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1. Measurement of the background in the CMS muon detector in $${p}{p}$$ pp -collisions at $$\sqrt{s} = 13$$ s = 13 $$\,\text {Te}\hspace{-.08em}\text {V}$$ Te V

Author

CMS Muon Group, M. Tytgat, A. Muhammad, G. De Lentdecker, J. Jaramillo, L. Moureaux, L. Pétré, Y. Yang, C. Rendón, G. Gokbulut, Y. Hong, A. Samalan, G. A. Alves, F. Marujo da Silva, E. Alves Coelho, M. Barroso Ferreira Filho, E. M. Da Costa, D. De Jesus Damiao, B. C. Ferreira, S. Fonseca De Souza, K. Mota Amarilo, H. Nogima, A. Santoro, M. Thiel, A. Aleksandrov, L. Dimitrov, R. Hadjiiska, P. Iaydjiev, M. Misheva, G. Mitev, L. Ratchev, G. Rashevski, M. Shopova, G. Sultanov, A. Dimitrov, L. Litov, B. Pavlov, P. Petkov, A. Petrov, E. Shumka, S. Keshri, S. Thakur, M. Chen, X. Dong, W. Gong, Q. Hou, C. Jiang, H. Kou, Z.-A. Liu, W. Luo, J. Song, L. Sun, N. Wang, Y. Wang, Z. Wang, C. Zhang, Y. Zhang, H. Zhang, J. Zhao, A. Agapitos, Y. Ban, A. Levin, Q. Li, S. J. Qian, D. Wang, K. Wang, Z. You, C. Avila, D. A. Barbosa Trujillo, A. Cabrera, C. A. Florez, J. Fraga, J. A. Reyes Vega, F. Ramirez, M. Rodriguez, J. D. Ruiz, N. Vanegas, H. Abdalla, A. A. Abdelalim, Y. Assran, A. Radi, I. Crotty, M. A. Mahmoud, L. Balleyguier, X. Chen, C. Combaret, G. Galbit, M. Gouzevitch, G. Grenier, I. B. Laktineh, A. Luciol, L. Mirabito, W. Tromeur, I. Bagaturia, I. Lomidze, O. Kemularia, Z. Tsamalaidze, U. Böttger, D. Eliseev, T. Hebbeker, K. Hoepfner, M. Merschmeyer, F. Ivone, S. Mukherjee, F. Nowotny, B. Philipps, H. Reithler, A. Sharma, F. Torres Da Silva De Araujo, S. Wiedenbeck, S. Zaleski, F. P. Zantis, M. Abbas, S. Mallows, G. Bencze, N. Beni, J. Molnar, Z. Szillasi, D. Teyssier, B. Ujvari, G. Zilizi, J. Babbar, S. Bansal, V. Bhatnagar, S. Chauhan, A. Kaur, H. Kaur, A. Kaur Sahota, S. Kumar, T. Sheokand, J. Singh, B. C. Choudhary, A. Kumar, M. Kumar Saini, M. Naimuddin, N. Majumdar, S. Mukhopadhyay, P. Rout, V. Amoozegar, B. Boghrati, M. Ebraimi, M. Mohammadi Najafabadi, E. Zareian, M. Abbrescia, R. Aly, M. Buonsante, A. Colaleo, N. De Filippis, D. Dell’Olio, G. De Robertis, W. Elmetenawee, N. Ferrara, M. Franco, G. Iaselli, N. Lacalamita, F. Licciulli, F. Loddo, M. Maggi, S. Martiradonna, S. Nuzzo, L. Longo, A. Pellecchia, G. Pugliese, R. Radogna, D. Ramos, A. Ranieri, F. M. Simone, A. Stamerra, D. Troiano, R. Venditti, P. Verwilligen, A. Zaza, G. Abbiendi, C. Baldanza, C. Battilana, A. Benvenuti, L. Borgonovi, V. Cafaro, F. R. Cavallo, A. Crupano, M. Cuffiani, G. M. Dallavalle, F. Fabbri, A. Fanfani, D. Fasanella, P. Giacomelli, V. Giordano, C. Guandalini, L. Guiducci, S. Lo Meo, L. Lunerti, S. Marcellini, G. Masetti, F. L. Navarria, G. Paggi, A. Perrotta, F. Primavera, A. M. Rossi, T. Rovelli, G. Torromeo, L. Benussi, S. Bianco, R. Campagnola, M. Caponero, S. Colafranceschi, S. Meola, L. Passamonti, D. Piccolo, D. Pierluigi, G. Raffone, A. Russo, G. Saviano, S. Buontempo, A. Cagnotta, F. Carnevali, F. Cassese, N. Cavallo, A. De Iorio, F. Fabozzi, A. O. M. Iorio, L. Lista, P. Paolucci, G. Passeggio, B. Rossi, L. Barcellan, M. Bellato, M. Benettoni, A. Bergnoli, A. Bragagnolo, R. Carlin, L. Castellani, P. Checchia, L. Ciano, A. Colombo, D. Corti, F. Gasparini, U. Gasparini, F. Gonella, A. Gozzelino, A. Griggio, G. Grosso, M. Gulmini, R. Isocrate, E. Lusiani, G. Maron, M. Margoni, A. T. Meneguzzo, M. Migliorini, L. Modenese, F. Montecassiano, M. Negrello, M. Passaseo, J. Pazzini, L. Ramina, M. Rampazzo, M. Rebeschini, P. Ronchese, R. Rossin, F. Simonetto, M. Toffano, N. Toniolo, A. Triossi, S. Ventura, M. Zanetti, P. G. Zatti, P. Zotto, A. Zucchetta, S. AbuZeid, C. Aimè, A. Braghieri, S. Calzaferri, D. Fiorina, S. Gigli, P. Montagna, C. Riccardi, P. Salvini, I. Vai, P. Vitulo, N. Amapane, G. Cotto, D. Dattola, P. De Remigis, B. Kiani, C. Mariotti, S. Maselli, M. Pelliccioni, F. Rotondo, A. Staiano, D. Trocino, G. Umoret, E. Asilar, T. J. Kim, J. A. Merlin, S. Choi, B. Hong, K. S. Lee, J. Goh, J. Choi, J. Kim, U. Yang, I. Yoon, W. Jang, J. Heo, D. Kang, Y. Kang, D. Kim, S. Kim, B. Ko, J. S. H. Lee, I. C. Park, I. J. Watson, S. Yang, Y. Jeong, Y. Lee, I. Yu, G. Alasfour, T. Beyrouthy, Y. Gharbia, Y. Maghrbi, M. Otkur, H. Castilla-Valdez, H. Crotte Ledesma, R. Lopez-Fernandez, A. Sánchez Hernández, M. Ramírez García, E. Vazquez, M. A. Shah, N. Zaganidis, I. Pedraza, C. Uribe Estrada, A. Ahmad, W. Ahmed, M. I. Asghar, H. R. Hoorani, S. Muhammad, A. Wajid, J. Alcaraz Maestre, A. Álvarez Fernández, Cristina F. Fernandez Bedoya, L. C. Blanco Ramos, E. Calvo, C. A. Carrillo Montoya, J. M. Cela Ruiz, M. Cepeda, M. Cerrada, N. Colino, S. Cuadrado Calzada, J. Cuchillo Ortega, B. De La Cruz, C. I. de Lara Rodríguez, D. Fernández Del Val, J. P. Fernández Ramos, M. C. Fouz, D. Francia Ferrero, J. García Romero, O. Gonzalez Lopez, S. Goy Lopez, M. I. Josa, J. León Holgado, O. Manzanilla Carretero, I. Martín Martín, J. J. Martínez Morales, E. Martín Viscasillas, D. Moran, Á. Navarro Tobar, R. Paz Herrera, J. C. Puras Sánchez, J. Puerta Pelayo, S. Pulido Ferrero, I. Redondo, D. D. Redondo Ferrero, V. Salto Parra, S. Sánchez Navas, J. Sastre, L. Urda Gómez, J. Vazquez Escobar, J. F. de Trocóniz, F. Frias Garcia-Lago, R. Reyes-Almanza, B. Alvarez Gonzalez, J. Cuevas, J. Fernandez Menendez, S. Folgueras, I. Gonzalez Caballero, P. Leguina López, E. Palencia Cortezon, C. Ramón Álvarez, J. Prado Pico, V. Rodríguez Bouza, A. Soto Rodríguez, A. Trapote, C. Vico Villalba, B. Kailasapathy, K. Malagalage, D. U. J. Sonnadara, D. D. C. Wickramarathna, W. G. D. Dharmaratna, K. Liyanage, N. Perera, N. Wickramage, P. Aspell, M. Bianco, D. Bozzato, S. Brachet, A. Conde Garcia, A. Dabrowski, R. De Oliveira, F. Fallavollita, P. Kicsiny, E. Hazen, S. May, A. Peck, K. Salyer, I. Suarez, S. Abbott, J. Bonilla, R. Breedon, H. Cai, P. T. Cox, R. Erbacher, O. Kukral, C. McLean, G. Mocellin, M. Mulhearn, B. Regnery, M. Tripathi, G. Waegel, Y. Yao, J. Carlson, R. Cousins, A. Dasgupta, A. Datta, J. Hauser, M. Ignatenko, M. A. Iqbal, C. Lo, D. Saltzberg, C. Schnaible, V. Valuev, R. Clare, M. Gordon, G. Hanson, N. Amin, J. Bradmiller-Feld, C. Campagnari, T. Danielson, A. Dishaw, A. Dorsett, B. Marsh, H. Mei, M. Oshiro, J. Richman, F. Setti, M. F. Sevilla, P. Siddireddy, S. Wang, C. Aruta, V. Barashko, V. Cherepanov, M. Dittrich, A. Korytov, E. Kuznetsova, A. Madorsky, G. Mitselmakher, A. Muthirakalayil Madhu, N. Rawal, N. Terentyev, J. Wang, B. Alsufyani, S. Butalla, T. Elkafrawy, M. Hohlmann, E. Yanes, J. Eysermans, E. Barberis, Y. Haddad, Y. Han, G. Madigan, D. M. Morse, V. Nguyen, D. Wood, S. Bhattacharya, J. Bueghly, Z. Chen, K. A. Hahn, Y. Liu, Y. Miao, D. G. Monk, M. H. Schmitt, A. Taliercio, M. Velasco, B. Bylsma, M. Carrigan, R. De Los Santos, L. S. Durkin, C. Hill, K. Banicz, J. Liu, M. Matveev, B. P. Padley, D. Aebi, M. Ahmad, T. Akhter, A. Bolshov, O. Bouhali, R. Eusebi, J. Gilmore, T. Huang, E. Juska, T. Kamon, H. Kim, M. Kizlov, S. Malhotra, R. Mueller, R. Rabadan, D. Rathjens, A. Safonov, P. E. Karchin, A. Aravind, K. Black, I. De Bruyn, P. Everaerts, C. Galloni, M. Herndon, A. Lanaro, R. Loveless, J. Madhusudanan Sreekala, S. Mondal, D. Teague, W. Vetens, A. Warden, I. Azhgirey, V. Borshch, L. Chtchipunov, A. Egorov, G. Gavrilov, V. Golovtcov, M. Ivanov, V. Ivantchenko, Y. Ivanov, V. Karjavine, A. Khodinov, V. Kim, I. A. Kurochkin, P. Levchenko, V. Murzin, S. Nasybulin, V. Oreshkin, V. Palichik, V. Perelygin, A. Riabchikova, D. Sosnov, V. Sulimov, L. Uvarov, S. Vavilov, and A. Vorobyev

Subjects
Astrophysics, QB460-466, Nuclear and particle physics. Atomic energy. Radioactivity, QC770-798
Abstract

Abstract The CMS detector, including its muon system, has been operating at the CERN LHC in increasingly challenging conditions for about 15 years. The muon detector was designed to provide excellent triggering and track reconstruction for muons produced in proton–proton collisons at an instantaneous luminosity ( $$\mathcal {L}$$ L ) of $$1 \times 10^{34}$$ 1 × 10 34 cm $$^{-2}$$ - 2 s $$^{-1}$$ - 1 . During the Run 2 data-taking period (2015–2018), the LHC achieved an instantaneous luminosity of twice its design value, resulting in larger background rates and making the efficient detection of muons more difficult. While some backgrounds result from natural radioactivity, cosmic rays, and interactions of the circulating protons with residual gas in the beam pipe, the dominant source of background hits in the muon system arises from proton–proton interactions themselves. Charged hadrons leaving the calorimeters produce energy deposits in the muon chambers. In addition, high-energy particles interacting in the hadron calorimeter and forward shielding elements generate thermal neutrons, which leak out of the calorimeter and shielding structures, filling the CMS cavern. We describe the method used to measure the background rates in the various muon subsystems. These rates, in conjunction with simulations, can be used to estimate the expected backgrounds in the High-Luminosity LHC. This machine will run for at least 10 years starting in 2029 reaching an instantaneous luminosity of $$\mathcal {L} = 5 \times \text {10}^\text {34}\,\text {cm}^\text {-2}\,\text {s}^\text {-1}$$ L = 5 × 10 34 cm -2 s -1 and increasing ultimately to $$\mathcal {L} = 7.5 \times \text {10}^\text {34}\,\text {cm}^\text {-2}\,\text {s}^\text {-1}$$ L = 7.5 × 10 34 cm -2 s -1 . These background estimates have been a key ingredient for the planning and design of the muon detector upgrade.

Published
2024
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2. The bright extragalactic ALMA redshift survey (BEARS) – II. Millimetre photometry of gravitational lens candidates

Author

G J Bendo, S A Urquhart, S Serjeant, T Bakx, M Hagimoto, P Cox, R Neri, M D Lehnert, H Dannerbauer, A Amvrosiadis, P Andreani, A J Baker, A Beelen, S Berta, E Borsato, V Buat, K M Butler, A Cooray, G De Zotti, L Dunne, S Dye, S Eales, A Enia, L Fan, R Gavazzi, J González-Nuevo, A I Harris, C N Herrera, D H Hughes, D Ismail, B M Jones, K Kohno, M Krips, G Lagache, L Marchetti, M Massardi, H Messias, M Negrello, A Omont, I Pérez-Fournon, D A Riechers, D Scott, M W L Smith, F Stanley, Y Tamura, P Temi, P van der Werf, A Verma, C Vlahakis, A Weiß, C Yang, and A J Young

Published
2022
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3. The bright extragalactic ALMA redshift survey (BEARS) I: redshifts of bright gravitationally lensed galaxies from the Herschel ATLAS

Author

S A Urquhart, G J Bendo, S Serjeant, T Bakx, M Hagimoto, P Cox, R Neri, M Lehnert, C Sedgwick, C Weiner, H Dannerbauer, A Amvrosiadis, P Andreani, A J Baker, A Beelen, S Berta, E Borsato, V Buat, K M Butler, A Cooray, G De Zotti, L Dunne, S Dye, S Eales, A Enia, L Fan, R Gavazzi, J González-Nuevo, A I Harris, C N Herrera, D Hughes, D Ismail, R Ivison, S Jin, B Jones, K Kohno, M Krips, G Lagache, L Marchetti, M Massardi, H Messias, M Negrello, A Omont, I Perez-Fournon, D A Riechers, D Scott, M W L Smith, F Stanley, Y Tamura, P Temi, C Vlahakis, A Weiß, P van der Werf, A Verma, C Yang, and A J Young

Published
2022
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5. Bright Extragalactic ALMA Redshift Survey (BEARS) III: Detailed study of emission lines from 71 Herschel targets

Author

M Hagimoto, T J L C Bakx, S Serjeant, G J Bendo, S A Urquhart, S Eales, K C Harrington, Y Tamura, H Umehata, S Berta, A R Cooray, P Cox, G De Zotti, M D Lehnert, D A Riechers, D Scott, P Temi, P P van der Werf, C Yang, A Amvrosiadis, P M Andreani, A J Baker, A Beelen, E Borsato, V Buat, K M Butler, H Dannerbauer, L Dunne, S Dye, A F M Enia, L Fan, R Gavazzi, J González-Nuevo, A I Harris, C N Herrera, D H Hughes, D Ismail, R J Ivison, B Jones, K Kohno, M Krips, G Lagache, L Marchetti, M Massardi, H Messias, M Negrello, R Neri, A Omont, I Perez-Fournon, C Sedgwick, M W L Smith, F Stanley, A Verma, C Vlahakis, B Ward, C Weiner, A Weiß, and A J Young

