Publications by Garret Cotter

Test bench for front end electronic of the GCT camera for the Cherenkov Telescope Array


A De Franco, G Cotter, CTAC Collaboration

The MeerKAT international GHz tiered extragalactic exploration (MIGHTEE) survey

Proceedings of Science Part F138095 (2016)

MJ Jarvis, AR Taylor, I Agudo, JR Allison, RP Deane, B Frank, N Gupta, I Heywood, N Maddox, K McAlpine, MG Santos, AMM Scaife, M Vaccari, JTL Zwart, E Adams, DJ Bacon, AJ Baker, BA Bassett, PN Best, R Beswick, S Blyth, ML Brown, M Brüggen, M Cluver, S Colafranceso, G Cotter, C Cress, R Davé, C Ferrari, MJ Hardcastle, C Hale, I Harrison, PW Hatfield, HR Klöckner, S Kolwa, E Malefahlo, T Marubini, T Mauch, K Moodley, R Morganti, R Norris, JA Peters, I Prandoni, M Prescott, S Oliver, N Oozeer, HJA Röttgering, N Seymour, C Simpson, O Smirnov, DJB Smith, K Spekkens, J Stil, C Tasse, K van der Heyden, IH Whittam, WL WIlliams

© Copyright owned by the author(s). The MIGHTEE large survey project will survey four of the most well-studied extragalactic deep fields, totalling 20 square degrees to µJy sensitivity at Giga-Hertz frequencies, as well as an ultra-deep image of a single ∼1 deg2MeerKAT pointing. The observations will provide radio continuum, spectral line and polarisation information. As such, MIGHTEE, along with the excellent multi-wavelength data already available in these deep fields, will allow a range of science to be achieved. Specifically, MIGHTEE is designed to significantly enhance our understanding of, (i) the evolution of AGN and star-formation activity over cosmic time, as a function of stellar mass and environment, free of dust obscuration; (ii) the evolution of neutral hydrogen in the Universe and how this neutral gas eventually turns into stars after moving through the molecular phase, and how efficiently this can fuel AGN activity; (iii) the properties of cosmic magnetic fields and how they evolve in clusters, filaments and galaxies. MIGHTEE will reach similar depth to the planned SKA all-sky survey, and thus will provide a pilot to the cosmology experiments that will be carried out by the SKA over a much larger survey volume.

The Cherenkov Telescope Array potential for the study of young supernova remnants


BS Acharya, C Aramo, A Babic, JA Barrio, A Baushev, JB Tjus, D Berge, M Bohacova, A Bonardi, A Brown, V Bugaev, T Bulik, M Burton, G Busetto, P Caraveo, R Carosi, J Carr, P Chadwick, J Chudoba, V Conforti, V Connaughton, JL Contreras, G Cotter, F Dazzi, A De Franco, I de la Calle, RDLR Lopez, B De Lotto, F De Palma, T Di Girolamo, C Di Giulio, F Di Pierro, J-L Dournaux, V Dwarkadas, J Ebr, K Egberts, M Fesquet, H Fleischhack, L Font, G Fontaine, A Foerster, M Fuessling, B Garcia, RG Lopez, M Garczarczyk, F Gargano, D Garrido, M Gaug, N Giglietto, F Giordano, A Giuliani, N Godinovic, MM Gonzalez, T Grabarczyk, T Hassan, J Hoerandel, M Hrabovsky, D Hrupec, TB Humensky, J Huovelin, M Jamrozy, P Janecek, PE Kaaret, U Katz, S Kaufmann, B Khelifi, W Kluzniak, J Kocot, N Komin, H Kubo, J Kushida, G Lamanna, WH Lee, J-P Lenain, T Lohse, S Lombardi, R Lopez-Coto, A Lopez-Oramas, F Lucarelli, MC Maccarone, G Maier, P Majumdar, G Malaguti, D Mandat, MN Mazziotta, K Meagher, N Mirabal, A Morselli, E Moulin, J Niemiec, M Nievas, K Nishijima, D Nosek, F Nunio, M Ohishi, S Ohm, RA Ong, R Orito, N Otte, M Palatka, G Pareschi, M Pech, M Persic, M Pohl, M Prouza, A Quirrenbach, S Raino, GR Fernandez, P Romano, AC Rovero, B Rudak, P Schovanek, M Shayduk, H Siejkowski, A Sillanpaa, S Stefanik, T Stolarczyk, M Szanecki, T Szepieniec, LA Tejedor, I Telezhinsky, M Teshima, L Tibaldo, O Tibolla, G Tovmassian, P Travnicek, M Trzeciak, P Vallania, C van Eldik, S Vercellone, C Vigorito, SJ Wagner, SP Wakely, A Weinstein, A Wierzcholska, A Wilhelm, P Wojcik, T Yoshikoshi

