LONG-TERM TeV AND X-RAY OBSERVATIONS OF THE GAMMA-RAY BINARY HESS J0632+057

Aliu, E.; Archambault, S.; Aune, T.; Behera, B.; Beilicke, M.; Benbow, W.; Berger, K.; Bird, R.; Bouvier, A.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cerruti, M.; Chen, X.; Ciupik, L.; Connolly, Michael; Cui, Wei; Duke, C.; Dumm, J.; Errando, M.; Falcone, A.; Federici, S.; Feng, Q.; Finley, J. P.; Fortin, P.; Fortson, L.; Furniss, A.; Galante, N.; Gillanders, G. H.; Griffin, S.; Griffiths, S.; Grube, J.; Gyuk, G.; Hanna, D.; Holder, J.; Hughes, G.; Humensky, T. B.; Kaaret, Philip; Kertzman, M.; Khassen, Y.; Kieda, D.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Madhavan, A. S.; Maier, G.; Majumdar, P.; McCann, A.; Moriarty, P.; Mukherjee, R.; Nieto, D.; Bhróithe, A. O'Faoláin De; Ong, R. A.; Otte, A. N.; Park, N.; Perkins, J. S.; Pohl, M.; Popkow, A.; Prokoph, H.; Quinn, J.; Ragan, K.; Rajotte, Jean-François; Reyes, Luis; Reynolds, P. T.; Richards, G.; Roache, E.; Rousselle, J.; Sembroski, G. H.; Sheidaei, F.; Skole, C.; Smith, A. W.; Staszak, D.; Stroh, M. C.; Telezhinsky, I.; Theiling, M.; Tucci, J. V.; Tyler, J.; Varlotta, A.; Vincent, Stéphane; Wakely, S. P.; Weinstein, A. J.R.; Welsing, R.; Williams, D. A.; Zajczyk, A.; Zitzer, B.; Abramowski, A.; Aharonian, F.; Benkhali, F. Ait; Akhperjanian, A. G.; Angüner, E. O.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Tjus, J. Becker; Bernlöhr, K.; Birsin, E.; Bissaldi, E.; Biteau, J.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Carrigan, S.; Casanova, S.; Chadwick, P. M.; Chalmé-Calvet, R.; Chaves, R. C. G.; Cheesebrough, A.; Chrétien, M.; Colafrancesco, S.; Cologna, G.; Conrad, J.; Couturier, C.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; deWilt, P.; Dickinson, H. J.; Djannati‐Ataï, A.; Domainko, W.; Drury, L. O’c.; Dubus, G.; Dutson, K.; Dyks, J.; Dyrda, M.; Edwards, T.; Egberts, K.; Eger, P.; Espigat, P.; Farnier, C.; Fegan, S. J.; Feinstein, F.; Fernandes, M. V.; Fernández, D.; Fiaßon, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gajdus, M.; Gallant, Y. A.; Garrigoux, T.; Giavitto, G.; Giebels, B.; Glicenstein, J. F.; Grondin, M.-H.; Grudzińska, M.; Häffner, S.; Hahn, Joachim; Harris, J.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hervet, O.; Hillert, Andreas; Hinton, J. A.; Hofmann, W.; Hofverberg, P.; Holler, M.; Horns, D.; Jachołkowska, A.; Jahn, C.; Jamrozy, M.; Janiak, M.; Jankowsky, F.; Jung, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Khélifi, B.; Kieffer, Michel; Klepser, S.; Klochkov, D.; Kluźniak, W.; Kneiske, T.; Kolitzus, D.; Komin, Nu.; Kosack, K.; Krakau, S.; Krayzel, F.; Krüger, P. P.; Laffon, H.; Lamanna, G.; Lefaucheur, J.; Lemière, A.; Lemoine‐Goumard, M.; Lenain, J.‐P.; Lennarz, D.; Löhse, T.; Lopatin, A.; Lu, Chia-Chun; Marandon, V.; Marcowith, A.; Marx, R.; Maurin, G.; Maxted, N.; Mayer, M.; McComb, T. J. L.; Méhault, J.; Menzler, U.; Meyer, M.; Moderski, R.; Mohamed, M.; Moulin, Emmanuel; Murach, T.; Naumann, C. L.; Naurois, M. de; Niemiec, J.; Nolan, S. J.; Oakes, L.; Ohm, S.; Oña-Wilhelmi, E.; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, R. D.; Arribas, M. Paz; Pekeur, N. W.; Pelletier, G.; Pérez, J.; Petrucci, Pierre-Olivier; Peyaud, B.; Pita, S.; Poon, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Raue, M.; Reimer, O.; Renaud, M.; Reyes, R. de los; Rieger, F.; Rob, L.; Romoli, C.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Sánchez, David; Santangelo, A.; Schlickeiser, R.; Schüßler, F.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Sol, H.; Spengler, G.; Spies, F.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Szostek, A.; Tavernet, J.‐P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tluczykont, M.; Trichard, C.; Valerius, K.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Viana, A.; Vincent, P.; Völk, H. J.; Volpe, F.; Vorster, M.; Wagner, S. J.; Wagner, P.; Ward, M. J.; Weidinger, M.; Weitzel, Q.; White, R.; Wierzcholska, A.; Willmann, P.; Wörnlein, A.; Wouters, D.; Zacharias, M.; Zdziarski, A. A.; Zech, A.; Zechlin, H. S.