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We analyse the molecular and atomic emission lines of 71 bright Herschel-selected galaxies between redshifts 1.4 to 4.6 detected by the Atacama Large Millimetre/submillimetre Array. These lines include a total of 156 CO, [C I], and H2O emission lines. For 46 galaxies, we detect two transitions of CO lines, and for these galaxies we find gas properties similar to those of other dusty star-forming galaxy (DSFG) samples. A comparison to photo-dissociation models suggests that most of Herschel-selected galaxies have similar interstellar medium conditions as local infrared-luminous galaxies and high-redshift DSFGs, although with denser gas and more intense far-ultraviolet radiation fields than normal star-forming galaxies. The line luminosities agree with the luminosity scaling relations across five orders of magnitude, although the star-formation and gas surface density distributions (i.e., Schmidt-Kennicutt relation) suggest a different star-formation phase in our galaxies (and other DSFGs) compared to local and low-redshift gas-rich, normal star-forming systems. The gas-to-dust ratios of these galaxies are similar to Milky Way values, with no apparent redshift evolution. Four of 46 sources appear to have CO line ratios in excess of the expected maximum (thermalized) profile, suggesting a rare phase in the evolution of DSFGs. Finally, we create a deep stacked spectrum over a wide rest-frame frequency (220-890 GHz) that reveals faint transitions from HCN and CH, in line with previous stacking experiments., Comment: 30 pages, 17 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society Main Journal. Comments are warmly welcomed

Published
2023
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6. A High-Resolution Investigation of the Multi-Phase ISM in a Galaxy during the First Two Billion Years

Author

S Dye, S A Eales, H L Gomez, G C Jones, M W L Smith, E Borsato, A Moss, L Dunne, J Maresca, A Amvrosiadis, M Negrello, L Marchetti, E M Corsini, R J Ivison, G J Bendo, T Bakx, A Cooray, P Cox, H Dannerbauer, S Serjeant, D Riechers, P Temi, and C Vlahakis

Subjects
010308 nuclear & particles physics, FOS: Physical sciences, gravitational lensing: strong, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, 13. Climate action, galaxies: ISM, galaxies: kinematics and dynamics, galaxies: star formation, submillimetre: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010303 astronomy & astrophysics
Abstract

We have carried out the first spatially-resolved investigation of the multi-phase interstellar medium (ISM) at high redshift, using the z=4.24 strongly-lensed sub-millimetre galaxy H-ATLASJ142413.9+022303 (ID141). We present high-resolution (down to ~350 pc) ALMA observations in dust continuum emission and in the CO(7-6), H_2O (2_{1,1} - 2_{0,2}), CI(1-0) and CI(2-1) lines, the latter two allowing us to spatially resolve the cool phase of the ISM for the first time. Our modelling of the kinematics reveals that the system appears to be dominated by a rotationally-supported gas disk with evidence of a nearby perturber. We find that the CI(1-0) line has a very different distribution to the other lines, showing the existence of a reservoir of cool gas that might have been missed in studies of other galaxies. We have estimated the mass of the ISM using four different tracers, always obtaining an estimate in the range (3.2-3.8) x 10^{11} M_sol, significantly higher than our dynamical mass estimate of (0.8-1.3) x 10^{11} M_sol. We suggest that this conflict and other similar conflicts reported in the literature is because the gas-to-tracer ratios are ~4 times lower than the Galactic values used to calibrate the ISM in high-redshift galaxies. We demonstrate that this could result from a top-heavy initial mass function and strong chemical evolution. Using a variety of quantitative indicators, we show that, extreme though it is at z=4.24, ID141 will likely join the population of quiescent galaxies that appears in the Universe at z~3., This article has been accepted for publication in MNRAS, published by Oxford University Press on behalf of the Royal Astronomical Society. 24 pages

Published
2022

7. Herschel-ATLAS Data Release III: Near-infrared counterparts in the South Galactic Pole field -- Another 100,000 submillimetre galaxies

Author

B A Ward, S A Eales, E Pons, M W L Smith, R G McMahon, L Dunne, R J Ivison, S J Maddox, and M Negrello

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

In this paper we present the third data release (DR3) of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). We identify likely near-infrared counterparts to submillimetre sources in the South Galactic Pole (SGP) field using the VISTA VIKING survey. We search for the most probable counterparts within 15 arcsec of each Herschel source using a probability measure based on the ratio between the likelihood the true counterpart is found close to the submillimetre source and the likelihood that an unrelated object is found in the same location. For 110 374 (57.0$\%$) sources we find galaxies on the near-infrared images where the probability that the galaxy is associated to the source is greater than 0.8. We estimate the false identification rate to be 4.8$\%$, with a probability that the source has an associated counterpart on the VIKING images of 0.835$\pm$0.009. We investigate the effects of gravitational lensing and present 41 (0.14 deg$^{-2}$) candidate lensed systems with observed flux densities > 100 mJy at 500 $��$m. We include in the data release a probability that each source is gravitationally lensed and discover an additional 5 923 sources below 100 mJy that have a probability greater than 0.94 of being gravitationally lensed. We estimate that $\sim$ 400 - 1 000 sources have multiple true identifications in VIKING based on the similarity of redshift estimates for multiple counterparts close to a Herschel source. The data described in this paper can be found at the H-ATLAS website., 16 pages, 13 figures, accepted for publication in MNRAS

Published
2022

8. The far-infrared/radio correlation for a sample of strongly lensed dusty star-forming galaxies detected by Herschel

Author

M Giulietti, M Massardi, A Lapi, M Bonato, A F M Enia, M Negrello, Q D’Amato, M Behiri, and G De Zotti

Subjects
radio continuum: galaxies, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, gravitational lensing: strong, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, quasars: general, galaxies: star formation, submillimetre: galaxies, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics
Abstract

We investigate the radio-far infrared (FIR) correlation for a sample of $28$ bright high-redshift ($1 \lesssim z \lesssim 4$) star-forming galaxies selected in the FIR from the Herschel-ATLAS fields as candidates to be strongly gravitationally lensed. The radio information comes either from high sensitivity dedicated ATCA observations at $2.1$ GHz or from cross-matches with the FIRST survey at $1.4$ GHz. By taking advantage of source brightness possibly enhanced by lensing magnification, we identify a weak evolution with redshift out to $z\lesssim 4$ of the FIR-to-radio luminosity ratio $q_{\rm FIR}$. We also find that the $q_{\rm FIR}$ parameter as a function of the radio power $L_{1.4\,\rm GHz}$ displays a clear decreasing trend, similarly to what is observed for optically/radio selected lensed quasars found in literature, yet covering a complementary region in the $q_{\rm FIR}-L_{1.4\,\rm GHz}$ diagram. We interpret such a behavior in the framework of an in-situ galaxy formation scenario, as a result of the transition from an early dust-obscured star-forming phase (mainly pinpointed by our FIR selection) to a late radio-loud quasar phase (preferentially sampled by the optical/radio selection)., 12 pages, 6 figures. Minor changes and references updated to match the published version

Published
2022

9. Inferior Olive: All Ins and Outs

Author

S. Loyola, L. W. J. Bosman, J. R. De Gruijl, M. T. G. De Jeu, M. Negrello, T. M. Hoogland, and C. I. De Zeeuw

Published
2021

10. Simulating infrared spectro-photometric surveys with a SPRITZ

Author

L. Bisigello, C. Gruppioni, F. Calura, A. Feltre, F. Pozzi, C. Vignali, L. Barchiesi, G. Rodighiero, M. Negrello, F. J. Carrera, K. M. Dasyra, J. A. Fernández-Ontiveros, M. Giard, E. Hatziminaoglou, H. Kaneda, E. Lusso, M. Pereira-Santaella, P. G. Pérez González, C. Ricci, D. Schaerer, L. Spinoglio, L. Wang, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Bisigello L., Gruppioni C., Calura F., Feltre A., Pozzi F., Vignali C., Barchiesi L., Rodighiero G., Negrello M., Carrera F.J., Dasyra K.M., Fernandez-Ontiveros J.A., Giard M., Hatziminaoglou E., Kaneda H., Lusso E., Pereira-Santaella M., Perez Gonzalez P.G., Ricci C., Schaerer D., Spinoglio L., Wang L., Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astronomy, Agenzia Spaziale Italiana, Ministero dell'Istruzione, dell'Università e della Ricerca, Comunidad de Madrid, Agencia Estatal de Investigación (España), and Ministerio de Ciencia, Innovación y Universidades (España)

Subjects
galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, galaxies -techniques, infrared: galaxies, techniques: photometric, photometric, 0103 physical sciences, galaxies, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, infrared: galaxie, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, spectroscopic -techniques, Astrophysics - Astrophysics of Galaxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], evolution -galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, techniques: spectroscopic, active -galaxies, star formation -infrared
Abstract

arXiv:2111.11453v1, Mid- and far-infrared (IR) photometric and spectroscopic observations are fundamental to a full understanding of the dust-obscured Universe and the evolution of both star formation and black hole accretion in galaxies. In this work, using the specifications of the SPace Infrared telescope for Cosmology and Astrophysics (SPICA) as a baseline, we investigate the capability to study the dust-obscured Universe of mid- and far-IR photometry at 34 and 70 µm and low-resolution spectroscopy at 17−36 µm using the state-of-the-art SpectroPhotometric Realisations of Infrared-selected Targets at all-z (SPRITZ) simulation. This investigation is also compared to the expected performance of the Origins Space Telescope and the Galaxy Evolution Probe. The photometric view of the Universe of a SPICA-like mission could cover not only bright objects (e.g. LIR > 1012 L) up to z = 10, but also normal galaxies (LIR < 1011 L) up to z ∼ 4. At the same time, the spectroscopic observations of such mission could also allow us to estimate the redshifts and study the physical properties for thousands of star-forming galaxies and active galactic nuclei by observing the polycyclic aromatic hydrocarbons and a large set of IR nebular emission lines. In this way, a cold, 2.5-m size space telescope with spectro-photometric capability analogous to SPICA, could provide us with a complete three-dimensional (i.e. images and integrated spectra) view of the dust-obscured Universe and the physics governing galaxy evolution up to z ∼ 4., We acknowledge the whole SPICA Collaboration Team. LB, CG, LS and JAFO acknowledge financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. AF and FC acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. MPS acknowledges support from the Comunidad de Madrid through the Atracción de Talento Investigador Grant 2018-T1/TIC11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). FJC acknowledges financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia Maria de Maeztu, ref. MDM-2017-0765.

Published
2021

11. Simulating the infrared sky with a S PRITZ

Author

Anna Feltre, L. Barchiesi, C. Vignali, L. Bisigello, G. Rodighiero, Francesco Calura, Carlotta Gruppioni, Francesca Pozzi, M. Negrello, Bisigello L., Gruppioni C., Feltre A., Calura F., Pozzi F., Vignali C., Barchiesi L., Rodighiero G., and Negrello M.

Subjects
Infrared: galaxie, Infrared, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxies: luminosity function, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Luminous infrared galaxy, Physics, Galaxy: evolution, 010308 nuclear & particles physics, Galaxies: statistic, Computer Science::Information Retrieval, Astronomy and Astrophysics, Galaxies: active, Galaxies: photometry, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Mass function, Astrophysics::Earth and Planetary Astrophysics
Abstract

Current hydrodynamical and semi-empirical simulations of galaxy formation and evolution have difficulties in reproducing the number densities of IR-detected galaxies. Therefore, a versatile, phenomenological new simulation tool is necessary to reproduce current and predict future observations at IR wavelengths. In this work we generate simulated catalogues starting from the Herschel infrared luminosity functions of different galaxy populations, in order to consider in a consistent way different populations of galaxies and active galactic nuclei. We associated a spectral energy distribution and physical properties, such as stellar mass, star-formation-rate and AGN contribution, to each simulated galaxy using a broad set of empirical relations. We compare the resulting simulated galaxies, extracted up to z$=$10, with a broad set of observational relations. The Spectro-Photometric Realisations of Infrared-selected Targets at all-z (SPRITZ) simulation will allow us to obtain in a fully consistent way simulated observations for a broad set of current and future facilities with photometric capabilities as well as low-resolution IR spectroscopy, like the James Webb Space Telescope (JWST) or the Origin Space Telescope (OST). The derived simulated catalogue contains galaxies and active galactic nuclei that by construction reproduce the observed IR galaxy number density, but it is also in agreement with the observed number counts from UV to far-IR wavelengths, the observed stellar mass function, the star-formation-rate vs. stellar mass plane and the luminosity function from the radio to the X-ray. The proposed simulation is therefore ideal to make predictions for current and future facilities, in particular, but not limited to, those operating at IR wavelengths. The SPRITZ simulation will be publicly available., Accepted for publication in A&A, 32 pages, 30 figures

Published
2021

12. Erratum: The Herschel Bright Sources (HerBS): sample definition and SCUBA-2 observations

Author

C Yang, P van der Werf, J L Wardlow, I Oteo, A Omont, M J Michałowski, L Marchetti, S Maddox, R J Ivison, C Furlanetto, S Dye, L Dunne, G De Zotti, H Dannerbauer, D L Clements, N Bourne, M Baes, W S Holland, E Valiante, M W L Smith, M Negrello, S A Eales, and Tom J L C Bakx

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

This is a correction to: Monthly Notices of the Royal Astronomical Society, Volume 473, Issue 2, January 2018, Pages 1751–1773, https://doi.org/10.1093/mnras/stx2267

Published
2020

13. Active Galactic Nuclei in Dusty Starbursts at z = 2: Feedback Still to Kick in

Author

Alvio Renzini, Andrea Lapi, W. Rujopakarn, G. Rodighiero, A. Enia, John D. Silverman, Ivano Baronchelli, Paolo Cassata, I. Delvecchio, Michele Perna, Alfio Puglisi, Alberto Franceschini, Georgios E. Magdis, L. Morselli, M. Negrello, E. Iani, Chiara Mancini, L. Rodríguez-Muñoz, E. Daddi, R. Carraro, and Carlotta Gruppioni

Subjects
active [Galaxies], 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Physics::Optics, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, infrared: galaxies, high-redshift [Galaxies], galaxies [Infrared], Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, Physics::Plasma Physics, 0103 physical sciences, galaxies: formation, galaxies: evolution, galaxies: Starburst, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, Quasar, Torus, evolution [Galaxies], formation [Galaxies], Galaxy, starburst [Galaxies], 13. Climate action, Space and Planetary Science, galaxies: evolution, galaxies: formation
Abstract

We investigate a sample of 152 dusty sources at 1.5 z Herschel-selected, having stellar masses M * > 1010 M ⊙ and SFR (~100–1000 M ⊙ yr−1) elevated (>4×) above the star-forming "main sequence," classifying them as starbursts (SBs). Through a multiwavelength fitting approach (including a dusty torus component), we divided the sample into active SBs (dominated by an active galactic nucleus (AGN) emission, SBs-AGN, ~23% of the sample) and purely star-forming SBs (SBs-SFR). We visually inspected their Hubble Space Telescope/ultraviolet (UV) rest frame maps: SBs-SFR are generally irregular and composite systems; ~50% of SBs-AGN are instead dominated by regular compact morphologies. We then found archival Atacama Large Millimeter/submillimeter Array continuum counterparts for 33 galaxies (12 SBs-AGN and 21 SBs-SFR). For these sources we computed dust masses, and, with standard assumptions, we also guessed total molecular gas masses. SBs turn into gas-rich systems (f gas = M gas/(M gas + M *) 20%–70%), and the gas fractions of the two SB classes are very similar (f gas = 43% ± 4% and f gas = 42% ± 2%). Our results show that SBs are consistent with a mixture of: (1) highly star-forming merging systems (dominating the SBs-SFR) and (2) primordial galaxies, rapidly growing their M * together with their black hole (mainly the more compact SBs-AGN). Feedback effects have not yet reduced their f gas. Indeed, SBs at z = 2, with relatively low bolometric AGN luminosities in the range 1044 L bol(AGN) 46 erg s−1 (compared to bright optical and X-ray quasars), are still relatively far from the epoch when the AGN feedback will quench the SFR in the host and will substantially depress the gas fractions.

