VERY HIGH ENERGY
                    <i>γ</i>
                    -RAYS FROM THE UNIVERSE’S MIDDLE AGE: DETECTION OF THE
                    <i>z</i>
                    = 0.940 BLAZAR PKS 1441+25 WITH MAGIC

Ahnen, M. L.; Ansoldi, S.; Antonelli, L. A.; Antoranz, P.; Babić, Ana; Banerjee, B.; Bangale, P.; Almeida, U. Barres de; Barrio, J. A.; 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; 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.; Barral, Alba Fernández; 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.; Hahn, Alexander; Hanabata, Y.; Hayashida, M.; Herrera, J.; Hose, J.; Hrupec, Dario; Hughes, G.; Idec, W.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Barbera, A. La; Lelas, D.; Lindfors, E.; Lombardi, S.; López, M.; Coto, Rubén López; 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.; Moretti, E.; Nakajima, D.; Neustroev, V.; Niedźwiecki, A.; Rosillo, M. Nievas; Nilsson, K.; Nishijima, K.; Noda, K.; Orito, R.; Overkemping, A.; Paiano, S.; Palacio, J.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Fortuny, X. Paredes; Peršić, M.; Poutanen, Juri; Moroni, Pier Giorgio Prada; Prandini, E.; Puljak, I.; Rhode, W.; Ribó, M.; Rico, J.; Garcia, J. Rodriguez; Saito, T.; Satalecka, K.; Schultz, C.; Schweizer, T.; Shore, Steven 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; Ward, J. E.; Will, Martin; H., Wu M.; Zanin, R.; Ajello, M.; Baldini, Luca; Barbiellini, G.; Bastieri, D.; González, J. Becerra; Bellazzini, R.; Bissaldi, E.; Blandford, R. D.; Bonino, R.; Bregeon, J.; Bruel, Pascal; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caragiulo, M.; Caraveo, P. A.; Cavazzuti, E.; Chiang, J.; Chiaro, G.; Ciprini, S.; D’Ammando, F.; Palma, F. de; Desiante, R.; Venere, L. Di; Domínguez, A.; Fusco, P.; Gargano, F.; Gasparrini, D.; Giglietto, N.; Giordano, F.; Giroletti, M.; Grenier, I. A.; Guiriec, S.; Hays, E.; Hewitt, J. W.; Jogler, T.; Kuss, M.; Larsson, Stefan; Li, J.; Li, L.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Maldera, S.; Mayer, M.; Mazziotta, M. N.; McEnery, J. E.; Mirabal, N.; Mizuno, T.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Nuss, E.; Ojha, R.; Ohsugi, T.; Omodei, N.; Orlando, E.; Perkins, J. S.; Pesce-Rollins, M.; Piron, F.; Pivato, G.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Sgrò, C.; Siskind, E. J.; Spada, F.; Spandre, G.; Spinelli, P.; Tajima, H.; Takahashi, H.; Thayer, J. B.; Thompson, D. J.; Troja, E.; Wood, K. S.; Baloković, Mislav; Berdyugin, A.; Carramiñana, A.; Carrasco, L.; Chavushyan, V.; Ramazani, Vandad Fallah; Feige, Martin; Haarto, S.; Haeusner, P.; Hovatta, T.; Kania, J.; Klamt, J.; Lähteenmäki, A.; Leon-Tavares, J.; Lorey, Christian; Pacciani, L.; Porras, A.; Recillas, E.; Reinthal, R.; Tornikoski, M.; Wolfert, D.; Zottmann, Nils

doi:10.1088/2041-8205/815/2/l23

Cited by 98 publications

(58 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, the shift in the synchrotron peak position during the flaring state puts it in the range of Intermediate-Synchrotron-Peaked (ISP) objects. Such a behavior has been observed before in the case of the LSP blazar PKS 1441+25, which showed an HSP-like SED during the elevated state which led to its TeV detection (Ahnen et al 2015). Another example of a similar time-dependent SED classification is the FSRQ 4C +49.22 (Cutini et al 2014).…”

