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19 results on '"Dowell CD"'

1. Joint Analysis of BICEP2/Keck Array and Planck Data

Author

Ade, PAR, Aghanim, N, Ahmed, Z, Aikin, RW, Alexander, KD, Arnaud, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barkats, D, Barreiro, RB, Bartlett, JG, Bartolo, N, Battaner, E, Benabed, K, Benoît, A, Benoit-Lévy, A, Benton, SJ, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bischoff, CA, Bock, JJ, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Brevik, JA, Bucher, M, Buder, I, Bullock, E, Burigana, C, Butler, RC, Buza, V, Calabrese, E, Cardoso, J-F, Catalano, A, Challinor, A, Chary, R-R, Chiang, HC, Christensen, PR, Colombo, LPL, Combet, C, Connors, J, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Delouis, J-M, Désert, F-X, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Dowell, CD, Duband, L, Ducout, A, Dunkley, J, Dupac, X, Dvorkin, C, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Falgarone, E, Filippini, JP, Finelli, F, Fliescher, S, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Gjerløw, E, Golwala, SR, González-Nuevo, J, Górski, KM, Gratton, S, Gregorio, A, Gruppuso, A, Gudmundsson, JE, Halpern, M, and Hansen, FK

Subjects
Space Sciences, Physical Sciences, (BICEP2/Keck and Planck Collaborations), astro-ph.CO, gr-qc, hep-ph, hep-th, Mathematical Sciences, Engineering, General Physics, Mathematical sciences, Physical sciences
Abstract

We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400  deg^{2} patch of sky centered on RA 0 h, Dec. -57.5°. The combined maps reach a depth of 57 nK deg in Stokes Q and U in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2  μK deg in Q and U at 143 GHz). We detect 150×353 cross-correlation in B modes at high significance. We fit the single- and cross-frequency power spectra at frequencies ≥150  GHz to a lensed-ΛCDM model that includes dust and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r), using a prior on the frequency spectral behavior of polarized dust emission from previous Planck analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the r constraint. Finally, we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for r, and yields an upper limit r_{0.05}

Published
2015

2. HerMES: Candidate high-redshift galaxies discovered with Herschel/Spire

Author

Dowell, CD, Conley, A, Glenn, J, Arumugam, V, Asboth, V, Aussel, H, Bertoldi, F, Béthermin, M, Bock, J, Boselli, A, Bridge, C, Buat, V, Burgarella, D, Cabrera-Lavers, A, Casey, CM, Chapman, SC, Clements, DL, Conversi, L, Cooray, A, Dannerbauer, H, De Bernardis, F, Ellsworth-Bowers, TP, Farrah, D, Franceschini, A, Griffin, M, Gurwell, MA, Halpern, M, Hatziminaoglou, E, Heinis, S, Ibar, E, Ivison, RJ, Laporte, N, Marchetti, L, Martínez-Navajas, P, Marsden, G, Morrison, GE, Nguyen, HT, O'Halloran, B, Oliver, SJ, Omont, A, Page, MJ, Papageorgiou, A, Pearson, CP, Petitpas, G, Pérez-Fournon, I, Pohlen, M, Riechers, D, Rigopoulou, D, Roseboom, IG, Rowan-Robinson, M, Sayers, J, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Smith, AJ, Streblyanska, A, Symeonidis, M, Vaccari, M, Valtchanov, I, Vieira, JD, Viero, M, Wang, L, Wardlow, J, Xu, CK, and Zemcov, M

Subjects
galaxies: high-redshift, galaxies: starburst, infrared: galaxies, submillimeter: galaxies, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 μm flux densities to search for red sources. We apply this method to 21 deg2 of data from the HerMES survey to produce a catalog of 38 high-z candidates. Follow-up of the first five of these sources confirms that this method is efficient at selecting high-z DSFGs, with 4/5 at z = 4.3-6.3 (and the remaining source at z = 3.4), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e.g., 850 μm) and in single-band surveys, shows that our method is much more efficient at selecting high-z DSFGs, in the sense that a much larger fraction are at z > 3. Correcting for the selection completeness and purity, we find that the number of bright (S 500 μm ≥ 30 mJy), red Herschel sources is 3.3 ± 0.8 deg-2. This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-z DSFGs is similar to that at z ∼ 2, rest-frame UV based studies may be missing a significant component of the star formation density at z = 4-6, even after correction for extinction. © 2014. The American Astronomical Society. All rights reserved.

Published
2014

3. Dust polarized emission observations of NGC 6334

Author

Arzoumanian, D, Furuya, RS, Hasegawa, T, Tahani, M, Sadavoy, S, Hull, CLH, Johnstone, D, Koch, PM, Inutsuka, S, Doi, Y, Hoang, T, Onaka, T, Iwasaki, K, Shimajiri, Y, Inoue, T, Peretto, N, André, P, Bastien, P, Berry, D, Chen, H-RV, Di Francesco, J, Eswaraiah, C, Fanciullo, L, Fissel, LM, Hwang, J, Kang, J-H, Kim, G, Kim, K-T, Kirchschlager, F, Kwon, W, Lee, CW, Liu, H-L, Lyo, A-R, Pattle, K, Soam, A, Tang, X, Whitworth, A, Ching, T-C, Coudé, S, Wang, J-W, Ward-Thompson, D, Lai, S-P, Qiu, K, Bourke, TL, Byun, D-Y, Chen, M, Chen, Z, Chen, WP, Cho, J, Choi, Y, Choi, M, Chrysostomou, A, Chung, EJ, Dai, S, Diep, PN, Duan, H-Y, Duan, Y, Eden, D, Fiege, J, Franzmann, E, Friberg, P, Fuller, G, Gledhill, T, Graves, S, Greaves, J, Griffin, M, Gu, Q, Han, I, Hatchell, J, Hayashi, S, Houde, M, Jeong, I-G, Kang, M, Kang, S-J, Kataoka, A, Kawabata, K, Kemper, F, Kim, M-R, Kim, KH, Kim, J, Kim, S, Kirk, J, Kobayashi, MIN, Könyves, V, Kusune, T, Kwon, J, Lacaille, K, Law, C-Y, Lee, C-F, Lee, Y-H, Lee, S-S, Lee, H, Lee, J-E, Li, H-B, Li, D, Li, DL, Liu, J, Liu, T, Liu, S-Y, Lu, X, Mairs, S, Matsumura, M, Matthews, B, Moriarty-Schieven, G, Nagata, T, Nakamura, F, Nakanishi, H, Ngoc, NB, Ohashi, N, Park, G, Parsons, H, Pyo, T-S, Qian, L, Rao, R, Rawlings, J, Rawlings, M, Retter, B, Richer, J, Rigby, A, Saito, H, Savini, G, Scaife, A, Seta, M, Shinnaga, H, Tamura, M, Tang, Y-W, Tomisaka, K, Tram, LN, Tsukamoto, Y, Viti, S, Wang, H, Xie, J, Yen, H-W, Yoo, H, Yuan, J, Yun, H-S, Zenko, T, Zhang, G, Zhang, C-P, Zhang, Y, Zhou, J, Zhu, L, de Looze, I, Dowell, CD, Eyres, S, Falle, S, Friesen, R, Robitaille, J-F, and van Loo, S