Published
2019

14. CO, H 2 O, H 2 O + line and dust emission in a z = 3.63 strongly lensed starburst merger at sub-kiloparsec scales

Author

Asantha Cooray, Eduardo González-Alfonso, C. Yang, Yang Gao, Alain Omont, R. Gavazzi, R. Neri, Hooshang Nayyeri, Michał J. Michałowski, Simon Dye, P. van der Werf, Hai Fu, Dominik A. Riechers, Pierre Cox, Rob Ivison, Steve Eales, A. Beelen, Ismael Perez-Fournon, L. Barcos-Muñoz, J. Nightingale, M. D. Lehnert, M. Negrello, A. M. Swinbank, Ian Smail, E. Ibar, Guangzhou Marine Geological Survey, Ministry of Land and Resources (MLR), Physics Department [Santa Barbara], University of California [Santa Barbara] (UCSB), University of California-University of California, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Royal Observatory Edinburgh (ROE), University of Edinburgh, California Institute of Technology (CALTECH), School of Physics and Astronomy [Cardiff], Cardiff University, Universidad de Alcalá - University of Alcalá (UAH), AUTRES, Instituto de Astrofisica de Canarias (IAC), Department of Astronomy [Ithaca], Cornell University [New York], Institute for Computational Cosmology (ICC), Durham University, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and Cornell University

Subjects
Einstein ring, Infrared, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Submillimeter Array, symbols.namesake, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, Effective radius, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Interstellar medium, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), symbols, Astrophysics::Earth and Planetary Astrophysics
Abstract

Using ALMA, we report high angular-resolution observations of the redshift z=3.63 galaxy, G09v1.97, one of the most luminous strongly lensed galaxies discovered by the H-ATLAS survey. We present 0"2-0"4 resolution images of the rest-frame 188 and 419$\mu$m dust continuum and the CO(6-5), H2O(211-202) and J=2 H2O+ line emission. We also report the detection of H$_2^{18}$O in this source. The dust continuum and molecular gas emission are resolved into a nearly complete ~1"5 diameter Einstein ring plus a weaker image in the center, which is caused by a special dual deflector lensing configuration. The observed line profiles of the CO, H2O and H2O+ lines are strikingly similar. In the source plane, we reconstruct the dust continuum images and the spectral cubes of the line emission at sub-kpc scales. The reconstructed dust emission in the source plane is dominated by a compact disk with an effective radius of 0.7kpc plus an overlapping extended disk with a radius twice as large. While the average magnification for the dust continuum is $\mu$~10-11, the magnification of the line emission varies 5 to 22 across different velocity components. The emission lines have similar spatial and kinematic distributions. The molecular gas and dust content reveal that G09v1.97 is a gas-rich major merger in its pre-coalescence phase. Both of the merging companions are intrinsically ULIRGs with LIR reaching $\gtrsim 4\times10^{12}L_\odot$, and the total LIR of G09v1.97 is $1.4\times10^{13}L_\odot$. The approaching southern galaxy shows no obvious kinematic structure with a semi-major half-light radius a_s=0.4kpc, while the receding galaxy resembles an a_s=1.2kpc rotating disk. The two galaxies are separated by a projected distance of 1.3kpc, bridged by weak line emission that is co-spatially located with the cold-dust-emission peak, suggesting a large amount of cold ISM in the interacting region. (abridged), Comment: 19 pages, 12 figures, and 4-page appendix, A&A in press. Minor changes to match language editing

Published
2019
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15. Exploring cosmic origins with CORE: Inflation

Author

F. Finelli, M. Bucher, A. Achúcarro, M. Ballardini, N. Bartolo, D. Baumann, S. Clesse, J. Errard, W. Handley, M. Hindmarsh, K. Kiiveri, M. Kunz, A. Lasenby, M. Liguori, D. Paoletti, C. Ringeval, J. Väliviita, B. van Tent, V. Vennin, P. Ade, R. Allison, F. Arroja, M. Ashdown, A.J. Banday, R. Banerji, J.G. Bartlett, S. Basak, P. de Bernardis, M. Bersanelli, A. Bonaldi, J. Borril, F.R. Bouchet, F. Boulanger, T. Brinckmann, C. Burigana, A. Buzzelli, Z.-Y. Cai, M. Calvo, C.S. Carvalho, G. Castellano, A. Challinor, J. Chluba, I. Colantoni, A. Coppolecchia, M. Crook, G. D'Alessandro, G. D'Amico, J. Delabrouille, V. Desjacques, G. De Zotti, J.M. Diego, E. Di Valentino, S. Feeney, J.R. Fergusson, R. Fernandez-Cobos, S. Ferraro, F. Forastieri, S. Galli, J. García-Bellido, G. de Gasperis, R.T. Génova-Santos, M. Gerbino, J. González-Nuevo, S. Grandis, J. Greenslade, S. Hagstotz, S. Hanany, D.K. Hazra, C. Hernández-Monteagudo, C. Hervias-Caimapo, M. Hills, E. Hivon, B. Hu, T. Kisner, T. Kitching, E.D. Kovetz, H. Kurki-Suonio, L. Lamagna, M. Lattanzi, J. Lesgourgues, A. Lewis, V. Lindholm, J. Lizarraga, M. López-Caniego, G. Luzzi, B. Maffei, N. Mandolesi, E. Martínez-González, C.J.A.P. Martins, S. Masi, D. McCarthy, S. Matarrese, A. Melchiorri, J.-B. Melin, D. Molinari, A. Monfardini, P. Natoli, M. Negrello, A. Notari, F. Oppizzi, A. Paiella, E. Pajer, G. Patanchon, S.P. Patil, M. Piat, G. Pisano, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, A. Ravenni, M. Remazeilles, A. Renzi, D. Roest, M. Roman, J.A. Rubiño-Martin, L. Salvati, A.A. Starobinsky, A. Tartari, G. Tasinato, M. Tomasi, J. Torrado, N. Trappe, T. Trombetti, M. Tucci, C. Tucker, J. Urrestilla, R. van de Weygaert, P. Vielva, N. Vittorio, K. Young, M. Zannoni, ITA, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut Lagrange de Paris, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), CORE, Department of Physics, Helsinki Institute of Physics, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Sorbonne Universités, Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Finelli, F, Bucher, M, Achúcarro, A, Ballardini, M, Bartolo, N, Baumann, D, Clesse, S, Errard, J, Handley, W, Hindmarsh, M, Kiiveri, K, Kunz, M, Lasenby, A, Liguori, M, Paoletti, D, Ringeval, C, Väliviita, J, Tent, B, Vennin, V, Ade, P, Allison, R, Arroja, F, Ashdown, M, Banday, A, Banerji, R, Bartlett, J, Basak, S, de Bernardis, P, Bersanelli, M, Bonaldi, A, Borril, J, Bouchet, F, Boulanger, F, Brinckmann, T, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Challinor, A, Chluba, J, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, D'Amico, G, Delabrouille, J, Desjacques, V, Zotti, G, Diego, J, Valentino, E, Feeney, S, Fergusson, J, Fernandez-Cobos, R, Ferraro, S, Forastieri, F, Galli, S, García-Bellido, J, de Gasperis, G, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Hazra, D, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hivon, E, Hu, B, Kisner, T, Kitching, T, Kovetz, E, Kurki-Suonio, H, Lamagna, L, Lattanzi, M, Lesgourgues, J, Lewis, A, Lindholm, V, Lizarraga, J, López-Caniego, M, Luzzi, G, Maffei, B, Mandolesi, N, Martínez-González, E, Martins, C, Masi, S, Mccarthy, D, Matarrese, S, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Oppizzi, F, Paiella, A, Pajer, E, Patanchon, G, Patil, S, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Ravenni, A, Remazeilles, M, Renzi, A, Roest, D, Roman, M, Rubiño-Martin, J, Salvati, L, Starobinsky, A, Tartari, A, Tasinato, G, Tomasi, M, Torrado, J, Trappe, N, Trombetti, T, Tucci, M, Tucker, C, Urrestilla, J, de Weygaert, R, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Finelli F., Bucher M., Achucarro A., Ballardini M., Bartolo N., Baumann D., Clesse S., Errard J., Handley W., Hindmarsh M., Kiiveri K., Kunz M., Lasenby A., Liguori M., Paoletti D., Ringeval C., Valiviita J., Tent B.V., Vennin V., Ade P., Allison R., Arroja F., Ashdown M., Banday A.J., Banerji R., Bartlett J.G., Basak S., De Bernardis P., Bersanelli M., Bonaldi A., Borril J., Bouchet F.R., Boulanger F., Brinckmann T., Burigana C., Buzzelli A., Cai Z.-Y., Calvo M., Carvalho C.S., Castellano G., Challinor A., Chluba J., Colantoni I., Coppolecchia A., Crook M., D'Alessandro G., D'Amico G., Delabrouille J., Desjacques V., Zotti G.D., Diego J.M., Valentino E.D., Feeney S., Fergusson J.R., Fernandez-Cobos R., Ferraro S., Forastieri F., Galli S., Garcia-Bellido J., De Gasperis G., Genova-Santos R.T., Gerbino M., Gonzalez-Nuevo J., Grandis S., Greenslade J., Hagstotz S., Hanany S., Hazra D.K., Hernandez-Monteagudo C., Hervias-Caimapo C., Hills M., Hivon E., Hu B., Kisner T., Kitching T., Kovetz E.D., Kurki-Suonio H., Lamagna L., Lattanzi M., Lesgourgues J., Lewis A., Lindholm V., Lizarraga J., Lopez-Caniego M., Luzzi G., Maffei B., Mandolesi N., Martinez-Gonzalez E., Martins C.J.A.P., Masi S., McCarthy D., Matarrese S., Melchiorri A., Melin J.-B., Molinari D., Monfardini A., Natoli P., Negrello M., Notari A., Oppizzi F., Paiella A., Pajer E., Patanchon G., Patil S.P., Piat M., Pisano G., Polastri L., Polenta G., Pollo A., Poulin V., Quartin M., Ravenni A., Remazeilles M., Renzi A., Roest D., Roman M., Rubino-Martin J.A., Salvati L., Starobinsky A.A., Tartari A., Tasinato G., Tomasi M., Torrado J., Trappe N., Trombetti T., Tucci M., Tucker C., Urrestilla J., De Weygaert R.V., Vielva P., Vittorio N., Young K., Zannoni M., String Theory (ITFA, IoP, FNWI), High-Energy Frontier, Astronomy, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), and Hélium : du fondamental aux applications (NEEL - HELFA)

Subjects
cosmological model, reheating, Cosmic microwave background, cosmic background radiation: polarization, SPECTRAL DISTORTIONS, astro-ph.CO, Astrophysics, cosmic background radiation, 7. Clean energy, 01 natural sciences, GRAVITATIONAL-WAVES, law.invention, law, 010303 astronomy & astrophysics, CMBR theory, ination, Astronomy and Astrophysics, CMBR theory, inflation, QC, QB, Physics, COSMIC cancer database, ST/J005673/1, ST/H008586/1, inflation: model, MICROWAVE BACKGROUND ANISOTROPY, Core inflation, Astrophysics - Cosmology and Nongalactic Astrophysics, Big Bang, scale: grand unified theory, Astrophysics and Astronomy, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), STANDARD MODEL, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, isocurvature: perturbation, frequency: high, PRIMORDIAL NON-GAUSSIANITY, NO, Telescope, power spectrum: primordial, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, LARGE-SCALE STRUCTURE, 0103 physical sciences, inflation, cosmic string, STFC, MODEL SELECTION, Inflation (cosmology), non-Gaussianity: primordial, ST/K00333X/1, ISOCURVATURE PERTURBATIONS, 010308 nuclear & particles physics, string tension, big bang, inflation: slow-roll approximation, RCUK, Spectral density, 115 Astronomy, Space science, cosmic background radiation: temperature, Cosmic string, detector: sensitivity, angular resolution, 13. Climate action, PRE-BIG-BANG, BAYESIAN-INFERENCE, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic background radiation: anisotropy
Abstract

We forecast the scientific capabilities to improve our understanding of cosmic inflation of CORE, a proposed CMB space satellite submitted in response to the ESA fifth call for a medium-size mission opportunity. The CORE satellite will map the CMB anisotropies in temperature and polarization in 19 frequency channels spanning the range 60-600 GHz. CORE will have an aggregate noise sensitivity of $1.7 ��$K$\cdot \,$arcmin and an angular resolution of 5' at 200 GHz. We explore the impact of telescope size and noise sensitivity on the inflation science return by making forecasts for several instrumental configurations. This study assumes that the lower and higher frequency channels suffice to remove foreground contaminations and complements other related studies of component separation and systematic effects, which will be reported in other papers of the series "Exploring Cosmic Origins with CORE." We forecast the capability to determine key inflationary parameters, to lower the detection limit for the tensor-to-scalar ratio down to the $10^{-3}$ level, to chart the landscape of single field slow-roll inflationary models, to constrain the epoch of reheating, thus connecting inflation to the standard radiation-matter dominated Big Bang era, to reconstruct the primordial power spectrum, to constrain the contribution from isocurvature perturbations to the $10^{-3}$ level, to improve constraints on the cosmic string tension to a level below the presumptive GUT scale, and to improve the current measurements of primordial non-Gaussianities down to the $f_{NL}^{\rm local} < 1$ level. For all the models explored, CORE alone will improve significantly on the present constraints on the physics of inflation. Its capabilities will be further enhanced by combining with complementary future cosmological observations., Latex 107 pages, revised with updated author list and minor modifications

Published
2018

16. Exploring cosmic origins with CORE: Gravitational lensing of the CMB

Author

A. Challinor, R. Allison, J. Carron, J. Errard, S. Feeney, T. Kitching, J. Lesgourgues, A. Lewis, Í. Zubeldía, A. Achucarro, P. Ade, M. Ashdown, M. Ballardini, A.J. Banday, R. Banerji, J. Bartlett, N. Bartolo, S. Basak, D. Baumann, M. Bersanelli, A. Bonaldi, M. Bonato, J. Borrill, F. Bouchet, F. Boulanger, T. Brinckmann, M. Bucher, C. Burigana, A. Buzzelli, Z.-Y. Cai, M. Calvo, C.-S. Carvalho, G. Castellano, J. Chluba, S. Clesse, I. Colantoni, A. Coppolecchia, M. Crook, G. d'Alessandro, P. de Bernardis, G. de Gasperis, G. De Zotti, J. Delabrouille, E. Di Valentino, J.-M. Diego, R. Fernandez-Cobos, S. Ferraro, F. Finelli, F. Forastieri, S. Galli, R. Genova-Santos, M. Gerbino, J. González-Nuevo, S. Grandis, J. Greenslade, S. Hagstotz, S. Hanany, W. Handley, C. Hernandez-Monteagudo, C. Hervías-Caimapo, M. Hills, E. Hivon, K. Kiiveri, T. Kisner, M. Kunz, H. Kurki-Suonio, L. Lamagna, A. Lasenby, M. Lattanzi, M. Liguori, V. Lindholm, M. López-Caniego, G. Luzzi, B. Maffei, E. Martinez-González, C.J.A.P. Martins, S. Masi, S. Matarrese, D. McCarthy, A. Melchiorri, J.-B. Melin, D. Molinari, A. Monfardini, P. Natoli, M. Negrello, A. Notari, A. Paiella, D. Paoletti, G. Patanchon, M. Piat, G. Pisano, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, M. Remazeilles, M. Roman, J.-A. Rubino-Martin, L. Salvati, A. Tartari, M. Tomasi, D. Tramonte, N. Trappe, T. Trombetti, C. Tucker, J. Valiviita, R. Van de Weijgaert, B. van Tent, V. Vennin, P. Vielva, N. Vittorio, K. Young, M. Zannoni, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Universités, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), CORE, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Challinor, A, Allison, R, Carron, J, Errard, J, Feeney, S, Kitching, T, Lesgourgues, J, Lewis, A, Zubeldía, Í, Achucarro, A, Ade, P, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Baumann, D, Bersanelli, M, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Chluba, J, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Zotti, G, Delabrouille, J, Valentino, E, Diego, J, Fernandez-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Genova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Handley, W, Hernandez-Monteagudo, C, Hervías-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Liguori, M, Lindholm, V, López-Caniego, M, Luzzi, G, Maffei, B, Martinez-González, E, Martins, C, Masi, S, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Paiella, A, Paoletti, D, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rubino-Martin, J, Salvati, L, Tartari, A, Tomasi, M, Tramonte, D, Trappe, N, Trombetti, T, Tucker, C, Valiviita, J, de Weijgaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Department of Physics, String Theory (ITFA, IoP, FNWI), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), and Hélium : du fondamental aux applications (NEEL - HELFA)