Section: Discussionsupporting

confidence: 68%

“…During all the flaring states, the peaks of both the synchrotron and Compton components of the SED shift to higher frequencies. This is similar to the flares detected by the FSRQ PKS 1441+25 (Abeysekara et al 2015;Ahnen et al 2015), although in that case the shift was even more extreme. For PKS 1441+25 the synchrotron peak was as high as ≈ 10 15 Hz, while for the flares from PKS 0346−27 reported here the peak reaches a frequency of 10 14.5 Hz.…”

Section: Sed Modelingsupporting

confidence: 78%

“…This implies that their place in classification schemes such as the ones mentioned above should be considered as time-dependent. Exemplary cases of time-dependent blazar classification are PKS 2155−304 (Foschini et al 2008), PKS 1510−089 (D'Ammando et al 2011), PMN J2345−1555 (Ghisellini et al 2013), 4C +49.22 (Cutini et al 2014) and PKS 1441+25 (Ahnen et al 2015).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The large gamma-ray flare of the flat-spectrum radio quasar PKS 0346−27

Angioni

Nesci²,

Finke³

et al. 2019

A&A

Self Cite

View full text Add to dashboard Cite

Aims. In this paper, we characterize the first γ-ray flaring episode of the FSRQ PKS 0346−27 (z = 0.991), as revealed by Fermi-LAT monitoring data, and the concurrent multi-wavelength variability observed from radio through X-rays. Methods. We study the long and short term flux and spectral variability from PKS 0346−27 by producing γ-ray light curves with different time binning. We complement the Fermi-LAT data with multi-wavelength observations from ALMA (radio mm-band), REM (NIR) and Swift (optical-UV, X-rays). This quasi-simultaneous multi-wavelength coverage allowed us to construct time-resolved spectral energy distributions (SEDs) of PKS 0346−27, and compare the broadband spectral properties of the source between different activity states using a one-zone leptonic emission model. Results. PKS 0346−27 entered an elevated γ-ray activity state starting from the beginning of 2018. The high-state continued throughout the year, displaying the highest fluxes in May 2018. We find evidence of short-time scale variability down to ∼ 1.5 hours, which constrains the γ-ray emission region to be compact. The extended flaring period was characterized by a persistently harder spectrum with respect to the quiescent state, indicating changes in the broadband spectral properties of the source. This was confirmed by the multi-wavelength observations, which show a shift in the position of the two SED peaks by ∼ 2 orders of magnitude in energy and peak flux value. As a result, during the high state the non-thermal jet emission completely outshines the thermal contribution from the dust torus and accretion disk. The broadband SED of PKS 0346−27 transitions from a typical Low-Synchrotron-Peaked (LSP) to the Intermediate-Synchrotron-Peaked (ISP) class, a behavior previously observed in other flaring γ-ray sources. Our one-zone leptonic emission model of the high-state SEDs constrains the γ-ray emission region to have a lower magnetic field, larger radius, and higher maximum electron Lorentz factors with respect to the quiescent SED. Finally, we note that the bright and hard γ-ray spectrum observed during the peak of flaring activity in May 2018 implies that PKS 0346−27 could be a promising target for future ground-based Cherenkov observatories such as the Cherenkov Telescope Array (CTA). The CTA could detect such a flare in the low-energy tail of its energy range during a high state such as the one observed in May 2018.

show abstract

Section: Discussionsupporting

confidence: 68%

Section: Sed Modelingsupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The large gamma-ray flare of the flat-spectrum radio quasar PKS 0346−27

