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37th International Cosmic Ray Conference, ICRC 2021, Berlin, online, Germany, 12 Jul 2021 - 23 Jul 2021; Proceedings of Science / International School for Advanced Studies (ICRC2021), 773 (2021). doi:10.22323/1.395.0773, The Cherenkov Telescope Array (CTA) is the future ground-based observatory for gamma-ray astronomy at very high energies. The atmosphere is an integral part of every Cherenkov telescope. Different atmospheric conditions, such as clouds, can reduce the fraction of Cherenkov photons produced in air showers that reach ground-based telescopes, which may affect the performance. Decreased sensitivity of the telescopes may lead to misconstructed energies and spectra. This study presents the impact of various atmospheric conditions on CTA performance. The atmospheric transmission in a cloudy atmosphere in the wavelength range from 203 nm to 1000 nm was simulated for different cloud bases and different optical depths using the MODerate resolution atmospheric TRANsmission (MODTRAN) code. MODTRAN output files were used as inputs for generic Monte Carlo simulations. The analysis was performed using the MAGIC Analysis and Reconstruction Software (MARS) adapted for CTA. As expected, the effects of clouds are most evident at low energies, near the energy threshold. Even in the presence of dense clouds, high-energy gamma rays may still trigger the telescopes if the first interaction occurs lower in the atmosphere, below the cloud base. A method to analyze very high-energy data obtained in the presence of clouds is presented. The systematic uncertainties of the method are evaluated. These studies help to gain more precise knowledge about the CTA response to cloudy conditions and give insights on how to proceed with data obtained in such conditions. This may prove crucial for alert-based observations and time-critical studies of transient phenomena., Published by SISSA, Trieste

The MAGIC collaboration reports the first detection of very-high-energy (VHE ; E>100 GeV) gamma-ray emission from the flaring blazar TXS1515-273 (RA=15 18 03.610, Dec= -27 31 31.40, J2000.0). The object was observed with the MAGIC telescopes for 1.9 hours on 2019/02/28 under moderate moonlight in the zenith distance range 55 - 60 deg. The preliminary real-time analysis of this data shows a detection of TXS1515-273 with a statistical significance more than 5 standard deviations. The MAGIC observations were triggered by the flaring activity reported by Fermi-LAT from 2019/02/24 to 2019/02/25 (ATel#12532). Few hours before that ATel, a communication from Dave Thompson from the Fermi team alerted the MAGIC collaboration about this source. The redshift of this source is uncertain, with an upper limit z

The MAGIC telescopes performed a rapid follow-up observation of GRB 190114C (Gropp et al., GCN 23688 ; Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et al. GCN 23693, Selsing et al. GCN 23695). This observation was triggered by the Swift-BAT alert ; we started observing at about 50s after Swift T0: 20:57:03.19. The MAGIC real-time analysis shows a significance >20 sigma in the first 20 min of observations (starting at T0+50s) for energies >300GeV. The relatively high detection threshold is due to the large zenith angle of observations (>60 degrees) and the presence of partial Moon. Given the brightness of the event, MAGIC will continue the observation of GRB 190114C until it is observable tonight and also in the next days. We strongly encourage follow-up observations by other instruments. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and K. Noda (nodak@icrr.u-tokyo.ac.jp). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Observatory Roque de los Muchachos on the Canary island La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC telescopes have observed an increase in the very-high-energy (VHE ; >100 GeV) gamma-ray flux from a position compatible with the blazar BL Lacertae (RA=22h02m43.3s Dec=+42d16m40s, J2000.0, z=0.07). The preliminary analysis of 0.76 hours of MAGIC data taken on 2019/05/03 (MJD 58606.18 to 58606.20) under zenith angle range from 46 to 53 deg and dark time conditions with the atmospheric transmission of 0.85, indicates a flux larger than 0.1 of the flux from the Crab nebula above 200 GeV, and detection significance over 6 sigma. The MAGIC observations were triggered by the flaring activity at HE gamma-rays reported by Fermi-LAT (ATel #12718), and optical observations by Astronomical Observatory of the University of Siena (ATel #12722). MAGIC observations on BL Lacertae will continue during the next days and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and D. Dominis Prester (dijana@phy.uniri.hr) MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC telescopes have observed an unprecedented level of very-high-energy (VHE ; >100 GeV) gamma-ray flux from 1ES 1218+304 (12h21m21.941s, +30d10m37.11s, J2000.0). The preliminary analysis of the data from 2018/12/31 to 2019/01/02 indicates a VHE gamma-ray flux reaching the level of ~25 % of the flux from the Crab nebula above 100 GeV. Compared to the quiescent state reported by VERITAS, this implies an increase by a factor of ~4. The previous record of VHE gamma-ray flux of this source was ~20% of the flux from the Crab nebula above 100 GeV. It was measured by VERITAS on the night of 30 January 2009 (2010ApJ, 709L, 163A). 1ES 1218+304 is a high-synchrotron-peaked BL Lac object located at redshift z=0.182. It was first recognized as a VHE gamma-ray emitter by the MAGIC Collaboration in 2005 (Albert, J., 2006, ApJ, 642L, 119A). The MAGIC observations were triggered by the flaring activity in the optical R-band, measured by the KVA telescope from 2018/12/24 to 2019/01/02. The KVA data showed a flux of 2.35+/-0.05 mJy on 2019/01/02, which is the highest optical flux measurement from this source in a time span of 15 years (http://users.utu.fi/kani/1m/1ES_1218+304_jy.html). MAGIC observations on 1ES 1218+304 will continue during the next weeks and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), V. Fallah Ramazani (vafara@utu.fi) and M. Cerruti (matteo.cerruti@icc.ub.edu). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The VERITAS and MAGIC collaborations report the detection of an enhanced TeV gamma-ray flux from the pulsar/ Be-star binary system PSR J2032+4127/ MT91 213 (RA 20h32m13.13s, Dec +41d27m24.4s, J2000.0). The binary nature of this system was identified in 2015 through radio and gamma-ray timing observations (Lyne et al., MNRAS, 451, 581, 2015). The orbital period is estimated at 45-50 years, with periastron expected to occur around November 2017. The X-ray flux has been steadily increasing as the system approaches periastron (Bird et al., arXiv:1708.04718). PSR J2032+4127 is co-located with the extended TeV gamma-ray source, TeV J2032+4130, and may be physically associated with it. Both VERITAS and MAGIC observations were conducted as part of a coordinated long-term monitoring campaign. The source was observed most recently by VERITAS between 16 September and 27 September 2017 for a total exposure of 15.3 hours. In a preliminary analysis, the integral flux measured by VERITAS above 200 GeV is 4.2e-12 ± 0.7e-12 photons cm^-2 s^-1 (~2% of the Crab Nebula flux), corresponding to approximately twice the flux measured at the same location in archival VERITAS observations from spring 2017. The emission is consistent with a point source at the location of PSR J2032+4127, offset from the center of the previously known extended TeV source. The VERITAS source name is VER J2032+414. The statistical significance of the gamma-ray excess at the pulsar position is 6.8 standard deviations. MAGIC observations comprise 5.6 hours taken between 10 September and 25 September. A preliminary analysis of the MAGIC data indicates a flux of 5.6e-12 ± 1.2e-12 photons cm^-2 s^-1 above 200 GeV, which implies an increase by about a factor of 2 with respect to the mean flux observed by MAGIC in June-August 2017. The MAGIC source name is MAGIC J2032+4127. The gamma-ray flux is predicted to continue to increase over the coming months (e.g. Takata et al., ApJ, 836, 241), and VERITAS and MAGIC observations will continue with highest priority. We strongly encourage coordinated multiwavelength observations.

The MAGIC collaboration reports on the first time detection of very-high-energy (VHE ; E>100 GeV) gamma-ray emission from Ton 0599 (RA:+11:59:31.83 DEC:+29:14:43.83, J2000). The object was observed with the MAGIC telescopes for ~1 hour on 2017/12/15 (MJD 58102.2). The preliminary analysis of these data resulted in the detection of Ton 0599 with a statistical significance of about 10 standard deviations. The VHE flux of this detection was estimated to be around 0.15x10^-9 [ph/cm2/s] (corresponding to about 0.3 CU) above 100 GeV, with a soft spectrum. TON599 is a gamma-ray FSRQ at z=0.72 which is in a remarkably high state from optical to gamma-ray since October 2017 (ATel #10931, #10932, #10937, #10938, #10948, #10949). MAGIC observations on TON 0599 will continue during the next days and multi-wavelength observations are strongly encouraged.

