A. U. AbeysekaraA. ArcherW. BenbowR. BirdR. BroseM. BuchoveckyJ. H. BuckleyV. BugaevA. J. ChromeyM. P. ConnollyW. CuiM. K. DanielA. FalconeQ. FengJ. P. FinleyL. FortsonA. FurnissM. HüttenD. HannaO. HervetJ. HolderG. HughesT. B. HumenskyC. A. JohnsonP. KaaretP. KarM. KertzmanD. KiedaM. KrauseF. KrennrichS. KumarM. J. LangT. T.Y. LinS. McArthurP. MoriartyR. MukherjeeS. O'BrienR. A. OngA. N. OtteN. ParkA. PetrashykM. PohlE. PueschelJ. QuinnK. RaganP. T. ReynoldsG. T. RichardsE. RoacheC. RultenI. SadehM. SantanderG. H. SembroskiK. ShahinyanI. SushchJ. TylerS. P. WakelyA. WeinsteinR. M. WellsP. WilcoxA. WilhelmD. A. WilliamsT. J. WilliamsonB. ZitzerS. AbdollahiM. AjelloL. BaldiniG. BarbielliniD. BastieriR. BellazziniB. BerenjiE. BissaldiR. D. BlandfordR. BoninoE. BottaciniT. J. BrandtP. BruelR. BuehlerR. A. CameronR. CaputoP. A. CaraveoD. CastroE. CavazzutiE. CharlesG. ChiaroS. CipriniJ. Cohen-TanugiD. CostantinS. CutiniF. D'AmmandoF. De PalmaN. Di LallaM. Di MauroL. Di VenereA. DominguezC. FavuzziS. J. FeganA. FranckowiakY. FukazawaS. FunkP. FuscoIstituto Nazionale di Fisica Nucleare, Sezione di TriesteIstituto Nazionale di Fisica Nucleare, Sezione di PerugiaIstituto Nazionale di Fisica Nucleare, Sezione di BariIstituto Nazionale di Fisica Nucleare, Sezione di TorinoIstituto Nazionale di Fisica Nucleare, Sezione di PisaIstituto Nazionale Di Fisica Nucleare, Sezione di PadovaLaboratoire Univers et Particules de MontpellierLaboratoire Leprince-RinguetKavli Institute for Particle Astrophysics and CosmologySanta Cruz Institute for Particle PhysicsINAF Istituto di Astrofisica Spaziale e Fisica Cosmica, BolognaINAF Istituto di Astrofisica Spaziale e Fisica Cosmica, MilanUniversity of Wisconsin-MadisonAgenzia Spaziale ItalianaCalifornia State University, East BayHiroshima UniversityCalifornia State University, Los AngelesDeutsches Elektronen-Synchrotron (DESY)Columbia University in the City of New YorkUniversity of Minnesota Twin CitiesUniversità di PisaAlma Mater Studiorum Università di BolognaUniversity of California, Los AngelesUniversidad Complutense de MadridClemson UniversityThe Enrico Fermi InstituteUniversity of UtahThe University of AlabamaTsinghua UniversityUniversity of IowaUniversità degli Studi di BariUniversität PotsdamHarvard-Smithsonian Center for AstrophysicsGeorgia Institute of TechnologyUniversità degli Studi di TriesteUniversità degli Studi di Napoli Federico IIUniversità degli Studi di TorinoWashington University in St. LouisBarnard CollegePurdue UniversityNational University of Ireland GalwayNASA Goddard Space Flight CenterDePauw UniversityUniversity College DublinIowa State UniversityMcGill UniversityPennsylvania State UniversityCork Institute of TechnologyFriedrich-Alexander-Universität Erlangen-NürnbergBartol Research InstituteUniversità degli Studi di Padova2019-08-232019-08-232018-10-10Astrophysical Journal. Vol.866, No.1 (2018)153843570004637X2-s2.0-85055336695https://repository.li.mahidol.ac.th/handle/20.500.14594/45735© 2018. The American Astronomical Society. All rights reserved. The High Altitude Water Cherenkov (HAWC) collaboration recently published their 2HWC catalog, listing 39 very high energy (VHE; >100 GeV) gamma-ray sources based on 507 days of observation. Among these, 19 sources are not associated with previously known teraelectronvolt (TeV) gamma-ray sources. We have studied 14 of these sources without known counterparts with VERITAS and Fermi-LAT. VERITAS detected weak gamma-ray emission in the 1 TeV-30 TeV band in the region of DA 495, a pulsar wind nebula coinciding with 2HWC J1953+294, confirming the discovery of the source by HAWC. We did not find any counterpart for the selected 14 new HAWC sources from our analysis of Fermi-LAT data for energies higher than 10 GeV. During the search, we detected gigaelectronvolt (GeV) gamma-ray emission coincident with a known TeV pulsar wind nebula, SNR G54.1+0.3 (VER J1930+188), and a 2HWC source, 2HWC J1930+188. The fluxes for isolated, steady sources in the 2HWC catalog are generally in good agreement with those measured by imaging atmospheric Cherenkov telescopes. However, the VERITAS fluxes for SNR G54.1+0.3, DA 495, and TeV J2032+4130 are lower than those measured by HAWC, and several new HAWC sources are not detected by VERITAS. This is likely due to a change in spectral shape, source extension, or the influence of diffuse emission in the source region.Mahidol UniversityEarth and Planetary SciencesPhysics and AstronomyArticleSCOPUS10.3847/1538-4357/aade4e