03 ± 0.08	212.03	−0.59	...	...	0, 4, 0	1.00	0.02
G263.9−03.3b	28	128.91 ± 0.02 ± 0.25	−45.49 ± 0.02 ± 0.21	263.84	−2.93	...	...	0, 7, 7	1.00	0.01
G286.5−01.2b	94	161.24 ± 0.03 ± 1.15	−59.53 ± 0.03 ± 1.81	287.51	−0.50	27	1.14 ± 0.05${}_{-0.37}^{+0.56}$	1, 1, 1	0.00	0.00
G306.3−00.8	83	199.33 ± 0.07 ± 0.17	−62.96 ± 0.07 ± 0.21	305.87	−0.24	19	0.53 ± 0.07${}_{-0.07}^{+0.08}$	0, 2, 0	0.00	0.00
G310.8−00.4	44	212.36 ± 0.19 ± 0.51	−60.68 ± 0.19 ± 0.25	312.34	0.76	43	0.99 ± 0.05${}_{-0.13}^{+0.15}$	0, 0, 0	0.00	0.00
G311.5−00.3	270	211.41 ± 0.07 ± 0.15	−61.41 ± 0.07 ± 0.03	311.69	0.19	17	0.30 ± 0.04${}_{-0.14}^{+0.29}$	0, 0, 0	0.00	0.00
G328.4+00.2	126	238.71 ± 0.03 ± 0.04	−53.33 ± 0.03 ± 0.05	328.31	0.26	22	0.32 ± 0.03${}_{-0.08}^{+0.11}$	0, 2, 0	0.17	0.02
G332.4−00.4	157	244.22 ± 0.03 ± 0.14	−51.09 ± 0.03 ± 0.24	332.31	−0.33	23	0.76 ± 0.05${}_{-0.17}^{+0.22}$	0, 0, 0	0.45	0.01
G336.7+00.5	260	248.42 ± 0.04 ± 0.04	−47.73 ± 0.04 ± 0.02	336.62	0.07	50	0.72 ± 0.02${}_{-0.02}^{+0.02}$	0, 0, 0	0.00	0.02
G337.0−00.1	253	248.99 ± 0.02 ± 0.01	−47.57 ± 0.02 ± 0.00	337.00	−0.11	43	0.29 ± 0.03${}_{-0.01}^{+0.01}$	0, 0, 0	1.00	0.00
G337.2+00.1	137	248.98 ± 0.03 ± 0.02	−47.53 ± 0.03 ± 0.03	337.03	−0.08	49	0.41 ± 0.04${}_{-0.05}^{+0.05}$	0, 0, 0	0.00	0.00
G337.2−00.7b	355	248.93 ± 0.05 ± 0.12	−47.59 ± 0.05 ± 0.06	336.96	−0.10	37	0.31 ± 0.03${}_{-0.03}^{+0.04}$	2, 3, 1	0.00	0.00
G337.3+01.0	114	247.35 ± 0.05 ± 1.43	−46.87 ± 0.05 ± 0.12	336.75	1.18	57	2.04 ± 0.10${}_{-0.13}^{+0.13}$	0, 0, 0	0.00	0.00
G338.3−00.0	178	250.13 ± 0.02 ± 0.02	−46.48 ± 0.02 ± 0.02	338.33	0.04	28	0.24 ± 0.03${}_{-0.02}^{+0.03}$	0, 1, 0	0.00	0.08
G345.7−00.2	73	257.53 ± 0.09 ± 0.75	−40.84 ± 0.18 ± 0.96	346.08	−0.58	31	1.92 ± 0.09${}_{-0.80}^{+1.37}$	0, 0, 0	0.00	0.00
G348.5−00.0	173	258.64 ± 0.02 ± 0.01	−38.50 ± 0.01 ± 0.03	348.47	0.11	...	...	0, 5, 0	0.00	0.66
G351.9−00.9	25	262.20 ± 0.06 ± 0.05	−34.53 ± 0.06 ± 0.02	353.36	0.01	...	...	0, 3, 0	0.00	0.00
G352.7−00.1	79	261.86 ± 0.05 ± 0.02	−35.74 ± 0.05 ± 0.09	352.20	−0.43	23	0.66 ± 0.08${}_{-0.11}^{+0.14}$	0, 0, 0	0.00	0.01
G355.9−02.5	129	266.73 ± 0.17 ± 0.09	−31.59 ± 0.17 ± 0.14	357.88	−1.62	70	2.99 ± 0.03${}_{-0.08}^{+0.08}$	0, 0, 0	0.00	0.00
G357.7+00.3	187	266.58 ± 0.01 ± 0.04	−31.02 ± 0.29 ± 0.12	358.30	−1.22	147	3.00 ± 0.02${}_{-0.00}^{+0.00}$	0, 0, 0	0.00	0.00
G358.1+00.1	97	264.77 ± 0.10 ± 0.36	−29.82 ± 0.15 ± 0.05	358.50	0.74	78	3.00 ± 0.01${}_{-0.03}^{+0.03}$	0, 0, 0	0.00	0.00
G358.5−00.9	76	266.53 ± 0.09 ± 0.16	−30.19 ± 0.09 ± 0.24	358.98	−0.75	28	2.09 ± 0.07${}_{-0.12}^{+0.13}$	0, 0, 0	0.00	0.00
G359.0−00.9	94	266.30 ± 0.08 ± 0.06	−30.14 ± 0.08 ± 0.19	358.92	−0.55	56	2.12 ± 0.06${}_{-0.04}^{+0.04}$	0, 0, 0	0.00	0.01
G359.1−00.5	135	266.78 ± 0.09 ± 0.12	−31.16 ± 0.09 ± 0.20	358.27	−1.43	33	2.93 ± 0.04${}_{-0.10}^{+0.11}$	0, 0, 0	0.00	0.00

Notes. Results of the spatial analysis for the 102 detected candidates, ordered by increasing Galactic longitude within their classification category. The detected candidate's test statistic is listed in the TS column; the best fit position is reported in the R.A. and decl. columns, reproduced as Galactic longitude and latitude $(l,b)$ for ease of use. Those candidates with errors listed as 0.00 had shifts in position $\lt 0\buildrel{\circ}\over{.}005$. The test statistic for extension is listed under TS_ext. The column entitled Alt IEMs Effect lists the number of alternate IEMs for which a candidate's significance became less than 9; for which the best extension hypothesis changed between extended and point-like; and for which the likelihood maximization had convergence problems (see Section 3.2.3). The Location and Extension Overlap columns list the fractional overlap in the GeV candidate's position and extension with respect to Green's catalog's radio SNR, Equations (7)–(9), respectively, described in detail in Section 3.1.1.

^aCandidates with emission consistent with a known, non-SNR source, detailed in Section 3.2.2. ^bEmission from regions that should be considered especially uncertain; see Section 3.2.3 for details.