Subjects
Astrophysics::Galaxy Astrophysics
Abstract

Context. Molecular filaments and hubs have received special attention recently thanks to new studies showing their key role in star formation. While the (column) density and velocity structures of both filaments and hubs have been carefully studied, their magnetic field (B-field) properties have yet to be characterized. Consequently, the role of B-fields in the formation and evolution of hub-filament systems is not well constrained. Aims. We aim to understand the role of the B-field and its interplay with turbulence and gravity in the dynamical evolution of the NGC 6334 filament network that harbours cluster-forming hubs and high-mass star formation. Methods. We present new observations of the dust polarized emission at 850 μm toward the 2 pc × 10 pc map of NGC 6334 at a spatial resolution of 0.09 pc obtained with the James Clerk Maxwell Telescope (JCMT) as part of the B-field In STar-forming Region Observations (BISTRO) survey. We study the distribution and dispersion of the polarized intensity (PI), the polarization fraction (PF), and the plane-of-the-sky B-field angle (χB_POS) toward the whole region, along the 10 pc-long ridge and along the sub-filaments connected to the ridge and the hubs. We derived the power spectra of the intensity and χBPOS along the ridge crest and compared them with the results obtained from simulated filaments. Results. The observations span ~3 orders of magnitude in Stokes I and PI and ~2 orders of magnitude in PF (from ~0.2 to ~ 20%). A large scatter in PI and PF is observed for a given value of I. Our analyses show a complex B-field structure when observed over the whole region (~ 10 pc); however, at smaller scales (~1 pc), χBPOS varies coherently along the crests of the filament network. The observed power spectrum of χBPOS can be well represented with a power law function with a slope of − 1.33 ± 0.23, which is ~20% shallower than that of I. We find that this result is compatible with the properties of simulated filaments and may indicate the physical processes at play in the formation and evolution of star-forming filaments. Along the sub-filaments, χBPOS rotates frombeing mostly perpendicular or randomly oriented with respect to the crests to mostly parallel as the sub-filaments merge with the ridge and hubs. This variation of the B-field structure along the sub-filaments may be tracing local velocity flows of infalling matter in the ridge and hubs. Our analysis also suggests a variation in the energy balance along the crests of these sub-filaments, from magnetically critical or supercritical at their far ends to magnetically subcritical near the ridge and hubs. We also detect an increase in PF toward the high-column density (NH2 ≳ 1023 cm−2) star cluster-forming hubs. These latter large PF values may be explained by the increase in grain alignment efficiency due to stellar radiation from the newborn stars, combined with an ordered B-field structure. Conclusions. These observational results reveal for the first time the characteristics of the small-scale (down to ~ 0.1 pc) B-field structure of a 10 pc-long hub-filament system. Our analyses show variations in the polarization properties along the sub-filaments that may be tracing the evolution of their physical properties during their interaction with the ridge and hubs. We also detect an impact of feedback from young high-mass stars on the local B-field structure and the polarization properties, which could put constraints on possible models for dust grain alignment and provide important hints as to the interplay between the star formation activity and interstellar B-fields.

Published
2021

4. The JCMT BISTRO Survey:The Magnetic Field of the Barnard 1 Star-forming Region

Author

Coude, S, Bastien, P, Houde, M, Sadavoy, S, Friesen, R, Di Francesco, J, Johnstone, D, Mairs, S, Hasegawa, T, Kwon, W, Lai, S-P, Qiu, K, Ward-Thompson, D, Berry, D, Chen, MC-Y, Fiege, J, Franzmann, E, Hatchell, J, Lacaille, K, Matthews, BC, Moriarty-Schieven, GH, Pon, A, Andre, P, Arzoumanian, D, Aso, Y, Byun, D-Y, Eswaraiah, C, Chen, H-R, Chen, WP, Ching, T-C, Cho, J, Choi, M, Chrysostomou, A, Chung, EJ, Doi, Y, Drabek-Maunder, E, Dowell, CD, Eyres, SPS, Falle, S, Friberg, P, Fuller, G, Furuya, RS, Gledhill, T, Graves, SF, Greaves, JS, Griffin, MJ, Gu, Q, Hayashi, SS, Hoang, T, Holland, W, Inoue, T, Inutsuka, S-I, Iwasaki, K, Jeong, I-G, Kanamori, Y, Kataoka, A, Kang, J-H, Kang, M, Kang, S-J, Kawabata, KS, Kemper, F, Kim, G, Kim, J, Kim, K-T, Kim, KH, Kim, M-R, Kim, S, Kirk, JM, Kobayashi, MIN, Koch, PM, Kwon, J, Lee, J-E, Lee, CW, Lee, S-S, Li, D, Li, H-B, Liu, H-L, Liu, J, Liu, S-Y, Liu, T, van Loo, S, Lyo, A-R, Matsumura, M, Nagata, T, Nakamura, F, Nakanishi, H, Ohashi, N, Onaka, T, Parsons, H, Pattle, K, Peretto, N, Pyo, T-S, Qian, L, Rao, R, Rawlings, MG, Retter, B, Richer, J, Rigby, A, Robitaille, J-F, Saito, H, Savini, G, Scaife, AMM, Seta, M, Shinnaga, H, Soam, A, Tamura, M, Tang, Y-W, Tomisaka, K, Tsukamoto, Y, Wang, H, Wang, J-W, Whitworth, AP, Yen, H-W, Yoo, H, Yuan, J, Zenko, T, Zhang, C-P, Zhang, G, Zhou, J, Zhu, L, and The BISTRO Collaboration