doi:10.1088/0004-637x/780/2/168

Cited by 48 publications

(79 citation statements)

References 75 publications

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“…In this context, the object exhibits a main outburst, at TeV and X-rays, at orbital phases ∼0.3 and a secondary lower outburst at orbital phases ∼0.7 (Aliu et al 2014). Therefore, one might expect the geometry of the circumstellar envelope to also change during these phases.…”

Section: Discussionmentioning

confidence: 99%

“…Multicolour polarimetry for HESS J0632+057 from this work (Set "I" and Set "II") and polarimetric data of "UBV" monitoring early published by Yudin & Evans (1998 or phase 0.006 (if the period is 321 days) (see Aliu et al (2014)). The Set "II" observations fall at a phase of 0.975 (for 315 days), or 0.826 (for 321 days).…”

Section: Observationsmentioning

confidence: 99%

“…Assuming the orbital phase 0 is at T0=MJD 2454857 (Aliu et al 2014), the date of Set "I" observations correspond to an orbital phase of 0.140 (if the period is 315 days), Table 2. Multicolour polarimetry for HESS J0632+057 from this work (Set "I" and Set "II") and polarimetric data of "UBV" monitoring early published by Yudin & Evans (1998 or phase 0.006 (if the period is 321 days) (see Aliu et al (2014)).…”

Section: Observationsmentioning

confidence: 99%

“…The object displays periodic variations on several different timescales. The most pronounced variations, derived from X-ray data, were detected with a period of 315 +6 −4 (or 321±5) days (Aliu et al 2014) which is considered to be the orbital period of the binary system. Other variability includes:…”

Section: Introductionmentioning

confidence: 99%

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First multicolour polarimetry of TeV γ-ray binary HESS J0632+057 close to periastron passage

Yudin¹,

Potter²,

Townsend³

2016

Mon. Not. R. Astron. Soc.

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(2014) to identify the wavelength dependence of the intrinsic polarisation in HESS J0632+057. It was found that after subtraction of the interstellar component (for both p is estimates), the wavelength dependence of the intrinsic polarisation in HESS J0632+057 is essentially flat. We propose that the formation of an additional source of polarisation or some perturbation of circumstellar material at this orbital phase can explain the changes in the level of polarisation in HESS J0632+057 close to periastron passage.

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Section: Discussionmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

First multicolour polarimetry of TeV γ-ray binary HESS J0632+057 close to periastron passage

Yudin¹,

Potter²,

Townsend³

2016

Mon. Not. R. Astron. Soc.

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“…[6] and MAGIC [7] revealed a pattern of variability, with significant gamma-ray emission above 1 TeV in two different phases ranges of the orbit. The orbital period of the binary system of (315 ± 5) days has been derived from X-ray data [6], the orbital solution obtained from radial spectroscopy measurements at optical wavelengths points towards an eccentric orbit (e ≈ 0.83, [8]). HESS J0632+057 is the only gamma-ray binary which has not been detected at MeV-GeV energies with the Fermi LAT [9].…”

Section: Introductionmentioning

confidence: 99%

Long-term TeV Observations of the Gamma-ray Binary HESS J0632+057 with VERITAS

Maier¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The gamma-ray binary HESS J0632+057 has been observed at very-high energies for almost ten years by all major systems of imaging atmospheric Cherenkov telescopes. We present new observations taken by the VERITAS observatory and an updated analysis of the previously published observations. HESS J0632+057 has been detected by VERITAS with a total significance > 20σ at energies above 350 GeV in about 200 hours of observations. The exposure covers now almost the entire orbital period of 315 days including the flux enhancements at phases ≈0.35 and, for the first time, detected with VERITAS, at phases ≈0.75. The results are discussed along with simultaneous observations by the X-ray satellite Swift XRT.

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X‐ray observations of Galactic H.E.S.S. sources: An update

et al. 2017

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X‐ray diagnostics of TeV (teraelectronvolt) sources continues to be an important tool to identify the nature of newly detected sources as well as to pinpoint the physics processes that are at work in these highly energetic objects. This paper gives a review of recent studies that have been performed on TeV sources with H.E.S.S. and XMM‐Newton and also other X‐ray facilities. Here, we mainly focus on the galactic object types γ‐ray binaries and supernova remnants (SNRs). γ‐ray binaries form a small class of objects whose identification and study is challenging because of the sometimes very long orbital periods that need to be established from data. Particular emphasis is given to SNR studies, including recently identified SNRs such as HESS J1731−347 and HESS J1534−571, as well as a revisit of RX J1713.7−3946.

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LONG-TERM TeV AND X-RAY OBSERVATIONS OF THE GAMMA-RAY BINARY HESS J0632+057

Abstract: • a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.

Cited by 48 publications

References 75 publications

First multicolour polarimetry of TeV γ-ray binary HESS J0632+057 close to periastron passage

First multicolour polarimetry of TeV γ-ray binary HESS J0632+057 close to periastron passage

Long-term TeV Observations of the Gamma-ray Binary HESS J0632+057 with VERITAS

X‐ray observations of Galactic H.E.S.S. sources: An update

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