Radio Galaxy Zoo: host galaxies and radio morphologies derived from visual inspection


JK Banfield, OI Wong, KW Willett, RP Norris, L Rudnick, SS Shabala, BD Simmons, C Snyder, A Garon, N Seymour, E Middelberg, H Andernach, CJ Lintott, K Jacob, AD Kapinska, MY Mao, KL Masters, MJ Jarvis, K Schawinski, E Paget, R Simpson, H-R Kloeckner, S Bamford, T Burchell, KE Chow, G Cotter, L Fortson, I Heywood, TW Jones, S Kaviraj, AR Lopez-Sanchez, WP Maksym, K Polsterer, K Borden, RP Hollow, L Whyte

New constraints on the structure and dynamics of black hole jets


WJ Potter, G Cotter

The small size telescope projects for the Cherenkov Telescope Array

Proceedings of Science 30-July-2015 (2015)

T Montaruli, W Bilnik, J BŁocki, L Bogacz, T Bulik, F Cadoux, A Christov, M CuryŁo, D Della Volpe, M Dyrda, Y Favre, A Frankowski, L Grudniki, M Grudzińska, M Heller, B Idźkowski, M Jamrozy, M Janiak, J Kasperek, K Lalik, E Lyard, E Mach, D Mandat, A MarszaŁek, J MichaŁowski, R Moderski, A Neronov, J Niemiec, M Ostrowski, P Pásko, M Pech, A Porcelli, E Prandini, P Rajda, M Rameez, E Schioppa, P Schovanek, K Seweryn, K Skowron, V Sliusar, M Sowiński, L Stawarz, M Stodulska, M Stodulski, S Toscano, I Troyano Pujadas, R Walter, M Wiȩcek, A Zagdanński, K Ziȩtara, P Zychowski, A Abchiche, JP Amans, T Armstrong, A Balzer, D Berge, JJ Bousquet, A Brown, M Bryan, G Buchholtz, P Chadwick, H Costantini, G Cotter, M Daniel, F De Frondat, JL Dournaux, D Dumas, JP Ernenwein, G Fasola, A De Franco, J Gaudemard, J Hinton, JM Huet, J Lapington, P Laporte, SJ Nolan, J Osborne, S Rosen, D Ross, H Sol, G Rowell, J Schmoll, R Stuik, P Sutcliffe, J Sykes, H Tajima, R White, A Zech

The small size telescopes (SSTs), spread over an area of several square km, dominate the CTA sensitivity in the photon energy range from a few TeV to over 100 TeV, enabling for the detailed exploration of the very high energy gamma-ray sky. The proposed telescopes are innovative designs providing a wide field of view. Two of them, the ASTRI (Astrophysics con Specchi a Tecnologia Replicante Italiana) and the GCT (Gamma-ray Cherenkov Telescope) telescopes, are based on dual mirror Schwarzschild-Couder optics, with primary mirror diameters of 4 m. The third, SST-1M, is a Davies-Cotton design with a 4 m diameter mirror. Progress with the construction and testing of prototypes of these telescopes is presented. The SST cameras use silicon photomultipliers, with preamplifier and readout/trigger electronics designed to optimize the performance of these sensors for (atmospheric) Cherenkov light. The status of the camera developments is discussed. The SST sub-array will consist of about 70 telescopes at the CTA southern site. Current plans for the implementation of the array are presented.