Subjects
010504 meteorology & atmospheric sciences, INFRARED POLARIMETRY, RADIATIVE TORQUES, FOS: Physical sciences, Astrophysics, F500, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, 01 natural sciences, ISM: clouds, MOLECULAR, 0103 physical sciences, POLARIZATION MEASUREMENTS, SCUBA-2, GOULD BELT SURVEY, ISM: individual objects (Barnard 1), individual objects (Barnard 1) [ISM], ISM [submillimeter], 010303 astronomy & astrophysics, James Clerk Maxwell Telescope, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, LINEAR-POLARIZATION, polarization, stars: formation, formation [stars], Magnetic energy, Linear polarization, Molecular cloud, F510, CLOUDS, magnetic fields [ISM], Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, H2O MASERS, Magnetic field, ALIGNMENT, Amplitude, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, ISM: magnetic fields, INTERSTELLAR GRAINS, clouds [ISM]
Abstract

著者人数: The B-fields In STar-forming Regions Observations (BISTRO) Collaboration 121名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 權, 靜美), Number of authors: The B-fields In STar-forming Regions Observations (BISTRO) Collaboration 121 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Kwon, Jungmi), Accepted: 2019-04-18, 資料番号: SA1190042000

Published
2019

5. The Herschel Multi-Tiered Extragalactic Survey: source extraction and cross-identifications in confusion-dominated SPIRE images

Author

Roseboom, IG, Oliver, SJ, Kunz, M, Altieri, B, Amblard, A, Arumugam, V, Auld, R, Aussel, H, Babbedge, T, Bethermin, M, Blain, A, Bock, J, Boselli, A, Brisbin, D, Buat, V, Burgarella, D, Castro-Rodriguez, N, Cava, A, Chanial, P, Chapin, E, Clements, DL, Conley, A, Conversi, L, Cooray, A, Dowell, CD, Dwek, E, Dye, S, Eales, S, Elbaz, D, Farrah, D, Fox, M, Franceschini, A, Gear, W, Glenn, J, Solares, EAG, Griffin, M, Halpern, M, Harwit, M, Hatziminaoglou, E, Huang, J, Ibar, E, Isaak, K, Ivison, RJ, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Marsden, G, Mortier, AMJ, Nguyen, HT, O'Halloran, B, Omont, A, Page, MJ, Panuzzo, P, Papageorgiou, A, Patel, H, Pearson, CP, Perez-Fournon, I, Pohlen, M, Rawlings, JI, Raymond, G, Rigopoulou, D, Rizzo, D, Rowan-Robinson, M, Sanchez Portal, M, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Smith, AJ, Stevens, JA, Symeonidis, M, Trichas, M, Tugwell, KE, Vaccari, M, Valtchanov, I, Vieira, JD, Vigroux, L, Wang, L, Ward, R, Wright, G, Xu, CK, Zemcov, M, 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), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the cross-identification and source photometry techniques used to process Herschel SPIRE imaging taken as part of the Herschel Multi-Tiered Extragalactic Survey (HerMES). Cross-identifications are performed in map-space so as to minimise source blending effects. We make use of a combination of linear inversion and model selection techniques to produce reliable cross-identification catalogues based on Spitzer MIPS 24 micron source positions. Testing on simulations and real Herschel observations show that this approach gives robust results for even the faintest sources S250~10 mJy. We apply our new technique to HerMES SPIRE observations taken as part of the science demostration phase of Herschel. For our real SPIRE observations we show that, for bright unconfused sources, our flux density estimates are in good agreement with those produced via more traditional point source detection methods (SussExtractor; Savage & Oliver et al. 2006) by Smith et al. 2010. When compared to the measured number density of sources in the SPIRE bands, we show that our method allows the recovery of a larger fraction of faint sources than these traditional methods. However this completeness is heavily dependant on the relative depth of the existing 24 micron catalogues and SPIRE imaging. Using our deepest multi-wavelength dataset in GOODS-N, we estimate that the use of shallow 24 micron in our other fields introduces an incompleteness at faint levels of between 20-40 per cent at 250 micron., Accepted for publication in MNRAS, 19 pages, 11 figures

Published
2017

6. First Results From BISTRO - A Scuba-2 Polarimeter Survey Of The Gould Belt

Author

Ward-Thompson, D, Pattle, K, Bastien, P, Furuya, RS, Kwon, W, Lai, S-P, Qiu, K, Berry, D, Choi, M, Coude, S, Di Fransesco, J, Hoang, T, Franzmann, E, Friberg, P, Graves, S, Houde, M, Johnstone, D, Kirk, JM, Koch, PM, Kwon, J, Won Lee, C, Li, D, Matthews, BC, Mottram, JC, Parsons, H, Pon, A, Rao, R, Rawlings, M, Shinnaga, H, Sadavoy, S, Van Loo, S, Aso, Y, Byun, D-Y, Chakali, E, Chen, H-R, Chen, MC-Y, Chen, WP, Ching, T-C, Cho, J, Chrysostomou, A, Chung, EJ, Doi, Y, Drabek-Maunder, E, Eyres, SPS, Fiege, J, Friesen, RK, Fuller, G, Gledhill, T, Griffin, MJ, Gu, Q, Hasegawa, T, Hatchell, J, Hayashi, SS, Holland, W, Inoue, T, Inutsuka, S-I, Iwasaki, K, Jeong, I-G, Kang, J-H, Kang, M, Kang, S-J, Kawabata, KS, Kemper, F, Kim, G, Kim, J, Kim, K-T, Kim, KH, Kim, M-R, Kim, S, Lacaille, KM, Lee, J-E, Lee, S-S, Li, H-B, Liu, H-L, Liu, J, Liu, S-Y, Liu, T, Lyo, A-R, Mairs, S, Matsumura, M, Moriarty-Schieven, GH, Nakamura, F, Nakanishi, H, Ohashi, N, Onaka, T, Peretto, N, Pyo, T-S, Qian, L, Retter, B, Richer, J, Rigby, A, Robitaille, J-F, Savini, G, Scaife, AMM, Soam, A, Tamura, M, Tang, Y-W, Tomisaka, K, Wang, H, Wang, J-W, Withworth, AP, Yen, H-W, Yoo, H, Yuan, J, Zhang, C-P, Zhang, G, Zhou, J, Zhu, L, Andre, P, Dowell, CD, Falle, SAEG, and Tsukamoto, Y

Abstract

We present the rst results from the B- elds In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array 2 (SCUBA-2) camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope (JCMT) in Hawaii. We discuss the survey's aims and objectives. We describe the rationale behind the survey, and the questions which the survey will aim to answer. The most important of these is the role of magnetic fields in the star formation process on the scale of individual filaments and cores in dense regions. We describe the data acquisition and reduction processes for POL-2, demonstrating both repeatability and consistency with previous data. We present a first-look analysis of the rst results from the BISTRO survey in the OMC 1 region. We see that the magnetic field lies approximately perpendicular to the famous `integral filament' in the densest regions of that filament. Furthermore, we see an `hour-glass' magnetic field morphology extending beyond the densest region of the integral filament into the less-dense surrounding material, and discuss possible causes for this. We also discuss the more complex morphology seen along the Orion Bar region. We examine the morphology of the field along the lower-density north-eastern filament. We find consistency with previous theoretical models that predict magnetic fields lying parallel to low-density, non-self-gravitating filaments, and perpendicular to higher-density, self-gravitating filaments.

