Observations of the unidentified gamma-ray source TeV J2032+4130 by VERITAS E. Aliu1, T. Aune2, B. Behera3, M. Beilicke4, W. Benbow5, K. Berger6, R. Bird7, J. H. Buckley4, V. Bugaev4, J. V Cardenzana8, M. Cerruti5, X. Chen9,3, L. Ciupik10, 4 1 M. P. Connolly11, W. Cui12, C. Duke13, J. Dumm14, M. Errando1, A. Falcone15, 0 2 S. Federici3,9, Q. Feng12, J. P. Finley12, P. Fortin5, L. Fortson14, A. Furniss16, N. Galante5, n a G. H. Gillanders11, S. Griffin17, S. T. Griffiths18, J. Grube10, G. Gyuk10, D. Hanna17, J 6 J. Holder6, G. Hughes3 ,1T. B. Humensky19, P. Kaaret18, O. Kargaltsev32, M. Kertzman20, 1 Y. Khassen7, D. Kieda21, H. Krawczynski4, M. J. Lang11, A. S Madhavan8, G. Maier3, ] E H P. Majumdar2,22 ,2A. McCann23, P. Moriarty24, R. Mukherjee1, D. Nieto1, A. O’Faola´in de . h Bhro´ithe7, R. A. Ong2, A. N. Otte25, D. Pandel26, J. S. Perkins27, M. Pohl9,3, A. Popkow2, p - o H. Prokoph3, J. Quinn7, K. Ragan17, J. Rajotte17, L. C. Reyes28, P. T. Reynolds29, r t s G. T. Richards25, E. Roache5, G. H. Sembroski12, C. Skole3, D. Staszak17, I. Telezhinsky9,3, a [ M. Theiling12, J. V. Tucci12, J. Tyler17, A. Varlotta12, S. Vincent3, S. P. Wakely30, 2 v T. C. Weekes5, A. Weinstein8, R. Welsing3, D. A. Williams16, B. Zitzer31 8 2 8 2 . 1 0 4 1 : v i X r a – 2 – 1Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA 2Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA 3DESY, Platanenallee 6, 15738 Zeuthen, Germany 4Department of Physics, Washington University, St. Louis, MO 63130, USA 5Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA 6Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA 7School of Physics, University College Dublin, Belfield, Dublin 4, Ireland 8Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA 9Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Ger- many 10AstronomyDepartment,AdlerPlanetariumandAstronomyMuseum,Chicago,IL60605, USA 11School of Physics, National University of Ireland Galway, University Road, Galway, Ireland 12Department of Physics, Purdue University, West Lafayette, IN 47907, USA 13Department of Physics, Grinnell College, Grinnell, IA 50112-1690, USA 14School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA 15Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State Uni- versity, University Park, PA 16802, USA 16Santa Cruz Institute for Particle Physics and Department of Physics, University of Cal- – 3 – Received ; accepted ifornia, Santa Cruz, CA 95064, USA 17Physics Department, McGill University, Montreal, QC H3A 2T8, Canada 18Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA 19Physics Department, Columbia University, New York, NY 10027, USA 20Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA 21Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA 22Saha Institute of Nuclear Physics, Kolkata 700064, India 23Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA 24Department of Life and Physical Sciences, Galway-Mayo Institute of Technology, Dublin Road, Galway, Ireland 25School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Tech- nology, 837 State Street NW, Atlanta, GA 30332-0430 26Department of Physics, Grand Valley State University, Allendale, MI 49401, USA 27N.A.S.A./Goddard Space-Flight Center, Code 661, Greenbelt, MD 20771, USA 28Physics Department, California Polytechnic State University, San Luis Obispo, CA 94307, USA 29DepartmentofAppliedPhysicsandInstrumentation, CorkInstituteofTechnology, Bish- opstown, Cork, Ireland 30Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA 31Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA 32Department of Physics, The George Washington University, Washington, DC 20052, USA – 4 – Accepted to ApJ: January, 2014 – 5 – Abstract TeV J2032+4130 was the first unidentified source discovered at very high energies (VHE; E > 100 GeV), with no obvious counterpart in any other wavelength. It is also the first extended source to be observed in VHE gamma rays. Following its discovery, intensive observational campaigns have been carried out in all wavelengths in order to understand the nature of the object, which have met with limited success. We report here on a deep observation of TeV J2032+4130 based on 48.2 hours of data taken from 2009 to 2012 by the VERITAS (Very Energetic Radiation Imaging Telescope Array System) experiment. The source is detected at 8.7 standard deviations (σ) and is found to be extended and asymmetric with a width of 9.5(cid:48)±1.2(cid:48) along the major axis and 4.0(cid:48)±0.5(cid:48) along the minor axis. The spectrum is well described by a differential power law with an index of 2.10 ± 0.14 ± 0.21 and a normalization of (9.5 ± 1.6 ± 2.2 ) × 10−13TeV−1cm−2s−1 stat sys stat sys at 1 TeV. We interpret these results in the context of multiwavelength scenarios which particularly favor the pulsar wind nebula (PWN) interpretation. Keywords: gamma-ray sources: individual: (TeV J2032+4130 = VER J2031+415), pulsars: individual (PSR J2032+4127) 1. Introduction The Cygnus X complex is one of the brightest areas of the sky in all wavelengths and is host to a large number of sources and source types. These include active star forming