Multiwavelength Examination of the<i>COS B</i>Field 2CG 075+00 Yields a Blazar Identification for 3EG J2016+3657

Mukherjee, R.; Gotthelf, E. V.; Halpern, J. P.; Tavani, M.

doi:10.1086/317054

Cited by 43 publications

(57 citation statements)

References 43 publications

(44 reference statements)

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“…Often additional information from observations at other wave bands is used to aid in the identification of the EGRET sources. Progress has been made with recent studies in the X-ray band carried out for several EGRET fields (e.g., Roberts, Rowani, & Kawai 2001) and used to suggest counterparts for a few unidentified EGRET sources, such as 3EG J2227+6122 (Halpern et al 2001a), 3EG J1835+5918 (Mirabal et al 2000;Mirabal & Halpern 2001;Reimer et al 2001), and 3EG J2016+2657 (Mukherjee et al 2000;Halpern et al 2001b).…”

Section: Introductionmentioning

confidence: 99%

Is the EGRET Source 3EG J1621+8203 the Radio Galaxy NGC 6251?

Mukherjee

Halpern

Mirabal

et al. 2002

ApJ

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We discuss the nature of the unidentified EGRET source 3EG J1621+8203. In an effort to identify the gamma-ray source, we have examined X-ray images of the field from ROSAT PSPC, ROSAT HRI, and ASCA GIS. Of the several faint X-ray point sources in the error circle of 3EG J1621+8203, most are stars or faint radio sources, unlikely to be counterparts to the EGRET source. The most notable object in the gamma-ray error box is the bright FR I radio galaxy NGC 6251. If 3EG J1621+8203 corresponds to NGC 6251, then it would be the second radio galaxy to be detected in high-energy gamma rays after Cen A, which provided the first clear evidence of the detection above 100 MeV of an active galactic nucleus (AGN) with a large-inclination jet. If the detection of more radio galaxies by EGRET has been limited by its threshold sensitivity, there exists the exciting possibility that new high-energy gamma-ray instruments, with much higher sensitivity, will detect a larger number of radio galaxies in the future.

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Section: Introductionmentioning

confidence: 99%

Is the EGRET Source 3EG J1621+8203 the Radio Galaxy NGC 6251?

Mukherjee

Halpern

Mirabal

et al. 2002

ApJ

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“…3EG J2016+3657 was identified in a detailed study that was carried out on archival X-ray data, with follow-up optical observations of the γ-ray error box (Mukherjee et al 2000). The identification was soon confirmed by Halpern et al (2001), who concluded that B2013+370 was the most likely counterpart, after optical spectroscopic identifications of all the soft and hard X-ray sources in the error circle of the EGRET source eliminated the other candidates.…”

Section: A Blazar Counterpart For 3eg J2016+3657mentioning

confidence: 97%

“…In fact 2CG 078+2 (3EG J2020+4017) was thought to be a counterpart of the supernova remnant (SNR) γ-Cygni. Multiwavelength measurements were used to identify counterparts of 3EG J2016+3657 (Mukherjee et al 2000;Halpern et al 2001) and of 3EG J2020+4017 (Becker et al 2004;Weisskopf et al 2006;Bykov et al 2004Bykov et al , 2006 with some success.…”

Section: Introductionmentioning

confidence: 99%

Gamma-ray absorption method (GRAM) application to the identification of EGRET unidentified sources