Download table as:  ASCIITypeset images: 1 2

Table 2.  LAT SNR Catalog: Results of Spectral Analysis

SNR Name	TS	Spectral	Flux ± stat ± sys	Index	β	Alt IEM	Location	Extension
		Form	(10−9 ph cm−2 s−1)	±stat ± sys	±stat ± sys	Effect	Overlap	Overlap
Classified SNRs:
G006.4−00.1	1622	PL	51.77 ± 1.54${}_{-3.72}^{+4.25}$	2.64 ± 0.04${}_{-0.08}^{+0.08}$	...	0, 0, 0	1.00	0.61
G008.7−00.1	788	PL	31.27 ± 1.32${}_{-5.27}^{+6.22}$	2.50 ± 0.05${}_{-0.10}^{+0.10}$	...	0, 0, 0	1.00	0.71
G020.0−00.2	32	PL	4.56 ± 0.84${}_{-2.20}^{+4.06}$	3.58 ± 0.47${}_{-0.54}^{+0.54}$	...	0, 4, 0	0.93	1.00
G023.3−00.3	208	PL	14.64 ± 1.18${}_{-6.81}^{+12.56}$	2.38 ± 0.09${}_{-0.15}^{+0.15}$	...	0, 7, 0	1.00	0.46
G024.7+00.6	89	PL	8.63 ± 1.58${}_{-4.13}^{+7.65}$	2.10 ± 0.15${}_{-0.13}^{+0.13}$	...	0, 4, 0	1.00	0.47
G034.7−00.4	832	logP	54.95 ± 2.68${}_{-4.05}^{+4.71}$	2.27 ± 0.09${}_{-0.10}^{+0.10}$	0.41 ± 0.09${}_{-0.05}^{+0.05}$	0, 0, 0	1.00	0.71
G034.7−00.4	...	PL	...	2.34 ± 0.09${}_{-0.07}^{+0.07}$	...	0, 0, 0	...	...
G043.3−00.2	787	PL	19.24 ± 1.01${}_{-1.75}^{+1.94}$	2.36 ± 0.05${}_{-0.08}^{+0.08}$	...	0, 1, 0	0.55	1.00
G045.7−00.4	45	PL	3.72 ± 0.66${}_{-1.99}^{+3.97}$	2.60 ± 0.23${}_{-0.32}^{+0.28}$	...	0, 3, 0	0.53	0.49
G049.2−00.7	1309	PL	31.31 ± 1.27${}_{-2.76}^{+3.12}$	2.30 ± 0.04${}_{-0.08}^{+0.08}$	...	0, 0, 0	1.00	0.62
G074.0−08.5	417	PL	10.60 ± 0.60${}_{-1.82}^{+2.16}$	2.48 ± 0.08${}_{-0.10}^{+0.10}$	...	0, 0, 0	1.00	0.82
G078.2+02.1	228	PL	12.27 ± 2.00${}_{-11.24}^{+75.26}$	1.90 ± 0.09${}_{-0.35}^{+0.35}$	...	0, 0, 0	1.00	0.53
G089.0+04.7	193	PL	8.37 ± 0.66${}_{-5.16}^{+13.20}$	3.00 ± 0.17${}_{-0.27}^{+0.27}$	...	0, 5, 0	1.00	0.77
G109.1−01.0	45	PL	1.09 ± 0.29${}_{-0.27}^{+0.34}$	1.91 ± 0.21${}_{-0.12}^{+0.12}$	...	0, 1, 0	1.00	0.73
G111.7−02.1	584	PL	6.25 ± 0.42${}_{-0.67}^{+0.75}$	2.09 ± 0.07${}_{-0.07}^{+0.06}$	...	0, 0, 0	0.72	1.00
G180.0−01.7	77	PL	5.87 ± 0.74${}_{-0.69}^{+0.77}$	2.28 ± 0.13${}_{-0.10}^{+0.10}$	...	0, 0, 0	1.00	0.92
G189.1+03.0	5807	logP	57.27 ± 1.15${}_{-4.43}^{+4.63}$	2.09 ± 0.04${}_{-0.07}^{+0.07}$	0.10 ± 0.02${}_{-0.03}^{+0.03}$	0, 0, 0	1.00	0.76
G189.1+03.0	...	PL	...	2.34 ± 0.09${}_{-0.07}^{+0.07}$	...	0, 0, 0	...	...
G205.5+00.5	130	PL	13.71 ± 1.27${}_{-2.08}^{+2.34}$	2.56 ± 0.12${}_{-0.10}^{+0.10}$	...	0, 0, 0	1.00	0.54
G260.4−03.4	432	PL	8.04 ± 0.56${}_{-0.61}^{+0.67}$	2.17 ± 0.07${}_{-0.07}^{+0.07}$	...	0, 0, 0	1.00	0.50
G266.2−01.2	411	PL	12.11 ± 0.89${}_{-2.40}^{+2.91}$	1.87 ± 0.05${}_{-0.10}^{+0.10}$	...	0, 0, 0	1.00	0.71
G291.0−00.1	551	PL	13.04 ± 0.78${}_{-1.68}^{+1.90}$	2.53 ± 0.07${}_{-0.08}^{+0.08}$	...	0, 1, 0	1.00	1.00
G292.0+01.8	381	PL	6.17 ± 0.43${}_{-1.32}^{+1.64}$	2.89 ± 0.12${}_{-0.08}^{+0.08}$	...	0, 4, 0	1.00	1.00
G296.5+10.0	27	PL	0.78 ± 0.24${}_{-0.07}^{+0.08}$	1.62 ± 0.21${}_{-0.09}^{+0.09}$	...	0, 8, 0	1.00	0.57
G298.6−00.0	159	PL	7.59 ± 0.71${}_{-0.77}^{+0.85}$	2.92 ± 0.16${}_{-0.19}^{+0.19}$	...	0, 5, 0	0.89	1.00
G321.9−00.3	223	PL	8.85 ± 0.70${}_{-1.64}^{+1.97}$	2.87 ± 0.12${}_{-0.08}^{+0.07}$	...	0, 3, 0	1.00	0.47
G326.3−01.8	341	PL	6.20 ± 0.52${}_{-1.35}^{+1.69}$	1.98 ± 0.07${}_{-0.13}^{+0.13}$	...	0, 2, 0	1.00	0.43
G347.3−00.5	134	PL	4.94 ± 0.81${}_{-3.36}^{+10.08}$	1.53 ± 0.10${}_{-0.41}^{+0.41}$	...	0, 0, 0	1.00	0.86
G348.5+00.1	175	PL	13.05 ± 1.15${}_{-1.07}^{+1.62}$	2.64 ± 0.10${}_{-0.09}^{+0.12}$	...	0, 3, 0	0.82	0.94
G349.7+00.2	59	PL	4.00 ± 0.76${}_{-0.99}^{+1.28}$	2.19 ± 0.16${}_{-0.15}^{+0.15}$	...	0, 1, 0	1.00	1.00
G355.4+00.7	39	PL	4.69 ± 0.80${}_{-1.62}^{+2.39}$	3.09 ± 0.25${}_{-0.24}^{+0.21}$	...	0, 2, 0	0.80	0.48
G357.7−00.1	60	PL	6.34 ± 0.98${}_{-3.57}^{+7.93}$	2.60 ± 0.17${}_{-0.18}^{+0.18}$	...	0, 5, 0	1.00	1.00
Classified Candidates Identified as Not SNRs:a
G005.4−01.2	28	PL	3.29 ± 0.68${}_{-2.39}^{+8.44}$	2.85 ± 0.31${}_{-0.45}^{+0.45}$	...	0, 4, 0	1.00	0.48
G184.6−05.8	868	PL	108.12 ± 18.54${}_{-1.94}^{+1.98}$	2.24 ± 0.05${}_{-0.01}^{+0.01}$	...	0, 0, 0	1.00	1.00
G284.3−01.8	923	PL	24.81 ± 1.04${}_{-2.05}^{+2.24}$	2.91 ± 0.06${}_{-0.02}^{+0.02}$	...	0, 1, 0	1.00	0.66
G320.4−01.2	92	PL	2.61 ± 0.75${}_{-0.44}^{+0.51}$	1.61 ± 0.16${}_{-0.08}^{+0.08}$	...	0, 0, 0	1.00	0.48
Marginally Classified Candidates:
G011.4−00.1	48	PL	4.57 ± 0.84${}_{-1.22}^{+1.19}$	2.48 ± 0.20${}_{-0.20}^{+0.10}$	...	0, 1, 0	0.33	1.00
G017.4−00.1	110	PL	8.83 ± 1.19${}_{-2.59}^{+3.60}$	2.33 ± 0.13${}_{-0.08}^{+0.07}$	...	0, 2, 0	0.16	1.00
G018.9−01.1	59	PL	5.77 ± 0.83${}_{-0.87}^{+0.79}$	2.96 ± 0.25${}_{-0.22}^{+0.19}$	...	0, 2, 0	0.63	0.26
G032.4+00.1b	31	PL	4.76 ± 0.90${}_{-2.10}^{+3.73}$	4.14 ± 0.58${}_{-0.40}^{+0.20}$	...	2, 1, 0	0.85	1.00
G073.9+00.9b	30	PL	2.33 ± 0.47${}_{-2.21}^{+37.89}$	3.34 ± 0.56${}_{-1.56}^{+1.56}$	...	8, 3, 6	1.00	0.70
G074.9+01.2	341	PL	8.38 ± 0.59${}_{-0.56}^{+0.63}$	2.79 ± 0.11${}_{-0.09}^{+0.09}$	...	0, 0, 0	0.19	1.00
G132.7+01.3	226	PL	13.15 ± 0.97${}_{-2.45}^{+2.91}$	2.71 ± 0.12${}_{-0.10}^{+0.10}$	...	0, 0, 0	0.64	0.32
G179.0+02.6	145	PL	2.61 ± 0.28${}_{-0.29}^{+0.32}$	3.18 ± 0.21${}_{-0.08}^{+0.08}$	...	0, 0, 0	1.00	0.12
G292.2−00.5	233	PL	8.41 ± 0.69${}_{-2.37}^{+3.23}$	2.48 ± 0.10${}_{-0.12}^{+0.12}$	...	0, 4, 0	0.72	0.29
G304.6+00.1	35	PL	1.36 ± 0.56${}_{-0.47}^{+0.68}$	1.76 ± 0.25${}_{-0.27}^{+0.27}$	...	0, 3, 0	0.21	1.00
G316.3−00.0	84	PL	6.46 ± 0.78${}_{-1.11}^{+1.31}$	2.98 ± 0.25${}_{-0.13}^{+0.13}$	...	0, 5, 0	0.37	0.48
G332.0+00.2	83	PL	8.52 ± 1.07${}_{-6.38}^{+25.37}$	2.67 ± 0.16${}_{-0.39}^{+0.39}$	...	0, 8, 0	0.17	0.89
G337.8−00.1	108	PL	11.47 ± 1.28${}_{-1.37}^{+1.53}$	2.73 ± 0.13${}_{-0.10}^{+0.10}$	...	0, 3, 0	0.15	1.00
G356.3−00.3	64	PL	5.72 ± 0.86${}_{-2.92}^{+5.84}$	2.65 ± 0.20${}_{-0.23}^{+0.23}$	...	0, 7, 0	0.39	0.98
Other Detected Candidate Sources:
G000.0+00.0	1168	logP	65.02 ± 2.90${}_{-6.45}^{+6.86}$	2.25 ± 0.08${}_{-0.05}^{+0.05}$	0.25 ± 0.05${}_{-0.04}^{+0.04}$	0, 1, 0	0.53	0.01