Angioni

Nesci²,

Finke³

et al. 2019

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…The similarity of the non-thermal (likely jet-dominated) components of the SEDs of γ-NLS1s and FSRQs seems to suggest that similar processes (i.e., external-Compton dominated γ-ray emission) may be at work in both classes of sources (e.g., Abdo et al 2009a;Berton et al 2016;Arrieta-Lobo et al 2017). Currently, seven FSRQs have been detected by IACTs (Mirzoyan 2017;Mukherjee & VERITAS Collaboration 2017;Cerruti et al 2017;Ahnen et al 2015;Abeysekara et al 2015;Sitarek et al 2015;Aleksić et al 2011;H.E.S.S. Collaboration et al 2013;MAGIC Collaboration et al 2008; also see TeVCat 5 for further references).…”

Section: Discussionmentioning

confidence: 99%

Prospects for gamma-ray observations of narrow-line Seyfert 1 galaxies with the Cherenkov Telescope Array

Romano

Vercellone

Foschini

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Gamma-ray emitting narrow-line Seyfert 1 (γ-NLS1) galaxies possibly harbour relatively low-mass black holes (10 6 -10 8 M ⊙ ) accreting close to the Eddington limit, and share many characteristics with their sibling sources, flat-spectrum radio quasars. Although they have been detected in the MeV-GeV band with Fermi-LAT, they have never been seen in the very high energy band with current imaging atmospheric Cherenkov telescopes (IACTs). Thus, they are key targets for the next-generation IACT, the Cherenkov Telescope Array (CTA). In a previous work we selected, by means of extensive simulations, the best candidates for a prospective CTA detection (SBS 0846+513, PMN J0948+0022, and PKS 1502+036) taking into account the effects of both the intrinsic absorption (approximated with a cut-off at 30 GeV), and the extra-galactic background light on the propagation of γ-rays. In this work we simulate the spectra of these three sources by adopting more realistic broad-line region (BLR) absorption models. In particular, we consider the detailed treatment of γ-γ absorption in the radiation fields of the BLR as a function of the location of the γ-ray emission region with parameters inferred from observational constraints. We find that, due to the energy range extent and its sensitivity, CTA is particularly well suited to locate the γ-ray emitting region in γ-NLS1. In particular CTA will be able not only to distinguish whether the γ-ray emitting region is located inside or outside the BLR, but also where inside the BLR it may be.

show abstract

“…With the recent detection by the MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes of VHE gamma-ray emission from two sources at a redshift z ∼ 0.94: QSO B0218+357 [1] and PKS1441+25 [2], the boundaries of the known gamma-ray universe nearly doubled. Observations of distant sources in VHE gamma-rays are strongly affected by an absorption in the extragalactic background light (EBL).…”

Section: Introductionmentioning

confidence: 99%

Broad Band Observations of Gravitationally Lensed Blazar during a Gamma-Ray Outburst

et al. 2016

View full text Add to dashboard Cite

QSO B0218+357 is a gravitationally lensed blazar located at a cosmological redshift of 0.944. In July 2014 a GeV flare was observed by Fermi-LAT, triggering follow-up observations with the MAGIC telescopes at energies above 100 GeV. The MAGIC observations at the expected time of arrival of the trailing component resulted in the first detection of QSO B0218+357 in Very-High-Energy (VHE, >100 GeV) gamma rays. We report here the observed multiwavelength emission during the 2014 flare.

show abstract

VERY HIGH ENERGY γ -RAYS FROM THE UNIVERSE’S MIDDLE AGE: DETECTION OF THE z = 0.940 BLAZAR PKS 1441+25 WITH MAGIC

Cited by 98 publications

References 37 publications

The large gamma-ray flare of the flat-spectrum radio quasar PKS 0346−27

The large gamma-ray flare of the flat-spectrum radio quasar PKS 0346−27

Prospects for gamma-ray observations of narrow-line Seyfert 1 galaxies with the Cherenkov Telescope Array

Broad Band Observations of Gravitationally Lensed Blazar during a Gamma-Ray Outburst

Contact Info

Product

Resources

About