regions, pulsars, and supernova remnants (SNRs). Objects connected to this region include [email protected] [email protected] – 6 – the star association Cygnus OB2, the microquasar Cygnus X-3, the SNR G78.2+2.1, and TeV J2032+4130 making it a natural laboratory for the study of cosmic ray acceleration. TeV J2032+4130 was discovered serendipitously by the HEGRA imaging atmospheric Cherenkov telescope (IACT) system (Aharonian et al. 2002, 2005) during observations made in the years 1999–2001. It was the first TeV gamma-ray detection to have no obvious counterpart at any other wavelength and was also the first extended source to be discovered in the VHE range. Analysis of combined HEGRA data from 1999–2002 gave a final position for the extended VHE source of R.A. = 20h31m57.0s ± 6.2(cid:48) ± 13.7(cid:48)(cid:48) , Decl. = stat sys +41◦29(cid:48)57(cid:48)(cid:48) ± 1.1(cid:48) ± 1.0(cid:48) (excess events center of gravity), and a Gaussian standard stat sys deviation width of σ = 6.2(cid:48) ± 1.2(cid:48) ± 0.9(cid:48) (Aharonian et al. 2005). HEGRA reported an stat sys integral gamma-ray flux above 1 TeV of (6.9 ± 1.8) × 10−13 cm−2 s−1 with spectral index of 1.9 ± 0.3. Following the discovery, an archival search of the Whipple 10m telescope data was carried out that showed evidence of a source consistent with TeV J2032+4130 (Lang et al. 2004). However, it is worth noting that the peak emission in the Whipple data had an offset of ∼ 3.6(cid:48) with respect to the HEGRA position. The gamma-ray flux measured by Whipple was 12% of the Crab nebula flux above 400 GeV. Based on observations carried out by Whipple in 2003-05, and assuming a spectral shape the same as that of the Crab nebula, it was later reported to be 8% of the Crab nebula flux (Konopelko et al. 2007). The MAGIC collaboration, too, has reported a deep exposure of this region (Albert et al. 2008). The MAGIC collaboration has also found the source to be extended, with an integral flux and spectral index comparable to that measured by HEGRA. These measurements have been extended to even higher energies by the air shower array detectors Milagro and ARGO (Abdo et al. 2012; The ARGO-YBJ Collaboration et al. 2013). Summaries of the positions and morphologies of the results discussed can be found in Table 1. – 7 – Since the discovery of TeV J2032+4130, several observations of the region have been made by X-ray telescopes including Chandra and XMM-Newton, which operate in the energy range of 0.1 – 10 keV and 0.2 – 12 keV respectively. Multiple (∼ 20) point sources were detected in a 5 ksec Chandra observation (Butt et al. 2003). A deep follow-up 50 ksec observation yielded 240 X-ray sources within the same field of view (Butt et al. 2006). A ∼ 50 ksec XMM-Newton exposure was also obtained (Horns et al. 2007). After the known X-ray sources were subtracted, Horns et al. (2007) reported an extended X-ray emission region with a FWHM of ∼12 arcmins. An analysis of the Chandra data also showed the presence of diffuse X-ray emission; however, low photon statistics did not allow for a detailed study of the spectrum. Mukherjee et al. (2003) carried out optical observations of several of the brightest X-ray sources and found that most of these were either O stars or foreground late-type stars. Observations were also made by Suzaku (Murakami et al. 2011) in the energy range 2-10 keV. The authors found two structures within the TeV gamma-ray emission region. After estimating the contribution from the point sources identified by Chandra, the X-ray spectra of the diffuse components were extracted. The diffuse X-ray spectrum was best-fit with a power-law with a photon index of ∼ 2. Radio observations of the region have been made using the Giant Metrewave Radio Telescope (Paredes et al. 2007), yielding several radio sources. At least three of the sources were reported to be non-thermal along with an extended non-thermal diffuse emission. A previously unknown gamma-ray pulsar, PSR J2032+4127, with a pulse period of 142 ms, was discovered in a blind search by Fermi-Large Area Telescope (LAT), located 0.07◦ from the center of the HEGRA detection (Camilo et al. 2009). Subsequent radio measurements made by the Green Bank Telescope (Camilo et al. 2009) localized the position to within a few arcseconds. A characteristic age of 0.11 Myr and a spin-down power of 2.7 × – 8 – 1035 erg s−1 were derived (Camilo et al. 2009). A dispersion measure of 114.8±1.0 pc cm−3 resulted in a distance of 3.6 kpc when standard models for dispersion in the Milky Way were applied (Cordes & Lazio 2002). However, based on the pulsar’s gamma-ray luminosity, a revised estimate of 1.7 kpc was suggested (Camilo et al. 2009), which would place it at the same distance as the Cygnus OB2 star-forming region. The discovery of the pulsar has led several authors to establish a connection between TeV J2032+4130 and PSR J2032+4127 (for more details see Cui (2009)). This argument has been strengthened by the detection of the X-ray emission that is spatially coincident with TeV J2032+4130. However arguments based on spatial coincidence alone can be suspect