G000.3+00.0	48	PL	14.63 ± 2.95${}_{-9.92}^{+28.00}$	2.65 ± 0.17${}_{-0.10}^{+0.10}$	...	0, 5, 0	0.00	0.75
G004.5+06.8b	48	PL	13.12 ± 1.97${}_{-3.40}^{+4.27}$	2.33 ± 0.17${}_{-0.21}^{+0.21}$	...	1, 1, 1	0.00	0.00
G005.2−02.6b	28	PL	2.17 ± 0.44	5.00	...	8, 3, 9	0.00	0.00
G006.1+00.5	190	PL	33.47 ± 2.93${}_{-3.33}^{+8.30}$	2.33 ± 0.06${}_{-0.40}^{+0.40}$	...	0, 4, 3	0.00	0.00
G008.3−00.0	354	PL	22.13 ± 1.63${}_{-11.70}^{+23.78}$	2.29 ± 0.06${}_{-0.11}^{+0.11}$	...	0, 4, 0	0.00	0.01
G010.5−00.0	47	PL	6.06 ± 0.96${}_{-0.87}^{+0.59}$	2.95 ± 0.28${}_{-0.26}^{+0.15}$	...	0, 0, 0	0.00	0.68
G012.5+00.2	159	PL	14.11 ± 1.18${}_{-2.41}^{+10.87}$	2.90 ± 0.18${}_{-0.28}^{+0.28}$	...	0, 2, 2	0.00	0.00
G015.4+00.1	97	PL	17.75 ± 2.87${}_{-10.58}^{+25.69}$	1.75 ± 0.09${}_{-0.66}^{+0.66}$	...	0, 0, 0	0.00	0.00
G016.4−00.5	96	PL	18.05 ± 2.85${}_{-8.78}^{+15.42}$	1.76 ± 0.09${}_{-0.38}^{+0.38}$	...	0, 1, 1	0.00	0.00
G016.7+00.1	132	PL	20.28 ± 2.14${}_{-3.88}^{+4.73}$	2.12 ± 0.09${}_{-0.14}^{+0.14}$	...	0, 0, 0	0.00	0.00
G017.0−00.0	92	PL	18.22 ± 2.71${}_{-6.15}^{+8.84}$	1.82 ± 0.09${}_{-0.41}^{+0.41}$	...	0, 0, 0	0.00	0.00
G017.8−02.6b	49	PL	3.04 ± 0.63${}_{-0.24}^{+0.34}$	1.86 ± 0.15${}_{-0.09}^{+0.09}$	...	4, 7, 0	0.00	0.08
G018.1−00.1b	68	PL	14.55 ± 2.98${}_{-13.34}^{+35.30}$	1.80 ± 0.12${}_{-0.20}^{+0.21}$	...	1, 1, 0	0.00	0.00
G022.7−00.2b	204	PL	14.62 ± 1.18${}_{-6.50}^{+11.54}$	2.38 ± 0.10${}_{-0.32}^{+0.32}$	...	2, 3, 3	0.00	0.00
G023.6+00.3b	211	PL	14.85 ± 1.17${}_{-10.03}^{+30.61}$	2.41 ± 0.10${}_{-0.27}^{+0.27}$	...	2, 3, 1	0.00	0.00
G024.7−00.6	238	PL	26.86 ± 2.39${}_{-2.34}^{+2.66}$	2.13 ± 0.08${}_{-0.08}^{+0.08}$	...	0, 0, 0	0.00	0.01
G027.4+00.0	279	PL	23.20 ± 1.63${}_{-15.87}^{+48.25}$	2.30 ± 0.07${}_{-0.12}^{+0.12}$	...	0, 3, 0	0.00	0.00
G027.8+00.6	163	PL	22.96 ± 2.16${}_{-18.16}^{+86.60}$	2.32 ± 0.09${}_{-0.20}^{+0.20}$	...	0, 4, 0	0.00	0.11
G028.6−00.1	124	PL	10.01 ± 1.05${}_{-2.26}^{+2.84}$	2.74 ± 0.13${}_{-0.14}^{+0.13}$	...	0, 2, 0	0.00	0.51
G028.8+01.5	79	PL	22.07 ± 2.53${}_{-18.20}^{+94.10}$	2.53 ± 0.15${}_{-0.34}^{+0.34}$	...	0, 2, 0	0.99	0.09
G029.6+00.1	98	PL	12.37 ± 1.30${}_{-11.42}^{+32.13}$	2.94 ± 0.20${}_{-0.33}^{+0.33}$	...	0, 3, 0	0.00	0.01
G030.7+01.0b	64	PL	18.92 ± 2.41${}_{-17.04}^{+154.16}$	2.74 ± 0.21${}_{-0.44}^{+0.44}$	...	3, 5, 3	0.00	0.01
G031.5−00.6	39	PL	4.81 ± 0.81${}_{-3.32}^{+9.29}$	3.71 ± 0.46${}_{-0.90}^{+1.08}$	...	0, 6, 0	0.00	0.00
G031.9+00.0	273	PL	20.17 ± 1.33${}_{-4.43}^{+11.59}$	2.55 ± 0.09${}_{-0.09}^{+0.09}$	...	0, 3, 0	1.00	0.01
G032.8−00.1	33	PL	4.72 ± 0.86${}_{-3.34}^{+10.09}$	3.55 ± 0.46${}_{-0.99}^{+0.99}$	...	0, 6, 0	0.00	0.00
G033.2−00.6	88	PL	15.00 ± 1.64${}_{-10.38}^{+34.33}$	2.91 ± 0.21${}_{-0.56}^{+0.56}$	...	0, 3, 2	0.00	0.02
G035.6−00.4	180	PL	10.92 ± 0.96${}_{-4.57}^{+7.72}$	2.96 ± 0.14${}_{-0.30}^{+0.30}$	...	0, 3, 0	0.00	0.86
G036.6−00.7	334	PL	21.89 ± 1.26${}_{-4.35}^{+5.33}$	2.85 ± 0.11${}_{-0.09}^{+0.09}$	...	0, 0, 0	0.00	0.00
G192.8−01.1	26	PL	1.53 ± 0.34${}_{-0.46}^{+0.65}$	2.84 ± 0.43${}_{-0.18}^{+0.18}$	...	0, 2, 0	1.00	0.09
G213.3−00.4	45	PL	1.51 ± 0.30${}_{-0.34}^{+0.42}$	2.53 ± 0.28${}_{-0.19}^{+0.19}$	...	0, 4, 0	1.00	0.02
G263.9−03.3b	28	PL	17.33 ± 1.91${}_{-20.04}^{+171.59}$	3.85 ± 0.48${}_{-1.60}$	...	0, 7, 7	1.00	0.01
G286.5−01.2b	94	PL	13.08 ± 1.53${}_{-14.58}^{+135.50}$	2.32 ± 0.11${}_{-0.21}^{+0.21}$	...	1, 1, 1	0.00	0.00
G306.3−00.8	83	PL	7.77 ± 0.94${}_{-2.62}^{+3.99}$	2.56 ± 0.18${}_{-0.10}^{+0.10}$	...	0, 2, 0	0.00	0.00
G310.8−00.4	44	PL	4.29 ± 1.11${}_{-5.81}^{+16.26}$	1.53 ± 0.13${}_{-0.41}^{+0.41}$	...	0, 0, 0	0.00	0.00
G311.5−00.3	270	PL	16.54 ± 1.16${}_{-6.82}^{+11.60}$	2.51 ± 0.09${}_{-0.10}^{+0.10}$	...	0, 0, 0	0.00	0.00
G328.4+00.2	126	PL	11.75 ± 1.26${}_{-3.71}^{+5.31}$	2.34 ± 0.11${}_{-0.13}^{+0.13}$	...	0, 2, 0	0.17	0.02
G332.4−00.4	157	PL	24.43 ± 2.73${}_{-7.02}^{+9.58}$	2.12 ± 0.07${}_{-0.09}^{+0.09}$	...	0, 0, 0	0.45	0.01
G336.7+00.5	260	PL	38.19 ± 3.37${}_{-6.59}^{+7.51}$	2.18 ± 0.06${}_{-0.08}^{+0.07}$	...	0, 0, 0	0.00	0.02
G337.0−00.1	253	PL	24.91 ± 1.90${}_{-1.86}^{+2.27}$	2.48 ± 0.08${}_{-0.08}^{+0.08}$	...	0, 0, 0	1.00	0.00
G337.2+00.1	137	PL	28.20 ± 3.03${}_{-2.64}^{+3.85}$	2.38 ± 0.08${}_{-0.08}^{+0.07}$	...	0, 0, 0	0.00	0.00
G337.2−00.7b	355	PL	27.89 ± 1.84${}_{-22.24}^{+104.91}$	2.44 ± 0.07${}_{-0.10}^{+0.10}$	...	2, 3, 1	0.00	0.00
G337.3+01.0	114	PL	20.33 ± 2.08${}_{-9.47}^{+16.48}$	2.22 ± 0.10${}_{-0.13}^{+0.13}$	...	0, 0, 0	0.00	0.00
G338.3−00.0	178	PL	11.75 ± 1.17${}_{-2.82}^{+3.62}$	2.19 ± 0.09${}_{-0.16}^{+0.16}$	...	0, 1, 0	0.00	0.08
G345.7−00.2	73	logP	7.81 ± 1.95${}_{-4.74}^{+11.66}$	0.86 ± 0.48${}_{-1.12}^{+1.12}$	0.18 ± 0.17${}_{-0.18}^{+0.18}$	0, 0, 0	0.00	0.00
G348.5−00.0	173	PL	12.81 ± 1.17${}_{-4.72}^{+7.45}$	2.58 ± 0.10${}_{-0.08}^{+0.10}$	...	0, 5, 0	0.00	0.66
G351.9−00.9	25	PL	3.96 ± 0.86${}_{-1.26}^{+1.79}$	3.93 ± 0.71${}_{-0.56}^{+0.56}$	...	0, 3, 0	0.00	0.00
G352.7−00.1	79	PL	10.22 ± 1.29${}_{-4.23}^{+7.30}$	3.43 ± 0.39${}_{-0.56}^{+0.56}$	...	0, 0, 0	0.00	0.01
G355.9−02.5	129	PL	31.80 ± 2.92${}_{-10.78}^{+14.73}$	2.34 ± 0.09${}_{-0.10}^{+0.10}$	...	0, 0, 0	0.00	0.00
G357.7+00.3	187	logP	38.04 ± 3.06${}_{-10.82}^{+14.62}$	1.78 ± 0.20${}_{-0.14}^{+0.14}$	0.68 ± 0.30${}_{-0.52}^{+0.52}$	0, 0, 0	0.00	0.00
G358.1+00.1	97	logP	24.21 ± 3.57${}_{-9.39}^{+13.99}$	0.16 ± 0.66${}_{-0.37}^{+0.37}$	1.73 ± 0.64${}_{-0.44}^{+0.44}$	0, 0, 0	0.00	0.00
G358.5−00.9	76	PL	23.68 ± 2.87${}_{-12.13}^{+21.96}$	2.38 ± 0.12${}_{-0.14}^{+0.13}$	...	0, 0, 0	0.00	0.00
G359.0−00.9	94	PL	27.14 ± 2.96${}_{-13.45}^{+25.68}$	2.32 ± 0.10${}_{-0.14}^{+0.14}$	...	0, 0, 0	0.00	0.01
G359.1−00.5	135	PL	30.43 ± 2.74${}_{-13.05}^{+20.61}$	2.34 ± 0.09${}_{-0.17}^{+0.17}$	...	0, 0, 0	0.00	0.00

