Torus and active galactic nucleus properties of nearby Seyfert galaxies: Results from fitting infrared spectral energy distributions and spectroscopy
Astrophysical Journal 736:2 (2011)
Authors:
A Alonso-Herrero, C Ramos Almeida, R Mason, A Asensio Ramos, PF Roche, NA Levenson, M Elitzur, C Packham, JM Rodríguez Espinosa, S Young, T Díaz-Santos, AM Pérez-GarcíaAbstract:
We used the CLUMPY torus models and a Bayesian approach to fit the infrared spectral energy distributions and ground-based high angular resolution mid-infrared spectroscopy of 13 nearby Seyfert galaxies. This allowed us to put tight constraints on torus model parameters such as the viewing angle i, the radial thickness of the torus Y, the angular size of the cloud distribution σtorus, and the average number of clouds along radial equatorial rays N0. We found that the viewing angle i is not the only parameter controlling the classification of a galaxy into type 1 or type2. In principle, type 2s could be viewed at any viewing angle i as long as there is one cloud along the line of sight. A more relevant quantity for clumpy media is the probability for an active galactic nucleus (AGN) photon to escape unabsorbed. In our sample, type 1s have relatively high escape probabilities, Pesc ∼ 12%-44%, while type 2s, as expected, tend to have very low escape probabilities. Our fits also confirmed that the tori of Seyfert galaxies are compact with torus model radii in the range 1-6pc. The scaling of the models to the data also provided the AGN bolometric luminosities L bol(AGN), which were found to be in good agreement with estimates from the literature. When we combined our sample of Seyfert galaxies with a sample of PG quasars from the literature to span a range of Lbol(AGN) ∼ 1043-1047 erg s-1, we found plausible evidence of the receding torus. That is, there is a tendency for the torus geometrical covering factor to be lower (f2 ∼ 0.1-0.3) at high AGN luminosities than at low AGN luminosities (f2 ∼ 0.9-1 at ∼ 1043-1044 erg s-1). This is because at low AGN luminosities the tori appear to have wider angular sizes (larger σtorus) and more clouds along radial equatorial rays. We cannot, however, rule out the possibility that this is due to contamination by extended dust structures not associated with the dusty torus at low AGN luminosities, since most of these in our sample are hosted in highly inclined galaxies. © 2011. The American Astronomical Society. All rights reserved.Measurement of the W+W- Cross Section in s=7 TeV pp Collisions with ATLAS
Physical Review Letters American Physical Society (APS) 107:4 (2011) 041802
Authors:
G Aad, B Abbott, J Abdallah, AA Abdelalim, A Abdesselam, O Abdinov, B Abi, M Abolins, H Abramowicz, H Abreu, E Acerbi, BS Acharya, DL Adams, TN Addy, J Adelman, M Aderholz, S Adomeit, P Adragna, T Adye, S Aefsky, JA Aguilar-Saavedra, M Aharrouche, SP Ahlen, F Ahles, A Ahmad, M Ahsan, G Aielli, T Akdogan, TPA Åkesson, G Akimoto, AV Akimov, A Akiyama, MS Alam, MA Alam, S Albrand, M Aleksa, IN Aleksandrov, F Alessandria, C Alexa, G Alexander, G Alexandre, T Alexopoulos, M Alhroob, M Aliev, G Alimonti, J Alison, M Aliyev, PP Allport, SE Allwood-Spiers, J Almond, A Aloisio, R Alon, A Alonso, MG Alviggi, K Amako, P Amaral, C Amelung, VV Ammosov, A Amorim, G Amorós, N Amram, C Anastopoulos, T Andeen, CF Anders, KJ Anderson, A Andreazza, V Andrei, M-L Andrieux, XS Anduaga, A Angerami, F Anghinolfi, N Anjos, A Annovi, A Antonaki, M Antonelli, S Antonelli, A Antonov, J Antos, F Anulli, S Aoun, L Aperio Bella, R Apolle, G Arabidze, I Aracena, Y Arai, ATH Arce, JP Archambault, S Arfaoui, J-F Arguin, E Arik, M Arik, AJ Armbruster, O Arnaez, C Arnault, A Artamonov, G Artoni, D Arutinov, S Asai, R Asfandiyarov, S Ask, B Åsman, L Asquith, K Assamagan, A Astbury, A Astvatsatourov, G Atoian, B Aubert, B Auerbach, E Auge, K Augsten, M Aurousseau, N Austin, R Avramidou, D Axen, C Ay, G Azuelos, Y Azuma, MA Baak, G Baccaglioni, C Bacci, AM Bach, H Bachacou, K Bachas, G Bachy, M Backes, M Backhaus, E Badescu, P Bagnaia, S Bahinipati, Y Bai, DC Bailey, T Bain, JT Baines, OK Baker, MD Baker, S Baker, F Baltasar Dos Santos Pedrosa, E Banas, P Banerjee, Sw Banerjee, D Banfi, A Bangert, V Bansal, HS Bansil, L Barak, SP Baranov, A Barashkou, A Barbaro Galtieri, T Barber, EL Barberio, D Barberis, M Barbero, DY Bardin, T Barillari, M Barisonzi, T Barklow, N Barlow, BM Barnett, RM Barnett, A Baroncelli, AJ Barr, F Barreiro, J Barreiro Guimarães da Costa, P Barrillon, R Bartoldus, AE Barton, D Bartsch, V Bartsch, RL Bates, L Batkova, JR Batley, A