Published
2017

7. Erratum to The herschel* pep/hermes luminosity function - i. probing the evolution of PACS selected galaxies to z ̃ 4 [MNRAS 436, (2013) 2875-2876]

Author

Gruppioni, C, Pozzi, F, Rodighiero, G, Delvecchio, I, Berta, S, Pozzetti, L, Zamorani, G, Andreani, P, Cimatti, A, Ilbert, O, Le Floc'h, E, Lutz, D, Magnelli, B, Marchetti, L, Monaco, L, Nordon, R, Oliver, S, Popesso, P, Riguccini, L, Roseboom, I, Rosario, DJ, Sargent, M, Vaccari, M, Altieri, B, Aussel, H, Bongiovanni, A, Cepa, J, Daddi, E, Doḿlnguez-Śanchez, H, Elbaz, D, F̈orster Schreiber, N, Genzel, R, Iribarrem, A, Magliocchetti, M, Maiolino, R, Poglitsch, A, Ṕerez Garćla, A, Sanchez-Portal, M, Sturm, E, Tacconi, L, Valtchanov, I, Amblard, A, Arumugam, V, Bethermin, M, Bock, J, Boselli, A, Buat, V, Burgarella, D, Castro-Rodŕlguez, N, Cava, A, Chania, P, Clements, DL, Conley, A, Cooray, A, Dowell, CD, Dwek, E, Eales, S, Franceschini, A, Glenn, J, Griffin, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, RJ, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Nguyen, HT, O'Halloran, B, Page, MJ, Panuzzo, P, Papageorgiou, A, Pearson, CP, Ṕerez-Fournon, I, Pohlen, M, Rigopoulou, D, Rowan-Robinson, M, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Smith, AJ, Stevens, JA, Symeonidis, M, Trichas, M, Tugwell, KE, Vigroux, L, Wang, L, Wright, G, Xu, CK, Zemcov, M, Bardelli, S, Carollo, M, Contini, T, Le F́evre, O, Lilly, S, Mainieri, V, Renzini, A, Scodeggio, M, and Zucca, E

Published
2013

8. The Herschel PEP/HerMES Luminosity Function - I. Probing the Evolution of PACS selected Galaxies to z similar or equal to 4 (vol 432, pg 23, 2013)

Author

Gruppioni, C, Pozzi, F, Rodighiero, G, Delvecchio, I, Berta, S, Pozzetti, L, Zamorani, G, Andreani, P, Cimatti, A, Ilbert, O, Le Floc'h, E, Lutz, D, Magnelli, B, Marchetti, L, Monaco, P, Nordon, R, Oliver, S, Popesso, P, Riguccini, L, Roseboom, I, Rosario, DJ, Sargent, M, Vaccari, M, Altieri, B, Aussel, H, Bongiovanni, A, Cepa, J, Daddi, E, Dominguez-Sanchez, H, Elbaz, D, Schreiber, NF, Genzel, R, Iribarrem, A, Magliocchetti, M, Maiolino, R, Poglitsch, A, Garcia, AP, Sanchez-Portal, M, Sturm, E, Tacconi, L, Valtchanov, I, Amblard, A, Arumugam, V, Bethermin, M, Bock, J, Boselli, A, Buat, V, Burgarella, D, Castro-Rodriguez, N, Cava, A, Chanial, P, Clements, DL, Conley, A, Cooray, A, Dowell, CD, Dwek, E, Eales, S, Franceschini, A, Glenn, J, Griffin, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, RJ, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Nguyen, HT, O'Halloran, B, Page, MJ, Panuzzo, P, Papageorgiou, A, Pearson, CP, Perez-Fournon, I, Pohlen, M, Rigopoulou, D, Rowan-Robinson, M, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Smith, AJ, Stevens, JA, Symeonidis, M, Trichas, M, Tugwell, KE, Vigroux, L, Wang, L, Wright, G, Xu, CK, Zemcov, M, Bardelli, S, Carollo, M, Contini, T, Le Fevre, O, Lilly, S, Mainieri, V, Renzini, A, Scodeggio, M, and Zucca, E

Published
2013

9. The Herschel Multi-tiered Extragalactic Survey: HerMES

Author

Oliver, SJ, Bock, J, Altieri, B, Amblard, A, Arumugam, V, Aussel, H, Babbedge, T, Beelen, A, Béthermin, M, Blain, A, Boselli, A, Bridge, C, Brisbin, D, Buat, V, Burgarella, D, Castro-Rodríguez, N, Cava, A, Chanial, P, Cirasuolo, M, Clements, DL, Conley, A, Conversi, L, Cooray, A, Dowell, CD, Dubois, EN, Dwek, E, Dye, S, Eales, S, Elbaz, D, Farrah, D, Feltre, A, Ferrero, P, Fiolet, N, Fox, M, Franceschini, A, Gear, W, Giovannoli, E, Glenn, J, Gong, Y, González Solares, EA, Griffin, M, Halpern, M, Harwit, M, Hatziminaoglou, E, Heinis, S, Hurley, P, Hwang, HS, Hyde, A, Ibar, E, Ilbert, O, Isaak, K, Ivison, RJ, Lagache, G, Le Floc'h, E, Levenson, L, Faro, BL, Lu, N, Madden, S, Maffei, B, Magdis, G, Mainetti, G, Marchetti, L, Marsden, G, Marshall, J, Mortier, AMJ, Nguyen, HT, O'Halloran, B, Omont, A, Page, MJ, Panuzzo, P, Papageorgiou, A, Patel, H, Pearson, CP, Pérez-Fournon, I, Pohlen, M, Rawlings, JI, Raymond, G, Rigopoulou, D, Riguccini, L, Rizzo, D, Rodighiero, G, Roseboom, IG, and Rowan-Robinson, M

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling ~380deg 2. Fields range in size from 0.01 to ~20deg 2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500μm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160μm), with an additional wider component of 270deg 2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. The survey will detect of the order of 100000 galaxies at 5σ in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results. © 2012 The Authors. Monthly Notices of the Royal Astronomical Society © 2012 RAS.