We report an enhanced emission of VHE gamma-rays from the direction of the blazar TXS 0506+056 (05 09 25.96370, +05 41 35.3279 (J2000), [Lani et al., Astron. J., 139, 1695-1712 (2010)]), located 6 arcmin from the estimated direction of the high energy IceCube neutrino event IceCube-170922A (ATel #10791). On Dec 3rd 2018 the MAGIC telescopes observed this source for about 2 hours under good weather conditions. The source was detected at VHE gamma-rays above 90 GeV with a significance larger than 5 sigma. The preliminary analysis yields an estimate of the VHE gamma-ray flux above 90 GeV of ~10-15% of the flux from the Crab Nebula above the same energy threshold, and a spectral index of ~4. This flux is consistent with the emission level integrated between September 28th 2017 to October 3rd 2017, when the source was discovered at VHE gamma-rays (ATel #10817). The MAGIC telescopes will continue monitoring the VHE gamma-ray emission of TXS 0506+056. Soft-X-rays and ultraviolet ToO observations with the Neil Gehrels Swift Observatory have been approved for the next three nights (PI: Cerruti, on behalf of MAGIC), to occur within the time-window 00:00 to 04:00 UTC. NuSTAR ToO observations have also been approved (PI: Satalecka). Multi-wavelength observations (quasi)-simultaneous with MAGIC in this time-window are strongly encouraged.

The MAGIC telescopes have observed a strong increase in the very-high-energy (VHE ; >100 GeV) gamma-ray flux from S50716+714 (RA: 7:21:53.45, Dec: 71:20:36.36, J2000.0). MAGIC observed the source for ~2 hours on 2017/12/28. The preliminary analysis of the MAGIC data indicates increasing flux reaching up to 1.5 times the flux of the Crab nebula above 150 GeV, which is ~6 times higher than the VHE flux from this source during the 2015 flare (ATel #6999). S50716+714 is an intermediate Synchrotron peaked blazar (IBL, Giommi et al. 1999, A&A, 351, 59 ; Ackermann et al. 2011, ApJ, 743, 171) located at the redshift of ~0.3 (Nilsson et al., 2008, A&A, 487, L29 ; Danforth et al., 2013, ApJ, 764, 57). VHE gamma-ray emission from S50716+714 was first reported by the MAGIC collaboration during high optical state of the source (Anderhub et al. 2009, ApJ, 704, L129). Observations of MAGIC were triggered by the hard spectrum of the source (spectral index = -1.86 +/- 0.14, Flux (100MeV-300 GeV) = 0.58 +/- 0.12 e-06 ph cm^-2.) found in the Fermi-LAT data in the 24 hour period started on 2017-12-25 at 18:00:00 UTC. MAGIC observations on S50716+714 will continue during the next two nights and possibly after the moon break and multi-wavelength observations are encouraged. The MAGIC contact person for these observations is R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located on the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports the first detection of very-high-energy (VHE ; E>100 GeV) gamma-ray emission from PGC 2402248, also known as 2WHSP J073326.7+515354 (Chang et al. 2016, A&A, 598, A17) with coordinates R.A.: 07:33:26.7 h, Dec: +51:53:54.99 deg. The source is classified as an extreme high-energy peaked BL Lacertae object of unknown redshift, included in the 2WHSP catalog with a synchrotron peak located at 10^17.9 Hz. PGC 2402248 was observed with the MAGIC telescopes from 2018/01/23 to 2018/04/18 (MJD 58141-58226) for about 23 h. The preliminary analysis of these data resulted in the detection of PGC 2402248 with a statistical significance of more than 6 standard deviations. The VHE integral flux was estimated to be (2.2 +/- 0.6)e-12 ph cm^-2 s-1 above 200 GeV, corresponding to around 1% of the Crab Nebula flux above the same energy threshold. The source was also observed with the XRT instrument on-board the Neil Gehrels Swift Observatory from 2018/01/26 to 2018/04/08 (MJD 58144-58216) with 7 visits almost contemporaneous to the MAGIC observations. The preliminary analysis performed with the publicly available tools (http://www.swift.ac.uk/results/index.php) shows a hint of flux variability from a minimum count rate of 0.43 (MJD 58164) to a maximum of 0.62 cnt/s during the last observation (MJD 58216), in the 0.3-10 keV range. MAGIC and Swift/XRT observations of PGC 2402248 will continue during the next days and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), L. Foffano (luca.foffano@phd.unipd.it) and J. Becerra Gonzalez (jbecerra@iac.es). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located on the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV. We would like to thank the Swift Team for making these observations possible.

The MAGIC and VERITAS collaborations report a continuing increase in TeV gamma-ray emission from the 50-year period pulsar/ Be-star binary system PSR J2032+4127/ MT91 213 (RA 20h32m13.13s, Dec +41d27m24.4s, J2000.0). The system reached periastron on 13 November 2017. The Swift X-ray flux has dropped dramatically over the past two weeks (see ATEL #10920 and the Swift light curve). MAGIC and VERITAS observations are being conducted as part of a coordinated long-term monitoring campaign. TeV emission associated with the binary was first reported in ATEL #10810, covering observations up to late September 2017. The TeV flux has further increased since then. Preliminary analysis of the most recent observations gives integral fluxes above 200 GeV of 1.9e-11 ± 0.4e-11 photons cm^-2 s^-1 for an observation of 1.9 hours on Nov 12 (MJD 58069.8) with MAGIC. This implies an increase in the flux of almost a factor 10 with respect to the average flux in June-August. The flux measured by VERITAS is also enhanced, at the level of 1.3e-11 ± 0.2e-11 photons cm^-2 s^-1 for 4 hours of observations between Nov 10 and Nov 13. TeV observations with both instruments will continue with highest priority. We strongly encourage multi-wavelength observations.

The astrophysical journal 863(1), L10 (2018). doi:10.3847/2041-8213/aad083, A neutrino with energy ∼290 TeV, IceCube-170922A, was detected in coincidence with the BL Lac object TXS 0506+056 during enhanced gamma-ray activity, with chance coincidence being rejected at ∼3σ level. We monitored the object in the very-high-energy (VHE) band with the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes for ∼41 hr from 1.3 to 40.4 days after the neutrino detection. Day-timescale variability is clearly resolved. We interpret the quasi-simultaneous neutrino and broadband electromagnetic observations with a novel one-zone lepto-hadronic model, based on interactions of electrons and protons co-accelerated in the jet with external photons originating from a slow-moving plasma sheath surrounding the faster jet spine. We can reproduce the multiwavelength spectra of TXS 0506+056 with neutrino rate and energy compatible with IceCube-170922A, and with plausible values for the jet power of $\sim 10^{45} - 4 \times 10^{46} erg s^{-1}$. The steep spectrum observed by MAGIC is concordant with internal γγ absorption above ∼100 GeV entailed by photohadronic production of a ∼290 TeV neutrino, corroborating a genuine connection between the multi-messenger signals. In contrast to previous predictions of predominantly hadronic emission from neutrino sources, the gamma-rays can be mostly ascribed to inverse Compton upscattering of external photons by accelerated electrons. The X-ray and VHE bands provide crucial constraints on the emission from both accelerated electrons and protons. We infer that the maximum energy of protons in the jet comoving frame can be in the range $∼10^{14} – 10^{18}$ eV., Published by IOP, Chicago, Ill. [u.a.]

The MAGIC telescopes have observed an increase in the very-high-energy (VHE ; >50 GeV) gamma- ray flux from PKS 1424+240, RA: 14:27:00.4 and DEC: +23:48:00, J2000.0 (Wenger, M. et al., 2000, A&AS, v.143, 9). The preliminary analysis of the MAGIC data taken on 2017/03/09, indicates an integral photon flux of (7.6 +/- 2.3) x 10^-11 [cm^-2/s] above 70 GeV. The estimated flux corresponds to 10+/-3 % of the Crab Nebula integral flux above the same energy threshold (70 GeV), and shows a hint of elevated flux in comparison with the previous detections (Archambault, S. et al., 2014, ApJL, 785, 1, L16 and the references therein). PKS 1424+240 is a BL Lac object located at redshift z=0.604 (Paiano et al. 2017, arXiv:1701.04305) and was previously reported as a VHE gamma-ray emitter by VERITAS (Acciari, V.A. et al., 2010, ApJ 708 L100) and MAGIC (Aleksi?, J. et al., 2014, A&A 567, 135). It is the most distant VHE emitter whose source type is confirmed as a BL Lac object. The MAGIC observations were triggered by the hard spectrum in HE gamma-ray band (0.1-300 GeV), estimated from daily analysis of Fermi data, and showing a photon spectral index = -1.47 +/- 0.28 (TS = 25.9) during 2017/03/06 and 2017/03/07. MAGIC will observe PKS 1424+240 tonight and multi- wavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), V. Fallah Ramazani (vafara@utu.fi) and Gaia Vanzo (gvanzo@iac.es). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