Battaglia, M Battistin, G Battistoni, F Bauer, 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S Yamamoto, T Yamamura, J Yamaoka, T Yamazaki, Y Yamazaki, Z Yan, H Yang, UK Yang, Y Yang, Y Yang, Z Yang, S Yanush, W-M Yao, Y Yao, Y Yasu, GV Ybeles Smit, J Ye, S Ye, M Yilmaz, R Yoosoofmiya, K Yorita, R Yoshida, C Young, S Youssef, D Yu, J Yu, J Yu, L Yuan, A Yurkewicz, VG Zaets, R Zaidan, AM Zaitsev, Z Zajacova, Yo K Zalite, L Zanello, P Zarzhitsky, A Zaytsev, C Zeitnitz, M Zeller, A Zemla, C Zendler, AV Zenin, O Zenin, T Ženiš, Z Zenonos, S Zenz, D Zerwas, G Zevi della Porta, Z Zhan, D Zhang, H Zhang, J Zhang, X Zhang, Z Zhang, L Zhao, T Zhao, Z Zhao, A Zhemchugov, S Zheng, J Zhong, B Zhou, N Zhou, Y Zhou, CG Zhu, H Zhu, Y Zhu, X Zhuang, V Zhuravlov, D Zieminska, R Zimmermann, S Zimmermann, S Zimmermann, M Ziolkowski, R Zitoun, L Živković, VV Zmouchko, G Zobernig, A Zoccoli, Y Zolnierowski, A Zsenei, M zur Nedden, V Zutshi, L ZwalinskiOxford SWIFT IFS and multi-wavelength observations of the Eagle galaxy at z=0.77
ArXiv 1107.2931 (2011)
Authors:
Susan A Kassin, L Fogarty, T Goodsall, FJ Clarke, RWC Houghton, G Salter, N Thatte, M Tecza, Roger L Davies, Benjamin J Weiner, CNA Willmer, Samir Salim, Michael C Cooper, Jeffrey A Newman, Kevin Bundy, CJ Conselice, AM Koekemoer, Lihwai Lin, Leonidas A Moustakas, Tao WangAbstract:
The `Eagle' galaxy at a redshift of 0.77 is studied with the Oxford Short Wavelength Integral Field Spectrograph (SWIFT) and multi-wavelength data from the All-wavelength Extended Groth strip International Survey (AEGIS). It was chosen from AEGIS because of the bright and extended emission in its slit spectrum. Three dimensional kinematic maps of the Eagle reveal a gradient in velocity dispersion which spans 35-75 +/- 10 km/s and a rotation velocity of 25 +/- 5 km/s uncorrected for inclination. Hubble Space Telescope images suggest it is close to face-on. In comparison with galaxies from AEGIS at similar redshifts, the Eagle is extremely bright and blue in the rest-frame optical, highly star-forming, dominated by unobscured star-formation, and has a low metallicity for its size. This is consistent with its selection. The Eagle is likely undergoing a major merger and is caught in the early stage of a star-burst when it has not yet experienced metal enrichment or formed the mass of dust typically found in star-forming galaxies.Discovery of an active galactic nucleus driven molecular outflow in the local early-type galaxy NGC 1266
Astrophysical Journal 735:2 (2011)
Authors:
K Alatalo, L Blitz, LM Young, TA Davis, M Bureau, LA Lopez, M Cappellari, N Scott, KL Shapiro, AF Crocker, S Martín, M Bois, F Bournaud, RL Davies, PT De Zeeuw, PA Duc, E Emsellem, J Falcón-Barroso, S Khochfar, D Krajnović, H Kuntschner, PY Lablanche, RM McDermid, R Morganti, T Naab, T Oosterloo, M Sarzi, P Serra, A WeijmansAbstract:
We report the discovery of a powerful molecular wind from the nucleus of the non-interacting nearby S0 field galaxy NGC 1266. The single-dish CO profile exhibits emission to 400kms-1 and requires a nested Gaussian fit to be properly described. Interferometric observations reveal a massive, centrally concentrated molecular component with a mass of 1.1 × 109 M and a molecular outflow with a molecular mass of 2.4 × 107 M . The molecular gas close to the systemic velocity consists of a rotating, compact nucleus with a mass of about 4.1 × 108 M within a radius of 60pc. This compact molecular nucleus has a surface density of 2.7 × 104 M pc-2, more than two orders of magnitude larger than that of giant molecular clouds in the disk of the Milky Way, and it appears to sit on the Kennicutt-Schmidt relation despite its extreme kinematics and energetic activity. We interpret this nucleus as a disk that confines the outflowing wind. A mass outflow rate of 13 M yr-1 leads to a depletion timescale of ≲85 Myr. The star formation in NGC 1266 is insufficient to drive the outflow, and thus it is likely driven by the active galactic nucleus. The concentration of the majority of the molecular gas in the central 100pc requires an extraordinary loss of angular momentum, but no obvious companion or interacting galaxy is present to enable the transfer. NGC 1266 is the first known outflowing molecular system that does not show any evidence of a recent interaction. © 2011. The American Astronomical Society. All rights reserved..Search for contact interactions in dimuon events from pp collisions at s=7 TeV with the ATLAS detector
Physical Review D American Physical Society (APS) 84:1 (2011) 011101