Subjects
deflection, Cosmic microwave background, cosmic background radiation: polarization, astro-ph.CO, Astrophysics, ST/N000927/1, ST/L000652/1, 7. Clean energy, 01 natural sciences, CMBR polarisation, gravitational lensing, inflation, neutrino masses from cosmology, ART. NO. 023003, estimator, neutrino: mass, 010303 astronomy & astrophysics, Physics, FLUCTUATIONS, GRAVITY-WAVES, Amplitude, non-Gaussianity, galaxy: cluster, Halo, gravitational radiation: power spectrum, Neutrino, CMBR polarization, gravitational lensing, ination, neutrino masses from cosmology, Astronomy and Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, CMBR polarisation, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), B-mode: lens, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, NO, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ddc:530, RECONSTRUCTION, inflation, Galaxy cluster, STFC, halo: mass, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, RCUK, 115 Astronomy, Space science, redshift, calibration, Redshift, Gravitational lens, CROSS-CORRELATION, RADIATION, neutrino: oscillation, GALAXY CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], MICROWAVE BACKGROUND POLARIZATION, MATTER
Abstract

Lensing of the CMB is now a well-developed probe of large-scale clustering over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission can produce a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that it will enable. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous BAO measurements, three times smaller than the minimum total mass allowed by neutrino oscillations. In the search for B-mode polarization from primordial gravitational waves with CORE, lens-induced B-modes will dominate over instrument noise, limiting constraints on the gravitational wave power spectrum amplitude. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60%. This improves to 70% by combining lensing and CIB measurements from CORE, reducing the error on the gravitational wave amplitude by 2.5 compared to no delensing (in the null hypothesis). Lensing measurements from CORE will allow calibration of the halo masses of the 40000 galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. CORE can accurately remove Galactic emission from CMB maps with its 19 frequency channels. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE. [abridged], 44 pages, 12 figures

Published
2018

17. Candidate high-z proto-clusters among the Planck compact sources, as revealed by Herschel-SPIRE

Author

P. van der Werf, Douglas Scott, D. L. Harrison, T. Cheng, Ivan Valtchanov, Maarten Baes, G. de Zotti, M. N. Bremer, Mark Birkinshaw, Stephen Anthony Eales, J. Greenslade, Lingyu Wang, Asantha Cooray, Elisabetta Valiante, Simon Dye, Loretta Dunne, Michał J. Michałowski, Helmut Dannerbauer, M. Negrello, Duncan Farrah, David L. Clements, Ivan Oteo, Astronomy, Science and Technology Facilities Council (STFC), Imperial College Trust, and Science and Technology Facilities Council

Subjects
Hubble Deep Field, DEEP FIELD, galaxies: starburst, Astrophysics, 01 natural sciences, OVERDENSITY, clusters: general [galaxies], NUMBER COUNTS, 010303 astronomy & astrophysics, POPULATION, QB, Physics, education.field_of_study, Line-of-sight, SPECTROSCOPY, starburst [galaxies], H-ATLAS, CLUSTER CATALOG, SCIENCE, galaxies: clusters: general, Physical Sciences, symbols, Cirrus, galaxies: evolution, submillimetre: galaxies, Population, FOS: Physical sciences, Astronomy & Astrophysics, infrared: galaxies, symbols.namesake, galaxies [submillimetre], 0103 physical sciences, STAR-FORMING GALAXIES, Planck, Spectroscopy, education, evolution [galaxies], Science & Technology, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, REDSHIFT DUSTY GALAXIES, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, 0201 Astronomical And Space Sciences, Spire, Physics and Astronomy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOLLOW-UP
Abstract

By determining the nature of all the Planck compact sources within 808.4 deg^2 of large Herschel surveys, we have identified 27 candidate proto-clusters of dusty star forming galaxies (DSFGs) that are at least 3�� overdense in either 250, 350 or 500 $��$mm sources. We find roughly half of all the Planck compact sources are resolved by Herschel into multiple discrete objects, with the other half remaining unresolved by Herschel. We find a significant difference between versions of the Planck catalogues, with earlier releases hosting a larger fraction of candidate proto-clusters and Galactic Cirrus than later releases, which we ascribe to a difference in the filters used in the creation of the three catalogues. We find a surface density of DSFG candidate proto-clusters of (3.3 $\pm$ 0.7) x 10^(-2) sources deg^(-2), in good agreement with previous similar studies. We find that a Planck colour selection of S_{857}/S_{545} < 2 works well to select candidate proto-clusters, but can miss proto-clusters at z < 2. The Herschel colours of individual candidate proto-cluster members indicate our candidate proto-clusters all likely all lie at z > 1. Our candidate proto-clusters are a factor of 5 times brighter at 353 GHz than expected from simulations, even in the most conservative estimates. Further observations are needed to confirm whether these candidate proto-clusters are physical clusters, multiple proto-clusters along the line of sight, or chance alignments of unassociated sources., Resubmitted to MNRAS after request for minor revision

Published
2017
Full Text
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19. The major upgrade of the MAGIC telescopes, Part I: The hardware improvements and the commissioning of the system

Author

R. Zanin, Adrian Biland, I. Lozano, J. Rico, Masahiro Teshima, W. Idec, Takashi Saito, J. Krause, B. De Lotto, Nikola Godinovic, Benito Marcote, Stefano Ansoldi, I. Snidaric, David Fink, K. Mallot, R. J. García López, D. Corti, Alessandro Carosi, Mosè Mariotti, A.-K. Overkemping, J. M. Illa, Riccardo Paoletti, Massimo Persic, Gianluca Giavitto, A. González Muñoz, Reiko Orito, P. Temnikov, M. Palatiello, J. Becerra González, Marcel Strzys, Dario Hrupec, M. Bitossi, Ruben Lopez-Coto, Jose Luis Lemus, D. Nakajima, Elina Lindfors, E. Lorenz, Abelardo Moralejo, Saverio Lombardi, A. Treves, Vitaly Neustroev, M. Makariev, Thomas Bretz, Daniel Mazin, Jose Miguel Miranda, M. A. Lopez, S. Rügamer, Juan Abel Barrio, S. Schmidl, T. Steinbring, Francesco Dazzi, J. M. Paredes, Antonio Stamerra, C. Delgado Mendez, G. Maneva, Stefano Covino, B. Biasuzzi, A. Dettlaff, M. Hayashida, D. Hildebrand, Francesco Longo, G. De Caneva, D. Fidalgo, Daniela Dorner, Jose Luis Contreras, Wolfgang Rhode, M. I. Martínez, Marc Ribó, S. Bonnefoy, K. Saito, Natalia Lewandowska, Patrick Vogler, E. Colombo, M. Gaug, Juan Cortina, D. Tescaro, Roberto Cecchi, P. Bangale, H. Wetteskind, A. La Barbera, A. Deangelis, J. Herrera, Hidetoshi Kubo, Sabrina Einecke, S. R. Gozzini, Luis Ángel Tejedor, M. V. Fonseca, Hanna Kellermann, Koji Noda, Louis Antonelli, G. Bonnoli, J. Rodriguez Garcia, Elisa Bernardini, X. Paredes-Fortuny, J. Hose, U. Menzel, K. Kodani, J. Storz, Yusuke Konno, Christian Fruck, A. Sillanpää, D. Elsaesser, L. O. Takalo, F. Borracci, W. Haberer, H. Takami, Oscar Blanch, K. Frantzen, P. G. Prada Moroni, Diego F. Torres, W. Bednarek, Fabrizio Tavecchio, V. Kadenius, S. Paiano, Ll. Font, D. Garrido Terrats, A. Lorca, Karl Mannheim, O. Tibolla, Alicia López-Oramas, T. Schweizer, Felix Spanier, R. Mirzoyan, P. Munar-Adrover, D. Eisenacher, V. Scalzotto, Markus Garczarczyk, N. Mankuzhiyil, Juri Poutanen, Kyoshi Nishijima, D. Dominis Prester, Y. Hanabata, C. Schultz, V. Scapin, P. Antoranz, M. L. Knoetig, Ana Babić, Julia Thaele, E. Carmona, Kari Nilsson, M. Will, L. Maraschi, E. Prandini, Tomislav Terzić, R. Reinthal, M. Negrello, Damir Lelas, Dorota Sobczyńska, Ivica Puljak, Pierre Colin, E. de Oña Wilhelmi, Jelena Aleksić, A. Niedzwiecki, David Paneque, M. Barcelo, D. Galindo, Konstancja Satalecka, Michele Doro, Julian Sitarek, Daniela Hadasch, T. Toyama, Junko Kushida, P. Da Vela, J. Schlammer, Universitat de Barcelona, Aleksić, J, Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Bangale, P., Barceló, M., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Biasuzzi, B., Biland, A., Bitossi, M., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Carmona, E., Carosi, A., Cecchi, R., Colin, P., Colombo, E., Contreras, J. L., Corti, D., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., Deangelis, A., De Caneva, G., De Lotto, B., De Oña Wilhelmi, E., Delgado Mendez, C., Dettlaff, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher, D., Elsaesser, D., Fidalgo, D., Fink, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., García López, R. J., Garczarczyk, M., Garrido Terrats, D., Gaug, M., Giavitto, G., Godinović, N., González Muñoz, A., Gozzini, S. R., Haberer, W., Hadasch, D., Hanabata, Y., Hayashida, M., Herrera, J., Hildebrand, D., Hose, J., Hrupec, D., Idec, W., Illa, J. M., Kadenius, V., Kellermann, H., Knoetig, M. L., Kodani, K., Konno, Y., Krause, J., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lemus, J. L., Lewandowska, N., Lindfors, E., Lombardi, S., Longo, Francesco, López, M., López Coto, R., López Oramas, A., Lorca, A., Lorenz, E., Lozano, I., Makariev, M., Mallot, K., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martínez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Munar Adrover, P., Nakajima, D., Negrello, M., Neustroev, V., Niedzwiecki, A., Nilsson, K., Nishijima, K., Noda, K., Orito, R., Overkemping, A., Paiano, S., Palatiello, Michele, Paneque, D., Paoletti, R., Paredes, J. M., Paredes Fortuny, X., Persic, M., Poutanen, J., Prada Moroni, P. G., Prandini, E., Puljak, I., Reinthal, R., Rhode, W., Ribó, M., Rico, J., Rodriguez Garcia, J., Rügamer, S., Saito, T., Saito, K., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schlammer, J., Schmidl, S., Schweizer, T., Sillanpää, A., Sitarek, J., Snidaric, I., Sobczynska, D., Spanier, F., Stamerra, A., Steinbring, T., Storz, J., Strzys, M., Takalo, L., Takami, H., Tavecchio, F., Tejedor, L. A., Temnikov, P., Terzić, T., Tescaro, D., Teshima, M., Thaele, J., Tibolla, O., Torres, D. F., Toyama, T., Treves, A., Vogler, P., Wetteskind, H., Will, M., and Zanin, R.

Subjects
Astrofísica, Physics::Instrumentation and Detectors, MAGIC, Imaging Atmospheric Cherenkov Telescopes, Instruments, TeV astrophysics, Very High Energy Gamma Rays, Stereoscopy, Astrophysics, 01 natural sciences, law.invention, Raigs gamma, law, Overall performance, MAGIC (telescope), TeV, astrophysics, CRAB-NEBULA, PERFORMANCE, STEREO, 010303 astronomy & astrophysics, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Instrument, Upgrade, ddc:540, Electrónica, Física nuclear, Astrophysics::Earth and Planetary Astrophysics, Electricidad, Astrophysics - Instrumentation and Methods for Astrophysics, TeV astrophysic, Noise (radio), Computer hardware, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Telescope, 0103 physical sciences, Very High Energy Gamma Ray, Instrumentation and Methods for Astrophysics (astro-ph.IM), Cherenkov radiation, ta115, Telescopis, 010308 nuclear & particles physics, business.industry, Gamma rays, Cherenkov Telescope Array, Imaging Atmospheric Cherenkov Telescope, business, astro-ph.IM, Telescopes
Abstract

The MAGIC telescopes are two Imaging Atmospheric Cherenkov Telescopes (IACTs) located on the Canary island of La Palma. The telescopes are designed to measure Cherenkov light from air showers initiated by gamma rays in the energy regime from around 50 GeV to more than 50 TeV. The two telescopes were built in 2004 and 2009, respectively, with different cameras, triggers and readout systems. In the years 2011-2012 the MAGIC collaboration undertook a major upgrade to make the stereoscopic system uniform, improving its overall performance and easing its maintenance. In particular, the camera, the receivers and the trigger of the first telescope were replaced and the readout of the two telescopes was upgraded. This paper (Part I) describes the details of the upgrade as well as the basic performance parameters of MAGIC such as raw data treatment, dead time of the system, linearity in the electronic chain and sources of noise. In Part II, we describe the physics performance of the upgraded system., 19 pages, 18 figures, accepted by Astroparticle Physics

Published
2016

20. Herschel-ATLAS: VISTA VIKING near-infrared counterparts in the Phase 1 GAMA 9-h data★

Author

Jacopo Fritz, Asantha Cooray, David Bonfield, William J. Sutherland, Andrea Lapi, R. Hopwood, Aaron S. G. Robotham, A. Dariush, M. L. P. Gunawardhana, Pasquale Temi, Rob Ivison, E. Ibar, Maarten Baes, L. Kelvin, Michał J. Michałowski, Robbie Richard Auld, Matthew Prescott, Maggie A. Thompson, Matt J. Jarvis, Joseph R. Findlay, N. Bourne, Enzo Pascale, G. de Zotti, Elisabetta Valiante, S. J. Maddox, E. E. Rigby, S. Fleuren, Simon P. Driver, P. van der Werf, J. González-Nuevo, Douglas Scott, M. Negrello, Simon Dye, S. Buttiglione, Steve Eales, Loretta Dunne, Nicholas A. Bond, M. Pohlen, Antonio Cava, Jochen Liske, and D. J. B. Smith

Subjects
Identification rate, Physics, Spire, medicine.anatomical_structure, Space and Planetary Science, Atlas (anatomy), Phase (waves), medicine, Astronomy and Astrophysics, Astrophysics, Field population, Galaxy, Redshift
Abstract

We identify near-infrared Ks band counterparts to Herschel-ATLAS sub-mm sources, using a preliminary object catalogue from the VISTA VIKING survey. The sub-mm sources are selected from the H-ATLAS Phase 1 catalogue of the GAMA 9h field, which includes all objects detected at 250, 350 or 500 um with the SPIRE instrument. We apply and discuss a likelihood ratio (LR) method for VIKING candidates within a search radius of 10" of the 22,000 SPIRE sources with a 5 sigma detection at 250 um. We find that 11,294(51%) of the SPIRE sources have a best VIKING counterpart with a reliability $R\ge 0.8$, and the false identification rate of these is estimated to be 4.2%. We expect to miss ~5% of true VIKING counterparts. There is evidence from Z-J and J-Ks colours that the reliable counterparts to SPIRE galaxies are marginally redder than the field population. We obtain photometric redshifts for ~68% of all (non-stellar) VIKING candidates with a median redshift of 0.405. Comparing to the results of the optical identifications supplied with the Phase I catalogue, we find that the use of medium-deep near-infrared data improves the identification rate of reliable counterparts from 36% to 51%.

Published
2012

21. Clustering of submillimetre galaxies in a self-regulated baryon collapse model

Author

M. Viel, L. Danese, Andrea Lapi, G. de Zotti, M. Negrello, and Jun-Qing Xia

Subjects
Physics, Initial mass function, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Baryon, Space and Planetary Science, Cosmic infrared background, 0103 physical sciences, Galaxy formation and evolution, Satellite galaxy, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We have investigated the Cosmic Infrared Background (CIB) anisotropies in the framework of the physical evolutionary model for proto-spheroidal galaxies by Granato et al. (2004). After having re-calibrated the cumulative flux function $dS/dz$ at $\lambda \ge 850\,\mu$m using the available determinations of the shot noise amplitude (the original model already correctly reproduces it at shorter wavelengths) the CIB power spectra at wavelengths from $250\,\mu$m to $2\,$mm measured by {\it Planck}, {\it Herschel}, SPT and ACT experiments have been fitted using the halo model with only 2 free parameters, the minimum halo mass and the power-law index of the mean occupation function of satellite galaxies. The best-fit {\it minimum} halo mass is $\log(M_{\rm min}/M_\odot) = 12.24 \pm 0.06$, higher than, but consistent within the errors, with the estimate by Amblard et al. (2011) and close to the estimate by Planck Collaboration (2011). The redshift evolution of the volume emissivity of galaxies yielded by the model is found to be consistent with that inferred from the data. The derived {\it effective} halo mass, $M_{\rm eff} \simeq 5\times 10^{12}\,M_\odot$, of $z\simeq 2$ sub-millimeter galaxies is close to that estimated for the most efficient star-formers at the same redshift. The effective bias factor and the comoving clustering radius at $z\simeq 2$ yielded by the model are substantially lower than those found for a model whereby the star formation is fueled by steady gas accretion, but substantially higher than those found for a merging-driven galaxy evolution with a top-heavy initial mass function.