Note. Results of the spectral analysis for the 102 detected candidates, ordered by increasing Galactic longitude within their classification category. Spectral Form denotes if the candidate was best fit with a PL or a logP. Index reflects the PL index or logP α (Equation (2)) for the specified spectral form. For those classified candidates with logP spectral forms, which appear in plots showing other candidates' (PL) indexes, we also report here their best fit PL index and errors for completeness. The β column lists the logP β specified in Equation (2), as applicable. The column entitled Alt IEM Effect lists the number of alternate IEMs for which a candidate's significance became less than 9; for which the best extension hypothesis changed between extended and point-like; and for which the likelihood maximization had convergence problems (see Section 3.2.3). The Location and Extension Overlap columns list the fractional overlap in the GeV candidate's position and extension with respect to Green's catalog's radio SNR, Equations (7)–(9), respectively, described in detail in Section 3.1.1.

^aCandidates with emission consistent with a known, non-SNR source, detailed in Section 3.2.2. ^bEmission from regions that should be treated with care; see Section 3.2.3 for details.

Download table as:  ASCIITypeset images: 1 2

Table 3.  LAT SNR Catalog: SNRs Not Detected by the LAT

SNR	R.A.radio	decl.radio	l	b	Radiusradio	${\rm{\Gamma }}=2.0$		${\rm{\Gamma }}=2.5$
	(deg) (J2000)	(deg) (J2000)	(deg)	(deg)	(deg)	95% UL	99% UL	95% UL	99% UL
G000.0+00.0	266.43	−29.00	359.96	−0.05	0.02	3.0E−08	3.1E−08	4.4E−08	4.5E−08
G000.3+00.0	266.56	−28.63	0.33	0.04	0.09	7.0E−09	7.6E−09	1.2E−08	1.3E−08
G000.9+00.1	266.84	−28.15	0.87	0.08	0.07	7.3E−10	1.0E−09	1.2E−10	1.9E−10
G001.0−00.1	267.12	−28.15	1.00	−0.13	0.07	7.6E−10	1.0E−09	9.7E−10	1.4E−09
G001.4−00.1	267.41	−27.77	1.46	−0.15	0.08	2.6E−10	4.0E−10	3.0E−10	4.6E−10
G001.9+00.3	267.19	−27.17	1.87	0.32	0.01	1.4E−10	2.2E−10	1.8E−10	2.7E−10
G003.7−00.2	268.86	−25.83	3.78	−0.28	0.10	6.7E−10	9.4E−10	1.1E−09	1.4E−09
G003.8+00.3	268.23	−25.47	3.81	0.39	0.15	4.4E−10	6.4E−10	5.3E−10	7.9E−10
G004.2−03.5	272.23	−27.05	4.21	−3.51	0.23	2.9E−09	2.9E−09	1.0E−09	1.3E−09
G004.5+06.8	262.68	−21.48	4.53	6.82	0.03	3.8E−10	4.8E−10	5.4E−10	6.7E−10
G004.8+06.2	263.35	−21.57	4.79	6.24	0.15	8.4E−09	8.5E−09	8.8E−10	1.1E−09
G005.2−02.6	271.88	−25.75	5.20	−2.60	0.15	3.8E−10	5.3E−10	5.3E−10	7.3E−10
G005.5+00.3	269.27	−24.00	5.55	0.32	0.11	1.4E−08	1.5E−08	3.8E−09	4.2E−09
G005.7−00.0	269.70	−24.05	5.71	−0.05	0.10	3.1E−09	3.5E−09	4.7E−09	5.2E−09
G005.9+03.1	266.83	−22.27	5.90	3.13	0.17	1.1E−09	1.3E−09	1.4E−09	1.7E−09
G006.1+00.5	269.37	−23.42	6.10	0.53	0.12	1.2E−09	1.5E−09	1.7E−09	2.1E−09
G006.1+01.2	268.73	−23.08	6.10	1.21	0.23	8.9E−08	8.9E−08	5.6E−09	5.6E−09
G006.4+04.0	266.29	−21.37	6.41	4.03	0.26	2.2E−09	2.2E−09	1.3E−10	1.9E−10
G006.5−00.4	270.55	−23.57	6.51	−0.48	0.15	2.9E−09	3.4E−09	8.3E−09	9.0E−09
G007.0−00.1	270.46	−22.90	7.05	−0.08	0.12	1.7E−09	2.1E−09	2.8E−09	3.3E−09
G007.2+00.2	270.28	−22.63	7.20	0.20	0.10	1.1E−09	1.4E−09	1.3E−09	1.7E−09
G007.7−03.7	274.35	−24.07	7.75	−3.77	0.18	4.9E−10	6.5E−10	6.8E−10	8.9E−10
G008.3−00.0	271.14	−21.82	8.30	−0.10	0.04	8.5E−09	8.9E−09	1.1E−08	1.2E−08
G008.7−05.0	276.04	−23.80	8.71	−5.01	0.22	1.0E−09	1.2E−09	1.0E−08	1.0E−08
G008.9+00.4	270.99	−21.05	8.90	0.40	0.20	9.6E−10	1.3E−09	1.3E−09	1.7E−09
G009.7−00.0	271.84	−20.58	9.70	−0.06	0.11	1.3E−09	1.6E−09	1.6E−09	2.1E−09
G009.8+00.6	271.28	−20.23	9.75	0.57	0.10	7.9E−10	1.1E−09	1.1E−09	1.4E−09
G009.9−00.8	272.67	−20.72	9.95	−0.81	0.10	7.9E−10	1.1E−09	1.6E−09	2.0E−09
G010.5−00.0	272.28	−19.78	10.60	−0.03	0.05	2.4E−09	2.7E−09	4.1E−09	4.5E−09
G011.0−00.0	272.52	−19.42	11.03	−0.06	0.08	7.8E−08	7.8E−08	3.6E−09	4.1E−09
G011.1+00.1	272.45	−19.20	11.19	0.11	0.09	4.5E−08	4.5E−08	2.0E−09	2.1E−09
G011.1−01.0	273.51	−19.77	11.17	−1.04	0.12	4.1E−10	5.9E−10	6.1E−10	8.7E−10
G011.1−00.7	273.19	−19.63	11.15	−0.71	0.07	3.8E−10	5.5E−10	5.6E−10	8.0E−10
G011.2−00.3	272.86	−19.42	11.18	−0.34	0.03	2.2E−09	2.5E−09	2.4E−09	2.7E−09
G011.4−00.1	272.70	−19.08	11.41	−0.04	0.07	3.1E−09	3.4E−09	4.5E−09	4.9E−09
G011.8−00.2	273.10	−18.73	11.89	−0.20	0.03	1.4E−09	1.7E−09	2.2E−09	2.6E−09
G012.0−00.1	273.05	−18.62	11.97	−0.11	0.06	1.2E−09	1.5E−09	1.9E−09	2.2E−09
G012.2+00.3	272.82	−18.17	12.26	0.30	0.05	1.1E−09	1.3E−09	1.7E−09	2.1E−09
G012.5+00.2	273.06	−17.92	12.59	0.22	0.05	1.9E−09	2.2E−09	2.8E−09	3.2E−09
G012.7−00.0	273.33	−17.90	12.73	0.00	0.05	8.2E−09	8.2E−09	7.8E−09	7.8E−09
G012.8−00.0	273.40	−17.82	12.83	−0.02	0.03	1.3E−08	1.3E−08	3.2E−09	3.6E−09
G013.3−01.3	274.83	−18.00	13.32	−1.30	0.44	2.7E−10	4.1E−10	3.2E−10	4.8E−10
G013.5+00.2	273.56	−17.20	13.45	0.15	0.04	2.0E−09	2.0E−09	1.6E−09	1.9E−09
G014.1−00.1	273.97	−16.57	14.19	0.10	0.05	7.8E−10	1.0E−09	1.3E−09	1.6E−09
G014.3+00.1	273.99	−16.45	14.30	0.14	0.04	6.4E−10	8.7E−10	1.1E−09	1.4E−09
G015.1−01.6	276.00	−16.57	15.11	−1.61	0.22	6.5E−10	8.7E−10	6.6E−10	9.3E−10
G015.4+00.1	274.51	−15.45	15.42	0.18	0.12	1.1E−09	1.4E−09	1.7E−09	2.2E−09
G015.9+00.2	274.72	−15.03	15.89	0.20	0.05	8.2E−10	1.0E−09	1.3E−09	1.6E−09
G016.0−00.5	275.48	−15.23	16.05	−0.54	0.10	2.5E−09	2.9E−09	3.8E−09	4.3E−09
G016.2−02.7	277.42	−16.13	16.13	−2.62	0.14	1.2E−09	1.4E−09	1.4E−09	1.6E−09
G016.4−00.5	275.66	−14.92	16.41	−0.55	0.11	1.6E−09	1.9E−09	2.7E−09	3.1E−09
G016.7+00.1	275.23	−14.33	16.74	0.09	0.03	2.8E−09	3.1E−09	4.1E−09	4.5E−09
G016.8−01.1	276.33	−14.77	16.85	−1.05	0.22	2.9E−09	3.4E−09	4.6E−09	5.2E−09
G017.0−00.0	275.49	−14.13	17.03	−0.04	0.04	1.5E−09	1.8E−09	2.3E−09	2.6E−09
G017.4−00.1	275.78	−13.77	17.48	−0.11	0.05	5.8E−09	6.2E−09	7.4E−09	7.8E−09
G017.4−02.3	277.73	−14.87	17.39	−2.30	0.20	1.5E−09	1.7E−09	1.9E−09	2.2E−09
G017.8−02.6	278.21	−14.65	17.80	−2.61	0.20	1.4E−09	1.6E−09	9.7E−10	1.2E−09
G018.1−00.1	276.14	−13.18	18.17	−0.15	0.07	1.8E−09	2.2E−09	3.1E−09	3.5E−09
G018.6−00.2	276.48	−12.83	18.63	−0.28	0.05	1.0E−09	1.4E−09	1.5E−09	2.0E−09
G018.8+00.3	276.00	−12.38	18.81	0.35	0.11	2.1E−10	3.1E−10	2.3E−09	2.7E−09
G018.9−01.1	277.46	−12.97	18.95	−1.19	0.28	3.1E−09	3.5E−09	4.6E−09	5.1E−09
G019.1+00.2	276.23	−12.12	19.14	0.27	0.23	2.5E−09	3.0E−09	2.9E−09	3.5E−09
G020.4+00.1	276.96	−11.00	20.47	0.16	0.07	1.3E−09	1.6E−09	8.2E−09	8.3E−09
G021.0−00.4	277.80	−10.78	21.05	−0.47	0.07	3.7E−10	5.4E−10	6.0E−10	8.5E−10
G021.5−00.1	277.71	−10.15	21.56	−0.10	0.04	7.9E−10	1.1E−09	1.6E−09	2.0E−09
G021.5−00.9	278.39	−10.58	21.49	−0.89	0.03	1.2E−09	1.5E−09	2.4E−09	2.7E−09
G021.8−00.6	278.19	−10.13	21.80	−0.51	0.17	1.3E−09	1.7E−09	1.8E−09	2.4E−09
G022.7−00.2	278.31	−9.22	22.66	−0.19	0.22	4.1E−09	4.4E−09	4.6E−09	5.2E−09