Published
2012

10. First results from HerMES on the evolution of the submillimetre luminosity function

Author

Simon Dye, Bruno Altieri, V. Buat, Walter Kieran Gear, Antonio Cava, Rob Ivison, S. C. Madden, Jamie Stevens, C. D. Dowell, N. Castro-Rodriguez, Tom Babbedge, Asantha Cooray, Angela M. J. Mortier, A. Boselli, Robbie Richard Auld, D. Elbaz, G. E. Morrison, Robyn L. Ward, Andrew Blain, Nick Seymour, Gwenifer Raymond, K. Xu, Michael Pohlen, Duncan Farrah, L. Vigroux, Frazer N. Owen, Dimitra Rigopoulou, Isaac Roseboom, Lucia Marchetti, I. Perez-Fournon, Maurilio Pannella, Michael Rowan-Robinson, E. Dwek, David L. Shupe, G. Mainetti, Luca Conversi, D. Rizzo, Matthew Joseph Griffin, K. E. Tugwell, H. Aussel, V. Arumugam, Stephen Anthony Eales, Chris Pearson, A. Conley, Lingyu Wang, M. Trichas, M. Sanchez Portal, Douglas Scott, M. J. Page, Alberto Franceschini, Evanthia Hatziminaoglou, Denis Burgarella, M. Fox, Edo Ibar, Bruno Maffei, A. Amblard, Mattia Vaccari, V. Strazzullo, Michael Zemcov, P. Chanial, J. J. Bock, L. R. Levenson, Hien Nguyen, Nanyao Y. Lu, M. Symeonidis, Benjamin L. Schulz, David L. Clements, Drew Brisbin, Jason Glenn, Gillian S. Wright, Andreas Papageorgiou, C. J. Lonsdale, J.-S. Huang, P. Panuzzo, Seb Oliver, A. Omont, B. O'Halloran, I. Valtchanov, Martin Harwit, A. J. Smith, E. A. González Solares, Jonathan Rawlings, K. G. Isaak, Guilaine Lagache, Eales, Sa, Raymond, G, Roseboom, Ig, Altieri, B, Amblard, A, Arumugam, V, Auld, R, Aussel, H, Babbedge, T, Blain, A, Bock, J, Boselli, A, Brisbin, D, Buat, V, Burgarella, D, Castro-Rodriguez, N, Cava, A, Chanial, P, Clements, Dl, Conley, A, Conversi, L, Cooray, A, Dowell, Cd, Dwek, E, Dye, S, Elbaz, D, Farrah, D, Fox, M, Franceschini, A, Gear, W, Glenn, J, Solares, Eag, Griffin, M, Harwit, M, Hatziminaoglou, E, Huang, J, Ibar, E, Isaak, K, Ivison, Rj, Lagache, G, Levenson, L, Lonsdale, Cj, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Morrison, Ge, Mortier, Amj, Nguyen, Ht, O'Halloran, B, Oliver, Sj, Omont, A, Owen, Fn, Page, Mj, Pannella, M, Panuzzo, P, Papageorgiou, A, Pearson, Cp, Perez-Fournon, I, Pohlen, M, Rawlings, Ji, Rigopoulou, D, Rizzo, D, Rowan-Robinson, M, Portal, M, Schulz, B, Scott, D, Seymour, N, Shupe, Dl, Smith, Aj, Stevens, Ja, Strazzullo, V, Symeonidis, M, Trichas, M, Tugwell, Ke, Vaccari, M, Valtchanov, I, Vigroux, L, Wang, L, Ward, R, Wright, G, Xu, Ck, Zemcov, M, Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, submillimeter: galaxies, Spiral galaxy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Significant part, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Spire, Stars, Space and Planetary Science, galaxies: high-redshift, [SDU]Sciences of the Universe [physics], galaxies: formation, Astrophysics::Earth and Planetary Astrophysics, galaxies: evoluton, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have carried out two extremely deep surveys with SPIRE, one of the two cameras on Herschel, at 250 microns, close to the peak of the far-infrared background. We have used the results to investigate the evolution of the rest-frame 250-micron luminosity function out to z=2. We find evidence for strong evolution out to a redshift of around 1 but evidence for at most weak evolution beyond this redshift. Our results suggest that a significant part of the stars and metals in the Universe today were formed at z, Astronomy and Astrophysics, Herschel Special Issue, in press as a Letter; 5 pages

Published
2016

11. Herschel reveals a T-dust-unbiased selection of z similar to 2 ultraluminous infrared galaxies

Author

Magdis, G. E., Elbaz, D., Hwang, H. S., Amblard, A., Arumugam, V., Aussel, H., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodriguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Farrah, D., Franceschini, A., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Huang, J., Ibar, E., Isaak, K., Le Floc'H, E., Lagache, Guilaine, Levenson, L., Lonsdale, C. J., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Owen, F. N., Page, M. J., Pannella, M., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Rizzo, D., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Strazzullo, V., Symeonidis, M., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vigroux, L., Wang, L., Wright, Gavin, Xu, C. K., Zemcov, M., 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), Magdis, Ge, Elbaz, D, Hwang, H, Amblard, A, Arumugam, V, Aussel, H, Blain, A, Bock, J, Boselli, A, Buat, V, Castro-Rodriguez, N, Cava, A, Chanial, P, Clements, Dl, Conley, A, Conversi, L, Cooray, A, Dowell, Cd, Dwek, E, Eales, S, Farrah, D, Franceschini, A, Glenn, J, Griffin, M, Halpern, M, Hatziminaoglou, E, Huang, J, Ibar, E, Isaak, K, Le Floc'h, E, Lagache, G, Levenson, L, Lonsdale, Cj, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Morrison, Ge, Nguyen, Ht, O'Halloran, B, Oliver, Sj, Omont, A, Owen, Fn, Page, Mj, Pannella, M, Panuzzo, P, Papageorgiou, A, Pearson, Cp, Perez-Fournon, I, Pohlen, M, Rigopoulou, D, Rizzo, D, Roseboom, Ig, Rowan-Robinson, M, Schulz, B, Scott, D, Seymour, N, Shupe, Dl, Smith, Aj, Stevens, Ja, Strazzullo, V, Symeonidis, M, Trichas, M, Tugwell, Ke, Vaccari, M, Valtchanov, I, Vigroux, L, Wang, L, Wright, G, Xu, Ck, and Zemcov, M