Published
2012

22. Herschel-ATLAS: the far-infrared-radio correlation at z < 0.5★

Author

Matt J. Jarvis, D. J. B. Smith, D. G. Bonfield, M. J. Hardcastle, J. T. Falder, J. A. Stevens, R. J. Ivison, R. Auld, M. Baes, I. K. Baldry, S. P. Bamford, N. Bourne, S. Buttiglione, A. Cava, A. Cooray, A. Dariush, G. De Zotti, J. S. Dunlop, L. Dunne, S. Dye, S. Eales, J. Fritz, D. T. Hill, R. Hopwood, D. H. Hughes, E. Ibar, D. H. Jones, L. Kelvin, A. Lawrence, L. Leeuw, J. Loveday, S. J. Maddox, M. J. Michałowski, M. Negrello, P. Norberg, M. Pohlen, M. Prescott, E. E. Rigby, A. Robotham, G. Rodighiero, D. Scott, R. Sharp, P. Temi, M. A. Thompson, P. Van Der Werf, E. Van Kampen, C. Vlahakis, and G. White

Subjects
Physics, Stellar population, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Universe, Redshift, Luminosity, Wavelength, Far infrared, Space and Planetary Science, Sky, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract

We use data from the Herschel-ATLAS to investigate the evolution of the far-infrared--radio correlation over the redshift range 0 5sigma sources in the Herschel-ATLAS Science Demonstration Field and cross-matching these data with radio data from the Faint Images of the Radio Sky at Twenty-Centimetres (FIRST) survey and the NRAO VLA Northern Sky Survey (NVSS), we obtain 104 radio counterparts to the Herschel sources. With these data we find no evidence for evolution in the far-infrared--radio correlation over the redshift range 0

Published
2010

23. Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources

Author

G. de Zotti, Gian Luigi Granato, F. Perrotta, C. Baccigalupi, L. Danese, M. Negrello, J. Gonzalez-Nuevo Gonzalez, and Laura Silva

Subjects
Physics, galaxies : evolution, Astrophysics (astro-ph), gravitational lensing, FOS: Physical sciences, cosmology : observations, submillimetre, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Expected value, Galaxy, Redshift, Luminosity, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, symbols, Planck, Cluster analysis, Blazar, Astrophysics::Galaxy Astrophysics
Abstract

We present a quantitative analysis of the astrophysical and cosmological information that can be extracted from the many important wide-area, shallow surveys that will be carried out in the next few years. Our calculations combine the predictions of the physical model by Granato et al. (2004) for the formation and evolution of spheroidal galaxies with up-to-date phenomenological models for the evolution of starburst and normal late-type galaxies and of radio sources. We compute the expected number counts and the redshift distributions of these source populations separately and then focus on proto-spheroidal galaxies. For the latter objects we predict the counts and redshift distributions of strongly lensed sources at 250, 350, 500, and 850 micron, the angular correlation function of sources detected in the surveys considered, the angular power spectra due to clustering of sources below the detection limit in Herschel and Planck surveys. An optimal survey for selecting strongly lensed proto-spheroidal galaxies is described, and it is shown how they can be easily distinguished from the other source populations. We also discuss the detectability of the imprints of the 1-halo and 2-halo regimes on angular correlation functions and clustering power spectra, as well as the constraints on cosmological parameters that can be obtained from the determinations of these quantities. The novel data relevant to derive the first sub-millimeter estimates of the local luminosity functions of starburst and late-type galaxies, and the constraints on the properties of rare source populations, such as blazars, are also briefly described., 16 pages, 10 figures. Accepted for publication on MNRAS

Published
2007

24. Radio Observations of Star Forming Galaxies in the SKA era

Author

Andrea Lapi, L. Danese, C. Mancuso, Zhen-Yi Cai, F. Perrotta, M. Negrello, and Gianfranco De Zotti

Subjects
Physics, Star formation, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), Astrophysics - Astrophysics of Galaxies, Synchrotron, Galaxy, Redshift, law.invention, Square degree, Luminosity, South Pole Telescope, Settore FIS/05 - Astronomia e Astrofisica, law, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics
Abstract

We have combined determinations of the epoch-dependent star formation rate (SFR) function with relationships between SFR and radio (synchrotron and free-free) emission to work out detailed predictions for the counts and the redshift distributions of star-forming galaxies detected by planned Square Kilometer Array (SKA) surveys. The evolving SFR function comes from recent models fitting the far-infrared (FIR) to millimeter-wave luminosity functions and the ultraviolet (UV) luminosity functions up to z=10, extended to take into account additional UV survey data. We used very deep 1.4 GHz number counts from the literature to check the relationship between SFR and synchrotron emission, and the 95 GHz South Pole Telescope (SPT) counts of dusty galaxies to test the relationship between SFR and free-free emission. We show that the SKA will allow us to investigate the SFRs of galaxies down to few Msun/yr up to z=10, thus extending by more than two orders of magnitude the high-z SFR functions derived from Herschel surveys. SKA1-MID surveys, down to microJy levels, will detect hundreds of strongly lensed galaxies per square degree; a substantial fraction of them will show at least two images above the detection limits., Comment: 11 pages, 4 figures, to appear in proceedings of "Advancing Astrophysics with the Square Kilometre Array" PoS(AASKA14)082

Published
2015

25. Lens Models of Herschel-selected Galaxies from High-resolution Near-IR Observations

Author

J. A. Calanog, Hai Fu, A. Cooray, J. Wardlow, B. Ma, S. Amber, A. J. Baker, M. Baes, J. Bock, N. Bourne, R. S. Bussmann, C. M. Casey, S. C. Chapman, D. L. Clements, A. Conley, H. Dannerbauer, G. De Zotti, L. Dunne, S. Dye, S. Eales, D. Farrah, C. Furlanetto, A. I. Harris, R. J. Ivison, S. Kim, S. J. Maddox, G. Magdis, H. Messias, M. J. Michałowski, M. Negrello, J. Nightingale, J. M. O'Bryan, S. J. Oliver, D. Riechers, D. Scott, S. Serjeant, J. Simpson, M. Smith, N. Timmons, C. Thacker, E. Valiante, and J. D. Vieira

Subjects
submillimeter: galaxies, ULTRALUMINOUS INFRARED GALAXIES, Terahertz radiation, FOS: Physical sciences, galaxies [submillimeter], Magnification, High resolution, COSMOLOGICAL HYDRODYNAMIC SIMULATIONS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, HIGH-REDSHIFT GALAXIES, law.invention, law, Hubble space telescope, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, SPACE-TELESCOPE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, ADAPTIVE OPTICS, Physics, 010308 nuclear & particles physics, gravitational lensing: strong, Astronomy and Astrophysics, LUMINOUS SUBMILLIMETER GALAXIES, Astrophysics - Astrophysics of Galaxies, Galaxy, 1ST DATA RELEASE, Lens (optics), Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, strong [gravitational lensing], DEEP-FIELD-SOUTH, DIGITAL SKY SURVEY, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies]
Abstract

We present Keck-Adaptive Optics and Hubble Space Telescope high resolution near-infrared (IR) imaging for 500 um-bright candidate lensing systems identified by the Herschel Multi-tiered Extra-galactic Survey (HerMES) and Herschel Astrophysical Terahertz Survey (H-ATLAS). Out of 87 candidates with near-IR imaging, 15 (~17%) display clear near-IR lensing morphologies. We present near-IR lens models to reconstruct and recover basic rest-frame optical morphological properties of the background galaxies from 12 new systems. Sources with the largest near-IR magnification factors also tend to be the most compact, consistent with the size bias predicted from simulations and pre- vious lensing models for sub-millimeter galaxies. For four new sources that also have high-resolution sub-mm maps, we test for differential lensing between the stellar and dust components and find that the 880 um magnification factor (u_880) is ~1.5 times higher than the near-IR magnification factor (u_NIR), on average. We also find that the stellar emission is ~2 times more extended in size than dust. The rest-frame optical properties of our sample of Herschel-selected lensed SMGs are consistent with those of unlensed SMGs, which suggests that the two populations are similar., Comment: 27 pages, 13 figures, 7 tables, ApJ accepted

Published
2014

26. Confusion noise at far-infrared to millimetre wavelengths

Author

G. de Zotti, Laura Silva, Lauro Moscardini, M. Magliocchetti, M. Negrello, and Gian Luigi Granato

Subjects
Physics, media_common.quotation_subject, Dark matter, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, Universe, symbols.namesake, Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics, Halo, Planck, Cluster analysis, Astrophysics::Galaxy Astrophysics, Noise (radio), media_common
Abstract

We present detailed predictions for the confusion noise due to extragalactic sources in the far-IR/(sub)-millimeter channels of ESA/ISO, NASA/Spitzer, ESA/Herschel and ESA/Planck satellites, including the contribution from clustering of unresolved SCUBA galaxies. Clustering is found to increase the confusion noise, compared to the case of purely Poisson fluctuations, by 10-15% for the lowest frequency (i.e. lowest angular resolution) Spitzer and Herschel channels, by 25-35% for the 175 micron ISOPHOT channel, and to dominate in the case of Planck/HFI channels at nu>143GHz. Although our calculations make use of a specific evolutionary model (Granato et al. 2004), the results are strongly constrained by the observed counts and by data on the redshift distribution of SCUBA sources, and therefore are not expected to be heavily model dependent. The main uncertainty arises from the poor observational definition of the source clustering properties. Two models have been used for the latter: a power-law with constant slope and a redshift-independent comoving correlation length,r_0, and the standard theoretical model for clustering evolution in a LambdaCDM universe, with a redshift-dependent bias factor. In both cases, the clustering amplitude has been normalized to yield a unit angular correlation function at theta_0=1-2 arcsec for 850 micron sources fainter than 2 mJy, consistent with the results by Peacock et al. (2000). This normalization yields, for the first model, r_0=8.3$ Mpc/h, and, for the second model, an effective mass of dark matter haloes in which these sources reside of M_halo=1.8*10^{13} M_sun/h. These results are consistent with independent estimates for SCUBA galaxies and for other, likely related, sources.

Published
2004

27. THE

Author

M. P. Viero, V. Asboth, I. G. Roseboom, L. Moncelsi, G. Marsden, E. Mentuch Cooper, M. Zemcov, G. Addison, A. J. Baker, A. Beelen, J. Bock, C. Bridge, A. Conley, M. J. Devlin, O. Dorxe9, D. Farrah, S. Finkelstein, A. Font-Ribera, J. E. Geach, K. Gebhardt, A. Gill, J. Glenn, A. Hajian, M. Halpern, S. Jogee, P. Kurczynski, A. Lapi, M. Negrello, S. J. Oliver, C. Papovich, R. Quadri, and et al. (including L. Wang)

Published
2014

28. Cross-correlation between the CMB lensing potential measured by Planck and high-z sub-mm galaxies detected by the Herschel-ATLAS survey

Author

Steve Eales, L. Danese, Simon Dye, G. de Zotti, M. W. L. Smith, C. Baccigalupi, Loretta Dunne, J. González-Nuevo, P. Bielewicz, S. J. Maddox, Elisabetta Valiante, Andrea Lapi, N. Bourne, Federico Bianchini, Douglas Scott, M. Negrello, Rob Ivison, Asantha Cooray, Ministerio de Ciencia e Innovación (España), European Commission, Istituto Nazionale di Astrofisica, Consejo Superior de Investigaciones Científicas (España), and European Research Council

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmic background radiation, 01 natural sciences, high-redshift [Galaxies], symbols.namesake, gravitational lensing: weak, Settore FIS/05 - Astronomia e Astrofisica, galaxies: high-redshift, 0103 physical sciences, Planck, Density contrast, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Cross-correlation, 010308 nuclear & particles physics, Null (mathematics), Cosmology: observations, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods: data analysis, Redshift, Galaxy, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), symbols, weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada.-- et al., We present the first measurement of the correlation between the map of the cosmic microwave background (CMB) lensing potential derived from the Planck nominal mission data and galaxies detected by the Herschel-ATLAS (H-ATLAS) survey covering about , i.e., about 1.4% of the sky. We reject the hypothesis that there is no correlation between CMB lensing and galaxy detection at asignificance, checking the result by performing a number of null tests. The significance of the detection of the theoretically expected cross-correlation signal is found to be. The galaxy bias parameter, b, derived from a joint analysis of the cross-power spectrum and of the autopower spectrum of the galaxy density contrast is found to be , consistent with earlier estimates for H-ATLAS galaxies at similar redshifts. On the other hand, the amplitude of the cross-correlation is found to be a factor 1.62 ± 0.16 higher than expected from the standard model and also found by cross-correlation analyses with other tracers of the large-scale structure. The enhancement due to lensing magnification can account for only a fraction of the excess cross-correlation signal. We suggest that part of it may be due to an incomplete removal of the contamination of the cosmic infrared background, which includes the H-ATLAS sources we are cross-correlating with. In any case, the highly significant detection reported here using a catalog covering only 1.4% of the sky demonstrates the potential of CMB lensing correlations with submillimeter surveys., We gratefully acknowledge support from INAF PRIN 2012/2013 >Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Terahertz Large Area Survey,> and from ASI/INAF agreement 2014-024 R.0. F.B. acknowledges partial support from the INFN-INDARK initiative. L.D., R.J.I., and S.M. acknowledge support from the European Research Council (ERC) in the form of Advanced Investigator Program COSMICISM. J.G.N. acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, cofunded by the European Social Fund. The work has been supported in part by the Spanish Ministerio de Ciencia e Innovacion, AYA2012-39475-C02-01, and Consolider-Ingenio 2010, CSD2010-00064, projects.

Published
2014
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29. HerMES: Candidate Gravitationally Lensed Galaxies and Lensing Statistics at Submillimeter Wavelengths

Author

E. Chapin, Antonio Cava, A. Strom, P. Martinez-Navajas, Andrew J. Baker, Asantha Cooray, G. Marsden, John M. Carpenter, B. O'Halloran, A. Conley, Bernhard Schulz, Simon Dye, V. Arumugam, M. J. Page, N. Z. Scoville, Matthew Joseph Griffin, David T. Frayer, Rob Ivison, R. Hopwood, Patrizia Ferrero, Alain Omont, Seb Oliver, Guilaine Lagache, Carrie Bridge, C. K. Xu, Alexandre Amblard, Herve Aussel, Andreas Papageorgiou, Christopher C. Frazer, C. D. Dowell, Douglas Scott, Evanthia Hatziminaoglou, Ismael Perez-Fournon, V. Buat, Anthony J. Smith, Alberto Franceschini, Pierre Cox, Scott Chapman, Mattia Vaccari, Lucia Marchetti, Lian-Tao Wang, Julie Wardlow, M. Negrello, Caitlin M. Casey, Markos Trichas, Pasquale Panuzzo, R. S. Bussmann, Joaquin Vieira, Dimitra Rigopoulou, Michael Rowan-Robinson, M. Symeonidis, Mark Gurwell, Alessandro Boselli, Andrew I. Harris, Jae Calanog, Matthieu Béthermin, Raphael Gavazzi, Ray Blundell, Nick Seymour, Jason Glenn, D. L. Shupe, A. Hyde, Dominik A. Riechers, Isaac Roseboom, C. P. Pearson, Lin Yan, Michael Pohlen, Pierre Chanial, N. Castro-Rodríguez, James J. Bock, Francesco De Bernardis, Denis Burgarella, Hai Fu, Edo Ibar, L. R. Levenson, Antonio Cabrera-Lavers, Michael Zemcov, Duncan Farrah, Hien Nguyen, David L. Clements, Stephen Anthony Eales, Roberto Neri, E. A. González Solares, Marco P. Viero, S. Kim, Alina Streblyanska, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, FOS: Physical sciences, Magnification, Flux, Astronomy and Astrophysics, Statistical model, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Wavelength, Gravitational lens, Space and Planetary Science, Primary (astronomy), Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a list of 13 candidate gravitationally lensed submillimeter galaxies (SMGs) from 95 square degrees of the Herschel Multi-tiered Extragalactic Survey, a surface density of 0.14\pm0.04deg^{-2}. The selected sources have 500um flux densities (S_500) greater than 100mJy. Gravitational lensing is confirmed by follow-up observations in 9 of the 13 systems (70%), and the lensing status of the four remaining sources is undetermined. We also present a supplementary sample of 29 (0.31\pm0.06deg^{-2}) gravitationally lensed SMG candidates with S_500=80--100mJy, which are expected to contain a higher fraction of interlopers than the primary candidates. The number counts of the candidate lensed galaxies are consistent with a simple statistical model of the lensing rate, which uses a foreground matter distribution, the intrinsic SMG number counts, and an assumed SMG redshift distribution. The model predicts that 32--74% of our S_500>100mJy candidates are strongly gravitationally lensed (mu>2), with the brightest sources being the most robust; this is consistent with the observational data. Our statistical model also predicts that, on average, lensed galaxies with S_500=100mJy are magnified by factors of ~9, with apparently brighter galaxies having progressively higher average magnification, due to the shape of the intrinsic number counts. 65% of the sources are expected to have intrinsic 500micron flux densities less than 30mJy. Thus, samples of strongly gravitationally lensed SMGs, such as those presented here, probe below the nominal Herschel detection limit at 500 micron. They are good targets for the detailed study of the physical conditions in distant dusty, star-forming galaxies, due to the lensing magnification, which can lead to spatial resolutions of ~0.01" in the source plane., ApJ in press. 31 pages, 16 figures, 5 tables. This version updated to match accepted version