Redshift measurement of fermi blazars for the cherenkov telescope array

Proceedings of Science 30-July-2015 (2015)

P Goldoni, S Pita, C Boisson, G Cotter, DA Williams, E Lindfors

Blazars are active galactic nuclei, and the most numerous High Energy (HE) and Very High Energy (VHE) γ-ray emitters. Their optical emission is often dominated by non-thermal, and, in the case of BL Lacs, featureless continuum radiation. This renders the determination of their redshift extremely difficult. Indeed, as of today only about 50% of γ-ray blazars have a measured spectroscopic redshift. The knowledge of redshift is fundamental because it allows the precise modeling of the VHE emission and also of its interaction with the extragalactic background light (EBL). The beginning of the Cherenkov Telescope Array (CTA) operations in the near future will allow the detection of several hundreds of new BL Lacs. Using the first Fermi catalogue of sources above 10 GeV (1FHL), we performed simulations which demonstrate that at least half of the 1FHL BL Lacs detectable by CTA will not have a measured redshift. Indeed the organization of observing campaigns to measure the redshift of these blazars has been recognized as a necessary support for the AGN Key Science Project of CTA. Taking advantage of the recent success of an X-shooter GTO observing campaign, we thus devised an observing campaign to measure the redshifts of as many as possible of these candidates. The main characteristic of this campaign with respect to previous ones will be the use of higher resolution spectrographs and of 8 meter class telescopes. We are starting submitting proposals for these observations. In this paper we will briefly describe the selection of the candidates, the characteristics of these observation and the expected results.

Black holes in 4 nearby radio galaxies

Astrophysics and Space Science 356 (2015) 347-351

J Mould, T Readhead, G Cotter, D Batt, M Durré

© 2014, Springer Science+Business Media Dordrecht. We study the velocity dispersion profiles of the nuclei of NGC 1326, 2685, 5273 and 5838 in the CO first overtone band. There is evidence for a black hole (BH) in NGC 1326 and 5838. Gas is seen flowing out of the nuclear region of NGC 5273. We put upper limits on the nuclear BHs responsible for its activity and that of NGC 2685.

Magnetospherically driven optical and radio aurorae at the end of the stellar main sequence.

Nature 523 (2015) 568-571

G Hallinan, SP Littlefair, G Cotter, S Bourke, LK Harding, JS Pineda, RP Butler, A Golden, G Basri, JG Doyle, MM Kao, SV Berdyugina, A Kuznetsov, MP Rupen, A Antonova

Aurorae are detected from all the magnetized planets in our Solar System, including Earth. They are powered by magnetospheric current systems that lead to the precipitation of energetic electrons into the high-latitude regions of the upper atmosphere. In the case of the gas-giant planets, these aurorae include highly polarized radio emission at kilohertz and megahertz frequencies produced by the precipitating electrons, as well as continuum and line emission in the infrared, optical, ultraviolet and X-ray parts of the spectrum, associated with the collisional excitation and heating of the hydrogen-dominated atmosphere. Here we report simultaneous radio and optical spectroscopic observations of an object at the end of the stellar main sequence, located right at the boundary between stars and brown dwarfs, from which we have detected radio and optical auroral emissions both powered by magnetospheric currents. Whereas the magnetic activity of stars like our Sun is powered by processes that occur in their lower atmospheres, these aurorae are powered by processes originating much further out in the magnetosphere of the dwarf star that couple energy into the lower atmosphere. The dissipated power is at least four orders of magnitude larger than what is produced in the Jovian magnetosphere, revealing aurorae to be a potentially ubiquitous signature of large-scale magnetospheres that can scale to luminosities far greater than those observed in our Solar System. These magnetospheric current systems may also play a part in powering some of the weather phenomena reported on brown dwarfs.

