FIRST<i>NuSTAR</i>OBSERVATIONS OF MRK 501 WITHIN A RADIO TO TeV MULTI-INSTRUMENT CAMPAIGN

Furniss, A.; Noda, K.; Boggs, Steven E.; Chiang, J.; Christensen, Finn Erland; Craig, William W.; Giommi, P.; Hailey, C. J.; Harisson, F.; Madejski, G. M.; Nalewajko, Krzysztof; Perri, M.; Stern, Daniel; Urry, C. Megan; Verrecchia, F.; Zhang, W.; Ahnen, M. L.; Ansoldi, S.; Antonelli, L. A.; Antoranz, P.; Babić, Ana; Banerjee, B.; Bangale, P.; Almeida, U. Barres de; Barrio, J. A.; González, J. Becerra; Bednarek, W.; Bernardini, E.; Biasuzzi, B.; Biland, A.; Blanch, O.; Bonnefoy, S.; Bonnoli, G.; Borracci, F.; Bretz, T.; Carmona, E.; Carosi, A.; Chatterjee, A.; Clavero, R.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; Vela, P. Da; Dazzi, F.; Angelis, A. De; Caneva, G. De; Lotto, B. De; Wilhelmi, E. de Oña; Mendez, C. Delgado; Pierro, F. Di; Prester, D. Dominis; Dorner, D.; Doro, M.; Einecke, S.; Glawion, D.; Elsäesser, D.; Fernández-Barral, A.; Fidalgo, D.; Fonseca, M. V.; Font, L.; Frantzen, K.; Fruck, C.; Galindo, D.; López, R. J. García; Garczarczyk, M.; Terrats, D. Garrido; Gaug, M.; Giammaria, P.; Godinović, N.; Muñoz, A. González; Guberman, D.; Hanabata, Y.; Hayashida, M.; Herrera, Javier; Hose, J.; Hrupec, Dario; Hughes, G.; Idec, W.; Kellermann, H.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Barbera, A. La; Lelas, D.; Lewandowska, N.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; López-Oramas, A.; Lorenz, E.; Majumdar, P.; Makariev, M.; Mallot, K.; Maneva, G.; Manganaro, M.; Mannheim, K.; Maraschi, L.; Marcote, B.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Menzel, U.; Miranda, J. M.; Mirzoyan, R.; Moralejo, A.; Nakajima, D.; Neustroev, V.; Niedźwiecki, A.; Rosillo, M. Nievas; Nilsson, K.; Nishijima, K.; Orito, R.; Overkemping, A.; Paiano, S.; Palacio, J.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Paredes-Fortuny, X.; Peršić, M.; Poutanen, Juri; Moroni, P. G. Prada; Prandini, E.; Puljak, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Garcia, J. Rodriguez; Saito, T.; Saito, Koji; Satalecka, K.; Scapin, V.; Schultz, C.; Schweizer, T.; Shore, S. N.; Sillanpää, A.; Sitarek, J.; Šnidarić, Iva; Sobczyńska, D.; Stamerra, A.; Steinbring, T.; Strzys, M.; Takalo, L. O.; Takami, H.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thaele, J.; Torres, D. F.; Toyama, Takeshi; Treves, A.; Verguilov, V.; Vovk, Ievgen; Will, Martin; Zanin, R.; Archer, A.; Benbow, W.; Bird, R.; Biteau, J.; Bugaev, V.; Cardenzana, J. V; Cerruti, M.; Chen, X.; Ciupik, L.; Connolly, Michael; Cui, Wei; Dickinson, H. J.; Dumm, J.; Eisch, J.; Falcone, A.; Feng, Q.; Finley, J. P.; Fleischhack, Henrike; Fortin, P.; Fortson, L.; Gérard, L.; Gillanders, G. H.; Griffin, S.; Griffiths, S.; Grube, J.; Gyuk, G.; Håkansson, N.; Holder, J.; Humensky, T. B.; Johnson, C. A.; Kaaret, Philip; Kertzman, M.; Kieda, D.; Krause, M.; Krennrich, F.; Lang, M. J.; Lin, T. T. Y.; Maier, G.; McArthur, S.; McCann, A.; Meagher, K.; Moriarty, P.; Mukherjee, R.; Nieto, D.; Bhróit, A. O’Faoláin de; Ong, R. A.; Park, N.; Petry, D.; Pohl, M.; Popkow, A.; Ragan, K.; Ratliff, G.; Reyes, Luis; Reynolds, P. T.; Richards, G.; Roache, E.; Santander, M.; Sembroski, G. H.; Shahinyan, K.; Staszak, D.; Telezhinsky, I.; Tucci, J. V.; Tyler, J.; Vassiliev, V. V.; Wakely, S. P.; Weiner, O. M.; Weinstein, A. J.R.; Wilhelm, A.; Williams, D. A.; Zitzer, B.; Vince, O.; Fuhrmann, L.; Angelakis, E.; Karamanavis, V.; Myserlis, I.; Krichbaum, T. P.; Zensus, J. A.; Ungerechts, H.; Sievers, A.; Bachev, R.; Böttcher, M.; Chen, W. P.; Damljanović, G.; Eswaraiah, Chakali; Güver, T.; Hovatta, T.; Hughes, Zachary; Ibryamov, S.; Joner, M. D.; Jordan, B.; Jorstad, S. G.; Joshi, M.; Kataoka, J.; Kurtanidze, O. M.; Kurtanidze, S. O.; Lähteenmäki, A.; Latev, G.; Lin, H. C.; Larionov, V. M.; Mokrushina, A. A.; Morozova, D. A.; Nikolashvili, M. G.; Raiteri, C. M.; Ramakrishnan, Venkatessh; Readhead, A. C. R.; Sadun, A. C.; Sigua, L. A.; Semkov, E.; Strigachev, A.; Tammi, J.; Tornikoski, M.; Troitskaya, Yu. V.; Troitsky, I. S.; Villata, M.