G023.6+00.3	278.26	−8.22	23.53	0.31	0.08	1.6E−09	2.0E−09	3.1E−09	3.7E−09
G024.7−00.6	279.68	−7.53	24.79	−0.62	0.12	1.5E−09	1.8E−09	1.9E−09	2.3E−09
G027.4+00.0	280.33	−4.93	27.39	0.00	0.03	3.8E−09	4.2E−09	5.2E−09	5.7E−09
G027.8+00.6	279.96	−4.40	27.69	0.57	0.32	6.0E−09	6.5E−09	8.1E−09	8.7E−09
G028.6−00.1	280.98	−3.88	28.62	−0.10	0.09	6.4E−09	6.9E−09	5.4E−09	5.4E−09
G028.8+01.5	279.75	−2.92	28.91	1.43	0.83	1.3E−09	1.7E−09	4.6E−09	5.2E−09
G029.6+00.1	281.22	−2.95	29.56	0.11	0.04	3.7E−09	4.1E−09	6.0E−09	6.5E−09
G029.7−00.3	281.60	−2.98	29.71	−0.24	0.03	1.8E−09	2.1E−09	2.6E−08	2.6E−08
G030.7+01.0	281.00	−1.53	30.72	0.96	0.17	1.1E−09	1.5E−09	2.3E−09	2.7E−09
G030.7−02.0	283.60	−2.90	30.69	−1.98	0.13	2.2E−10	3.3E−10	3.0E−10	4.4E−10
G031.5−00.6	282.79	−1.52	31.55	−0.63	0.15	1.2E−09	1.5E−09	2.4E−09	2.9E−09
G031.9+00.0	282.35	−0.92	31.89	0.03	0.05	4.7E−09	5.1E−09	6.5E−09	6.9E−09
G032.0−04.9	286.50	−3.00	31.92	−4.61	0.50	5.2E−10	6.9E−10	4.7E−10	6.6E−10
G032.1−00.9	283.29	−1.13	32.12	−0.90	0.33	1.7E−09	2.1E−09	2.7E−09	3.1E−09
G032.4+00.1	282.52	−0.42	32.40	0.11	0.05	2.0E−09	2.3E−09	3.7E−09	4.1E−09
G032.8−00.1	282.85	−0.13	32.81	−0.05	0.14	3.9E−10	5.1E−10	1.0E−08	1.0E−08
G033.2−00.6	283.46	−0.03	33.18	−0.55	0.15	7.0E−10	9.5E−10	1.1E−09	1.4E−09
G033.6+00.1	283.20	0.68	33.69	0.01	0.08	2.0E−09	2.4E−09	3.5E−09	4.1E−09
G035.6−00.4	284.40	2.06	35.47	−0.43	0.08	7.0E−09	7.5E−09	1.1E−08	1.1E−08
G036.6+02.6	282.20	4.43	36.58	2.60	0.12	2.6E−10	3.8E−10	4.3E−10	6.1E−10
G036.6−00.7	285.15	2.93	36.58	−0.70	0.21	2.0E−09	2.3E−09	2.5E−09	3.0E−09
G039.2−00.3	286.03	5.47	39.24	−0.32	0.06	8.8E−10	1.1E−09	1.9E−09	1.9E−09
G039.7−02.0	288.08	4.92	39.70	−2.38	0.71	6.3E−10	8.8E−10	7.3E−10	1.0E−09
G040.5−00.5	286.79	6.52	40.52	−0.51	0.18	1.1E−09	1.5E−09	2.0E−09	2.5E−09
G041.1−00.3	286.89	7.13	41.11	−0.31	0.03	2.1E−09	2.4E−09	7.7E−09	7.7E−09
G042.8+00.6	286.83	9.08	42.82	0.64	0.20	8.4E−10	1.1E−09	1.7E−09	2.1E−09
G043.9+01.6	286.46	10.50	43.91	1.61	0.50	5.5E−10	7.7E−10	8.5E−10	1.2E−09
G046.8−00.3	289.54	12.15	46.77	−0.30	0.12	3.4E−10	4.9E−10	4.8E−10	6.9E−10
G053.6−02.2	294.71	17.23	53.62	−2.26	0.25	8.4E−10	1.0E−09	4.7E−09	4.8E−09
G054.1+00.3	292.63	18.87	54.10	0.26	0.01	7.9E−10	9.6E−10	1.1E−09	1.4E−09
G054.4−00.3	293.33	18.93	54.47	−0.29	0.33	1.5E−09	1.8E−09	2.1E−09	2.5E−09
G055.0+00.3	293.00	19.83	55.11	0.42	0.14	5.8E−10	7.9E−10	1.0E−09	1.3E−09
G055.7+03.4	290.33	21.73	55.59	3.52	0.19	4.8E−10	6.4E−10	7.6E−10	9.7E−10
G057.2+00.8	293.75	21.95	57.30	0.83	0.10	3.1E−10	4.3E−10	4.1E−10	5.9E−10
G059.5+00.1	295.64	23.58	59.58	0.11	0.12	7.6E−10	9.7E−10	1.8E−09	2.1E−09
G059.8+01.2	294.73	24.32	59.81	1.20	0.15	6.0E−10	7.8E−10	7.3E−10	9.5E−10
G063.7+01.1	296.97	27.75	63.79	1.16	0.07	1.6E−09	1.6E−09	9.5E−10	1.1E−09
G065.1+00.6	298.67	28.58	65.27	0.30	0.56	1.1E−09	1.4E−09	2.3E−09	2.8E−09
G065.3+05.7	293.25	31.17	65.18	5.66	2.27	4.4E−10	6.5E−10	4.0E−10	6.0E−10
G065.7+01.2	298.04	29.43	65.71	1.21	0.18	6.0E−10	7.8E−10	8.6E−10	1.1E−09
G067.7+01.8	298.63	31.48	67.73	1.82	0.11	1.8E−10	2.7E−10	3.0E−10	4.3E−10
G068.6−01.2	302.17	30.62	68.61	−1.20	0.19	4.5E−10	6.2E−10	6.9E−10	9.1E−10
G069.0+02.7	298.33	32.92	68.84	2.78	0.67	1.3E−09	1.4E−09	3.6E−09	4.0E−09
G069.7+01.0	300.67	32.72	69.69	1.00	0.12	6.0E−10	7.6E−10	7.4E−10	9.6E−10
G073.9+00.9	303.56	36.20	73.91	0.88	0.23	1.7E−09	2.0E−09	2.8E−09	3.2E−09
G074.9+01.2	304.01	37.20	74.94	1.14	0.06	4.5E−09	4.8E−09	6.1E−09	6.4E−09
G076.9+01.0	305.58	38.72	76.90	0.98	0.07	6.2E−10	7.8E−10	1.2E−09	1.4E−09
G082.2+05.3	304.75	45.50	82.15	5.32	0.65	9.7E−10	1.2E−09	9.7E−10	1.3E−09
G083.0−00.3	311.73	42.87	83.00	−0.27	0.07	3.1E−10	4.3E−10	4.0E−10	5.6E−10
G084.2−00.8	313.33	43.45	84.19	−0.80	0.15	1.9E−10	2.8E−10	2.3E−10	3.4E−10
G085.4+00.7	312.67	45.37	85.37	0.78	0.20	1.3E−09	1.5E−09	1.9E−09	2.2E−09
G085.9−00.6	314.67	44.88	85.91	−0.61	0.20	1.4E−09	1.6E−09	2.0E−09	2.1E−09
G093.3+06.9	313.10	55.35	93.28	6.91	0.19	4.4E−10	5.6E−10	4.5E−10	5.9E−10
G093.7−00.2	322.33	50.83	93.75	−0.22	0.67	5.1E−10	7.2E−10	7.3E−10	1.0E−09
G094.0+01.0	321.21	51.88	93.97	1.02	0.23	3.0E−10	4.4E−10	4.3E−10	6.2E−10
G096.0+02.0	322.62	53.98	96.04	1.95	0.22	2.9E−10	4.1E−10	5.0E−10	6.9E−10
G106.3+02.7	336.88	60.83	106.27	2.70	0.32	1.6E−09	1.9E−09	2.2E−09	2.5E−09
G108.2−00.6	343.42	58.83	108.19	−0.63	0.51	1.6E−09	1.8E−09	1.8E−09	2.1E−09
G113.0+00.2	354.15	61.37	114.09	−0.21	0.22	9.5E−10	1.1E−09	1.2E−09	1.4E−09
G114.3+00.3	354.25	61.92	114.29	0.30	0.59	1.5E−09	1.8E−09	1.8E−09	2.1E−09
G116.5+01.1	358.42	63.25	116.49	1.10	0.58	1.2E−09	1.4E−09	1.5E−09	1.8E−09
G116.9+00.2	359.79	62.43	116.92	0.17	0.28	6.5E−09	6.5E−09	1.3E−09	1.5E−09
G119.5+10.2	1.67	72.75	119.58	10.17	0.75	5.1E−09	5.4E−09	2.9E−08	2.9E−08
G120.1+01.4	6.33	64.15	120.09	1.42	0.07	2.1E−09	2.1E−09	1.7E−09	1.7E−09
G126.2+01.6	20.50	64.25	126.24	1.58	0.58	5.8E−10	7.8E−10	9.2E−10	1.2E−09
G127.1+00.5	22.08	63.17	127.08	0.60	0.38	1.3E−09	1.5E−09	1.9E−09	2.1E−09
G130.7+03.1	31.42	64.82	130.73	3.08	0.06	2.1E−08	2.1E−08	2.0E−09	2.1E−09
G132.7+01.3	34.42	62.75	132.62	1.51	0.67	4.4E−09	4.7E−09	5.9E−09	6.3E−09
G156.2+05.7	74.67	51.83	156.12	5.66	0.92	1.3E−09	1.6E−09	1.7E−09	2.0E−09
G160.9+02.6	75.25	46.67	160.43	2.79	1.08	1.9E−09	2.2E−09	2.5E−09	2.8E−09
G166.0+04.3	81.63	42.93	166.12	4.28	0.37	1.1E−09	1.2E−09	1.5E−09	1.7E−09
G179.0+02.6	88.42	31.08	179.06	2.60	0.58	2.5E−09	2.8E−09	3.3E−09	3.5E−09
G182.4+04.3	92.04	29.00	182.42	4.30	0.42	5.0E−10	6.5E−10	6.4E−10	8.2E−10
G192.8−01.1	92.33	17.33	192.77	−1.11	0.65	2.7E−09	3.0E−09	3.6E−09	3.9E−09
G206.9+02.3	102.17	6.43	206.89	2.32	0.41	9.9E−10	1.2E−09	1.3E−09	1.5E−09
G213.3−00.4	102.53	−0.41	213.15	−0.48	1.33	2.2E−09	2.5E−09	3.2E−09	3.6E−09
G261.9+05.5	136.08	−38.70	261.95	5.48	0.29	2.6E−10	3.6E−10	2.6E−10	3.7E−10
G263.9−03.3	128.50	−45.83	263.94	−3.37	2.12	5.0E−08	5.0E−08	1.0E−09	1.6E−09
G272.2−03.2	136.71	−52.12	272.22	−3.18	0.12	6.0E−10	7.7E−10	1.0E−09	1.2E−09
G279.0+01.1	149.42	−53.25	278.63	1.22	0.79	4.0E−09	4.0E−09	2.5E−09	2.8E−09
G286.5−01.2	158.92	−59.70	286.57	−1.21	0.10	9.3E−10	1.2E−09	1.3E−09	1.6E−09
G289.7−00.3	165.31	−60.30	289.68	−0.29	0.13	2.7E−09	2.8E−09	1.5E−09	1.8E−09
G290.1−00.8	165.77	−60.93	290.15	−0.78	0.14	2.2E−10	2.5E−10	4.3E−10	4.6E−10
G292.2−00.5	169.83	−61.47	292.16	−0.54	0.14	4.8E−09	5.0E−09	4.4E−09	4.7E−09
G293.8+00.6	173.75	−60.90	293.77	0.60	0.17	6.2E−10	8.4E−10	1.3E−09	1.6E−09
G294.1−00.0	174.04	−61.63	294.11	−0.05	0.33	7.7E−10	1.0E−09	1.7E−09	2.1E−09
G296.1−00.5	177.79	−62.57	296.05	−0.51	0.25	1.1E−09	1.3E−09	1.7E−09	2.0E−09
G296.8−00.3	179.62	−62.58	296.88	−0.33	0.14	7.6E−10	9.8E−10	1.1E−09	1.4E−09
G298.5−00.3	183.17	−62.87	298.53	−0.33	0.04	2.0E−10	2.7E−10	1.6E−09	1.9E−09
G299.2−02.9	183.80	−65.50	299.18	−2.89	0.12	4.9E−10	6.4E−10	5.8E−10	7.6E−10