Wavefront sensing from the image domain with the Oxford-SWIFT integral field spectrograph


B Pope, N Thatte, R Burruss, M Tecza, F Clarke, G Cotter

The cosmic evolution of Fermi BL Lacertae objects

Astrophysical Journal 780 (2014)

M Ajello, RW Romani, D Gasparrini, MS Shaw, J Bolmer, G Cotter, J Finke, J Greiner, SE Healey, O King, W Max-Moerbeck, PF Michelson, WJ Potter, A Rau, ACS Readhead, JL Richards, P Schady

Fermi has provided the largest sample of γ-ray-selected blazars to date. In this work we use a uniformly selected set of 211 BL Lacertae (BL Lac) objects detected by Fermi during its first year of operation. We obtained redshift constraints for 206 out of the 211 BL Lac objects in our sample, making it the largest and most complete sample of BL Lac objects available in the literature. We use this sample to determine the luminosity function of BL Lac objects and its evolution with cosmic time. We find that for most BL Lac classes the evolution is positive, with a space density peaking at modest redshift (z ≈ 1.2). Low-luminosity, high-synchrotron-peaked (HSP) BL Lac objects are an exception, showing strong negative evolution, with number density increasing for z ≲ 0.5. Since this rise corresponds to a drop-off in the density of flat-spectrum radio quasars (FSRQs), a possible interpretation is that these HSPs represent an accretion-starved end state of an earlier merger-driven gas-rich phase. We additionally find that the known BL Lac correlation between luminosity and photon spectral index persists after correction for the substantial observational selection effects with implications for the so-called "blazar sequence." Finally, by estimating the beaming corrections to the luminosity function, we find that BL Lac objects have an average Lorentz factor of , and that most are seen within 10° of the jet axis. © 2014. The American Astronomical Society. All rights reserved.

The dual-mirror small size telescope for the Cherenkov Telescope Array

Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013 2013-October (2013)

G Pareschi, G Agnetta, LA Antonelli, D Bastieri, G Bellassai, M Belluso, S Billotta, B Biondo, G Bonanno, G Bonnoli, P Bruno, A Bulgarelli, R Canestrari, P Caraveo, A Carosi, E Cascone, O Catalano, M Cereda, P Conconi, V Conforti, G Cusumano, V de Caprio, A de Luca, A Di Paola, F Di Pierro, D Fantinel, M Fiorini, D Fugazza, D Gardiol, M Ghigo, F Gianotti, S Giarrusso, E Giro, A Grillo, D Impiombato, S Incorvaia, A la Barbera, N la Palombara, V la Parola, G la Rosa, L Lessio, G Leto, S Lombardi, F Lucarelli, MC Maccarone, G Malaguti, G Malaspina, A Mangano, V Mangano, D Marano, E Martinetti, R Millul, T Mineo, A Mistó, C Morello, MR Panzera, C Perna, G Rodeghiero, P Romano, F Russo, B Sacco, N Sartore, J Schwarz, A Segreto, G Sironi, G Sottile, E Strazzeri, L Stringhetti, G Tagliaferri, V Testa, MC Timpanaro, G Toso, G Tosti, M Trifoglio, P Vallania, S Vercellone, V Zitelli, D Dumas, P Laporte, H Sol, F de Frondat, JM Huet, JL Dournaux, JP Amans, S Blanc, G Fasola, R Fleurisson, O Hervet, I Jegouzo-Giroux, D Massol, C Rulten, F Sayede, D Savoie, A Zech, C Boisson, P Delevoye, N Ollivier, R White, J Hinton, D Ross