Published
2013

30. A DETAILED GRAVITATIONAL LENS MODEL BASED ON SUBMILLIMETER ARRAY AND KECK ADAPTIVE OPTICS IMAGING OF A HERSCHEL-ATLAS SUBMILLIMETER GALAXY AT z=4.243

Author

P. van der Werf, A. Verma, Daniel J. Smith, Pasquale Temi, Michał J. Michałowski, K. Coppin, E. E. Rigby, David Bonfield, Sungeun Kim, G. de Zotti, Loretta Dunne, Helmut Dannerbauer, Rob Ivison, Mark Gurwell, Stephen Anthony Eales, Jacopo Fritz, Asantha Cooray, Maarten Baes, Edo Ibar, Antonio Cava, Julie Wardlow, R. S. Bussmann, Matt J. Jarvis, A. Dariush, Hai Fu, D. L. Clements, Douglas Scott, M. Negrello, Enzo Pascale, Dominik Riechers, Simon Dye, Steve Maddox, L. Leeuw, Robbie Richard Auld, M. Pohlen, R. Hopwood, David J. Wilner, Andrew J. Baker, and Science and Technology Facilities Council (STFC)

Subjects
ULTRALUMINOUS INFRARED GALAXIES, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 0306 Physical Chemistry (Incl. Structural), Infrared, astro-ph.GA, BILLION YEARS, FOS: Physical sciences, Astrophysics, Astronomy & Astrophysics, LUMINOSITY FUNCTIONS, 0305 Organic Chemistry, 01 natural sciences, Submillimeter Array, law.invention, Luminosity, galaxies: high-redshift, law, 0103 physical sciences, Angular resolution, 010303 astronomy & astrophysics, Physics, DEGREE EXTRAGALACTIC SURVEY, Science & Technology, galaxies: evolution, galaxies: fundamental parameters, gravitational lensing: strong, Astronomy and Astrophysics, Space and Planetary Science, 010308 nuclear & particles physics, SPACE-TELESCOPE MORPHOLOGIES, STAR-FORMATION HISTORY, Astrophysics - Astrophysics of Galaxies, MOLECULAR GAS, Galaxy, Redshift, Lens (optics), 0201 Astronomical And Space Sciences, Gravitational lens, ALL-SKY SURVEY, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, astro-ph.CO, DEEP-FIELD-SOUTH, SCIENCE DEMONSTRATION PHASE, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present high-spatial resolution imaging obtained with the Submillimeter Array (SMA) at 880um and the Keck Adaptive Optics (AO) system at Ks-band of a gravitationally lensed sub-millimeter galaxy (SMG) at z=4.243 discovered in the Herschel-Astrophysical Terahertz Large Area Survey. The SMA data (angular resolution ~0.6") resolve the dust emission into multiple lensed images, while the Keck AO Ks-band data (angular resolution ~0.1") resolve the lens into a pair of galaxies separated by 0.3". We present an optical spectrum of the foreground lens obtained with the Gemini-South telescope that provides a lens redshift of z_lens = 0.595 +/- 0.005. We develop and apply a new lens modeling technique in the visibility plane that shows that the SMG is magnified by a factor of mu = 4.1 +/- 0.2 and has an intrinsic infrared (IR) luminosity of L_IR = (2.1 +/- 0.2) x 10^13 Lsun. We measure a half-light radius of the background source of r_s = 4.4 +/- 0.5 kpc which implies an IR luminosity surface density of Sigma_IR = (3.4 +/- 0.9) x 10^11 Lsun kpc^-2, a value that is typical of z > 2 SMGs but significantly lower than IR luminous galaxies at z~0. The two lens galaxies are compact (r_lens ~ 0.9 kpc) early-types with Einstein radii of theta_E1 = 0.57 +/- 0.01 and theta_E2 = 0.40 +/- 0.01 that imply masses of M_lens1 = (7.4 +/- 0.5) x 10^10 Msun and M_lens2 = (3.7 +/- 0.3) x 10^10 Msun. The two lensing galaxies are likely about to undergo a dissipationless merger, and the mass and size of the resultant system should be similar to other early-type galaxies at z~0.6. This work highlights the importance of high spatial resolution imaging in developing models of strongly lensed galaxies discovered by Herschel., Accepted to the ApJ. 12 pages, 6 figures, 3 tables

Published
2012

31. Herschel-Astrophysical Terahertz Large Area Survey: detection of a far-infrared population around galaxy clusters★

Author

K. E. K. Coppin, J. E. Geach, Ian Smail, L. Dunne, A. C. Edge, R. J. Ivison, S. Maddox, R. Auld, M. Baes, S. Buttiglione, A. Cava, D. L. Clements, A. Cooray, A. Dariush, G. De Zotti, S. Dye, S. Eales, J. Fritz, R. Hopwood, E. Ibar, M. Jarvis, M. J. Michałowski, D. N. A. Murphy, M. Negrello, E. Pascale, M. Pohlen, E. Rigby, G. Rodighiero, D. Scott, S. Serjeant, D. J. B. Smith, P. Temi, and P. van der Werf

Subjects
Physics, education.field_of_study, Active galactic nucleus, 010308 nuclear & particles physics, Star formation, Population, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, 01 natural sciences, Galaxy, Far infrared, Space and Planetary Science, 0103 physical sciences, Cluster (physics), education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy cluster
Abstract

We report the detection of a significant excess in the surface density of far-infrared sources from the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) within ∼ 1 Mpc of the centres of 66 optically-selected clusters of galaxie s in the SDSS with hzi ∼0.25. From the analysis of the multiwavelength properties of their cou nterparts we conclude that the farinfrared emission is associated with dust-obscured star fo rmation and/or active galactic nuclei within galaxies in the clusters themselves. The excess reaches a maximum at a radius of ∼ 0.8 Mpc, where we find 1.0±0.3 S250 >34 mJy sources on average per cluster above what would be expected for random field locations. If the far-infr ared emission is dominated by star formation (as opposed to AGN) then this corresponds to an average star formation rate of ∼7 M⊙ yr −1 per cluster in sources with LIR > 5×10 10 L⊙. Although lensed sources make a negligible contribution to the excess signal, a fraction of the sources around the clusters could be gravitationally lensed, and we have identified a sample of potential cases of cluster-lensed Herschel sources that could be targeted in follow-up studies.

Published
2011

33. GREEN BANK ℡ESCOPE ZPECTROMETER CO(1-0) OBSERVATIONS OF THE STRONGLY LENSED SUBMILLIMETER GALAXIES FROM THE HERSCHEL ATLAS

Author

Mark Birkinshaw, Maarten Baes, Jacopo Fritz, Asantha Cooray, Andrew J. Baker, J. González-Nuevo, Steve Serjeant, Denis Burgarella, Maggie A. Thompson, Itziar Aretxaga, D. J. B. Smith, David H. Hughes, A. Verma, G. Rodighiero, E. E. Rigby, A. M. Swinbank, Andrew I. Harris, A. Omont, Simon Dye, G. de Zotti, Loretta Dunne, James Dunlop, R. Hopwood, S. J. Maddox, David T. Frayer, A. Dariush, S. Buttiglione, Pasquale Temi, M. Pohlen, Ronald J. Maddalena, Rob Ivison, L. Leeuw, Michał J. Michałowski, E. Ibar, D. Herranz, P. van der Werf, M. López-Caniego, Steve Eales, Antonio Cava, Ian Smail, Matt J. Jarvis, M. Negrello, Douglas Scott, David Bonfield, Helmut Dannerbauer, D. L. Clements, G. Lagache, I. Valtchanov, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science and Technology Facilities Council (STFC), and Universidad de Cantabria

Subjects
Terahertz radiation, Population, LINE, galaxies: starburst, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, galaxies: individual (SDP.81: H-ATLAS J090311.6+003906, SDP.130: H-ATLAS J091305.0-005343), Atlas (anatomy), 0103 physical sciences, medicine, galaxies: formation, 10. No inequality, education, Galaxies: individual (SDP.81: H-ATLAS J090311.6+003906, SDP.130: H-ATLAS J091305.0−005343), 010303 astronomy & astrophysics, POPULATION, Physics, education.field_of_study, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Green Bank Telescope, CONSTRAINTS, Astronomy and Astrophysics, DISK GALAXIES, REGIONS, evolution [Galaxies], LUMINOUS INFRARED GALAXIES, formation [Galaxies], MOLECULAR GAS, Galaxy, Redshift, 0201 Astronomical And Space Sciences, Wavelength, starburst [Galaxies], medicine.anatomical_structure, Space and Planetary Science, Physical Sciences, REDSHIFT DISTRIBUTION, astro-ph.CO, galaxies: evolution, EMISSION, CLUSTERS
Abstract

6 páginas, 3 figuras, 2 tablas.-- El Pdf del artículo es la versión pre-print: arXiv:1009.2194v2.-- et al., The Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) has uncovered a population of strongly lensed submillimeter galaxies (SMGs). The Zpectrometer instrument on the Green Bank Telescope (GBT) was used to measure the redshifts and constrain the masses of the cold molecular gas reservoirs for two candidate high-redshift lensed sources. We derive CO(1-0) redshifts of z = 3.042 ± 0.001 and z = 2.625 ± 0.001, and measure molecular gas masses of (1-3) ×1010 M ☉, corrected for lens amplification and assuming a conversion factor of α = 0.8 M ☉( K km s–1 pc2)–1. We find typical L(IR)/L'(CO) ratios of 120 ± 40 and 140 ± 50 L ☉( K km s–1 pc2)–1, which are consistent with those found for local ultraluminous infrared galaxies (ULIRGs) and other high-redshift SMGs. From analysis of published data, we find no evidence for enhanced L(IR)/L'(CO(1-0)) ratios for the SMG population in comparison to local ULIRGs. The GBT results highlight the power of using the CO lines to derive blind redshifts, which is challenging for the SMGs at optical wavelengths given their high obscuration., A.J.B. acknowledges support from the National Science Foundation through grant AST-0708653.

Published
2011

34. Herschel-ATLAS: Extragalactic number counts from 250 to 500 microns

Author

Rob Ivison, A. Verma, G. Lagache, Maarten Baes, Dave Frayer, E. E. Rigby, M. Pohlen, M. López-Caniego, Enzo Pascale, Antonio Cava, David Bonfield, A. Amblard, Loretta Dunne, Simon Dye, A. Dariush, Pasquale Temi, S. Buttiglione, P. van der Werf, Jacopo Fritz, Asantha Cooray, Lerothodi Leonard Leeuw, Chris Pearson, Robbie Richard Auld, Angela M. J. Mortier, D. Herranz, Saumyadip Samui, Jonathan P. Gardner, D. J. B. Smith, D. L. Clements, Matt J. Jarvis, Denis Burgarella, Maggie A. Thompson, S. J. Maddox, Steve Serjeant, M. Negrello, J. González-Nuevo, E. Ibar, Douglas Scott, I. Valtchanov, B. Sibthorpe, G. Rodighiero, G. de Zotti, Steve Eales, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad de Cantabria, and Science and Technology Facilities Council (STFC)

Subjects
statistics [galaxies], UNIVERSE, galaxies [submillimeter], Astrophysics, Submilimeter: galaxies, 01 natural sciences, galaxies [Infrared], MAPS, 010303 astronomy & astrophysics, QB, media_common, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atlas (topology), Galaxies: evolution, Wavelength, Physical Sciences, astro-ph.CO, statistics [Galaxy], Galaxies: statistics, Infrared: galaxies, Submillimeter: galaxies, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Population, PREDICTIONS, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, STAR-FORMATION, Submillimetre: galaxies, Galaxy: statistics, 0103 physical sciences, Galaxy formation and evolution, 14. Life underwater, FIELD, education, Astrophysics::Galaxy Astrophysics, SURVEY SHADES, galaxies [Submilimeter], Science & Technology, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, evolution [Galaxies], EVOLUTION, Redshift, Galaxy, MODEL, SPITZER, 0201 Astronomical And Space Sciences, Physics and Astronomy, Sky, Extraction methods
Abstract

4 páginas, 1 figura, 1 tabla.-- Letter to the editor.-- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.-- et al., [Aims]: The Herschel-ATLAS survey (H-ATLAS) will be the largest area survey to be undertaken by the Herschel Space Observatory. It will cover 550 sq. deg. of extragalactic sky at wavelengths of 100, 160, 250, 350 and 500 μm when completed, reaching flux limits (5σ) from 32 to 145 mJy. We here present galaxy number counts obtained for SPIRE observations of the first ∼14 sq. deg. observed at 250, 350 and 500 μm. [Methods]: Number counts are a fundamental tool in constraining models of galaxy evolution. We use source catalogs extracted from the H-ATLAS maps as the basis for such an analysis. Correction factors for completeness and flux boosting are derived by applying our extraction method to model catalogs and then applied to the raw observational counts. [Results]: We find a steep rise in the number counts at flux levels of 100−200 mJy in all three SPIRE bands, consistent with results from BLAST. The counts are compared to a range of galaxy evolution models. None of the current models is an ideal fit to the data but all ascribe the steep rise to a population of luminous, rapidly evolving dusty galaxies at moderate to high redshift.

Published
2010

35. Herschel-ATLAS: Blazars in the Science Demonstration Phase field

Author

Mark Birkinshaw, M. López-Caniego, B. Sibthorpe, T. Mauch, Laura Bonavera, Hans-Rainer Klöckner, David H. Hughes, Giulia Rodighiero, I. Valtchanov, A. Amblard, Matt J. Jarvis, E. J. Barton, M. Pohlen, P. Andreani, Antonio Cava, Jeff Cooke, A. Verma, G. Lagache, Glenn J. White, Steve Serjeant, Robbie Richard Auld, Jacopo Fritz, Asantha Cooray, Simon Dye, D. J. B. Smith, M. Negrello, S. Buttiglione, Andy Lawrence, L. Leeuw, David Bonfield, Rob Ivison, D. Herranz, Denis Burgarella, David T. Frayer, D. L. Clements, Evanthia Hatziminaoglou, G. de Zotti, Frank Bertoldi, E. Ibar, S. J. Maddox, Lulu Fan, Marcella Massardi, Andrea Lapi, J. González-Nuevo, Maggie A. Thompson, Steve Eales, A. Dariush, G. Danese, Maarten Baes, Loretta Dunne, Enzo Pascale, Pasquale Temi, Joaquin Vieira, Saumyadip Samui, Michał J. Michałowski, Steve Rawlings, E. E. Rigby, Universidad de Cantabria, and Science and Technology Facilities Council (STFC)

Subjects
Submillimeter: general, SAMPLE, Field (physics), SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics, Astronomy & Astrophysics, general [Submillimeter], Settore FIS/05 - Astronomia e Astrofisica, GHZ, VIEW, Atlas (anatomy), medicine, BL Lacertae objects: general, quasars: general, submillimeter: general, Blazar, QB, SKY-SURVEY, COUNTS, Physics, Science & Technology, RADIO, general [BL Lacertae objects], Quasars: general, Astronomy and Astrophysics, Space and Planetary Science, Spectral properties, general [Quasars], BL-LACERTAE OBJECTS, CATALOG, CMB cold spot, 0201 Astronomical And Space Sciences, QUASARS, medicine.anatomical_structure, Physics and Astronomy, Early results, Physical Sciences, astro-ph.CO, Fermi Gamma-ray Space Telescope
Abstract

4 páginas, 2 figuras, 3 tablas.-- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.-- et al., To investigate the poorly constrained sub-mm counts and spectral properties of blazars we searched for these in the Herschel-ATLAS (H-ATLAS) science demonstration phase (SDP) survey catalog. We cross-matched 500 μm sources brighter than 50 mJy with the FIRST radio catalogue. We found two blazars, both previously known. Our study is among the first blind blazar searches at sub-mm wavelengths, i.e., in the spectral regime where little is still known about the blazar SEDs, but where the synchrotron peak of the most luminous blazars is expected to occur. Our early results are consistent with educated extrapolations of lower frequency counts and question indications of substantial spectral curvature downwards and of spectral upturns at mm wavelengths. One of the two blazars is identified with a Fermi/LAT γ-ray source and a WMAP source. The physical parameters of the two blazars are briefly discussed. These observations demonstrate that the H-ATLAS survey will provide key information about the physics of blazars and their contribution to sub-mm counts., Work partially supported by the Italian Space Agency (contract I/016/07/0 “COFIS” and ASI/INAF Agreement I/072/09/0 for the Planck LFI Activity of Phase E2).