G299.6−00.5	185.44	−63.15	299.59	−0.47	0.11	5.9E−10	7.7E−10	8.4E−10	1.1E−09
G301.4−01.0	189.48	−63.82	301.44	−0.99	0.24	5.8E−10	7.9E−10	9.6E−10	1.3E−09
G302.3+00.7	191.48	−62.13	302.29	0.73	0.14	9.2E−10	1.2E−09	8.4E−10	1.1E−09
G304.6+00.1	196.50	−62.70	304.60	0.12	0.07	2.4E−09	2.7E−09	3.3E−09	3.6E−09
G306.3−00.8	200.46	−63.56	306.31	−0.89	0.02	8.1E−07	8.1E−07	8.8E−10	1.1E−09
G308.1−00.7	204.40	−63.07	308.13	−0.67	0.11	3.2E−10	4.8E−10	5.0E−10	7.2E−10
G308.4−01.4	205.43	−63.70	308.46	−1.37	0.07	2.8E−10	4.1E−10	4.1E−10	5.8E−10
G308.8−00.1	205.62	−62.38	308.81	−0.09	0.20	2.4E−09	2.7E−09	1.6E−09	2.0E−09
G309.2−00.6	206.63	−62.90	309.16	−0.70	0.11	4.9E−10	6.9E−10	6.8E−10	9.6E−10
G309.8+00.0	207.62	−62.08	309.78	0.00	0.18	8.6E−09	8.6E−09	3.1E−09	3.6E−09
G310.6−00.3	209.50	−62.15	310.62	−0.28	0.07	5.4E−10	7.2E−10	7.5E−10	1.0E−09
G310.8−00.4	210.00	−62.28	310.81	−0.46	0.10	6.1E−10	8.4E−10	9.5E−10	1.3E−09
G311.5−00.3	211.41	−61.97	311.53	−0.34	0.04	5.3E−10	7.3E−10	2.4E−09	2.7E−09
G312.4−00.4	213.25	−61.73	312.43	−0.37	0.32	5.1E−09	5.7E−09	1.1E−08	1.1E−08
G312.5−03.0	215.25	−64.20	312.49	−3.00	0.16	7.1E−10	8.9E−10	1.0E−09	1.2E−09
G315.1+02.7	216.12	−57.83	315.08	2.83	1.41	1.7E−09	2.2E−09	2.0E−09	2.5E−09
G315.4−00.3	218.98	−60.60	315.41	−0.29	0.15	9.7E−10	1.3E−09	1.6E−09	2.1E−09
G315.4−02.3	220.75	−62.50	315.42	−2.36	0.35	6.7E−10	8.7E−10	3.4E−08	3.4E−08
G315.9−00.0	219.60	−60.18	315.86	−0.02	0.16	9.9E−10	1.3E−09	1.9E−09	2.3E−09
G316.3−00.0	220.38	−60.00	316.29	−0.01	0.17	6.9E−09	7.2E−09	7.4E−09	8.0E−09
G317.3−00.2	222.42	−59.77	317.31	−0.24	0.09	2.3E−09	2.6E−09	3.5E−09	4.0E−09
G318.2+00.1	223.71	−59.07	318.21	0.09	0.31	5.7E−10	8.3E−10	8.6E−10	1.2E−09
G318.9+00.4	224.62	−58.48	318.91	0.40	0.17	4.4E−10	6.4E−10	9.2E−10	1.3E−09
G320.6−01.6	229.46	−59.27	320.68	−1.54	0.35	4.0E−09	4.1E−09	2.0E−09	2.4E−09
G321.9−01.1	230.94	−58.22	321.89	−1.07	0.23	7.0E−10	9.5E−10	9.6E−10	1.3E−09
G322.5−00.1	230.85	−57.10	322.46	−0.11	0.12	8.5E−10	1.1E−09	1.0E−09	1.4E−09
G323.5+00.1	232.18	−56.35	323.49	0.11	0.11	6.0E−10	8.1E−10	7.1E−10	9.8E−10
G327.1−01.1	238.60	−55.15	327.09	−1.10	0.15	1.0E−09	1.3E−09	1.5E−09	1.9E−09
G327.2−00.1	237.73	−54.30	327.24	−0.13	0.04	5.1E−10	7.1E−10	1.1E−09	1.4E−09
G327.4+00.4	237.08	−53.82	327.24	0.49	0.17	1.8E−09	2.3E−09	2.8E−09	3.4E−09
G327.4+01.0	236.70	−53.33	327.37	1.01	0.12	6.9E−10	9.3E−10	1.0E−09	1.4E−09
G327.6+14.6	225.71	−41.93	327.58	14.57	0.25	5.4E−10	6.6E−10	5.9E−10	7.2E−10
G328.4+00.2	238.87	−53.28	328.41	0.23	0.04	4.6E−09	4.9E−09	4.6E−08	4.6E−08
G329.7+00.4	240.33	−52.30	329.72	0.41	0.30	6.2E−10	9.0E−10	1.0E−09	1.4E−09
G330.0+15.0	227.50	−40.00	329.80	15.53	1.50	3.3E−10	4.8E−10	3.3E−10	4.8E−10
G330.2+01.0	240.27	−51.57	330.17	0.98	0.08	2.8E−10	4.2E−10	4.4E−10	6.4E−10
G332.0+00.2	243.32	−50.88	332.05	0.21	0.10	5.9E−09	6.4E−09	8.8E−09	9.4E−09
G332.4−00.4	244.39	−51.03	332.43	−0.36	0.08	4.2E−09	4.6E−09	4.4E−10	4.6E−10
G332.4+00.1	243.83	−50.70	332.41	0.12	0.12	4.0E−09	4.4E−09	8.1E−10	8.9E−10
G332.5−05.6	250.83	−54.50	332.58	−5.57	0.29	5.9E−10	7.4E−10	1.0E−09	1.1E−09
G335.2+00.1	246.94	−48.78	335.18	0.06	0.17	1.3E−10	2.0E−10	7.0E−10	7.6E−10
G336.7+00.5	248.05	−47.32	336.75	0.53	0.10	6.0E−09	6.5E−09	4.6E−07	4.6E−07
G337.0−00.1	248.99	−47.60	336.98	−0.13	0.01	8.8E−09	9.3E−09	1.3E−08	1.3E−08
G337.2+00.1	248.98	−47.33	337.17	0.06	0.02	4.8E−09	5.2E−09	7.5E−09	7.9E−09
G337.2−00.7	249.87	−47.85	337.19	−0.74	0.05	3.7E−09	3.7E−09	8.4E−10	1.1E−09
G337.3+01.0	248.16	−46.60	337.33	0.96	0.11	1.7E−09	2.0E−09	8.9E−09	8.9E−09
G337.8−00.1	249.75	−46.98	337.79	−0.10	0.06	6.3E−09	6.7E−09	9.5E−09	1.0E−08
G338.1+00.4	249.50	−46.40	338.10	0.42	0.12	9.9E−09	1.0E−08	2.0E−09	2.5E−09
G338.3−00.0	250.25	−46.57	338.32	−0.08	0.07	8.6E−09	9.1E−09	1.1E−08	1.2E−08
G338.5+00.1	250.29	−46.32	338.52	0.06	0.07	3.2E−09	3.7E−09	5.5E−09	6.1E−09
G340.4+00.4	251.63	−44.65	340.40	0.45	0.07	1.2E−09	1.5E−09	2.2E−09	2.6E−09
G340.6+00.3	251.92	−44.57	340.60	0.34	0.05	1.4E−08	1.4E−08	1.5E−09	1.8E−09
G341.2+00.9	251.90	−43.78	341.19	0.86	0.16	1.5E−07	1.5E−07	1.4E−09	1.8E−09
G341.9−00.3	253.75	−44.02	341.86	−0.32	0.06	4.6E−10	6.5E−10	6.3E−10	8.9E−10
G342.0−00.2	253.71	−43.88	341.95	−0.21	0.09	7.8E−10	1.1E−09	1.1E−09	1.5E−09
G342.1+00.9	252.68	−43.07	342.10	0.89	0.08	2.6E−10	3.8E−10	3.5E−10	5.2E−10
G343.0−06.0	261.25	−46.50	342.99	−6.04	2.08	2.4E−08	2.4E−08	1.4E−09	1.9E−09
G343.1−02.3	257.00	−44.27	343.09	−2.31	0.27	7.2E−10	1.0E−09	8.8E−10	1.3E−09
G343.1−00.7	255.10	−43.23	343.08	−0.59	0.20	3.3E−10	4.9E−10	4.9E−10	7.3E−10
G344.7−00.1	255.96	−41.70	344.68	−0.15	0.08	1.5E−08	1.5E−08	4.2E−09	4.5E−09
G345.7−00.2	256.83	−40.88	345.73	−0.18	0.05	8.7E−10	1.1E−09	1.2E−09	1.5E−09
G346.6−00.2	257.58	−40.18	346.63	−0.22	0.07	1.1E−09	1.3E−09	1.4E−09	1.7E−09
G348.5−00.0	258.86	−38.47	348.60	−0.01	0.08	6.0E−09	6.4E−09	9.2E−09	9.7E−09
G348.7+00.3	258.48	−38.18	348.66	0.40	0.14	5.7E−09	5.7E−09	1.1E−08	1.1E−08
G349.2−00.1	259.31	−38.07	349.13	−0.07	0.06	4.5E−10	6.5E−10	7.2E−10	1.0E−09
G350.0−02.0	261.96	−38.53	349.93	−2.04	0.38	4.1E−10	5.9E−10	4.3E−10	6.3E−10
G350.1−00.3	260.25	−37.45	350.06	−0.32	0.03	6.6E−10	8.4E−10	3.3E−09	3.3E−09
G351.2+00.1	260.61	−36.18	351.27	0.16	0.06	3.4E−10	5.0E−10	5.2E−10	7.5E−10
G351.7+00.8	260.25	−35.45	351.70	0.82	0.13	7.8E−10	1.0E−09	9.6E−10	1.3E−09
G351.9−00.9	262.22	−36.27	351.92	−0.96	0.09	1.3E−09	1.6E−09	2.3E−09	2.7E−09
G352.7−00.1	261.92	−35.12	352.74	−0.12	0.06	1.1E−09	1.4E−09	2.5E−09	2.9E−09
G353.6−00.7	263.00	−34.73	353.56	−0.65	0.27	1.3E−09	1.6E−09	1.7E−09	2.2E−09
G353.9−02.0	264.73	−35.18	353.94	−2.08	0.11	2.5E−10	3.7E−10	3.8E−10	5.4E−10
G354.1+00.1	262.62	−33.77	354.19	0.14	0.06	9.4E−10	1.2E−09	9.6E−10	1.1E−09
G354.8−00.8	264.00	−33.70	354.87	−0.78	0.16	1.2E−09	1.5E−09	1.8E−09	2.2E−09
G355.6−00.0	263.82	−32.63	355.69	−0.08	0.06	1.5E−09	1.7E−09	2.9E−09	3.3E−09
G355.9−02.5	266.47	−33.72	355.94	−2.54	0.11	7.7E−10	9.4E−10	3.9E−09	3.9E−09
G356.2+04.5	259.75	−29.67	356.21	4.46	0.21	1.2E−09	1.4E−09	1.5E−09	1.8E−09
G356.3−00.3	264.48	−32.27	356.29	−0.35	0.07	3.1E−09	3.4E−09	4.3E−09	4.7E−09
G356.3−01.5	265.65	−32.87	356.31	−1.51	0.14	1.9E−09	2.0E−09	1.4E−09	1.8E−09
G357.7+00.3	264.65	−30.73	357.67	0.35	0.20	1.8E−09	2.2E−09	3.0E−09	3.6E−09
G358.0+03.8	261.50	−28.60	357.96	3.80	0.32	1.7E−09	1.9E−09	1.2E−08	1.2E−08
G358.1+00.1	264.25	−29.98	358.12	1.04	0.17	1.1E−08	1.1E−08	4.6E−09	4.7E−09
G358.5−00.9	266.54	−30.67	358.58	−1.00	0.14	1.6E−09	2.0E−09	2.2E−10	3.3E−10
G359.0−00.9	266.70	−30.27	358.99	−0.91	0.19	1.4E−09	1.7E−09	4.9E−09	5.5E−09
G359.1+00.9	264.90	−29.18	359.10	0.99	0.10	9.7E−10	1.3E−09	1.4E−09	1.8E−09
G359.1−00.5	266.38	−29.95	359.12	−0.51	0.20	1.1E−09	1.5E−09	1.9E−09	2.6E−09