doi:10.1088/0004-637x/812/1/65

Cited by 60 publications

(58 citation statements)

References 77 publications

(94 reference statements)

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“…Since we detect a linear relationship, this would argue that the scattering cross section is diminished, possibly because the scattering takes place in the less efficient Klein-Nishina regime. For example, a quadratic relation has recently been observed in a similar HBL object, Mrk 501 (Furniss et al 2015). It has been shown previously (e.g., Katarzyński et al 2005) that this implication is valid only if the normalization of the entire electron distribution is changed to produce flux variations.…”

Section: Correlated Variability In the X-ray And Vhe Spectral Bandsmentioning

confidence: 86%

“…Note that the vertical scale is linear in all panels, but has a different dynamic range in each one. often directly observable in the Swift-XRT band, as in other similar HBL sources (e.g., Tramacere et al 2007a;Furniss et al 2015). Its location in frequency space can be estimated from the UV/optical and X-ray data, using a reasonable smooth interpolation or extrapolation model (e.g., Massaro et al 2004;Błażejowski et al 2005;Tramacere et al 2009;Ushio et al 2010).…”

Section: The Peak Of the Synchrotron Sed Componentmentioning

confidence: 99%

See 1 more Smart Citation

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

Baloković¹,

Paneque²,

Madejski³

et al. 2016

ApJ

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113

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We present coordinated multiwavelength observations of the bright, nearby BL Lacertae object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very high energy(VHE) γ-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep 3 G » power law, with no evidence for an exponential cutoff or additional hard components up to ∼80keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure that relates to the two bumps of the broadband SED. In each bump, the variability increases with energy, which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in situ electron acceleration and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states.

show abstract

Section: Correlated Variability In the X-ray And Vhe Spectral Bandsmentioning

confidence: 86%

Section: The Peak Of the Synchrotron Sed Componentmentioning

confidence: 99%

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

Baloković¹,

Paneque²,

Madejski³

et al. 2016

ApJ

Self Cite

113

View full text Add to dashboard Cite

show abstract

“…Figure 2 presents the four very fast instances from the 3-79 keV observations of Mrk 421 performed on 6 and 12 February 2013 with NuSTAR (see Table 3 for the corresponding summary). The observations at hard X-ray frequencies provide a direct insight into the highest energy particles through detection of synchrotron emission [25]. Moreover, the NuSTAR observations allow us to study the properties of the lower energy particles via the detection of the IC-emission produced via the photon upscattering by lower energy electrons.…”