Using the MAGIC telescopes, we have observed an increase in the very-high-energy (VHE ; >100 GeV) gamma-ray flux from NGC 1275 (3C 84, 03:19:48.16, +41:30:42.10, J2000.0). The preliminary analysis of the MAGIC data taken during the night between 31 December 2016 and 1 January 2017 indicates a flux of about 1.5 times the flux from the Crab nebula (C.U.) above 100 GeV. The flux was nearly 10 times larger than the flare reported in October 2016 (ATel #9689) and about 60 times larger than the low state of the source (Aleksic et al. 2014, A&A, 564, A5). Further observations by MAGIC performed on the night of 2nd to 3rd of January still reveal a flaring state of about 0.7 C.U. above 100 GeV. MAGIC observed the source for 2.4 hours in each of the two nights, 4.8 hours in total. NGC 1275 is a Fanaroff-Riley I radio galaxy located at redshift 0.018 in the Perseus Cluster of galaxies, and was first reported as a VHE gamma-ray emitter in Aleksic et al., 2012 (A&A, 539, L2). It is one of only few radio galaxies detected in the VHE gamma-ray range. MAGIC observations of NGC 1275 will continue during the next days and multi-wavelength observations are encouraged. The MAGIC contact person for these observations is R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The Fermi-LAT, FACT, MAGIC and VERITAS collaborations report the detection of enhanced gamma-ray activity from a source positionally consistent with the very-high-energy peaked BL Lac object 1ES 1959+650 (a.k.a 3FGL J2000.0+6509, in the 3rd LAT source catalog, 3FGL, Acero et al. 2015, ApJS 218, 23) with radio coordinates (J2000) R.A.: 299.999384 deg, Dec.: 65.148514 deg (Beasley et al. 2002, ApJS, 141, 13). This source has a redshift z=0.047 (Schachter et al. 1993, ApJ, 412, 541). Preliminary analysis indicates that on 2016 April 27, 1ES 1959+650 was significantly detected by the LAT with a daily gamma-ray flux (E>100MeV) of (0.2+/-0.1) x 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). The corresponding daily average photon index is 1.5+/-0.2 which is smaller than the average index of 1.88+/-0.02 reported in the 3FGL. The MeV-GeV brightening coincides with the detection of the source in an enhanced state in the TeV band as observed by the FACT, MAGIC and VERITAS telescopes. Due to bright and varying moonlight conditions, the energy threshold of Cherenkov telescopes is increased (and their sensitivity decreased). All quoted results are based on online analyses and should be treated as very preliminary. FACT observations on April 29, from 04:30 UTC until 05:20 UTC showed an average flux corresponding to about 1 Crab Unit, with a hint of brightening over time. The preliminary results can be seen at http://www.fact-project.org/monitoring/index.php?y=2016&m=04&d=28&source=7&timebin=3&plot=night MAGIC observed the source for 1hr on 29 April 2016, 4:10-5:10 UTC. The preliminary analysis of the MAGIC data indicates a flux of at least 80% of the flux from the Crab Nebula (CN) above 1TeV. The flux is reported as a lower limit as it was not corrected for the effect of the observations under moonlight conditions. It implies an increase by a factor of at least 4 with respect to the 20% of the CN flux above 180GeV reported previously in Albert et al. 2006 ApJ, 639, 761. VERITAS observed the source for about 2hrs under bright moonlight conditions on 2016 April 29, between 9:42 and 11:29 UTC. A preliminary analysis of the data shows a strong detection of the source with a statistical significance of ~40 standard deviations, and an average flux above 350GeV of approximately 1 x 10^-10 cm^-2 s^-1 (i.e. about the CN flux). A power-law fit to the gamma-ray spectrum between 0.35-5TeV is consistent with a spectral index of approximately 2.5, harder than the archival low spectral state (e.g. Aliu et al. 2014, ApJ, 797, 89). Increasing gamma-ray flux from this source was previously reported by the Fermi-LAT and VERITAS Collaborations in 2015 October (see ATel #8148, ATel #8193). 1ES 1959+650 is one of the "LAT Monitored Sources" and consequently preliminary estimates of the daily and weekly gamma-ray flux observed by Fermi LAT are publicly available (fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/1ES_1959p650). Recently, the source reached its highest historical X-ray brightness as reported in ATel #8468. 1ES 1959+650 is regularly monitored by FACT, but due to high zenith angle, it is currently outside the standard observation parameters. The results from past online analyses are publicly available at http://www.fact-project.org/monitoring/index.php?y=2016&m=04&d=28&source=7&timebin=12&plot=all The Fermi Gamma-ray Space Telescope began a Target of Opportunity observation on 29 April. Coordinated observations among Fermi-LAT, FACT, MAGIC, VERITAS and Swift are ongoing. In consideration of the current activity of this source, we encourage multiwavelength observations. For this source, the Fermi LAT contact person is S. Buson (sara.buson@nasa.gov), for FACT is D. Dorner (dorner@astro.uni-wuerzburg.de), for MAGIC is R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), for VERITAS is R. Mukherjee (muk@astro.columbia.edu).

The MAGIC collaboration reports on the detection of very high energy (VHE ; E>150 GeV) gamma-ray emission from OT 081 (RA=17 51 32.82, dec=+09 39 00.73, J2000.0 ; also known as PKS 1749+096 and 4C +09.57). OT 081 is a blazar at a red shift of 0.322 (Stickel, Fried, Kuehr 1988, A&A, 191, 16). The preliminary analysis of the MAGIC data taken on 2016 Jul. 24 (observation time: 1.64 hours) resulted in the detection of OT 081 with a statistical significance of 9 standard deviations. From the preliminary analysis, we estimate the VHE flux of this detection is about 8% of the flux from the Crab Nebula in the energy range above 150 GeV. The MAGIC observations were triggered by the observations in the high energy gamma-ray band by the Fermi-LAT, and X-ray and UV Swift (ATel #9260), an optical band flux increase observed by the MAGIC collaboration with a 35cm Celestron telescope at La Palma, and optical observations from other observatories (ATel #9259). MAGIC observations of OT 081 will continue during the following nights, and multi-wavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and D. Dominis Prester (dijana@phy.uniri.hr). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

FACT, MAGIC, VERITAS and Fermi-LAT collaborations report the measurement of a further increase of the gamma-ray flux together with bright X-ray emission seen by Swift-XRT from a position consistent with the high-energy peaked BL Lac type object 1ES 1959+650 (z=0.047, Schachter et al. 1993, ApJ, 412, 541). Enhanced TeV flux was reported by FACT between MJD 57546--57550 (ATel #9139). After a slight decrease within that period, a new maximum in the TeV flux was measured last night between MJD 57552.09 and 57552.25. Within about 2.7 hours of observations, FACT observed a a flux exceeding 2.5 Crab units, with a statistical significance of 16 standard deviations. This is twice the highest flux observed during the high states in the past week. The results of a preliminary automatic quick look analysis are publicly available, where this link: http://fact-project.org/monitoring/index.php?y=2016&m=06&d=12&source=7&timebin=12&plot=month shows the evolution of a nightly binned background subtracted light curve for the last month. These values are corrected neither for the effect of large zenith distance under which the source is observable nor for the amount of night-sky-background light, with both effects decreasing the measured gamma rate. FACT is regularly monitoring 1ES 1959+650. Currently, it is observing the source each night from 02:15 to 05:00 UTC if weather conditions permit. The source has also been monitored daily by the MAGIC telescopes. For the night of MJD 57552, the preliminary flux above 200GeV from automatic analysis is at the level of about 2.5 Crab units. MAGIC will continue observing the source. VERITAS observed the source for 3.5 hours under bright moonlight conditions on MJD 57552. A preliminary analysis of the data shows a strong detection of the source with a statistical significance of about 60 standard deviations, increasing in flux above 300 GeV from about 1.0e-10 cm^-2 s^-1 (80% of the Crab nebula) to a peak of over 2.6e-10 cm^-2 s^-1 (200% of the Crab nebula) at the end of the observing period. Preliminary analysis of Fermi-LAT data indicates that the object’s flux has almost doubled over the past three weeks. The observed gamma-ray flux (E>1GeV) was (1.9+/-0.5) x 10^-8 cm^-2 s^-1 during the week of 23-30 May, and (4.2+/-0.8) x 10^-8 cm^-2 s^-1 during the week of 6-13 May (statistical uncertainty only). The source detection significance (test statistic) for these weeks was 91 and 250, respectively. Monitoring with the X-ray Telescope onboard the Swift satellite (Swift-XRT) shows that the source underwent a strong X-ray flare comparable to that in 2015 November-December. The highest level during the ongoing flare is reached on June 9 with a 0.3-10 keV count rate of 20.50+/-0.15 cts/s which is only by 12% smaller than the highest historical rate recorded on 2015 December 26. Last night, where the observations was split into two orbits, the count rate was 18.55+/-0.15 cts/s, which corresponds to an unabsorbed 0.3-10 keV flux was (7.41-8.13)\times 10^{; ; -10) erg/cm^2/s during the today's observation. Activity in gamma rays and X-rays has been reported over the past 6 months (Atel #8014, #8107, #8148, #8165, #8193, #8289, #8337, #8342, #8468) with a recent increase seen in multiple different wavebands (ATel #9010, #9070, #9121). Coordinated observations among FACT, MAGIC, VERITAS Fermi-LAT and Swift are ongoing. In consideration of the current activity of this source, we encourage multiwavelength observations. For this source, the Fermi LAT contact person is S. Buson (sara.buson@nasa.gov), for FACT is D. Dorner (dorner@astro.uni-wuerzburg.de), for MAGIC is R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), for VERITAS is R. Mukherjee (muk@astro.columbia.edu).