Note. Upper limits for the 245 undetected SNRs in flux units of ph cm⁻² s⁻¹ in the 1–100 GeV energy range. Both the 95% and 99% confidence upper limits are provided for two different GeV PL indices, ${\rm{\Gamma }}=\{2.0,2.5\}$.

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2.3.1. Localization, Extension, and Spectral Curvature

2.3.2. Fluxes and Upper Limits

For sources with significant emission, we estimated the systematic error propagating from the systematic uncertainty of the effective area and from the choice of IEM. For the former, we propagated the error using the standard bracketing IRF procedure, described in Section 2.4.1. For the latter, we developed a new method in which we vary the underlying IEM, described in Section 2.4.2 with further details in Appendix B. As we take the effective area and underlying IEM systematic errors to be independent, when we can evaluate both components of the systematic uncertainty, we added them in quadrature and report them in Section 3. We briefly compare the total systematic and statistical errors in Section 3.4.

2.4.1. Effective Area Systematic Error

Following the standard method (Ackermann et al. 2012a), we estimated the systematic error associated with the effective area by calculating uncertainties in the IRFs which symmetrically bracket the standard effective area. The final spectral fit of each candidate's region was performed with each of the bracketing IRFs, as these changes primarily affect the spectral fit and have a minimal effect on the source localization and extension.

To estimate the systematic error on the spectral normalization, we created bracketing IRFs that uniformly scaled the effective area to its maximal systematic values. Using a $({E}^{2}-{E}_{0}^{2})/({E}^{2}+{E}_{0}^{2})$ function smoothly switches the effective area between its maximal systematic values at the pivot energy, providing a better estimate of the spectral index's systematic error. The pivot energy E₀ is defined as the energy at which the error on the differential flux is minimal and the errors on the spectral index and flux normalizations are decorrelated. For each detected candidate, the pivot energy was calculated from the gtlike fit's covariance matrix. For PL spectra, the pivot energy can be calculated as:

$$\begin{eqnarray}&&\mathrm{log}({E}_{0})=\displaystyle \frac{\mathrm{log}({E}_{1})+\mathrm{log}({E}_{2})}{2}+\displaystyle \frac{{C}_{K{\rm{\Gamma }}}}{{{KC}}_{{\rm{\Gamma }}{\rm{\Gamma }}}},\end{eqnarray} \tag{ 4 }$$

where E₁ and E₂ are the end points of the energy range, Γ is the PL index defined as in Equation (1), and K is the integral of the source spectrum. ${C}_{{\rm{\Gamma }}{\rm{\Gamma }}}$ and ${C}_{K{\rm{\Gamma }}}$ are the covariance matrix terms associated with the index and normalization, respectively. For the logP sources, as the covariance matrix for spectral models with $\geqslant 3$ parameters requires a more complex transformation than a simple shift in reference energy and our energy range is relatively small, we estimate these sources' pivot energies from the covariance matrices for the best fit PL models. Since the standard IEM was constructed from the data using the standard IRF, we only used the standard IRF with the IEM, rather than the bracketing IRFs, while the remaining components were fit with the bracketing IRFs.

Estimates of the systematic error on the candidates' flux and index due to the effective area's systematic uncertainty are reported in Table 2 of Section 3.2. Effective area systematic errors were not calculated for the candidates detailed in Section 3.2.2, identified as not SNRs, and for the candidate SNR G5.2−2.6, as the index remained at the extreme value allowed in the fit and thus was poorly determined, as noted in Section 3.2.3.

2.4.2. Systematic Error from the Choice of IEM

Interstellar emission contributes substantially to LAT observations in the Galactic plane, where the majority of SNRs are located. Moreover, interstellar γ-ray emission is highly structured on scales smaller than the RoIs typically used for this analysis. To explore the systematic effects on SNRs' fitted properties caused by interstellar emission modeling, we have developed a method employing alternative IEMs. By comparing the source analysis results using these alternative models to the results obtained with the standard IEM, we can approximate the systematic uncertainty. An earlier version of this method was described in de Palma et al. (2013).