Section: X-ray Microvariability Within 1 Ks Intervalsmentioning

confidence: 99%

“…The work in [22] revealed a VHE flux-doubling time of about 36 min from the MAGIC observation of Mrk 421 performed on 29 April 2006. In the case of Mrk 501 (z = 0.034), the most extreme variability with flux-doubling times down to 2 min and flux variations by a factor of 10 in less than one hour was reported by [23] from the MAGIC observations performed on 30 June and 9 June 2005. Moreover, it underwent an extreme VHE variability during the HEGRAobservations in April 1997, boosting its brightness by a factor 20 [24], and the MAGIC campaign showed a variability by a factor of 23, including a flare by a factor of four in 4 d in April-August 2013 [25]. Finally, the source showed a flux-doubling time shorter than 10 min during the HESSobservations of 23-24 June 2014 [26].…”

Section: Introductionmentioning

confidence: 96%

Sub-Hour X-Ray Variability of High-Energy Peaked BL Lacertae Objects

Kapanadze

2018

Galaxies

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Abstract:The study of multi-wavelength flux variability in BL Lacertae objects is very important to discern unstable processes and emission mechanisms underlying their extreme observational features. While the innermost regions of these objects are not accessible from direct observations, we may draw conclusions about their internal structure via the detection of flux variations on various timescales, based on the light-travel argument. In this paper, we review the sub-hour X-ray variability in high-energy peaked BL Lacertae sources (HBLs) that are bright at X-rays and provide us with an effective tool to study the details related to the physics of the emitting particles. The X-ray emission of these sources is widely accepted to be a synchrotron radiation from the highest-energy electrons, and the complex spectral variability observed in this band reflects the injection and radiative evolution of freshly-accelerated particles. The detection of sub-hour X-ray flux variability is very important since it can be related to the small-scale jet turbulent structures or triggered by unstable processes occurring in the vicinity of a central supermassive black hole. We summarize the fastest X-ray variability instances detected in bright HBLs and discuss their physical implications.

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“…Regular multi-wavelength campaigns have been carried out since 2009 [3,4,5], but the monitoring data are still rather sparse [7].…”

Section: Status Of Monitoring At Tev Energiesmentioning

confidence: 99%

Monitoring at TeV Energies with M@TE

Alfaro¹,

Bernal²,

Bretz³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Blazars are extremely variable objects emitting radiation across the electromagnetic spectrum and showing variability on time scales from minutes to years. Simultaneous multi-wavelength observations are crucial for understanding the emission mechanisms. In particular the study of their TeV emission is relevant to test the dominant radiative process at such energies (e.g. leptonic models predict a correlation between X-ray and TeV emission). As well, the correlation with the bump at low energy or the possible common detection with a neutrino signal can be relevant to constrain the physical model. From radio via optical and from X-ray to gamma rays, a variety of instruments, as OVRO and Fermi, are already monitoring blazars. At TeV energies, long-term monitoring is currently carried out by HAWC and FACT. Towards 24/7 continuous observations, the goal is to have similar monitoring telescopes at locations around the globe in order to close temporal gaps and compile light curves with homogeneous sensitivity. With the M@TE (Monitoring at TeV energies) project, we are planning to install an Imaging Air Cherenkov Telescope equipped with an improved version of the FACT camera and the mechanical structure of one of the mounts of the HEGRA experiment at the site of San Pedro Mártir in Mexico. Featuring excellent observation conditions, this location provides a variety of instruments from radio to optical wavelength allowing for coordinated multi-wavelength blazar studies. In this work, we will present the status of the project.

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FIRSTNuSTAROBSERVATIONS OF MRK 501 WITHIN A RADIO TO TeV MULTI-INSTRUMENT CAMPAIGN

Cited by 60 publications

References 77 publications

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

Sub-Hour X-Ray Variability of High-Energy Peaked BL Lacertae Objects

Monitoring at TeV Energies with M@TE

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