Iyudin

Burwitz

Greiner

et al. 2007

A&A

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Recently we reported the very first detection of γ-ray resonant absorption along the line of sight toward γ-ray bright quasars (QSOs) like 3C 273, 3C 279, PKS 0528+0134, and BL Lacertae. These detections resulted from the analysis of absorption troughs in SEDs derived on the base of mostly EGRET data that were collected during monitoring campaigns of the Virgo and galactic anticenter regions by the Compton Gamma Ray Observatory (CGRO), as well as during ToO observations of QSOs flares. Among three resonant absorption mechanisms that affect the γ-ray spectrum of point-like sources, we now pinpoint the ∆-isobar resonance that has a very stable peak energy of the absorption cross-section for all elements (nuclei) and for individual nucleons. From two absorbers that are usually detected on the sight lines towards γ-ray bright QSOs, we concentrate here on the only one that is at the QSO rest frame. We discuss the advantages and drawbacks of this method distinguishing between a galactic and extragalactic origin of the EGRET unidentified sources (EUIDs). This is compared to the multiwavelength identification approach that was succesfully used in a few cases to identify galactic and extragalactic objects among EUIDs. We applied the GRAM to identifying two of the EGRET unidentified sources as blazars, and predict their respective redshifts.

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“…The location of MGRO J2019+37 is consistent with those of the EGRET sources 3EG J2016+3657 and 3EG J2021+3716. The first of them is positionally coincident with the blazar-like source B2013+370 (G74.87+1.22) (Mukherjee et al 2000;Halpern et al 2001), although this blazar is well outside the inner box of MGRO J2019+37. The second is marginally coincident with the pulsar wind nebula PWN G75.2+0.1 (Hessels et al 2004).…”

Section: Observationsmentioning

confidence: 98%

Radio continuum and near-infrared study of the MGRO J2019+37 region

Paredes¹,

Martı́²,

Ishwara‐Chandra³

et al. 2009

A&A

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Context. MGRO J2019+37 is an unidentified extended source of very high energy gamma-rays originally reported by the Milagro Collaboration as the brightest TeV source in the Cygnus region. Its extended emission could be powered by either a single or several sources. The GeV pulsar AGL J2020.5+3653, discovered by AGILE and associated with PSR J2021+3651, could contribute to the emission from MGRO J2019+37. Aims. Our aim is to identify radio and near-infrared sources in the field of the extended TeV source MGRO J2019+37, and study potential counterparts to explain its emission. Methods. We surveyed a region of about 6 square degrees with the Giant Metrewave Radio Telescope (GMRT) at the frequency 610 MHz. We also observed the central square degree of this survey in the near-infrared K s -band using the 3.5 m telescope in Calar Alto. Archival X-ray observations of some specific fields are included. VLBI observations of an interesting radio source were performed. We explored possible scenarios to produce the multi-TeV emission from MGRO J2019+37 and studied which of the sources could be the main particle accelerator.Results. We present a catalogue of 362 radio sources detected with the GMRT in the field of MGRO J2019+37, and the results of a cross-correlation of this catalog with one obtained at near-infrared wavelengths, which contains ∼3 × 10 5 sources, as well as with available X-ray observations of the region. Some peculiar sources inside the ∼1 • uncertainty region of the TeV emission from MGRO J2019+37 are discussed in detail, including the pulsar PSR J2021+3651 and its pulsar wind nebula PWN G75.2+0.1, two new radio-jet sources, the H ii region Sh 2-104 containing two star clusters, and the radio source NVSS J202032+363158. We also find that the hadronic scenario is the most likely in case of a single accelerator, and discuss the possible contribution from the sources mentioned above. Conclusions. Although the radio and GeV pulsar PSR J2021+3651 / AGL J2020.5+3653 and its associated pulsar wind nebula PWN G75.2+0.1 can contribute to the emission from MGRO J2019+37, extrapolation of the GeV spectrum does not explain the detected multi-TeV flux. Other sources discussed here could contribute to the emission of the Milagro source.Key words. gamma rays: observations -H ii regions -infrared: stars -radio continuum: stars -X-rays: binaries Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via

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Multiwavelength Examination of theCOS BField 2CG 075+00 Yields a Blazar Identification for 3EG J2016+3657

Cited by 43 publications

References 43 publications

Is the EGRET Source 3EG J1621+8203 the Radio Galaxy NGC 6251?

Is the EGRET Source 3EG J1621+8203 the Radio Galaxy NGC 6251?

Gamma-ray absorption method (GRAM) application to the identification of EGRET unidentified sources

Radio continuum and near-infrared study of the MGRO J2019+37 region

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