due to the fact that the morphology of the source can be different at different wavelengths. In order to understand the nature of the emission, it is important to study the morphology of the source with a detector with an improved sensitivity and angular resolution. It is clear from the above discussions that despite several attempts to unravel the nature of TeV J2032+4130 since its discovery, the source along with its position, flux and morphology remains a mystery. This prompted VERITAS to perform a deep observation of this very interesting region of the Galaxy with the aim of better understanding the morphology and source position. The paper is split into several parts: Section 2 describes the VERITAS experiment and observations made on TeV J2032+4130. Section 3 describes the results obtained, and Section 4 presents a Fermi-LAT analysis of the region of TeV J2032+4130. Finally we discuss the implications of our observations on the source in the context of multiwavelength observations. 2. VERITAS Observations The VERITAS array of IACTs is located at the Fred Lawrence Whipple observatory in southern Arizona (1.3 km a.s.l., N 31◦40(cid:48), W 110◦57(cid:48)). It consists of four Davies-Cotton – 9 – telescopes (Cotton et al. 1964). Full array operations began in September 2007. Each telescope has a focal length and a dish diameter of 12 meters and comprises 345 tessellated identical hexagonal mirror facets for a total effective mirror area of 106 m2. Cherenkov light from nearby extensive air showers is focused onto the cameras that consist of 499 photomultiplier tube (PMT) pixels. The spacing between the PMT pixels corresponds to 0.15◦ on the sky, resulting in a total camera field of view of 3.5◦. VERITAS has a large effective area (greater than 105 m2 above 1 TeV), an energy resolution of 15-20% and a single-event angular resolution of 0.08◦ (for energies greater than 500 GeV). This enables the detection of a point source flux that is 1% of the Crab nebula at a 5σ significance in less than 30 hours (Ong et al. 2009). For more details on the VERITAS instrument, see Holder et al. (2008). VERITAS employs a three-level trigger system (Weinstein 2008). At the pixel level there must be a signal greater than 50 mV (3-4 photoelectrons produced by ∼ 20 photons), which is monitored by a constant fraction discriminator. An individual camera triggers when at least three adjacent pixels meet the first condition within a 5 ns time window. Finally, two or more telescopes must trigger within 50 ns for the event to be recorded. The photomultiplier tube relative gains are calculated using dedicated LED flasher calibration runs taken nightly (Hanna et al. 2010). Recorded showers are then parametrized by their second order moments, commonly referred to as Hillas parameters (Hillas 1985). The data presented here were collected between 2009 and 2012. In order to reduce the systematic uncertainties in the background determination, observations were made using the wobble technique (Fomin et al. 1994; Berge et al. 2007). In 2009, all data were collected with the telescopes pointing to regions in the sky offset 0.5◦ from the HEGRA source position. In later seasons almost all the data from 2010 until 2012 were collected centering the telescopes on points equidistant from both TeV J2032+4130 and Cygnus X-3 – 10 – 35 (see Figure 1). A small amount of data was taken with the telescopes aimed at four wobble positions offset 0.5◦ from Cygnus X-3. A total of 48.2 hours of data was selected after removing data taken under bad weather conditions. TeV J2032+4130 was observed with a mean telescope elevation of 68◦. The data were analyzed using the standard VERITAS calibration and reconstruction tools (Daniel 2008). Images from all participating telescopes in an event are combined to obtain the parameters of the arriving gamma-ray (Fegan 1997; Krawczynski et al. 2006). In order to suppress the large number of cosmic ray background events, gamma-ray/hadron separation criteria (cuts) are employed that compare the shapes of the shower images with those from simulated gamma-ray images. The results presented here required at least three telescopes to have recorded images of the shower with more than 1000 photons in each image. An additional cut on the square of the arrival angle of the incoming gamma ray with respect to the source position (θ2 < 0.055) is applied to extract the signal. The ring background model has been used to estimate the background (Berge et al. 2007). The cuts have been previously optimized using a simulated source that has a flux 5% of the flux of the Crab nebula, and whose spectrum is at least as hard as the Crab nebula. The resulting analysis threshold is 520 GeV, which corresponds to the peak of the reconstructed energy distribution. A significance is calculated using the surviving gamma-ray like events and equation 17 in Li & Ma (1983). 3. VERITAS Results The analysis resulted in 595 events recorded in the source region and 3054 events in the selected background region. The geometrical background region selected was 7.7 35Cygnus X-3 is 0.5◦ south of TeV J2032+4130.