© 2013 Sociedade Brasileira de Fisica. All Rights Reserved. In this paper, the development of the dual mirror Small Size Telescopes (SST) for the Cherenkov Telescope Array (CTA) is reviewed. Up to 70 SST, with a primary mirror diameter of ∼ 4 m, will be produced and installed at the CTA southern site. These will allow investigation of the gamma-ray sky at the highest energies accessible to CTA, in the range from about 1 TeV to 300 TeV. The telescope presented in this contribution is characterized by two major innovations: the use of a dual mirror Schwarzschild-Couder configuration and of an innovative camera using as sensors either multi-anode photomultipliers (MAPM) or silicon photomultipliers (SiPM). The reduced plate-scale of the telescope, achieved with the dual-mirror optics, allows the camera to be compact (∼ 40 cm in diameter), and low-cost. The camera, which has about 2000 pixels of size 6×6 mm2, covers a field of view of ∼ 10◦. The dual mirror telescopes and their cameras are being developed by three consortia, ASTRI (Astrofisica con Specchi a Tecnologia Replicante Italiana, Italy/INAF), GATE (Gamma-ray Telescope Elements, France/Paris Observ.) and CHEC (Compact High Energy Camera, universities in UK, US and Japan) which are merging their efforts in order to finalize an end-to-end design that will be constructed for CTA. A number of prototype structures and cameras are being developed in order to investigate various alternative designs. In this contribution, these designs are presented, along with the technological solutions under study.

A compact high energy camera for the cherenkov telescope array

Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013 2013-October (2013)

MK Daniel, RW White, D Berge, J Buckley, PM Chadwick, G Cotter, S Funk, T Greenshaw, N Hidaka, J Hinton, J Lapington, S Markoff, P Moore, S Nolan, S Ohm, A Okumura, D Ross, L Sapozhnikov, J Schmoll, P Sutcliffe, J Sykes, H Tajima, GS Varner, J Vandenbroucke, J Vink, D Williams

© 2013 Sociedade Brasileira de Fisica. All Rights Reserved. The Compact High Energy Camera (CHEC) is a camera-development project involving UK, US, Japanese and Dutch institutes for the dual-mirror Small-Sized Telescopes (SST-2M) of the Cherenkov Telescope Array (CTA). Two CHEC prototypes, based on different photosensors are funded and will be assembled and tested in the UK over the next ≈18 months. CHEC is designed to record flashes of Cherenkov light lasting from a few to a hundred nanoseconds, with typical RMS image width and length of ∼ 0.2◦ × 1.0◦, and has a 9◦ field of view. The physical camera geometry is dictated by the telescope optics: a curved focal surface with radius of curvature 1 m and diameter ∼35 cm is required. CHEC is designed to work with both the ASTRI and GATE SST-2M telescope structures and will include an internal LED flasher system for calibration. The first CHEC prototype will be based on multi-anode photomultipliers (MAPMs) and the second on silicon photomultipliers (SiPMs or MPPCs). The first prototype will soon be installed on the ASTRI SST-2M prototype structure on Mt. Etna.

Synchrotron and inverse-Compton emission from blazar jets - IV. BL Lac type blazars and the physical basis for the blazar sequence

Monthly Notices of the Royal Astronomical Society 436 (2013) 304-314

WJ Potter, G Cotter

In this paper, we investigate the properties of a sample of six BL Lacs by fitting their spectra using our inhomogeneous jet model with an accelerating, magnetically dominated, parabolic base, which transitions to a slowly decelerating conical jet with a geometry based on observations of M87. Our model is able to fit very well to the simultaneous multiwavelength spectra of all the BL Lacs including radio observations. We find that the BL Lacs have lower jet powers and bulk Lorentz factors than the sample of Compton-dominant blazars investigated in Paper III, consistent with the blazar sequence. Excitingly, we find a correlation between the radius at which the jet first comes into equipartition and the jet power, in agreement with our prediction from Paper III.We interpret this result as one of two physical scenarios: a universal jet geometry which scales linearly with black hole mass or a dichotomy in Eddington accretion rates between flat-spectrum radio quasars (FSRQs) and BL Lacs. If we assume that the jet geometry of all blazars scales linearly with black hole mass, then we find a plausible range of masses (~107-1010M⊙).We find that the quiescent gamma-ray spectrum ofMarkarian 421 is best fitted by scattering of external cosmic microwave background photons. We are unable to fit the spectrum using synchrotron self-Compton emission due to strong gamma-ray absorption via pair production even using a compact, rapidly decelerating, jet with a very large bulk Lorentz factor (50), as has been suggested recently. This is because the ratio of synchrotron to inverse-Compton emission requires a high density of synchrotron photons to scatter which makes the region opaque to TeV gamma-rays even with large bulk Lorentz factors. Finally, we fit to the spectral energy distributions of the four high power high synchrotron peak frequency BL Lacs recently found by Padovani et al. We find that their high peak frequency emission is caused by high maximum electron energies whilst the rest of their jet properties are typical of relatively high power BL Lacs and consistent with our predictions. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Uncovering the physics behind the blazar sequence using a realistic model for jet emission