The MAGIC collaboration reports the detection of very high energy (VHE) gamma-ray emission from 1ES 2037+521 (RA 20h39m23.5s, DEC +52d19m50s, J2000.0). The object was observed with the MAGIC telescopes for 11 hours between 2016/09/26 and 2016/09/30. The preliminary analysis of these data resulted in the detection of 1ES 2037+521 with a statistical significance of 5.7 standard deviations. The preliminary VHE flux from these observations was estimated to be about about 6e-12 cm-2 s-1 above 200 GeV, which is about 3% of the flux from the Crab nebula. 1ES 2037+521 is located at redshift 0.053 (Sbarufatti et al., 2006) and classified as a BL Lac candidate in Veron-Cetti & Veron, 2006. Its X-ray and gamma-ray spectra is hard, which suggest this source may be an extreme HBL (Costamante et al. 2001). MAGIC observations on 1ES 2037+521 will continue until October 3rd, and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and V. Fallah Ramazani (vafara@utu.fi). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports results from the follow-up observations of IceCube neutrino HESE/EHE 160731A (AMON GCN notice ; http://gcn.gsfc.nasa.gov/notices_amon/6888376_128290.amon ). Follow up observations from other observatories have been reported (ATels: #9294, #9295, #9298, #9301, #9303, GCN: #19743, #19752, #19758, #19760). MAGIC received the AMON GCN alert on Sun Jul 31 01:55:59 2016 UTC, when the reported sky location was not visible from La Palma. The initial EHE alert coordinates were observed by MAGIC on Sun Jul 31 21:25 - 22:47 UTC, at high zenith angle, 45-65 deg. Because of the 3.5 deg. field of view of the MAGIC cameras, these observations encompassed both the initial and revised IceCube alert positions (as reported in the HESE/EHE AMON GCN alert from Mon 01 Aug 16 02:35:54 UT). No significant VHE gamma-ray emission above 600 GeV was detected within the quoted IceCube 50% containment circle, neither from the initial, nor the revised HESE/EHE alert positions. The energy threshold of the analysis performed was higher than expected for this range of zenith angle because of the presence of a sand layer from the Saharan desert (calima), which somewhat deteriorated the atmospheric conditions during the MAGIC observations. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), K.Satalecka (konstancja.satalecka@desy.de) and D. Glawion (Dorit.Glawion@astro.uni-wuerzburg.de). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

Using the MAGIC telescopes, we have observed an increase in the very-high-energy (VHE ; >100 GeV) gamma-ray flux from NGC 1275 (3C 84, 03:19:48.16, +41:30:42.10, J2000.0). The preliminary analysis of the MAGIC data taken on 2016 Oct 29 indicates a flux of (8.5 +/- 0.9) x 10^-11 ph/cm^2/s corresponding to 16% of the flux from the Crab nebula (C.U.) above 100 GeV. This implies an increase by a factor of about 5 with respect to the previously measured VHE flux from this object above the same energy threshold. NGC 1275 is a Fanaroff-Riley I radio galaxy located at the red shift 0.018 in the Perseus Cluster of galaxies, and was first reported as a VHE emitter in Aleksic et al., 2012 (A&A, 539, L2). It is one of only a few radio galaxies detected in the VHE range. The typical VHE flux (>100 GeV) of this object is about 3% C.U. (Aleksic et al. 2014, A&A, 564, A5). MAGIC observations of NGC 1275 will continue during the next days and multi-wavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de), P. Colin (colin@mppmu.mpg.de) and D. Glawion (dorit.glawion@astro.uni-wuerzburg.de). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The FACT and MAGIC collaborations report the measurement of an enhanced gamma-ray flux at about 1 TeV from a position consistent with the HBL 1ES 1959+650 (z=0.047, Schachter et al. 1993, ApJ, 412, 541). Recent activities from this source were reported in gamma rays (ATel #9010, #9139, #9148, #9168), IR (ATel #9070) and X-rays (ATel #9121), and since Summer 2015 several periods of enhanced activity have been observed. After the bright flare of MJD 57552 (ATel #9148), the flux decayed within 1-2 nights to a level of 0.5-1 Crab units and stayed around or below that level for about 15 days. From MJD 57570.04 till 57570.18, FACT measures an increased average flux corresponding to at least 2 Crab units. The source is detected with about 13 standard deviations in 3.3 hours of observation. The results of a preliminary, automatic quick look analysis are publicly available. http://fact-project.org/monitoring/index.php?y=2016&m=06&d=30&source=7&timebin=3&plot=night shows the 20-minute-binned background subtracted light curve. These values are corrected neither for the effect of large zenith distance under which the source is observable nor for the amount of night-sky-background light, with both effects decreasing the measured gamma rate. The measurement might be affected the meteorologic phenomenon calima possibly causing an apparent lower flux. FACT is regularly monitoring 1ES 1959+650. Currently, it is observing the source each night from 1:00 to 04:30 UTC, if weather conditions permit. The FACT contact person for this source is D. Dorner (dorner@astro.uni-wuerzburg.de) The preliminary analysis of the MAGIC data taken from MJD 57570.00 to 57570.21 indicates a flux of about 2.6 that of the flux from the Crab Nebula above 300 GeV. MAGIC observations on 1ES 1959+650 will continue during the next days, and multi-wavelength observations are encouraged. The MAGIC contact person for these observations is R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV. The First G-APD Cherenkov Telescope (FACT) is an Imaging Atmospheric Cherenkov Telescope with 9.5 sqm mirror area, located next to the two MAGIC telescopes. It is pioneering the usage of silicon photosensors and monitoring bright, variable sources at energies above 750 GeV. The Collaboration includes ETH Zurich and the Universities of Dortmund, Geneva and Wuerzburg.