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract

International audience; Using Herschel Photodetector Array Camera (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) observations of Lockman Hole-North and Great Observatories Origins Deep Survey-North (GOODS-N) as part of the Herschel Multi-tiered Extragalactic Survey (HerMES) project, we explore the far-infrared (IR) properties of a sample of mid-IR-selected starburst-dominated ultraluminous infrared galaxies (ULIRGs) at z similar to 2. The selection of the sample is based on the detection of the stellar bump that appears in the spectral energy distribution of star-forming galaxies at 1.6 mu m. We derive robust estimates of infrared luminosities (L-IR) and dust temperatures (T-d) of the population and find that while the luminosities in our sample span less than an order of magnitude (12.24 \textless= log(L-IR/L-circle dot) \textless= 12.94), they cover a wide range of dust temperatures (25 \textless= T-d \textless= 62 K). Galaxies in our sample range from those that are as cold as high-z submillimetre galaxies (SMGs) to those that are as warm as optically faint radio galaxies (OFRGs) and local ULIRGs. Nevertheless, our sample has median T-d = 42.3 K, filling the gap between SMGs and OFRGs, bridging the two populations. We demonstrate that a significant fraction of our sample would be missed from ground-based (sub) mm surveys (850-1200 mu m), showing that the latter introduce a bias towards the detection of colder sources. We conclude that Herschel observations confirm the existence of high-z ULIRGs warmer than SMGs, show that the mid-IR selection of high-z ULIRGs is not T-d dependent, reveal a large dispersion in T-d of high-z ULIRGs and provide the means to characterize the bulk of the ULIRG population, free from selection biases introduced by ground-based (sub) mm surveys.

Published
2010

12. The Deep SPIRE HerMES Survey: spectral energy distributions and their astrophysical indications at high redshift

Author

Brisbin, D., Harwit, M., Altieri, B., Amblard, A., Arumugam, V., Aussel, H., Babbedge, T., Blain, A., Bock, J., Boselli, A., Buat, V., Castro-Rodriguez, N., Cava, A., Chanial, P., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Elbaz, D., Fox, M., Franceschini, A., Gear, W., Glenn, J., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, Guilaine, Levenson, L., Lonsdale, Carol J., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Owen, F. N., Pannella, M., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rizzo, D., Roseboom, I. G., Rowan-Robinson, M., Sanchez Portal, M., Schulz, B., Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Strazzullo, V., Symeonidis, M., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vigroux, L., Wang, L., Ward, R., Wright, Gavin, Xu, C. K., Zemcov, M., 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), Brisbin, D, Harwit, M, Altieri, B, Amblard, A, Arumugam, V, Aussel, H, Babbedge, T, Blain, A, Bock, J, Boselli, A, Buat, V, Castro-Rodriguez, N, Cava, A, Chanial, P, Clements, Dl, Conley, A, Conversi, L, Cooray, A, Dowell, Cd, Dwek, E, Eales, S, Elbaz, D, Fox, M, Franceschini, A, Gear, W, Glenn, J, Griffin, M, Halpern, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, Rj, Lagache, G, Levenson, L, Lonsdale, Cj, Lu, N, Madden, S, Maffei, B, Mainetti, G, Marchetti, L, Morrison, Ge, Nguyen, Ht, O'Halloran, B, Oliver, Sj, Omont, A, Owen, Fn, Pannella, M, Panuzzo, P, Papageorgiou, A, Pearson, Cp, Perez-Fournon, I, Pohlen, M, Rizzo, D, Roseboom, Ig, Rowan-Robinson, M, Portal, M, Schulz, B, Seymour, N, Shupe, Dl, Smith, Aj, Stevens, Ja, Strazzullo, V, Symeonidis, M, Trichas, M, Tugwell, Ke, Vaccari, M, Valtchanov, I, Vigroux, L, Wang, L, Ward, R, Wright, G, Xu, Ck, and Zemcov, M

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Spectral and Photometric Imaging Receiver (SPIRE) on Herschel has been carrying out deep extragalactic surveys, one of whose aims is to establish spectral energy distributions (SED)s of individual galaxies spanning the infrared/submillimeter (IR/SMM) wavelength region. We report observations of the (IR/SMM) emission from the Lockman North field (LN) and Great Observatories Origins Deep Survey field North (GOODS-N). Because galaxy images in the wavelength range covered by Herschel generally represent a blend with contributions from neighboring galaxies, we present sets of galaxies in each field especially free of blending at 250, 350, and 500 microns. We identify the cumulative emission of these galaxies and the fraction of the far infrared cosmic background radiation they contribute. Our surveys reveal a number of highly luminous galaxies at redshift z ~< 3 and a novel relationship between infrared and visible emission that shows a dependence on luminosity and redshift., 9 pages, 3 large tables, 2 tables in text, 5 figures Accepted for publication in MNRAS

Published
2010

13. Detection of B-mode polarization at degree angular scales by BICEP2.

Author

Ade PA, Aikin RW, Barkats D, Benton SJ, Bischoff CA, Bock JJ, Brevik JA, Buder I, Bullock E, Dowell CD, Duband L, Filippini JP, Fliescher S, Golwala SR, Halpern M, Hasselfield M, Hildebrandt SR, Hilton GC, Hristov VV, Irwin KD, Karkare KS, Kaufman JP, Keating BG, Kernasovskiy SA, Kovac JM, Kuo CL, Leitch EM, Lueker M, Mason P, Netterfield CB, Nguyen HT, O'Brient R, Ogburn RW 4th, Orlando A, Pryke C, Reintsema CD, Richter S, Schwarz R, Sheehy CD, Staniszewski ZK, Sudiwala RV, Teply GP, Tolan JE, Turner AD, Vieregg AG, Wong CL, and Yoon KW