Published
2010

36. The Herschel ATLAS

Author

S. Eales, L. Dunne, D. Clements, A. Cooray, G. De Zotti, S. Dye, R. Ivison, M. Jarvis, G. Lagache, S. Maddox, M. Negrello, S. Serjeant, M. A. Thompson, E. Van Kampen, A. Amblard, P. Andreani, M. Baes, A. Beelen, G. J. Bendo, D. Benford, F. Bertoldi, J. Bock, D. Bonfield, A. Boselli, C. Bridge, V. Buat, D. Burgarella, R. Carlberg, A. Cava, P. Chanial, S. Charlot, N. Christopher, P. Coles, L. Cortese, A. Dariush, E. da Cunha, G. Dalton, L. Danese, H. Dannerbauer, S. Driver, J. Dunlop, L. Fan, D. Farrah, D. Frayer, C. Frenk, J. Geach, J. Gardner, H. Gomez, J. González-Nuevo, E. González-Solares, M. Griffin, M. Hardcastle, E. Hatziminaoglou, D. Herranz, D. Hughes, E. Ibar, Woong-Seob Jeong, C. Lacey, A. Lapi, A. Lawrence, M. Lee, L. Leeuw, J. Liske, M. López-Caniego, T. Müller, K. Nandra, P. Panuzzo, A. Papageorgiou, G. Patanchon, J. Peacock, C. Pearson, S. Phillipps, M. Pohlen, C. Popescu, S. Rawlings, E. Rigby, M. Rigopoulou, A. Robotham, G. Rodighiero, A. Sansom, B. Schulz, D. Scott, D. J. B. Smith, B. Sibthorpe, I. Smail, J. Stevens, W. Sutherland, T. Takeuchi, J. Tedds, P. Temi, R. Tuffs, M. Trichas, M. Vaccari, I. Valtchanov, P. van der Werf, A. Verma, J. Vieria, C. Vlahakis, Glenn J. White, and Science and Technology Facilities Council (STFC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), submmilimeter, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, BRIGHT QUASAR SURVEY, NUMBER COUNTS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, instrumentation, DEGREE EXTRAGALACTIC SURVEY, Science & Technology, 010308 nuclear & particles physics, Atlas (topology), Astrophysics::Instrumentation and Methods for Astrophysics, Galaxies, Astronomy and Astrophysics, 1200-MU-M MAMBO SURVEY, STAR-FORMATION HISTORY, Space observatory, Galaxy, 0201 Astronomical And Space Sciences, Space and Planetary Science, Sky, Physical Sciences, GOODS-N FIELD, astro-ph.CO, Square (unit), DIGITAL SKY SURVEY, HIGH-REDSHIFT, STELLAR MASS, UNIVERSE GALAXY SURVEY, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

17 páginas, 11 figuras, 4 tablas.-- El Pdf del artículo es la versión pre-print: arXiv:0910.4279v1.-- et al., The Herschel ATLAS is the largest open-time key project that will be carried out on the Herschel Space Observatory. It will survey 570 deg2 of the extragalactic sky, 4 times larger than all the other Herschel extragalactic surveys combined, in five far-infrared and submillimeter bands. We describe the survey, the complementary multiwavelength data sets that will be combined with the Herschel data, and the six major science programs we are undertaking. Using new models based on a previous submillimeter survey of galaxies, we present predictions of the properties of the ATLAS sources in other wave bands.

Published
2010

37. The AKARI Extragalactic Large Area Survey Towards the North Ecliptic Pole

Author

T. Takagi, Y. Ohyama, H. Matsuhara, T. Wada, S. Oyabu, T. Goto, H. Hanami, C. P. Pearson, S. Serjeant, M. Negrello, G. J. White, H. M. Lee, M. Im, M. Malkan, Victor P. Debattista, and C. C. Popescu

Subjects
Photometry (optics), Physics, Wavelength, Infrared, Star formation, Astronomy, Flux, Ecliptic pole, Astrophysics, Galaxy, Luminosity
Abstract

Large area surveys in the infrared wavelengths have revealed a significant evolution of the star formation activity of the universe in the past. Extragalactic surveys we have conduced with AKARI towards the north ecliptic pole (NEP) are unique, in terms of a comprehensive wavelength coverage from 2 to 24 μm using all 9 photometric bands of the IRC. This includes new wavelength windows for extragalactic surveys, such as 18 μm. We demonstrate that this IRC all‐band photometry is capable of tracing a steep rise in the flux at the blue side of the polycyclic aromatic hydrocarbon (PAH) 6.2 μm emission feature of infrared luminous galaxies at z

Published
2010

38. Herschel-ATLAS: Evolution of the 250 μm luminosity function out to z = 0.5

Author

M. N. Bremer, Aaron S. G. Robotham, L. Leeuw, Ewan Cameron, Steve Eales, Richard J. Tuffs, G. Lagache, J. González-Nuevo, Andrew M. Hopkins, Denis Hill, Maggie A. Thompson, B. Sibthorpe, D. H. P. Jones, Antonio Cava, Haley Louise Gomez, A. Verma, D. J. B. Smith, L. Kelvin, David Bonfield, Simon Dye, Jacopo Fritz, James Dunlop, Asantha Cooray, D. L. Clements, R. G. Sharp, S. Buttiglione, Pasquale Temi, Andrew Blain, S. J. Maddox, Matthew Prescott, D. Herranz, Denis Burgarella, Saumyadip Samui, M. J. Page, I. Valtchanov, Maarten Baes, Michał J. Michałowski, Peder Norberg, H. Parkinson, D. Rigopoulou, Jon Loveday, G. Rodighiero, Steven P. Bamford, Simon P. Driver, M. Pohlen, G. de Zotti, Enzo Pascale, Steve Serjeant, A. Dariush, E. E. Rigby, E. van Kampen, Matt J. Jarvis, P. van der Werf, Douglas Scott, Jonathan P. Gardner, Cristina Popescu, M. Negrello, Ivan K. Baldry, Rob Ivison, Loretta Dunne, John A. Peacock, Robbie Richard Auld, Jochen Liske, M. López-Caniego, David T. Frayer, E. Ibar, Scott M. Croom, A. Amblard, Universidad de Cantabria, and Science and Technology Facilities Council (STFC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), luminosity function, mass function [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: observations, Galaxies: luminosity function, mass function, Large-scale structure of Universe, Astronomy and Astrophysics, Space and Planetary Science, Astronomy & Astrophysics, Luminosity, STAR-FORMATION, Atlas (anatomy), Galaxies: luminosity function, medicine, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), QB, luminosity function [galaxies], Physics, REDSHIFT SURVEY, Science & Technology, RADIO, SUBMILLIMETER LUMINOSITY, IDENTIFICATION, COUNTERPARTS, Galaxy, Redshift, observations [cosmology], GALAXIES, SPITZER, 0201 Astronomical And Space Sciences, medicine.anatomical_structure, Physics and Astronomy, mass function, Mass function, Physical Sciences, astro-ph.CO, Llarge-scale structure of Universe, DEEP-FIELD-SOUTH, large-scale structure of Universe, SKY SURVEY, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

5 páginas, 4 figuras.-- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.-- et al., We have determined the luminosity function of 250 μm-selected galaxies detected in the ~14 deg2 science demonstration region of the Herschel-ATLAS project out to a redshift of z = 0.5. Our findings very clearly show that the luminosity function evolves steadily out to this redshift. By selecting a sub-group of sources within a fixed luminosity interval where incompleteness effects are minimal, we have measured a smooth increase in the comoving 250 μm luminosity density out to z = 0.2 where it is 3.6+1.4-0.9 times higher than the local value., S.D. Acknowledges the UK STFC for support.

Published
2010

39. Herschel-ATLAS: The dust energy balance in the edge-on spiral galaxy UGC 4754

Author

L. Leeuw, C. Vlahakis, J. González-Nuevo, Maarten Baes, Steve Serjeant, M. López-Caniego, G. Rodighiero, Enzo Pascale, David Bonfield, Pasquale Temi, Rob Ivison, S. J. Maddox, G. de Zotti, A. Verma, Antonio Cava, E. Ibar, Robbie Richard Auld, Saumyadip Samui, A. Amblard, George J. Bendo, Dave Frayer, Simon Dye, Michał J. Michałowski, M. Negrello, D. J. B. Smith, S. Buttiglione, A. Dariush, D. Herranz, Steve Eales, E. E. Rigby, Matt J. Jarvis, M. Pohlen, Dimitri A. Gadotti, Loretta Dunne, P. van der Werf, Maggie A. Thompson, Jacopo Fritz, E. da Cunha, Asantha Cooray, Denis Burgarella, G. Lagache, D. L. Clements, and Universidad de Cantabria

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Energy balance, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Atmospheric radiative transfer codes, galaxies [Infrared], ISM [Galaxies], Radiative transfer, Emissivity, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Dust, extinction, QB, Physics, Spiral galaxy, Star formation, extinction, Dust, Astronomy and Astrophysics, Infrared: galaxies, Galaxy, Spire, Galaxies: ISM, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

5 páginas, 3 figuras.-- Herschel is an ESA space observatory with science instruments provided by European-led principal- investigator consortia and with important participation from NASA.-- et al., We use Herschel PACS and SPIRE observations of the edge-on spiral galaxy UGC 4754, taken as part of the H-ATLAS SDP observations, to investigate the dust energy balance in this galaxy. We build detailed SKIRT radiative models based on SDSS and UKIDSS maps and use these models to predict the far-infrared emission. We find that our radiative transfer model underestimates the observed FIR emission by a factor of two to three. Similar discrepancies have been found for other edge-on spiral galaxies based on IRAS, ISO, and SCUBA data. Thanks to the good sampling of the SED at FIR wavelengths, we can rule out an underestimation of the FIR emissivity as the cause for this discrepancy. Instead we support highly obscured star formation that contributes little to the optical extinction as a more probable explanation.

Published
2010

40. The MUNU experiment, general description

Author

A. Tadsen, D. Filippi, H. W. Becker, A. Paic, M. Treichel, Claude Amsler, J. Farine, G. Grgić, F. Mattioli, R. Brissot, C. Barnoux, P. Giarritta, D. Schenker, J.-L. Vuilleumier, J. Busto, G. Gervasio, B. Guerre Chaley, J.F. Cavaignac, M. Avenier, V. Joergens, D.H. Koang, G. Puglierin, C. Broggini, Jean-Luc Vuilleumier, M. Negrello, R. Luescher, A. Stutz, G. Bagieu, D. Lebrun, O. Piovan, F. Ould-Saada, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), and MUNU

Subjects
Physics, Nuclear and High Energy Physics, Time projection chamber, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, Scattering, Detector, Attenuation length, Nuclear reactor, 7. Clean energy, 01 natural sciences, law.invention, Computational physics, Nuclear physics, law, 0103 physical sciences, Electromagnetic shielding, Carbon–fluorine bond, 010306 general physics, Instrumentation, Image resolution
Abstract

We are building a low background detector based on a gas time projection chamber surrounded by an active anti-Compton shielding. The detector will be installed near a nuclear reactor in Bugey for the experimental study of νee− scattering. We give here a general description of the experiment, and an estimate of the expected counting rate and background. The construction of the time projection chamber is described in details. Results of first test measurements concerning the attenuation length and the spatial as well as energy resolution in the CF4 fill gas are reported.

Published
1997

41. GAS AND DUST IN A SUBMILLIMETER GALAXY ATz= 4.24 FROM THEHERSCHELATLAS

Author

A. M. Swinbank, Mark Gurwell, Friedrich Wyrowski, Axel Weiss, Itziar Aretxaga, David H. Hughes, P. van der Werf, R. Blundell, Simon Dye, M. Krips, Pierre Cox, D. J. B. Smith, R. Hopwood, S. Buttiglione, M. Negrello, Robbie Richard Auld, G. de Zotti, Alexandre Beelen, R. Gavazzi, R. Güsten, Dave Frayer, Loretta Dunne, Karl M. Menten, E. Ibar, Matt J. Jarvis, A. Dariush, Maarten Baes, A. Omont, Rob Ivison, Enzo Pascale, Steve Maddox, Stephen Anthony Eales, R. Neri, Jacopo Fritz, Asantha Cooray, Antonio Cava, Helmut Dannerbauer, I. Valtchanov, E. E. Rigby, Michael Pohlen, Pasquale Temi, and Michał J. Michałowski

Subjects
galaxies: active, galaxies: evolution, galaxies: high-redshift, galaxies: individual (ID 141), galaxies: starburst, submillimeter: galaxies, Astronomy and Astrophysics, Space and Planetary Science, Luminous infrared galaxy, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Plateau de Bure Interferometer, Astrophysics, Submillimeter Array, Galaxy, Redshift, law.invention, Telescope, Full width at half maximum, law, Emission spectrum, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report ground-based follow-up observations of the exceptional source, ID141, one the brightest sources detected so far in the H-ATLAS cosmological survey. ID141 was observed using the IRAM 30-meter telescope and Plateau de Bure interferometer (PdBI), the Submillimeter Array (SMA) and the Atacama Pathfinder Experiment (APEX) submillimeter telescope to measure the dust continuum and emission lines of the main isotope of carbon monoxide and carbon ([C I] and [C II]). The detection of strong CO emission lines with the PdBI confirms that ID141 is at high redshift (z=4.243 +/- 0.001). The strength of the continuum and emission lines suggests that ID141 is gravitationally lensed. The width (Delta V (FWHM) ~ 800 km/s}) and asymmetric profiles of the CO and carbon lines indicate orbital motion in a disc or a merger. The properties derived for ID141 are compatible with a ultraluminous (L_FIR ~ 8.5 +/- 0.3 x 10^13/mu_L Lsun, where mu_L is the amplification factor, dense (n ~ 10^4 cm^-3) and warm (T_kin ~ 40K) starburst galaxy, with an estimated star-formation rate of (0.7 to 1.7) x 10^4/mu_L Msun/yr. The carbon emission lines indicate a dense (n ~ 10^4 cm^-3) Photo-Dominated Region, illuminated by a far-UV radiation field a few thousand times more intense than that in our Galaxy. In conclusion, the physical properties of the high-z galaxy, ID141, are remarkably similar to those of local ultraluminous infrared galaxies., To appear in ApJ