The MAGIC telescopes have detected an increase in the Very High Energy gamma-ray flux from PKS 1510-089 (RA=15 12 50.5, dec=-09 06 00, J2000.0). The preliminary analysis of the MAGIC data taken on 2016/05/30 for 2.7 hours, indicates a highly significant signal (significance > 60 sigma). The flux at the beginning of the observations (MJD=57538.94) was larger than the flux from the Crab nebula above 150 GeV, and around 50% of the flux from the Crab nebula above 240 GeV, declining towards the end of our observations. This implies an increase of a factor of at least ~5 with respect to the flux reported during the VHE flare detected by MAGIC in May 2015 (http://www.astronomerstelegram.org/?read=7542). We roughly estimate the spectral slope to -4, and the flux at 90 GeV at the beginning of the observations to 5 times the flux from the Crab nebula. Automatic analysis of the MAGIC observations from 2016/05/31 show no significant signal of this source. Quasi-simultaneously to MAGIC observations, we also performed optical observations with a 35cm Celestron telescope at La Palma. The observations confirm the elevated optical state, the R-band magnitude being ~15.1. The light curve is available in the Tuorla Blazar monitoring webpage: http://users.utu.fi/kani/1m/PKS_1510-089_jy.html PKS 1510-089 is a FSRQ at z=0.36 and it is regularly monitored by MAGIC. MAGIC observations on 2016/05/30 were triggered by the alert by the H.E.S.S. collaboration due to a high flux observed on issued on 2016/05/29, and high-state reported in the high energy gamma-ray band as seen by Fermi-LAT (http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/1510-089). H.E.S.S. observations from the night 2016/05/29 were reported on 2016/05/31: http://www.astronomerstelegram.org/?read=9102. MAGIC observations on PKS1510-089 will continue during the following nights, and multi-wavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and D. Dominis Prester (dijana@phy.uniri.hr). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC telescopes performed follow-up observations in the very high energy band (VHE ; E>100 GeV) of a ~3 degree-diameter sky region centered at the proposed X-ray counterpart of the ANTARES-detected neutrino event (#ATel 7987). MAGIC observed the source under non-optimal conditions due to the large zenith angle (above 60 deg), starting from Sep. 3 at 20:54 UT, 2.5 days after ANTARES detection. Observations were carried out for 6 nights, ending on Sep. 8, and collecting a total on-source exposure of 4 hours. We neither detected significant emission from the location of the X-ray source, nor found any other gamma-ray source within the ~3 degree field of view of MAGIC. The preliminary analysis centered on the proposed X-ray counterpart gave an integral flux upper limit at 95 % c.l. of 4.7e-12 cm-2 s-1 above E>500 GeV, which corresponds to 8% of the Crab Nebula flux above the same energy, assuming a Crab-like spectral index. The nightly light curve above 500 GeV did not show any hint of a transient signal. The MAGIC contact persons for these observations are R. Mirzoyan (razmik.mirzoyan@mpp.mpg.de), A. Carosi (alessandro.carosi@oa-roma.inaf.it), K. Noda (knoda@mppmu.mpg.de) and G. Pedaletti (giovanna.pedaletti@desy.de). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC telescopes have observed an increase in the Very High Energy (VHE ; >100 GeV) gamma-ray flux from PKS 1510-089 (RA=15 12 50.5, Dec=-09 06 00, J2000.0). The preliminary analysis of the MAGIC data taken from 2015/05/18 to 2015/05/19 shows a highly significant signal and a flux of ~20% from that of the Crab nebula above 100 GeV. This implies an increase by a factor of ~5 with respect to the flux reported previously in 2012. PKS 1510-089 is a FSRQ at z=0.36 and it is regularly monitored by MAGIC. The source is also active in the high energy gamma-ray band as seen by Fermi-LAT ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/1510-089 ), and in optical band as reported by the Tuorla blazar monitoring program (http://users.utu.fi/kani/1m, R=14.75 on 2015/05/19). ATels #7495 and #7466 also report an increase in the IR brightness. We have also triggered ToO observations with the Swift satellite, which did not show any substantial enhancement in the X-ray flux (http://www.swift.psu.edu/monitoring/source.php?source=PKS1510-089). MAGIC observations on PKS1510-089 will continue during the following nights, and multi-wavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and E. Lindfors (elilin@utu.fi). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The blazar S5 0716+714 was recently reported to be at exceptionally high optical state (ATel#6902, ATel#6942, ATel#6944, ATel#6953, ATel#6957), which triggered MAGIC observations of the source in very high energy gamma rays (VHE, E>100 GeV). The preliminary analysis of the MAGIC data taken between 2015/01/22 and 2015/01/26 indicates potentially variable VHE flux in the range from 4x10^-11 cm^-2 s^-1 to 7x10^-11 cm^-2 s^-1 above 150GeV. S5 0716+714 is a blazar with z~0.31 (Nilsson et al. 2008, A&A...487L..29N), which was reported as VHE emitter in 2008 (Anderhub et al. 2009, ApJ, 704, 129). The measured integral flux above 400 GeV was (7.5 +- 2.2) * 10^-12 cm^-2 s^-1. The 2008 detection is the only significant detection of VHE gamma-ray emission prior to observations reported here. Notably, the 2008 MAGIC detection of the source took place during a high optical state, too. The MAGIC observations were accompanied with simultaneous optical observations with the KVA telescope. The R-band magnitude on 2015/01/26 was 11.84, the lightcurve is available at: http://users.utu.fi/kani/1m/S5_0716+714.html MAGIC observations on S5 0716+714 will continue for one more night and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and E. Lindfors (elilin@utu.fi). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports the discovery of very high energy (VHE ; E>100 GeV) gamma-ray emission from the FSRQ S4 0954+65 (RA=+9:58:47.00, DEC=+65:33:55.00, J2000.0), located at redshift z=0.368. The object was observed with the MAGIC telescopes for ~2 hours during the night 2015 February 13/14 (MJD 57067). A preliminary analysis of the data yields detection with a statistical significance of more than 5 standard deviations. This is the first time a significant signal at VHE gamma rays has been seen from S4 0954+65. The flux above 150GeV is estimated to be about 2e-11 cm^-2 s^-1. S4 0954+65 is entered an exceptionally high state at optical and near infrared frequencies (ATels #7057 ; #7055 ; #7046, #7001 ; #6996), which triggered the MAGIC observations. Optical observations performed with the KVA telescope suggests that this is the brightest state ever observed from this source since November 2006 (beginning of KVA observations). The preliminary lightcurve is available at: http://users.utu.fi/kani/1m/S4_0954+65.html. During the preparation of this ATel, we were informed by Fermi-LAT collaboration that the gamma-ray flux above 100 MeV from S4 0954+65 also increased substantially during the last few days. MAGIC observations on S4 0954+65 will continue during the following nights, and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and E. Lindfors (elilin@utu.fi). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC telescopes have detected an increase in the Very High Energy (VHE ; >100 GeV) gamma-ray flux from BL Lacertae (RA=22h02m43.3s Dec=+42d16m40s, J2000.0). The preliminary analysis of the MAGIC data taken from 2015/06/14 to 2015/06/17 indicates a highly significant signal above 200 GeV. The emission is variable, with a flux of 0.4 and 0.1 times the flux of the Crab nebula above 200 GeV in the nights 14/15 and 16/17, respectively. MAGIC telescopes observed BL Lacertae in 3 consecutive nights for duration of 1 hour per night, under excellent weather conditions. In the night of 15/16 June there was no detection. The flux level is similar to the flaring state reported in Arlen et al. 2013. In the low state the source is typically not detectable with IACTs. The MAGIC observations were triggered by the high activity measured at optical and gamma-ray energies. The source is active in the high energy gamma-ray band as seen by Fermi-LAT (http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/BL_Lac), and in optical band as reported by Tuorla blazar monitoring program (http://users.utu.fi/kani/1m/BL_Lac.html). We have also triggered ToO observations with the Swift satellite, which did not show any substantial enhancement in the X-ray flux (http://www.swift.psu.edu/monitoring/source.php?source=BLLacertae). MAGIC observations on BL Lacertae will continue during the following nights, and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and D. Dominis Prester (dijana@phy.uniri.hr). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports the discovery of very high energy (VHE ; E>100 GeV) gamma-ray emission from the FSRQ PKS 1441+25 (RA=14h43m56.9s DEC=+25d01m44s), located at redshift z=0.939 (Shaw et al. 2012, ApJ, 748, 49). The object was observed with the MAGIC telescopes for ~2 hours during the night 2015 April 17/18, and for ~4 hours during 18/19. A preliminary analysis of the data yields a detection with a statistical significance of more than 6 standard deviations for the night of April 17/18, and more than 11 standard deviations for 18/19. This is the first time a significant signal at VHE gamma rays has been seen from PKS 1441+25. The flux above 80 GeV is estimated to be about 8e-11 cm^-2 s^-1 (16% of Crab Nebula flux). PKS 1441+25 has entered an exceptionally high state at optical, X-, and Gamma-ray frequencies (ATel #7402), which triggered the MAGIC observations. The Swift Follow-up observation from April 18/19 revealed that the high state in X-rays is continuing: http://www.swift.psu.edu/monitoring/source.php?source=PKS1441+25 MAGIC observations on PKS1441+25 will continue during the following nights, and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and E. Lindfors (elilin@utu.fi). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports the discovery of very high energy (VHE ; E>100 GeV) gamma-ray emission from the BL Lac S2 0109+22 (RA: 01h12m05.8s Dec:+22d44m39s, J2000). The object was observed with the MAGIC telescopes for 5.3 hours from 2015/07/22 to 2015/07/25, following the high-flux state spotted in the high-energy (E>10 GeV) domain of the public Fermi/LAT data, according to the prescription of Pacciani et al. ApJ 790 (2014) 45. The preliminary analysis of the first three nights of MAGIC data showed an excess with a statistical significance of ~5 standard deviations. The VHE flux of this detection was estimated to be (1.6+/-0.7)e-11 ph/cm2/s above 100 GeV, about 3% of the flux from the Crab nebula. The daily flux shows a marked enhancement on the night of 25 July up to (9.7+/-1.5)e-11 ph/cm2/s, ~15% of the Crab flux at E>100 GeV, corresponding to an excess with >7 sigma statistical significance. S2 0109+22 is located at the red shift z=0.265 (from CGRaBS spectroscopy, Healey et al., ApJ 175 (2008) 97). It is classified as an intermediate-synchrotron peaked BL Lac object in the 2LAC (Ackermann et al. ApJ 743 (2011) 171). The multi-year optical and radio historical coverage (Ciprini et al. MNRAS 348 (2004) 1379) showed optical variations with typical timescales from weeks to months. The Fermi/LAT flaring activity triggered a ToO observation with Swift, started on 2015/07/21. The preliminary Swift/XRT analysis showed an unabsorbed flux (7.0+-0.3)E-12 erg/cm2/s in the 0.3-10 keV range. From archival Swift/XRT data the brightest state previously observed had a flux (2.5+-0.3)E-12 erg/cm2/s. This corresponds to a 2-3 fold flux enhancement in X-rays. Instead the optical (UV) flux is ~50% (~30%) lower than at the brightest state observed with Swift/UVOT. MAGIC observations on S2 0109+22 will continue during the next days until July 28 and multi-wavelength observations are encouraged. The MAGIC contact persons for these observations are A. Stamerra (INAF-SNS, stamerra@oato.inaf.it) and R. Mirzoyan (MPI, Razmik.Mirzoyan@mpp.mpg.de) MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports the discovery of very high energy (VHE ; E>100 GeV) gamma-ray emission from RX J1136.5+6737 (a.k.a. RBS 1004) (RA: 11:36:30.1 DEC: +67:37:04, J2000) at redshift z=0.1342. RX J1136.5+6737 is an X-ray bright high-peaked frequency BL Lac object as listed in the MAXI 3-year catalog (Hiroi et al. 2013), which includes 13 BL Lacs (all HBLs and 9 TeV HBLs). The source has also been detected by Fermi-LAT, in the Second Fermi-LAT source catalog (2FGL ; Nolan et al. 2012) with a hard photon index 1.68+/-0.12, and belongs to the first Fermi-LAT catalog of >10 GeV sources (1FHL ; Ackermann et al, 2013), showing bright (photon flux = 11.7e-11 ph cm^-2 s^-1) emission above 10 GeV, and identified as a good candidate for VHE detection. RX J1136.5+6737 was observed with the MAGIC telescopes starting on 2014 January 29. Data taken up to 2014 April 3 (about 20 hours in total) yielded a source detection with a statistical significance of more than 5 standard deviations. The averaged flux measured by MAGIC during the 2014 observations corresponded to about 1.5% of the Crab nebula at energies above 200 GeV. MAGIC is planning to resume observations of the source on April 18th (right after the full-moon break). Multi-wavelength observations are encouraged.