WJ Potter, G Cotter

Synchrotron and inverse-compton emission from blazar jets - II. An accelerating jet model with a geometry set by observations of M87

Monthly Notices of the Royal Astronomical Society 429 (2013) 1189-1205

WJ Potter, G Cotter

In this paper we develop the jet model of Potter & Cotter to include a magnetically dominated accelerating parabolic base transitioning to a slowly decelerating conical jet with a geometry set by recent radio observations of M87. We conserve relativistic energy-momentum and particle number along the jet and calculate the observed synchrotron emission from the jet by calculating the integrated line-of-sight synchrotron opacity through the jet in the rest frame of each section of plasma. We calculate the inverse-Compton emission from synchrotron, cosmic microwave background (CMB), accretion disc, starlight, broad-line region (BLR), dusty torus and narrow-line region photons by transforming into the rest frame of the plasma along the jet. We fit our model to simultaneous multi-wavelength observations of the Compton-dominant FSRQ type blazar PKS 0227-369, with a jet geometry set by M87 and an accelerating bulk Lorentz factor consistent with simulations and theory. We investigate models in which the jet comes into equipartition at different distances along the jet and equipartition is maintained via the conversion of jet bulk kinetic energy into particle acceleration. We find that the jet must still be magnetically dominated within the BLR and cannot be in equipartition due to the severe radiative energy losses. The model fits the observations, including radio data, very well if the jet comes into equipartition outside the BLR within the dusty torus (1.5 pc) or at further distances (34 pc). The fits require a high-power jet with a large bulk Lorentz factor observed close to the line of sight, consistent with our expectations for a Compton-dominant blazar. We find that our fit in which the jet comes into equipartition furthest along the jet, which has a jet with the geometry of M87 scaled linearly with black hole mass, has an inferred black hole mass close to previous estimates. This implies that the jet of PKS 0227 might be well described by the same jet geometry as M87. © 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

Spectroscopy of the largest ever γ-ray-selected BL Lac sample

Astrophysical Journal 764 (2013)

MS Shaw, RW Romani, G Cotter, SE Healey, PF Michelson, ACS Readhead, JL Richards, W Max-Moerbeck, OG King, WJ Potter

We report on spectroscopic observations covering most of the 475 BL Lacs in the second Fermi Large Area Telescope (LAT) catalog of active galactic nuclei (AGNs). Including archival measurements (correcting several erroneous literature values) we now have spectroscopic redshifts for 44% of the BL Lacs. We establish firm lower redshift limits via intervening absorption systems and statistical lower limits via searches for host galaxies for an additional 51% of the sample leaving only 5% of the BL Lacs unconstrained. The new redshifts raise the median spectroscopic from 0.23 to 0.33 and include redshifts as large as z = 2.471. Spectroscopic redshift minima from intervening absorbers have , showing a substantial fraction at large z and arguing against strong negative evolution. We find that detected BL Lac hosts are bright ellipticals with black hole masses M • 108.5-109, substantially larger than the mean of optical AGNs and LAT Flat Spectrum Radio Quasar samples. A slow increase in M • with z may be due to selection bias. We find that the power-law dominance of the optical spectrum extends to extreme values, but this does not strongly correlate with the γ-ray properties, suggesting that strong beaming is the primary cause of the range in continuum dominance. © 2013. The American Astronomical Society. All rights reserved.