Abstract

We report results from the BICEP2 experiment, a cosmic microwave background (CMB) polarimeter specifically designed to search for the signal of inflationary gravitational waves in the B-mode power spectrum around ℓ∼80. The telescope comprised a 26 cm aperture all-cold refracting optical system equipped with a focal plane of 512 antenna coupled transition edge sensor 150 GHz bolometers each with temperature sensitivity of ≈300  μK(CMB)√s. BICEP2 observed from the South Pole for three seasons from 2010 to 2012. A low-foreground region of sky with an effective area of 380 square deg was observed to a depth of 87 nK deg in Stokes Q and U. In this paper we describe the observations, data reduction, maps, simulations, and results. We find an excess of B-mode power over the base lensed-ΛCDM expectation in the range 30 < ℓ < 150, inconsistent with the null hypothesis at a significance of >5σ. Through jackknife tests and simulations based on detailed calibration measurements we show that systematic contamination is much smaller than the observed excess. Cross correlating against WMAP 23 GHz maps we find that Galactic synchrotron makes a negligible contribution to the observed signal. We also examine a number of available models of polarized dust emission and find that at their default parameter values they predict power ∼(5-10)× smaller than the observed excess signal (with no significant cross-correlation with our maps). However, these models are not sufficiently constrained by external public data to exclude the possibility of dust emission bright enough to explain the entire excess signal. Cross correlating BICEP2 against 100 GHz maps from the BICEP1 experiment, the excess signal is confirmed with 3σ significance and its spectral index is found to be consistent with that of the CMB, disfavoring dust at 1.7σ. The observed B-mode power spectrum is well fit by a lensed-ΛCDM+tensor theoretical model with tensor-to-scalar ratio r = 0.20&#95;(-0.05)(+0.07), with r = 0 disfavored at 7.0σ. Accounting for the contribution of foreground, dust will shift this value downward by an amount which will be better constrained with upcoming data sets.

Published
2014
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14. A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34.

Author

Riechers DA, Bradford CM, Clements DL, Dowell CD, Pérez-Fournon I, Ivison RJ, Bridge C, Conley A, Fu H, Vieira JD, Wardlow J, Calanog J, Cooray A, Hurley P, Neri R, Kamenetzky J, Aguirre JE, Altieri B, Arumugam V, Benford DJ, Béthermin M, Bock J, Burgarella D, Cabrera-Lavers A, Chapman SC, Cox P, Dunlop JS, Earle L, Farrah D, Ferrero P, Franceschini A, Gavazzi R, Glenn J, Solares EA, Gurwell MA, Halpern M, Hatziminaoglou E, Hyde A, Ibar E, Kovács A, Krips M, Lupu RE, Maloney PR, Martinez-Navajas P, Matsuhara H, Murphy EJ, Naylor BJ, Nguyen HT, Oliver SJ, Omont A, Page MJ, Petitpas G, Rangwala N, Roseboom IG, Scott D, Smith AJ, Staguhn JG, Streblyanska A, Thomson AP, Valtchanov I, Viero M, Wang L, Zemcov M, and Zmuidzinas J

Abstract

Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts--that is, increased rates of star formation--in the most massive dark-matter haloes at early epochs. However, it remains unknown how soon after the Big Bang massive starburst progenitors exist. The measured redshift (z) distribution of dusty, massive starbursts has long been suspected to be biased low in z owing to selection effects, as confirmed by recent findings of systems with redshifts as high as ~5 (refs 2-4). Here we report the identification of a massive starburst galaxy at z = 6.34 through a submillimetre colour-selection technique. We unambiguously determined the redshift from a suite of molecular and atomic fine-structure cooling lines. These measurements reveal a hundred billion solar masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at least 40 per cent of the baryonic mass. A 'maximum starburst' converts the gas into stars at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoch. Despite the overall downturn in cosmic star formation towards the highest redshifts, it seems that environments mature enough to form the most massive, intense starbursts existed at least as early as 880 million years after the Big Bang.

Published
2013
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15. The suppression of star formation by powerful active galactic nuclei.

Author

Page MJ, Symeonidis M, Vieira JD, Altieri B, Amblard A, Arumugam V, Aussel H, Babbedge T, Blain A, Bock J, Boselli A, Buat V, Castro-Rodríguez N, Cava A, Chanial P, Clements DL, Conley A, Conversi L, Cooray A, Dowell CD, Dubois EN, Dunlop JS, Dwek E, Dye S, Eales S, Elbaz D, Farrah D, Fox M, Franceschini A, Gear W, Glenn J, Griffin M, Halpern M, Hatziminaoglou E, Ibar E, Isaak K, Ivison RJ, Lagache G, Levenson L, Lu N, Madden S, Maffei B, Mainetti G, Marchetti L, Nguyen HT, O'Halloran B, Oliver SJ, Omont A, Panuzzo P, Papageorgiou A, Pearson CP, Pérez-Fournon I, Pohlen M, Rawlings JI, Rigopoulou D, Riguccini L, Rizzo D, Rodighiero G, Roseboom IG, Rowan-Robinson M, Sánchez Portal M, Schulz B, Scott D, Seymour N, Shupe DL, Smith AJ, Stevens JA, Trichas M, Tugwell KE, Vaccari M, Valtchanov I, Viero M, Vigroux L, Wang L, Ward R, Wright G, Xu CK, and Zemcov M

Abstract

The old, red stars that constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accretion onto black holes. It is widely suspected, but unproved, that the tight correlation between the mass of the black hole and the mass of the stellar bulge results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, whereas powerful star-forming galaxies are usually dust-obscured and are brightest at infrared and submillimetre wavelengths. Here we report submillimetre and X-ray observations that show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10(44) ergs per second. This suppression of star formation in the host galaxy of a powerful AGN is a key prediction of models in which the AGN drives an outflow, expelling the interstellar medium of its host and transforming the galaxy's properties in a brief period of cosmic time.

Published
2012
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16. Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 10(11) solar masses.

Author

Amblard A, Cooray A, Serra P, Altieri B, Arumugam V, Aussel H, Blain A, Bock J, Boselli A, Buat V, Castro-Rodríguez N, Cava A, Chanial P, Chapin E, Clements DL, Conley A, Conversi L, Dowell CD, Dwek E, Eales S, Elbaz D, Farrah D, Franceschini A, Gear W, Glenn J, Griffin M, Halpern M, Hatziminaoglou E, Ibar E, Isaak K, Ivison RJ, Khostovan AA, Lagache G, Levenson L, Lu N, Madden S, Maffei B, Mainetti G, Marchetti L, Marsden G, Mitchell-Wynne K, Nguyen HT, O'Halloran B, Oliver SJ, Omont A, Page MJ, Panuzzo P, Papageorgiou A, Pearson CP, Pérez-Fournon I, Pohlen M, Rangwala N, Roseboom IG, Rowan-Robinson M, Portal MS, Schulz B, Scott D, Seymour N, Shupe DL, Smith AJ, Stevens JA, Symeonidis M, Trichas M, Tugwell K, Vaccari M, Valiante E, Valtchanov I, Vieira JD, Vigroux L, Wang L, Ward R, Wright G, Xu CK, and Zemcov M

Abstract

The extragalactic background light at far-infrared wavelengths comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year. These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations. A previous attempt at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model. Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 μm. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M(min), such that log(10)[M(min)/M(⊙)] = 11.5(+0.7)(-0.2) at 350 μm, where M(⊙) is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analytical models for galaxy formation.