The MAGIC collaboration reports the discovery of very high energy (VHE ; E>100 GeV) gamma-ray emission from RBS 0723 (RA: 08:47:12.9 DEC: +11:33:50, J2000.0) RBS 0723 is a BL Lac object at redshift z=0.198. The source has been detected by Fermi-LAT, in the Second Fermi-LAT source Catalogue (2FGL ; Nolan et al. 2012) with F(>1 GeV) = (5.3+-1.2)e-10 cm^-2 s^-1 and with photon index 1.48+-0.16. It also belongs to the first Fermi-LAT catalog of >10 GeV sources (1FHL ; Ackermann et al, 2013), showing a hard (photon index = 1.4 +- 0.4) and bright (photon flux = 9.6e-11 ph cm^-2 s^-1) emission above 10 GeV, and identified as a good candidate for VHE detection. The shape of the SED indicates it is one of the subclass of the extreme HBL characterized by extremely hard X-ray and VHE continua. RBS 0723 was observed starting on 2013 December 3. Data taken between 2014 Jan 1 and Jan 8 (about 10 hours) yields a source detection with a statistical significance of more than 5 standard deviations. The non-detection in the earlier data taken in 2013 Dec. suggests VHE flux variability. The VHE emission measured with MAGIC has a flux of about 2.5% of the Crab nebula at energies above 200 GeV. Optical monitoring with KVA telescope (La Palma) also shows evidence of an increased flux (R=17.2 in December 2013, R=16.9 in January 2014). MAGIC observations of RBS 0723 will resume on Jan. 22. Multi-wavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (razmik.mirzoyan@mpp.mpg.de) and F. Tavecchio (fabrizio.tavecchio@brera.inaf.it). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration observed SN2014J, the nearest supernova (SN) explosion in 10 years, located in the galaxy M82. The MAGIC observations started 6 days after the first detection by the UCL Observatory (CBET #3792) and amounted to a total of 5.4 hours. This Ia-type SN is unique and follow-up observations in all wavelengths have been pursued (i.e. ATel #5835, #5809, #5812, #5851). The SN was observed with the MAGIC telescopes from January 27 to 29 under moderate moonlight conditions and on February 1 and 2 under dark-night conditions. The preliminary analysis of these data resulted in an integral flux upper limit of 1.6e-12 cm-2 s-1 above the energy 300 GeV at 95% c.l. (this corresponds to ~1.3% of the Crab Nebula flux ; for energies above 700 GeV the corresponding limit is ~2%), assuming a Crab-like spectral index. The daily flux upper limits (~1h observation per day) vary from 1.8e-12 to 18.e-12 cm-2 s-1 (E>300 GeV, 95% c.l.), due to different observational conditions. The VHE flux contribution from the host galaxy M82 was previously measured by VERITAS (Nature, 462, 700) at the level of 0.9% of the Crab flux for E>700 GeV. The MAGIC observations covered the maximum of the SN brightening (on Jan 31, mag=10.5 AAVSO data: PSN J09554214+6940260). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC and VERITAS telescopes have observed relatively long-duration flaring activity from the blazar 1ES 1011+496 at z = 0.212 (RA=10h 15m 04.1s, Dec=+49d 26m 01s). The brightest very high energy (VHE ; >100 GeV) gamma-ray flux previously recorded from this blazar is approximately 7% of the flux (>200 GeV) observed from the Crab Nebula (J. Albert et al. 2007, ApJ 667, L21). Recent VERITAS and MAGIC observations exceed roughly 10 times this flux. VERITAS observations were taken almost every night between February 3, 2014 UTC (MJD 56691) and February 11, 2014 (MJD 56699). The preliminary analysis of all good-weather data yields a strong signal of about 3300 gamma rays in 13 hours of exposure, corresponding to a statistical significance of 43 standard deviations. The observed nightly integral flux above 200 GeV ranges between 25% and 75% of the flux measured by MAGIC from the Crab Nebula. Following a VERITAS alert to ground-based VHE observatories, the MAGIC telescopes observed the source nightly from February 6, 2014 UTC (MJD 56694) through February 11, 2014 (MJD 56699). The preliminary analysis of these data results in integral fluxes above 200 GeV (nightly averaged) ranging between of 45% and 75% of the flux from the Crab Nebula. Follow-up observations were also taken with Swift XRT / UVOT and at optical wavelengths. The 0.3-10 keV X-ray flux of 1ES1011+496 is also at the highest level ever seen by Swift (http://www.swift.psu.edu/monitoring/). The latest MAGIC and VERITAS observations performed on the night of February 11, 2014 show the high VHE flux persists. The MAGIC and VERITAS telescopes are entering the full Moon period, however the observations will be resumed on February 20, 2014 (UTC), if the weather conditions permit. Additional multiwavelength observations are encouraged. MAGIC is a system of two 17m-diameter imaging atmospheric Cherenkov telescopes (IACTs) located at the Canary island of La Palma, Spain. VERITAS is an array of four 12-m diameter IACTs located near Tucson, Arizona, USA. VERITAS and MAGIC are sensitive to astronomical sources of gamma-rays with energies ranging from approximately 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports the discovery of very high energy (VHE ; E>100 GeV) gamma-ray emission from S3 0218+357 (RA=02h21m05.5s, DEC=+35d56m14s, J2000.0). The object was observed with the MAGIC telescopes for a total of 3.5 hours from 2014/07/23 to 2014/07/26. The preliminary analysis of these data resulted in the detection of S3 0218+357 with a statistical significance of more than 5 standard deviations. From the preliminary analysis, we estimate the VHE flux of this detection to be about 15% of the flux from the Crab Nebula in the energy range 100-200 GeV. S3 0218+357 is a gravitationally lensed blazar located at the redshift of 0.944+/-0.002 (Cohen et al., 2003, ApJ, 583, 67). Fermi-LAT observations during the flaring state of S3 0218+357 in 2012 revealed a series of flares with their counterparts after 11.46+/-0.16 days delay, interpreted as due to the gravitational lensing effect (Cheung et al. 2014, ApJ, 782, L14). On 2014 July 13 and 14 Fermi-LAT detected another flaring episode (ATel #6316). Due to the full-moon time, the MAGIC telescopes were not operational and could not observe S3 0218+357 after the original alert. However, observations scheduled at the expected time of arrival of the gravitationally lensed component led to the first significant detection of a gravitationally lensed blazar and the most distant source detected at VHE with Cherenkov telescopes to date. MAGIC observations on S3 0218+357 will continue during the next days and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and J. Sitarek (jsitarek@ifae.es). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astrophysics in the energy range from 50 GeV to greater than 50 TeV.