The alternative IEMs were built using a different approach than the standard IEM. The work in Ackermann et al. (2012e), using the GALPROP⁹⁰ CR propagation and interaction code, was the starting point for our alternative IEM building strategy. We varied the values of three input parameters that were found to be the most relevant in modeling the Galactic plane: CR source distribution, height of the CR propagation halo, and ${\rm{H}}\;{\rm{I}}$ spin temperature (Ackermann et al. 2012e). In this way, we obtained eight alternative IEMs. The models were constructed to have separate templates for emission associated with gas traced by ${\rm{H}}\;{\rm{I}}$ and CO in four Galactocentric rings and an IC template covering the full sky. By allowing separate scaling factors for these different components of the model, we allowed many more degrees of freedom in fitting the diffuse emission to each RoI.

For each candidate SNR we considered two hypotheses: the point source and that preferred by the previous fit between the disk and neardisk hypotheses, as described in Section 2.3.1. In both cases we started from the output model of the previous analysis, so the fitted parameters are as close as possible to their best values, replacing the standard IEM with the alternative ones. For each candidate SNR we performed independent fits for each hypothesis for each of the eight alternative IEMs as well as the standard IEM, for a total of 18 fits of the region. For each of the IEMs we chose the best extension model using the method described in Section 2.3.1. Appendix B contains further details on the alternative IEMs and their use in the likelihood analysis.

For each fitted parameter P we obtain a set of M = 8 values P_i that we compare to the value obtained with the standard model P_STD. Our estimate of the systematic uncertainty on P due to the modeling of interstellar emission is:

$$\begin{eqnarray}&&{\sigma }_{\mathrm{sys},w}=\sqrt{\displaystyle \frac{1}{{\displaystyle \sum }_{i}^{M}{w}_{i}}\displaystyle \sum _{i}^{M}{w}_{i}{({P}_{i}-{P}_{\mathrm{STD}})}^{2}},\end{eqnarray} \tag{ 5 }$$

where the weights are:

$$\begin{eqnarray}&&{w}_{i}=1/{\sigma }_{i}^{2}.\end{eqnarray} \tag{ 6 }$$

In Equation (6), σ_i is the statistical error of a parameter with a particular alternative IEM, used as a weight in Equation (5). We use the parameter value P_STD for the standard model calculated identically to that of the alternative IEMs, to ensure congruity given the necessary differences in degrees of freedom between this error analysis and the standard analysis. To estimate the systematic errors on the extension, we substitute 02 for σ_i in calculating the weight when the point hypothesis is preferred, as a proxy for the smallest extension resolvable by the LAT for this analysis (Lande et al. 2012, and further discussed in Section 3.1.1). In cases where the best hypothesis with all the alternative IEMs is the point hypothesis, we report this rather than an extension error estimate.

We weighted the parameters by their statistical error to prevent the parameters with values statistically compatible with the other alternative IEMs' parameters from causing overly large systematic errors. This was particularly important for the spectral index of a candidate. We exclude from our error calculation cases for which, during the likelihood fit, the index was at or close to the upper or lower limit of its allowed range of variation, indicating a fit convergence problem, further described in Section 3.2.3. In the cases where the index was at the limit, we fixed it to 2.5 and fit a flux that is used in the flux limit calculation. We tabulate these and other cases where the fit did not converge in the third column of the "Alt IEMs Effect" section in Tables 1 and 2. We discuss the implications of the convergence problems further in Section 3.2.3.

The mathematical minimum required number of alternative IEMs with solutions for a given parameter to calculate the average and the standard deviation and thus the systematic error in Equation (5) from the choice of IEMs is two. We include in the quoted error for all parameters listed in Tables 1 and 2 those which satisfy the mathematical minimum (two). Care should be used with all candidates for which the alternative IEMs had convergence problems. As IEM substructure can affect the significance of the final extension measured as well as the extension itself, we expect changes in the extension hypothesis, such as those seen for SNR G296.5+10.0, which is only just above the extension threshold when using the standard IEM. Such changes are also reflected in the size of the systematic error on the flux.

We note that this strategy for estimating systematic uncertainty from interstellar emission modeling does not represent the complete range of systematics involved. In particular, we have tested only one alternative method for building the IEM and varied only three of the input parameters. This ensemble of models therefore cannot be expected to encompass the full uncertainty associated with the IEM. Furthermore, as the alternative method differs from that used to create the standard IEM, the parameters estimated with the alternative IEM may not bracket the value determined using the standard IEM. Our estimate of the systematic error in Equation (5) accounts for this. Moreover, the estimated uncertainty does not contain other possibly important sources of systematic error in the definition of the IEMs (see Appendix B for details). While the resulting uncertainty should be considered a limited estimate of the systematic uncertainty due to interstellar emission modeling, rather than a full determination, it is critical for interpreting the data. This work represents our most complete and systematic effort to date.

In the past, γ-ray sources have been associated with radio SNRs based on characteristics including spatial coincidence, the lack of variability or pulsation, and spectral form. The degree of spatial coincidence is generally defined in terms of positional coincidence and size or morphology. In order to test for GeV emission associated with SNRs from Green's catalog, we searched for GeV emission in the region of each SNR (Section 2) and used the spatial overlap between the radio SNR and γ-ray candidate to evaluate the probability that the same source gives rise to the emission in both bands. Other SNR MW properties, such as evidence for interaction with MCs or the presence of nonthermal X-ray sources, can also help to identify counterparts. However, these tracers are incomplete and exhibit strong selection effects. Consequently, we do not use them in this general study.

By including all identified AGNs and pulsars in our models of the GeV emission using the 2FGL catalog and 2PC, we exclude these known sources from being identified as SNRs (Section 2.2). We also verified that candidates were not associated with already identified γ-ray sources, including binaries, pulsars, or PWNe (see Section 3.2.2). We further removed all time periods when a flaring source may affect our GeV SNR candidates (Section 2.1).

3.1.1. Spatial Coincidence

To define association probabilities for the candidates, we compared spatial information available from Green's catalog, namely the SNRs' radio positions and radii, with that of the GeV candidates' localizations, localization errors, and extensions. When a GeV candidate is significantly extended, we use the maximum likelihood disk radius as the measure of the extension (see Section 2.3.1).

Using this position and extension information, we derived two parameters. The first, called ${\mathrm{Overlap}}_{\mathrm{loc}}$, provides a quantitative measure of whether the GeV localization is within the SNR's angular extent in radio. This parameter, ranging from 0 to 1, is calculated as

$$\begin{eqnarray}&&{\mathrm{Overlap}}_{\mathrm{loc}}=\displaystyle \frac{\bar{{Radio}\cap {{GeV}}_{\mathrm{loc}}}}{\mathrm{min}(\bar{{Radio}},\bar{{{GeV}}_{\mathrm{loc}}})},\end{eqnarray} \tag{ 7 }$$

where Radio represents the SNR's radio disk and ${\mathrm{GeV}}_{{\rm{loc}}}$ is the GeV 95% error circle. The notation $\bar{X}$ represents the area of X. The second parameter, ${\mathrm{Overlap}}_{\mathrm{ext}}$, quantifies whether the GeV candidate's localization and extension are consistent with the location and extension of the radio SNR:

$$\begin{eqnarray}&&{\mathrm{Overlap}}_{\mathrm{ext}}=\displaystyle \frac{\bar{{Radio}\cap {{GeV}}_{\mathrm{ext}}}}{\mathrm{max}(\bar{{Radio}},\bar{{{GeV}}_{\mathrm{ext}}})},\end{eqnarray} \tag{ 8 }$$

where Radio is again the SNR's radio disk and ${\mathrm{GeV}}_{{\rm{ext}}}$ is the best fit GeV disk if the GeV candidate is significantly extended. If the GeV detection is consistent with a point source, we determined if the corresponding SNR's radio size was consistent with it by redefining the ${\mathrm{Overlap}}_{\mathrm{ext}}$ parameter as

$$\begin{eqnarray}&&{\mathrm{Overlap}}_{\mathrm{ext}}=\displaystyle \frac{\bar{{Radio}\cap {{GeV}}_{\mathrm{min}}}}{\bar{{Radio}}},\end{eqnarray} \tag{ 9 }$$

where GeV_min is the minimum resolvable radius, ${{GeV}}_{\mathrm{min}}\equiv 0\buildrel{\circ}\over{.}2$ for this analysis. Illustrations of the ${\mathrm{Overlap}}_{\mathrm{loc}}$ and ${\mathrm{Overlap}}_{\mathrm{ext}}$ parameters in the cases of an extended and a point GeV detection are shown in Figure 2.

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The value adopted for GeV_min is close to the smallest angular extension measured in our sample (Table 1, candidate for SNR G0.0 + 0.0). The minimum resolvable radius (GeV_min) in our analysis is also visible in Figure 3, and also affects the separation in extension overlap below the minimum radius. In addition, Monte Carlo simulations presented in (Lande et al. 2012, Section 4) showed that, for a similar data set with $E\gt 1\;{\rm{GeV}}$, the extension detection threshold is 02–03, depending on the source's spectral index and the diffuse background level.

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When comparing radio SNRs with GeV candidates, these overlap parameters are used to require that both the GeV centroid is within the SNR's radio area and that their extensions are comparable. The distributions of the ${\mathrm{Overlap}}_{\mathrm{ext}}$ and ${\mathrm{Overlap}}_{\mathrm{loc}}$ parameters for all GeV detections are shown in Figure 4. While all GeV candidates are listed in Table 1, we label the GeV detections with the most likely chance of true association as "classified candidates," defined as those sources with ${\mathrm{Overlap}}_{\mathrm{ext}}\gt 0.4$ and ${\mathrm{Overlap}}_{\mathrm{loc}}\gt 0.4$. "Marginally classified candidates" are those GeV sources with a moderate chance of true association, defined as ${\mathrm{Overlap}}_{\mathrm{ext}}\gt 0.1$ and ${\mathrm{Overlap}}_{\mathrm{loc}}\gt 0.1$ and at least one overlap estimator $\lt 0.4$. Candidates that have overlap parameters outside of these categories are referred to as "other" sources. The number of classified GeV candidates as a function of overlap threshold value is shown in Figure 5, while the choice of threshold value is discussed in the context of chance spatial coincidence in Section 3.1.2.

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