Synchrotron and inverse-Compton emission from blazar jets - III. Compton-dominant blazars


WJ Potter, G Cotter

Introducing the CTA concept


BS Acharya, M Actis, T Aghajani, G Agnetta, J Aguilar, F Aharonian, M Ajello, A Akhperjanian, M Alcubierre, J Aleksic, R Alfaro, E Aliu, AJ Allafort, D Allan, I Allekotte, E Amato, J Anderson, EO Anguener, LA Antonelli, P Antoranz, A Aravantinos, T Arlen, T Armstrong, H Arnaldi, L Arrabito, K Asano, T Ashton, HG Asorey, Y Awane, H Baba, A Babic, N Baby, J Baehr, A Bais, C Baixeras, S Bajtlik, M Balbo, D Balis, C Balkowski, A Bamba, R Bandiera, A Barber, C Barbier, M Barcelo, A Barnacka, J Barnstedt, U Barres de Almeida, JA Barrio, A Basili, S Basso, D Bastieri, C Bauer, A Baushev, J Becerra, Y Becherini, KC Bechtol, JB Tjus, V Beckmann, W Bednarek, B Behera, M Belluso, W Benbow, J Berdugo, K Berger, F Bernard, T Bernardino, K Bernloehr, N Bhat, S Bhattacharyya, C Bigongiari, A Biland, S Billotta, T Bird, E Birsin, E Bissaldi, J Biteau, M Bitossi, S Blake, O Blanch Bigas, P Blasi, A Bobkov, V Boccone, M Boettcher, L Bogacz, J Bogart, M Bogdan, C Boisson, J Boix Gargallo, J Bolmont, G Bonanno, A Bonardi, T Bonev, P Bonifacio, G Bonnoli, P Bordas, A Borgland, J Borkowski, R Bose, O Botner, A Bottani, L Bouchet, M Bourgeat, C Boutonnet, A Bouvier, S Brau-Nogue, I Braun, T Bretz, M Briggs, T Bringmann, P Brook, P Brun, L Brunetti, T Buanes, J Buckley, R Buehler, V Bugaev, A Bulgarelli, T Bulik, G Busetto, S Buson, K Byrum, M Cailles, R Cameron, J Camprecios, R Canestrari, S Cantu, M Capalbi, P Caraveo, E Carmona, A Carosi, J Carr, P-H Carton, S Casanova, M Casiraghi, O Catalano, S Cavazzani, S Cazaux, M Cerruti, E Chabanne, P Chadwick, C Champion, A Chen, J Chiang, L Chiappetti, M Chikawa, VR Chitnis, F Chollet, J Chudoba, M Cieslar, A Cillis, J Cohen-Tanugi, S Colafrancesco, P Colin, J Calome, S Colonges, M Compin, P Conconi, V Conforti, V Connaughton, J Conrad, JL Contreras, P Coppi, P Corona, D Corti, J Cortina, L Cossio, H Costantini, G Cotter, B Courty, S Couturier, S Covino, G Crimi, SJ Criswell, J Croston, G Cusumano, M Dafonseca, O Dale, M Daniel, J Darling, I Davids, F Dazzi, A De Angelis, V De Caprio, F De Frondat, EM de Gouveia Dal Pino, I de la Calle, GA De La Vega, RDLR Lopez, B De Lotto, A De Luca, JRT de Mello Neto, M de Naurois, Y de Oliveira, E de Ona Wilhelmi, V de Souza, G Decerprit, G Decock, C Deil, E Delagnes, G Deleglise, C Delgado, D Della Volpe, P Demange, G Depaola, A Dettlaff, A Di Paola, F Di Pierro, C Diaz, J Dick, R Dickherber, H Dickinson, V Diez-Blanco, S Digel, D Dimitrov, G Disset, A Djannati-Atai, M Doert, M Dohmke, W Domainko, DD Prester, A Donat, D Dorner, M Doro, J-L Dournaux, G Drake, D Dravins, L Drury, F Dubois, R Dubois, G Dubus, C Dufour, D Dumas, J Dumm, D Durand, J Dyks, M Dyrda, J Ebr, E Edy, K Egberts, P