The MAGIC collaboration reports the discovery of very high energy (VHE ; E>100 GeV) gamma-ray emission from MS1221.8+2452 (12h24m24.2s +24d36m24s, J2000.0). MS1221.8+2452 is a blazar located at a redshift of 0.218 (Sbarufatti et al., 2005, ApJ 635, 173) and classified as a high synchrotron peaked (HSP) BL Lac. It is one of the very few BL Lacs that has been imaged with the Hubble Space Telescope (Jannuzzi et al., 1997, ApJ 491, 146). It has been included in the ROSAT Bright Source Catalog (Voges et al., 1999, A&A 349, 389) and identified as XBL (X-Ray-Selected BL Lac) by the Einstein Extended Medium Sensitivity Survey (Rector et al. 2000, AJ 120, 1626). The object was observed with the MAGIC telescopes for 4 hours from 2013/04/30 to 2013/05/01. The preliminary analysis of these data resulted in the detection of MS1221.8+2452 with a statistical significance of more than 5 standard deviations. The VHE flux of this detection was estimated to be about 4% of the Crab nebula flux above 200 GeV. MS1221.8+2452 was observed with Swift during March and April 2013, showing flux variability ranging from 3e-12 erg/cm2/s to 13e-12 erg/cm2/s in the 0.3-10 keV energy range. This source was flagged as a promising VHE source candidate by the Fermi-LAT collaboration, information that was shared with the MAGIC collaboration (as well as other ground-based gamma-ray instruments). MAGIC observations on MS1221.8+2452 will continue during the next days until 2013/05/12 and multiwavelength observations are encouraged.

H1722+119 is a BL Lac object, that was listed as candidate TeV blazar in Costamante & Ghisellini (2002) based on its X-ray and radio properties. Its redshift is uncertain ; Sbarufatti et al. 2006 give z>0.17. The source has been detected by Fermi-LAT, in the Second Fermi Catalog with F(>1 GeV) (3.7+-0.3)e-09 cm^-2 s^-1 and with spectral index 1.92+-0.06. H1722+119 was observed for five nights by the MAGIC telescopes starting May 17th 2013 and collecting 11 hours of good quality data. A preliminary analysis yields a detection of the source with a statistical significance of more than 5 standard deviations. The VHE flux of this detection is about 2% of the flux from the Crab nebula above 140 GeV. The previous VHE gamma-ray observations of the source produced an upper limit of 4.2% Crab nebula flux above 140 GeV (Aleksic et al. 2011). The MAGIC observations were triggered by the extended optical high state of the source, reported by the Tuorla blazar monitoring program (http://users.utu.fi/kani/1m). At the beginning of May 2013 the source reached an R-band magnitude of 14.65, the brightest ever observed since 2005, when the monitoring started. We also analyzed the Fermi-LAT data, finding indication of a spectral index harder than reported in the Second Fermi Catalog. A Swift-XRT ToO observation was performed on 20th May. MAGIC will continue the observations of the source as soon as the moon conditions allow it again and multiwavelength observations are encouraged.

The MAGIC and VERITAS telescopes have observed an unprecedented flaring activity in the Very High Energy (VHE ; >100 GeV) gamma-ray flux from Markarian 421 (RA= 11 04 27.31, Dec=38 12 31.8, J2000.0). These observations were initially performed within a pre-planned extensive multi-instrument campaign that started in December 2012, and intensified in the last days because of the extreme VHE activity observed. Mrk421 is a high-synchrotron-peaked BL Lac located at redshift 0.031, which was first reported as a VHE emitter in 1992 (Punch et al 1992, Nature 358, 477). The typical VHE flux of this source is about 0.5 times the flux from the Crab Nebula (Crab Units, c.u.), as reported in Abdo et al 2011, ApJ 736, 131 and references therein, and the highest level of VHE activity ever measured for this source was about 10 c.u. (Gaidos et al. 1996, Nature 383, 319, and also Fortson et al. 2012, American Institute of Physics Conference Series, 1505, 514). The preliminary analysis of the VHE data taken with MAGIC and VERITAS during the last three consecutive nights (from 2013/04/11 to 2013/04/13) indicate a persistently high flux of about 5 c.u. above 300 GeV, but very variable and with maxima reaching beyond 11 c.u. This implies an increase by a factor of more than 20 with respect to the typical (not lowest) VHE flux from this source above 300 GeV, and represent the highest VHE activity recorded for this object to date. Besides MAGIC and VERITAS, the campaign also includes dedicated observations at radio and optical wavelengths with various instruments, and X-rays with Swift and NuSTAR. The source has been found to be also very high at optical and X-ray (see ATel #4974).

Following the communication from the Fermi-LAT collaboration on February 1st that PKS 1510-089 (z=0.36, R.A.= 15h 12m 50.5s, Dec.=-09d 05m 59.8s, J2000) underwent spectral hardening in MeV-GeV range (Dave Thompson, priv. comm. to TeV facilities) and ATel #3907 announcing enhanced gamma-ray emission observed by AGILE on February 2nd, the source was observed by MAGIC starting on February 3rd, just before the full moon shut down. The observations were resumed on February 19th and in total ~10 hours of data have been collected. The preliminary analysis of the data reveals a clear signal with a statistical significance of >5 sigma. The source had been previously detected to emit VHE gamma-rays by the H.E.S.S. telescope array in 2009 (Wagner, S., & Behera, B. 2010, 10th HEAD Meeting). Simultaneous to the MAGIC observations we have obtained optical R-band photometry and polarimetry with the KVA and Liverpool Telescopes. The source has undergone a minor optical outburst with a maximum brightness of R=15.3 (~2.3 mJy) measured on February 25th compared to a maximum brightness of R=13.1 (18 mJy) during the major outburst in 2009. The optical polarization has remained between 3% and 9% which is within the typical range for this quasar.

The source PG 1553+113 is a well-known TeV emitter, likely located at redshift 0.4-0.5 (Danforth et al. 2010). Its state has been monitored by MAGIC since February 2005. In March 2012, a high emission state at VHE, X-ray, optical, and infrared wavelengths was reported (ATel #3977). During the night of April 19-20th (MJD 56037), the source was observed by MAGIC for a total of 1.1 hour of good quality data. A strong signal corresponding to a statistical significance above 15 standard deviations in the VHE range was detected. The level obtained with the preliminary analysis reaches the Crab Nebula flux level at ~100 GeV. It is the highest state of PG 1553+113 ever detected at these energies. The mean flux at 100 GeV measured by MAGIC between 2005 and 2009 was ~50% of the Crab Nebula flux (J. Aleksic et al., 2012). Follow up observations carried out in the following nights confirm that the source persists in this high state. Simultaneous optical observations performed in the R band by the KVA telescope also show increased emission. The maximum flux reached is 13.14 ± 0.01 mJy (MJD 56040). The source is brighter than during the high state reported one month ago (12.2 ± 0.2 mJy ; http://users.utu.fi/kani/1m/PG_1553+113_jy.html ). Optical polarimetric observations were taken with the Liverpool telescope as part of a joint observational program with MAGIC. Preliminary photometric observations in the J, H and K bands with the REM telescope show an increasing activity of the source during the last week. In addition, automatic analysis procedures applied to Swift/XRT data collected on April 17th and 21st indicate that the source is also brightening in X rays. The preliminary Swift/XRT lightcurve is publicly available at: http://www.swift.psu.edu/monitoring/data/PG1553+113/lightcurve.png. Dedicated analyses are in progress. Given the high activity detected, we strongly encourage multi-wavelength observations of the source.

The MAGIC telescopes have observed a high VHE (E>~100 GeV) gamma-ray flux from the galaxy IC 310. The object (RA: 03h 16m 43.0s, Dec: +41d 19m 29s, J2000) is a TeV radio-loud galaxy located in the Perseus Cluster of galaxies at redshift 0.0189 (Falco et al. 1999). Although formerly considered to be an archetypical head-tail galaxy, recent radio-interferometric observations have shown that IC 310 hosts a blazar-type central engine (Kadler et al. 2012, A&A, 538, L1). The source was discovered as a VHE emitter by MAGIC in the 2009-2010 campaign, showing a mean flux level of (2.5 +- 0.4)% of the Crab Nebula flux above 300 GeV (J. Aleksic et al. (MAGIC Coll.), Astrophys. J. 723(2010) L207). MAGIC observations were carried out on November 12, 2012 (MJD 56243.9 - 56244.1) right after the upgrade of the MAGIC telescopes has been completed. Preliminary analysis resulted in a detection with the significance of 25 standard deviations. The mean flux above 300 GeV is higher than 50% of the Crab Nebula flux which is the highest ever detected from IC 310 in the VHE range. MAGIC will continue to observe the source and multi-frequency observations are strongly encouraged.