Published
2011
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17. α-Conotoxin BuIA[T5A;P6O]: a novel ligand that discriminates between α6ß4 and α6ß2 nicotinic acetylcholine receptors and blocks nicotine-stimulated norepinephrine release.

Author

Azam L, Maskos U, Changeux JP, Dowell CD, Christensen S, De Biasi M, and McIntosh JM

Subjects
Animals, Female, Hydroxylation, Ligands, Male, Mice, Mice, Inbred C57BL, Oocytes metabolism, Proline metabolism, Xenopus, Conotoxins metabolism, Nicotine metabolism, Norepinephrine metabolism, Receptors, Nicotinic metabolism
Abstract

α6* (asterisk indicates the presence of additional subunits) nicotinic acetylcholine receptors (nAChRs) are broadly implicated in catecholamine-dependent disorders that involve attention, motor movement, and nicotine self-administration. Different molecular forms of α6 nAChRs mediate catecholamine release, but receptor differentiation is greatly hampered by a paucity of subtype selective ligands. α-Conotoxins are nAChR-targeted peptides used by Conus species to incapacitate prey. We hypothesized that distinct conotoxin-binding kinetics could be exploited to develop a series of selective probes to enable study of native receptor subtypes. Proline6 of α-conotoxin BuIA was found to be critical for nAChR selectivity; substitution of proline6 with 4-hydroyxproline increased the IC(50) by 2800-fold at α6/α3β2β3 but only by 6-fold at α6/α3β4 nAChRs (to 1300 and 12 nM, respectively). We used conotoxin probes together with subunit-null mice to interrogate nAChR subtypes that modulate hippocampal norepinephrine release. Release was abolished in α6-null mutant mice. α-Conotoxin BuIA[T5A;P6O] partially blocked norepinephrine release in wild-type controls but failed to block release in β4(-/-) mice. In contrast, BuIA[T5A;P6O] failed to block dopamine release in the wild-type striatum known to contain α6β2* nAChRs. BuIA[T5A;P6O] is a novel ligand for distinguishing between closely related α6* nAChRs; α6β4* nAChRs modulate norepinephrine release in hippocampus but not dopamine release in striatum.

Published
2010
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18. Design and initial performance of SHARP, a polarimeter for the SHARC-II camera at the Caltech Submillimeter Observatory.

Author

Li H, Dowell CD, Kirby L, Novak G, and Vaillancourt JE

Abstract

We have developed a foreoptics module that converts the Submillimeter High Angular Resolution Camera generation II (SHARC-II) camera at the Caltech Submillimeter Observatory into a sensitive imaging polarimeter at wavelengths of 350 and 450 microm. We refer to this module as "SHARP." SHARP splits the incident radiation into two orthogonally polarized beams that are then reimaged onto opposite ends of the 32 x 12 pixel detector array in SHARC-II. A rotating half-wave plate is used just upstream from the polarization-splitting optics. The effect of SHARP is to convert SHARC-II into a dual-beam 12 x 12 pixel polarimeter. A novel feature of SHARP's design is the use of a crossed grid in a submillimeter polarimeter. Here we describe the detailed optical design of SHARP and present results of tests carried out during our first few observing runs. At 350 microm, the beam size (9 arc sec), throughput (75%), and instrumental polarization (<1%) are all very close to our design goals.

Published
2008
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19. Autoradiographic localization of N-type VGCCs in gerbil hippocampus and failure of omega-conotoxin MVIIA to attenuate neuronal injury after transient cerebral ischemia.

Author

Azimi-Zonooz A, Kawa CB, Dowell CD, and Olivera BM

Subjects
Animals, Autoradiography, Biomarkers, Calcium physiology, Calcium Channel Blockers pharmacology, Calcium Channels, N-Type drug effects, Calcium Channels, N-Type metabolism, Excitatory Postsynaptic Potentials drug effects, Gerbillinae, Hippocampus metabolism, Hippocampus pathology, Interneurons drug effects, Interneurons pathology, Ion Transport, Ischemic Attack, Transient pathology, Male, Nerve Tissue Proteins drug effects, Nerve Tissue Proteins metabolism, Neurons drug effects, Neuroprotective Agents pharmacology, Rats, Reperfusion Injury metabolism, Reperfusion Injury pathology, Reperfusion Injury prevention & control, Species Specificity, Time Factors, omega-Conotoxins administration & dosage, omega-Conotoxins pharmacology, Calcium Channel Blockers therapeutic use, Calcium Channels, N-Type analysis, Hippocampus blood supply, Ischemic Attack, Transient drug therapy, Nerve Tissue Proteins analysis, Neurons pathology, Neuroprotective Agents therapeutic use, omega-Conotoxin GVIA metabolism, omega-Conotoxins therapeutic use
Abstract

In the mammalian central nervous system, transient global ischemia of specific duration causes selective degeneration of CA1 pyramidal neurons in hippocampus. Many of the ischemia-induced pathophysiologic cascades that destroy the neurons are triggered by pre- and postsynaptic calcium entry. Consistent with this, many calcium channel blockers have been shown to be neuroprotective in global models of ischemia. omega-Conotoxin MVIIA, a selective N-type VGCC blocker isolated from the venom of Conus magus, protects CA1 neurons in the rat model of global ischemia, albeit transiently. The mechanism by which this peptide renders neuroprotection is unknown. We performed high-resolution receptor autoradiography with the radiolabeled peptide and observed highest binding in stratum lucidum of CA3 subfield, known to contain inhibitory neurons potentially important in the pathogenesis of delayed neuronal death. This finding suggested that the survival of stratum lucidum inhibitory neurons might be the primary event, leading to CA1 neuroprotection after ischemia. Testing of this hypothesis required the reproduction of its neuroprotective effects in the gerbil model of global ischemia. Surprisingly, we found that omega-MVIIA did not attenuate CA1 hippocampal injury after 5 min of cerebral ischemia in gerbil. Possible reasons are discussed. Lastly, we show that the peptide can be used as a synaptic marker in assessing short and long-term changes that occur in hippocampus after ischemic injury.

Published
2001
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