Eger, S Einecke, C Eleftheriadis, S Elles, D Emmanoulopoulos, D Engelhaupt, R Enomoto, J-P Ernenwein, M Errando, A Etchegoyen, P Evans, A Falcone, D Fantinel, K Farakos, C Farnier, G Fasola, B Favill, E Fede, S Federici, S Fegan, F Feinstein, D Ferenc, P Ferrando, M Fesquet, A Fiasson, E Fillin-Martino, D Fink, C Finley, JP Finley, M Fiorini, R Firpo Curcoll, H Flores, D Florin, W Focke, C Foehr, E Fokitis, L Font, G Fontaine, M Fornasa, A Foerster, L Fortson, N Fouque, A Franckowiak, C Fransson, G Fraser, R Frei, IFM Albuquerque, L Fresnillo, C Fruck, Y Fujita, Y Fukazawa, Y Fukui, S Funk, W Gaebele, S Gabici, R Gabriele, A Gadola, N Galante, D Gall, Y Gallant, J Gamez-Garcia, B Garcia, R Garcia Lopez, D Gardiol, D Garrido, L Garrido, D Gascon, M Gaug, J Gaweda, L Gebremedhin, N Geffroy, L Gerard, A Ghedina, M Ghigo, E Giannakaki, F Gianotti, S Giarrusso, G Giavitto, B Giebels, V Gika, P Giommi, N Girard, E Giro, A Giuliani, T Glanzman, J-F Glicenstein, N Godinovic, V Golev, M Gomez Berisso, J Gomez-Ortega, MM Gonzalez, A Gonzalez, F Gonzalez, A Gonzalez Munoz, KS Gothe, M Gougerot, R Graciani, P Grandi, F Granena, J Granot, G Grasseau, R Gredig, A Green, T Greenshaw, T Gregoire, O Grimm, J Grube, M Grudzinska, V Gruev, S Gruenewald, J Grygorczuk, V Guarino, S Gunji, G Gyuk, D Hadasch, R Hagiwara, J Hahn, N Hakansson, A Hallgren, N Hamer Heras, S Hara, MJ Hardcastle, J Harris, T Hassan, K Hatanaka, T Haubold, A Haupt, T Hayakawa, M Hayashida, R Heller, F Henault, G Henri, G Hermann, R Hermel, A Herrero, N Hidaka, J Hinton, D Hoffmann, W Hofmann, P Hofverberg, J Holder, D Horns, D Horville, J Houles, M Hrabovsky, D Hrupec, H Huan, B Huber, J-M Huet, G Hughes, TB Humensky, J Huovelin, A Ibarra, JM Illa, D Impiombato, S Incorvaia, S Inoue, Y Inoue, K Ioka, E Ismailova, C Jablonski, A Jacholkowska, M Jamrozy, M Janiak, P Jean, C Jeanney, JJ Jimenez, T Jogler, T Johnson, L Journet, C Juffroy, I Jung, P Kaaret, S Kabuki, M Kagaya, J Kakuwa, C Kalkuhl, R Kankanyan, A Karastergiou, K Kaercher, M Karczewski, S Karkar, A Kasperek, D Kastana, H Katagiri, J Kataoka, K Katarzynski, U Katz, N Kawanaka, B Kellner-Leidel, H Kelly, E Kendziorra, B Khelifi, DB Kieda, T Kifune, T Kihm, T Kishimoto, K Kitamoto, W Kluzniak, C Knapic, JW Knapp, J Knoedlseder, F Koeck, J Kocot, K 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Ziolkowski, V Zitelli, C Zurbach, P Zychowski, CTA Consortium

Infrared spectroscopy of nearby radio active elliptical galaxies

Astrophysical Journal, Supplement Series 203 (2012)

J Mould, T Reynolds, T Readhead, D Floyd, B Jannuzi, G Cotter, L Ferrarese, K Matthews, D Atlee, M Brown

In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ, and [Fe II]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. © 2012. The American Astronomical Society. All rights reserved..