Published
2011

43. Exploring Cosmic Origins with CORE: The Instrument

Author

P. de Bernardis, P.A.R. Ade, J.J.A. Baselmans, E.S. Battistelli, A. Benoit, M. Bersanelli, A. Bideaud, M. Calvo, F.J. Casas, M.G. Castellano, A. Catalano, I. Charles, I. Colantoni, F. Columbro, A. Coppolecchia, M. Crook, G. D'Alessandro, M. De Petris, J. Delabrouille, S. Doyle, C. Franceschet, A. Gomez, J. Goupy, S. Hanany, M. Hills, L. Lamagna, J. Macias-Perez, B. Maffei, S. Martin, E. Martinez-Gonzalez, S. Masi, D. McCarthy, A. Mennella, A. Monfardini, F. Noviello, A. Paiella, F. Piacentini, M. Piat, G. Pisano, G. Signorelli, C.Y. Tan, A. Tartari, N. Trappe, S. Triqueneaux, C. Tucker, G. Vermeulen, K. Young, M. Zannoni, A. Achúcarro, R. Allison, E. Artall, M. Ashdown, M. Ballardini, A.J. Banday, R. Banerji, J. Bartlett, N. Bartolo, S. Basak, A. Bonaldi, M. Bonato, J. Borrill, F. Bouchet, F. Boulanger, T. Brinckmann, M. Bucher, C. Burigana, A. Buzzelli, Z.Y. Cai, C.S. Carvalho, A. Challinor, J. Chluba, S. Clesse, G. De Gasperis, G. De Zotti, E. Di Valentino, J.M. Diego, J. Errard, S. Feeney, R. Fernandez-Cobos, F. Finelli, F. Forastieri, S. Galli, R. Génova-Santos, M. Gerbino, J. González-Nuevo, S. Hagstotz, J. Greenslade, W. Handley, C. Hernández-Monteagudo, C. Hervias-Caimapo, E. Hivon, K. Kiiveri, T. Kisner, T. Kitching, M. Kunz, H. Kurki-Suonio, A. Lasenby, M. Lattanzi, J. Lesgourgues, A. Lewis, M. Liguori, V. Lindholm, G. Luzzi, C.J.A.P. Martins, S. Matarrese, A. Melchiorri, J.B. Melin, D. Molinari, P. Natoli, M. Negrello, A. Notari, D. Paoletti, G. Patanchon, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, M. Remazeilles, M. Roman, J.A. Rubiño-Martín, L. Salvati, M. Tomasi, D. Tramonte, T. Trombetti, J. Väliviita, R. Van de Weyjgaert, B. van Tent, V. Vennin, P. Vielva, N. Vittorio, Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), CORE, Hélium : du fondamental aux applications (NEEL - HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Department of Physics, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Sorbonne Universités, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), de Bernardis, P, Ade, P, Baselmans, J, Battistelli, E, Benoit, A, Bersanelli, M, Bideaud, A, Calvo, M, Casas, F, Castellano, M, Catalano, A, Charles, I, Colantoni, I, Columbro, F, Coppolecchia, A, Crook, M, D'Alessandro, G, Petris, M, Delabrouille, J, Doyle, S, Franceschet, C, Gomez, A, Goupy, J, Hanany, S, Hills, M, Lamagna, L, Macias-Perez, J, Maffei, B, Martin, S, Martinez-Gonzalez, E, Masi, S, Mccarthy, D, Mennella, A, Monfardini, A, Noviello, F, Paiella, A, Piacentini, F, Piat, M, Pisano, G, Signorelli, G, Tan, C, Tartari, A, Trappe, N, Triqueneaux, S, Tucker, C, Vermeulen, G, Young, K, Zannoni, M, Achúcarro, A, Allison, R, Artall, E, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Carvalho, C, Challinor, A, Chluba, J, Clesse, S, Gasperis, G, Zotti, G, Valentino, E, Diego, J, Errard, J, Feeney, S, Fernandez-Cobos, R, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Hagstotz, S, Greenslade, J, Handley, W, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lasenby, A, Lattanzi, M, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Martins, C, Matarrese, S, Melchiorri, A, Melin, J, Molinari, D, Natoli, P, Negrello, M, Notari, A, Paoletti, D, Patanchon, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rubiño-Martín, J, Salvati, L, Tomasi, M, Tramonte, D, Trombetti, T, Väliviita, J, de Weyjgaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Subatomique et de Cosmologie ( LPSC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Institut Nanosciences et Cryogénie ( INAC ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), and Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Kinetic inductance detectors, Cosmic microwave background, KINETIC INDUCTANCE DETECTORS, cosmic background radiation: polarization, DUAL-REFLECTOR ANTENNAS, 01 natural sciences, 7. Clean energy, BAND, law.invention, law, CMBR experiments, physics.ins-det, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, QC, QB, CALIBRATION, Physics, COSMIC cancer database, COMBINATIONS, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Polarization (waves), PLANCK, Cardinal point, experimental equipment, astro-ph.CO, CMBR detectors, CMBR experiment, astro-ph.IM, physics - instrumentation and detectors, Astrophysics - Instrumentation and Methods for Astrophysics, CMBR polarization, ination, Astronomy and Astrophysics, CMBR detector, Astrophysics - Cosmology and Nongalactic Astrophysics, PRESCRIBED GEOMETRIC PARAMETERS, CMBR polarisation, Cosmic Vision, Cosmology and Nongalactic Astrophysics (astro-ph.CO), kinetic, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, PRE-LAUNCH STATUS, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, beam: polarization, detector, 010308 nuclear & particles physics, business.industry, beam: width, Polarimeter, PERFORMANCE, WAVELENGTHS, 115 Astronomy, Space science, sensitivity, CMBR detectors, CMBR experiments, CMBR polarisation, inflation, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

PdB acknowledges support from University of Rome La Sapienza (project “Cosmologia di Precisione 2015”) and from the Italian Space Agency (Agreement 2016-019-H.0 “Kinetic Inductance Detectors for Space”). CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). C.H.-M. acknowledges the financial support of the Spanish Ministry of Economy and Competitiveness via I+D project AYA-2015-66211-C2-2-P. GDZ acknowledges the financial support of ASI/INAF agreement n. 2014-024-R.1. J.G.N. acknowledges financial support from the Spanish MINECO for a “Ramon y Cajal” fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER). F.J.C., E.M.-G. and P.V. acknowledge support from the Spanish Ministerio de Econom´ıa y Competitividad project ESP2015-70646- C2-1-R co-financed with EU FEDER funds., De Bernardis, P., Ade, P.A.R., Baselmans, J.J.A., Battistelli, E.S., Benoit, A., Bersanelli, M., Bideaud, A., Calvo, M., Casas, F.J., Castellano, M.G., Catalano, A., Charles, I., Colantoni, I., Columbro, F., Coppolecchia, A., Crook, M., D'Alessandro, G., Petris, M.D., Delabrouille, J., Doyle, S., Franceschet, C., Gomez, A., Goupy, J., Hanany, S., Hills, M., Lamagna, L., Macias-Perez, J., Maffei, B., Martin, S., Martinez-Gonzalez, E., Masi, S., McCarthy, D., Mennella, A., Monfardini, A., Noviello, F., Paiella, A., Piacentini, F., Piat, M., Pisano, G., Signorelli, G., Tan, C.Y., Tartari, A., Trappe, N., Triqueneaux, S., Tucker, C., Vermeulen, G., Young, K., Zannoni, M., Achúcarro, A., Allison, R., Artall, E., Ashdown, M., Ballardini, M., Banday, A.J., Banerji, R., Bartlett, J., Bartolo, N., Basak, S., Bonaldi, A., Bonato, M., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Cai, Z.Y., Carvalho, C.S., Challinor, A., Chluba, J., Clesse, S., Gasperis, G.D., Zotti, G.D., Valentino, E.D., Diego, J.M., Errard, J., Feeney, S., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R., Gerbino, M., González-Nuevo, J., Hagstotz, S., Greenslade, J., Handley, W., Hernández-Monteagudo, C., Hervias-Caimapo, C., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lasenby, A., Lattanzi, M., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Martins, C.J.A.P., Matarrese, S., Melchiorri, A., Melin, J.B., Molinari, D., Natoli, P., Negrello, M., Notari, A., Paoletti, D., Patanchon, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rubiño-Martín, J.A., Salvati, L., Tomasi, M., Tramonte, D., Trombetti, T., Väliviita, J., De Weyjgaert, R.V., Tent, B.V., Vennin, V., Vielva, P., Vittorio, N.

44. High Dense Gas Fraction in Intensely Star-forming Dusty Galaxies.

Author

L. Dunne, I. Oteo, Z-Y. Zhang, R. J. Ivison, S. Bussmann, P. Cox, H. Dannerbauer, S. Eales, M. Negrello, C. Furlanetto, R. Gavazzi, Y. Gao, T. R. Greve, R. Tunnard, R. Neri, D. Riechers, J. Wagg, P. Van der Werf, C. Yang, and A. Omont

Subjects
STAR formation, GALACTIC evolution, REDSHIFT, STARBURSTS, ASTROPHYSICS
Abstract

We present ALMA and VLA observations of the dense molecular gas tracers HCN, HCO+, and HNC in two lensed, high-redshift starbursts selected from the Herschel-ATLAS survey: H-ATLAS J090740.0−004200 (SDP.9, ) and H-ATLAS J091043.1−000321 (SDP.11, ). In SDP.9 we have detected all transitions and also HCN(1–0) and HCO+(1–0). In SDP.11 we have detected HCN(3–2) and HCO+(3–2). The amplification factors for both galaxies have been determined from subarcsecond-resolution CO and dust emission observations carried out with NOEMA and the SMA. The HNC(1–0)/HCN(1–0) line ratio in SDP.9 suggests the presence of photon-dominated regions, as happens in most local (U)LIRGs. The CO, HCN, and HCO+ spectral line energy distribution (SLEDs) of SDP.9 are compatible to those found for many local, IR-bright galaxies, indicating that the molecular gas in local and high-redshift dusty starbursts can have similar excitation conditions. We obtain that the correlation between total IR () and dense line () luminosity in SDP.9 and SDP.11 and local star-forming galaxies can be represented by a single relation. We argue that the scatter of the correlation, together with the lack of sensitive dense molecular gas tracer observations for a homogeneous sample of high-redshift galaxies, prevents us from distinguishing differential trends with redshift. Our results suggest that the intense star formation found in some high-redshift, dusty, luminous starbursts is associated with more massive dense molecular gas reservoirs and higher dense molecular gas fractions. [ABSTRACT FROM AUTHOR]

Published
2017
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45. Herschel and Hubble Study of a Lensed Massive Dusty Starbursting Galaxy at z ∼ 3.

Author

H. Nayyeri, A. Cooray, E. Jullo, D. A. Riechers, T. K. D. Leung, D. T. Frayer, M. A. Gurwell, A. I. Harris, R. J. Ivison, M. Negrello, I. Oteo, S. Amber, A. J. Baker, J. Calanog, C. M. Casey, H. Dannerbauer, G. De Zotti, S. Eales, H. Fu, and M. J. Michałowski

Subjects
STARBURSTS, COSMIC dust, STAR formation, ASTRONOMICAL surveys, SUBMILLIMETER astronomy, STELLAR mass
Abstract

We present the results of combined deep Keck/NIRC2, HST/WFC3 near-infrared, and Herschel far-infrared observations of an extremely star-forming dusty lensed galaxy identified from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS J133542.9+300401). The galaxy is gravitationally lensed by a massive WISE-identified galaxy cluster at z ∼ 1. The lensed galaxy is spectroscopically confirmed at z = 2.685 from detection of by GBT and from detection of obtained with CARMA. We use the combined spectroscopic and imaging observations to construct a detailed model of the background dusty lensed submillimeter galaxy (SMG), which allows us to study the source plane properties of the target. The best-fit lens model provides magnifications of μstar = 2.10 ± 0.11 and μdust = 2.02 ± 0.06 for the stellar and dust components, respectively. Multiband data yield a magnification-corrected star formation rate of 1900(±200) M⊙ yr−1 and a stellar mass of , consistent with a main sequence of star formation at z ∼ 2.6. The CO observations yield a molecular gas mass of 8.3(±1.0) × 1010M⊙, similar to the most massive star-forming galaxies, which together with the high star formation efficiency, are responsible for the intense observed star formation rates. The lensed SMG has a very short gas depletion timescale of ∼40 Myr. The high stellar mass and small gas fractions observed indicate that the lensed SMG likely has already formed most of its stellar mass and could be a progenitor of the most massive elliptical galaxies found in the local universe. [ABSTRACT FROM AUTHOR]

Published
2017
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47. CROSS-CORRELATION BETWEEN THE CMB LENSING POTENTIAL MEASURED BY PLANCK AND HIGH-z SUBMILLIMETER GALAXIES DETECTED BY THE HERSCHEL-ATLAS SURVEY.

Author

F. Bianchini, P. Bielewicz, A. Lapi, J. Gonzalez-Nuevo, C. Baccigalupi, G. de Zotti, L. Danese, N. Bourne, A. Cooray, L. Dunne, S. Dye, S. Eales, R. Ivison, S. Maddox, M. Negrello, D. Scott, M. W. L. Smith, and E. Valiante

Subjects
COSMIC background radiation, ASTROPHYSICAL radiation, METAPHYSICAL cosmology, PLANCK'S constant, PLANCK'S energy
Abstract

We present the first measurement of the correlation between the map of the cosmic microwave background (CMB) lensing potential derived from the Planck nominal mission data and galaxies detected by the Herschel-ATLAS (H-ATLAS) survey covering about , i.e., about 1.4% of the sky. We reject the hypothesis that there is no correlation between CMB lensing and galaxy detection at a significance, checking the result by performing a number of null tests. The significance of the detection of the theoretically expected cross-correlation signal is found to be . The galaxy bias parameter, b, derived from a joint analysis of the cross-power spectrum and of the autopower spectrum of the galaxy density contrast is found to be , consistent with earlier estimates for H-ATLAS galaxies at similar redshifts. On the other hand, the amplitude of the cross-correlation is found to be a factor 1.62 ± 0.16 higher than expected from the standard model and also found by cross-correlation analyses with other tracers of the large-scale structure. The enhancement due to lensing magnification can account for only a fraction of the excess cross-correlation signal. We suggest that part of it may be due to an incomplete removal of the contamination of the cosmic infrared background, which includes the H-ATLAS sources we are cross-correlating with. In any case, the highly significant detection reported here using a catalog covering only 1.4% of the sky demonstrates the potential of CMB lensing correlations with submillimeter surveys. [ABSTRACT FROM AUTHOR]

Published
2015
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49. Purkinje cell models: past, present and future.

Author

Fernández Santoro EM, Karim A, Warnaar P, De Zeeuw CI, Badura A, and Negrello M

Abstract

The investigation of the dynamics of Purkinje cell (PC) activity is crucial to unravel the role of the cerebellum in motor control, learning and cognitive processes. Within the cerebellar cortex (CC), these neurons receive all the incoming sensory and motor information, transform it and generate the entire cerebellar output. The relatively homogenous and repetitive structure of the CC, common to all vertebrate species, suggests a single computation mechanism shared across all PCs. While PC models have been developed since the 70's, a comprehensive review of contemporary models is currently lacking. Here, we provide an overview of PC models, ranging from the ones focused on single cell intracellular PC dynamics, through complex models which include synaptic and extrasynaptic inputs. We review how PC models can reproduce physiological activity of the neuron, including firing patterns, current and multistable dynamics, plateau potentials, calcium signaling, intrinsic and synaptic plasticity and input/output computations. We consider models focusing both on somatic and on dendritic computations. Our review provides a critical performance analysis of PC models with respect to known physiological data. We expect our synthesis to be useful in guiding future development of computational models that capture real-life PC dynamics in the context of cerebellar computations., Competing Interests: The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest. The author(s) declared that they were an editorial board member of Frontiers, at the time of submission. This had no impact on the peer review process and the final decision., (Copyright © 2024 Fernández Santoro, Karim, Warnaar, De Zeeuw, Badura and Negrello.)

Published
2024
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50. How inhibitory and excitatory inputs gate output of the inferior olive.

Author

Loyola S, Hoogland TM, Hoedemaker H, Romano V, Negrello M, and De Zeeuw CI

Subjects
Mice, Animals, Neurons physiology, Purkinje Cells physiology, Cerebellum physiology, Action Potentials physiology, Cerebellar Nuclei, Olivary Nucleus physiology
Abstract

The inferior olive provides the climbing fibers to Purkinje cells in the cerebellar cortex, where they elicit all-or-none complex spikes and control major forms of plasticity. Given their important role in both short-term and long-term coordination of cerebellum-dependent behaviors, it is paramount to understand the factors that determine the output of olivary neurons. Here, we use mouse models to investigate how the inhibitory and excitatory inputs to the olivary neurons interact with each other, generating spiking patterns of olivary neurons that align with their intrinsic oscillations. Using dual color optogenetic stimulation and whole-cell recordings, we demonstrate how intervals between the inhibitory input from the cerebellar nuclei and excitatory input from the mesodiencephalic junction affect phase and gain of the olivary output at both the sub- and suprathreshold level. When the excitatory input is activated shortly (~50 ms) after the inhibitory input, the phase of the intrinsic oscillations becomes remarkably unstable and the excitatory input can hardly generate any olivary spike. Instead, when the excitatory input is activated one cycle (~150 ms) after the inhibitory input, the excitatory input can optimally drive olivary spiking, riding on top of the first cycle of the subthreshold oscillations that have been powerfully reset by the preceding inhibitory input. Simulations of a large-scale network model of the inferior olive highlight to what extent the synaptic interactions penetrate in the neuropil, generating quasi-oscillatory spiking patterns in large parts of the olivary subnuclei, the size of which also depends on the relative timing of the inhibitory and excitatory inputs., Competing Interests: SL, TH, HH, VR, MN, CD No competing interests declared, (© 2023, Loyola, Hoogland et al.)

Published
2023
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