The MAGIC telescopes have observed an increased VHE (E>~100 GeV) gamma-ray flux from the blazar PG 1553+113 in the course of a multi-wavelength campaign started on 2012 February 23. PG 1553+113 (RA: 15h 55m 43.0s Dec: +11d 11m 24s) is a TeV BL-Lac object likely located at redshift 0.4-0.5 (Danforth et al. 2010). Between February 23 and March 5 an extensive multi-wavelength campaign coordinated by the MAGIC Collaboration was performed, involving besides MAGIC, radio (Metsahovi), near-infrared (REM), optical (KVA), UV (Swift/UVOT), and X-ray (Swift/XRT) observations. Preliminary analysis of MAGIC data shows a firm detection with significance around 15 sigma in 4 hours of good quality data. According to this analysis the estimated flux is above 15% Crab in the VHE range, one of the highest fluxes ever detected from PG 1553+113. The analysis of MAGIC data is still in progress. Preliminary analysis of X-ray data taken with Swift/XRT reports a 2-10 keV flux rising from (16.8+/-1.0)E-12 erg/cm2/s to (23.0+/-1.3)E-12 erg/cm2/s between February 16 to March 2. The XRT spectrum obtained on single daily snapshots is fairly fitted with an absorbed power law with an absorbing column density fixed to the Galactic value of 3.65E20 cm-2 (Kalberla et al. 2005), yielding a photon index around 2.3+/-0.1, relatively stable within errors. Swift/UVOT observed with all the optical and UV filters, providing the following preliminary averaged magnitudes, not corrected for absorption, and fluxes, corrected for Galactic extinctions due to reddening of E(B-V)=0.052 mag in the direction of the source (Schlegel et al 1998).

The MAGIC Collaboration reports the discovery of Very High Energy (VHE ; E>100 GeV) gamma-ray emission from the BL Lac object 1ES 1727+502 (also known as OT546) with redshift z=0.055. The source was selected from the compilation of Costamante, L. & Ghisellini, G. 2002, A&A, 384, 56. Previous observations with the single MAGIC-I telescope yielded an upper limit on the level of 11.8% of the Crab Nebula flux above 140 GeV (J. Aleksic et al. (MAGIC Coll.), Astrophys. J. 729 (2010) 115). A total observation time of 12.5 hours was collected between 2011 May 6th to June 10th in stereoscopic mode with the two 17 m diameter imaging Cherenkov telescopes on La Palma, Canary Islands, Spain. The preliminary analysis of this data using the standard analysis chain yields a detection of 76 gamma-rays above 150 GeV, corresponding to a statistical significance of 5 standard deviations. The observed flux is estimated to be (1.7+/-0.6)% of the Crab Nebula flux above 150 GeV, well below the previous upper limit. Errors are statistical only.

The unidentified and variable TeV gamma-ray source HESS J0632+057 was recently reported to show a strong flux increase in X-rays by Swift (ATel #3152) starting Jan. 23, 2011 and staying active at least up to Feb. 6, 2011. Shortly afterwards an increase in the TeV flux around Feb. 7/8, 2011 was reported by the VERITAS collaboration (Atel #3153). The TeV source HESS J0632+057 was suggested to be a binary system and the recent X-ray measurements suggest an orbital period of ~ 320 days (ATel #3152). MAGIC monitored HESS J0632+057 during the same time period as Swift and VERITAS. We observed the source between Feb. 7-9, 2011 and our preliminary analysis results in a detection of a significant (above 5 standard deviations) gamma-ray signal above 200 GeV. The estimated flux corresponds to about 3.4% of the Crab Nebula flux in the same energy band. No indication of day-to-day variability is found. Further observations of HESS J0632+057 with MAGIC are planned for the next nights, to monitor the flux level and duration of the gamma-ray activity. MAGIC consists of two 17m diameter imaging air Cherenkov telescopes operating in stereoscopic mode located on La Palma, Canary Islands, Spain. Questions regarding the MAGIC observations should be directed to Mose Mariotti (mose.mariotti@pd.infn.it).

After re-analysis of archival data, the MAGIC Collaboration reports the discovery of very high energy (VHE ; E >100 GeV) gamma-ray emission from the BL Lac object 1ES0033+595 (RA: 00:35:52.63, Dec.: 59:50:04.56), of unknown redshift. The source was observed with the MAGIC stereoscopic system for about 24 hours in August through October 2009 during the commissioning phase of the instrument. Preliminary analysis using the standard analysis chain shows an excess of 357 photons above 100 GeV, that corresponds to a statistical significance of 5.2 sigmas after trials. The observed flux is estimated to be 1.5% of the Crab nebula flux above 150 GeV, and it rapidly decreases with energy. No hint of variability is seen in the preliminary VHE light curve. This blazar is currently observable from the Northern hemisphere.

The MAGIC Collaboration reports the discovery of Very High Energy (VHE ; >100 GeV) gamma-ray emission from the BL Lac object 1ES 1215+303 (also known as ON325) with z=0.130 (White et al. 2000 give z=0.237) based on a 5.6 hour-long observation performed from 2011 January 2nd to 5th in stereoscopic mode with the two 17m diameter imaging Cherenkov telescopes on La Palma, Canary Islands, Spain. The preliminary analysis of the MAGIC data using standard cuts yields a detection of 25 gamma-rays above 250 GeV, corresponding to a statistical significance of 5 standard deviations. The observed flux is estimated to be (2.0+/-1.0)% of the Crab nebula flux above 250 GeV. The source has been flagged as a promising VHE source candidate by the Fermi-LAT collaboration in October 2010. The MAGIC observations were triggered by an optical high-state of the source, reported by the Tuorla blazar monitoring program (http://users.utu.fi/kani/1m/ON_325.html). Target of Opportunity Observations with Swift have also been performed. Fast analysis of the data show that in X-rays the flux is almost doubled respect to previous observation (December 2009) but the spectral shape is almost unchanged. We thank the Swift team for accepting and promptly scheduling the X-ray observations. MAGIC observations suggest also a higher state of a known VHE gamma-ray emitter 1ES 1218+304 in the same field of view, from which an excess of above 5 standard deviation was observed. MAGIC will continue observations of both sources. Observations at other wavelengths are encouraged. Questions regarding the MAGIC observations should be directed to Mose Mariotti (mose.mariotti@pd.infn.it).

The MAGIC Collaboration reports the detection of Very High Energy (VHE) gamma-ray emission from a position consistent with NGC 1275, the central radio galaxy of the Perseus cluster of galaxies. The MAGIC observations were carried out in stereoscopic mode starting from August 2010, accumulating 14 h of good quality data. Preliminary analysis using the standard analysis chain with a energy threshold of 100 GeV, shows an excess of 280 gamma-rays, corresponding to a statistical significance of 5.2 standard deviations. The observed flux is estimated to be ~3% of the Crab nebula flux above 100 GeV, and it decreases rapidly with energy. No signal is detected above 400 GeV. The MAGIC VHE detection happened during a period of increased high gamma-ray activity of NGC 1275, as reported in July 2010 by the Fermi/LAT collaboration, ATel#2737, and continuing until October, according to an analysis of public Fermi/LAT data. MAGIC will continue observations of NGC1275. Observations at other wavelengths are encouraged.

The MAGIC Collaboration reports the discovery of Very High Energy (VHE ; >100 GeV) gamma-ray emission from the High Frequency peaking BL Lac object B3 2247+381 with z=0.1187. The source is positionally consistent with the Fermi-LAT gamma-ray source 1FGL J2250.1+3825 (RA 22 50 06.6 dec +38 25 58, J2000), which was flagged as a promising VHE source candidate by the Fermi-LAT collaboration, information which was shared with the MAGIC collaboration (as well as other IACTs) back in October 2009. The MAGIC observations were triggered by an optical high-state of the source, reported by the Tuorla blazar monitoring program (http://users.utu.fi/kani/1m/B3_2247+381.html). The VHE detection is based on a 9.3 hour-long observation performed on 2010 September 30th, October 1st, 2nd, 4th, 5th and 6th in stereoscopic mode with the two 17m diameter imaging Cherenkov telescopes on La Palma, Canary Islands, Spain. The preliminary analysis of the MAGIC data using standard cuts yields a detection of 64 gamma-rays above 150 GeV, corresponding to a pre-trial statistical significance of 5 standard deviations. The observed flux is estimated to be ~2% of the Crab nebula flux above 150 GeV. Target of Opportunity Observations with Swift have also been performed on this source location. A preliminary analysis of the Swift/XRT data shows that the X-ray flux from the source is ~4 times higher than during last observation (spring 2010). Further Swift observations are expected until October 15. We thank the Swift team for accepting and promptly scheduling the X-ray observations. MAGIC will continue observations of B3 2247+381. Observations at other wavelengths are encouraged.