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1. HerMES: Candidate High-Redshift Galaxies Discovered with Herschel/SPIRE

Author

Dowell, C. Darren, Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a method for selecting $z>4$ dusty, star forming galaxies (DSFGs) using Herschel/SPIRE 250/350/500 $\mu m$ flux densities to search for red sources. We apply this method to 21 deg$^2$ of data from the HerMES survey to produce a catalog of 38 high-$z$ candidates. Follow-up of the first 5 of these sources confirms that this method is efficient at selecting high-$z$ DSFGs, with 4/5 at $z=4.3$ to $6.3$ (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 $\mu m$) 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 ($S_{500\,\mu m} \ge 30$ mJy), red Herschel sources is $3.3 \pm 0.8$ 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 $z\sim2$, rest-frame UV based studies may be missing a significant component of the star formation density at $z=4$ to $6$, even after correction for extinction., Comment: Accepted for publication in ApJ

Published
2013
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2. Modeling of the HERMES J105751.1+573027 submillimeter source lensed by a dark matter dominated foreground group of galaxies

Author

Gavazzi, R., Cooray, A., Conley, A., Aguirre, J. E., Amblard, A., Auld, R., Beelen, A., Blain, A., Blundell, R., Bock, J., Bradford, C. M., Bridge, C., Brisbin, D., Burgarella, D., Chanial, P., Chapin, E., Christopher, N., Clements, D. L., Cox, P., Djorgovski, S. G., Dowell, C. D., Eales, S., Earle, L., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Fu, H., Glenn, J., Solares, E. A. González, Griffin, M., Gurwell, M. A., Halpern, M., Ibar, E., Ivison, R. J., Jarvis, M., Kamenetzky, J., Kim, S., Krips, M., Levenson, L., Lupu, R., Mahabal, A., Maloney, P. D., Maraston, C., Marchetti, L., Marsden, G., Matsuhara, H., Mortier, A. M. J., Murphy, E., Naylor, B. J., Neri, R., Nguyen, H. T., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rangwala, N., Rawlings, J. I., Raymond, G., Riechers, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Scott, K. S., Serra, P., Seymour, N., Shupe, D. L., Smith, A. J., Symeonidis, M., Tugwell, K. E., Vaccari, M., Valiante, E., Valtchanov, I., Verma, A., Vieira, J. D., Vigroux, L., Wang, L., Wardlow, J., Wiebe, D., Wright, G., Xu, C. K., Zeimann, G., Zemcov, M., and Zmuidzinas, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the results of a gravitational lensing analysis of the bright $\zs=2.957$ sub-millimeter galaxy (SMG), HERMES J105751.1+573027 found in {\it Herschel}/SPIRE Science Demonstration Phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high resolution imaging available in optical and Near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allow us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be $\mu=10.9\pm 0.7$. We measure the half-light radius $R_{\rm eff}$ of the source in the rest-frame Near-UV and $V$ bands that characterize the unobscured light coming from stars and find $R_{\rm eff,*}= [2.0 \pm 0.1]$ kpc, in good agreement with recent studies on the Submillimeter Galaxy population. This lens model is also used to estimate the size of the gas distribution ($R_{\rm eff,gas}= [1.1\pm0.5]$) kpc by mapping back in the source plane the CO (J=5-4) transition line emission. The lens modeling yields a relatively large Einstein radius $R_{\rm Ein}= 4\farcs10 \pm 0\farcs02$, corresponding to a deflector velocity dispersion of [$483\pm 16] \,\kms$. This shows that HERMES J105751.1+573027 is lensed by a {\it galaxy group-size} dark matter halo at redshift $\zl\sim 0.6$. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with $f_{\rm dm}(

Published
2011
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3. Discovery of a Multiply-Lensed Submillimeter Galaxy in Early HerMES Herschel/SPIRE Data

Author

Conley, A., Cooray, A., Vieira, J. D., Solares, E. A. González, Kim, S., Aguirre, J. E., Amblard, A., Auld, R., Baker, A. J., Beelen, A., Blain, A., Blundell, R., Bock, J., Bradford, C. M., Bridge, C., Brisbin, D., Burgarella, D., Carpenter, J. M., Chanial, P., Chapin, E., Christopher, N., Clements, D. L., Cox, P., Djorgovski, S. G., Dowell, C. D., Eales, S., Earle, L., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Frayer, D., Fu, H., Gavazzi, R., Glenn, J., Griffin, M., Gurwell, M. A., Halpern, M., Ibar, E., Ivison, R. J., Jarvis, M., Kamenetzky, J., Krips, M., Levenson, L., Lupu, R., Mahabal, A., Maloney, P. D., Maraston, C., Marchetti, L., Marsden, G., Matsuhara, H., Mortier, A. M. J., Murphy, E., Naylor, B. J., Neri, R., Nguyen, H. T., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Pérez-Fournon, I., Pohlen, M., Rangwala, N., Rawlings, J. I., Raymond, G., Riechers, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Scott, K., Serra, P., Seymour, N., Shupe, D. L., Smith, A. J., Symeonidis, M., Tugwell, K. E., Vaccari, M., Valiante, E., Valtchanov, I., Verma, A., Viero, M. P., Vigroux, L., Wang, L., Wiebe, D., Wright, G., Xu, C. K., Zeimann, G., Zemcov, M., and Zmuidzinas, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery of a bright ($f(250\mum) > 400$ mJy), multiply-lensed submillimeter galaxy \obj\ in {\it Herschel}/SPIRE Science Demonstration Phase data from the HerMES project. Interferometric 880\mum\ Submillimeter Array observations resolve at least four images with a large separation of $\sim 9\arcsec$. A high-resolution adaptive optics $K_p$ image with Keck/NIRC2 clearly shows strong lensing arcs. Follow-up spectroscopy gives a redshift of $z=2.9575$, and the lensing model gives a total magnification of $\mu \sim 11 \pm 1$. The large image separation allows us to study the multi-wavelength spectral energy distribution (SED) of the lensed source unobscured by the central lensing mass. The far-IR/millimeter-wave SED is well described by a modified blackbody fit with an unusually warm dust temperature, $88 \pm 3$ K. We derive a lensing-corrected total IR luminosity of $(1.43 \pm 0.09) \times 10^{13}\, \mathrm{L}_{\odot}$, implying a star formation rate of $\sim 2500\, \mathrm{M}_{\odot}\, \mathrm{yr}^{-1}$. However, models primarily developed from brighter galaxies selected at longer wavelengths are a poor fit to the full optical-to-millimeter SED. A number of other strongly lensed systems have already been discovered in early {\it Herschel} data, and many more are expected as additional data are collected., Comment: Accepted for publication in ApJL

Published
2011
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4. HerMES: SPIRE Science Demonstration Phase Maps

Author

Levenson, L., Marsden, G., Zemcov, M., Amblard, A., Blain, A., Bock, J., Chapin, E., Conley, A., Cooray, A., Dowell, C. D., Ellsworth-Bowers, T. P., Franceschini, A., Glenn, J., Griffin, M., Halpern, M., Nguyen, H. T., Oliver, S. J., Page, M. J., Papageorgiou, A., Perez-Fournon, I., Pohlen, M., Rangwala, N., Rowan-Robinson, M., Schulz, B., Scott, Douglas, Serra, P., Shupe, D. L., Valiante, E., Vieira, J. D., Vigroux, L., Wiebe, D., Wright, G., and Xu, C. K.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the production and verification of sky maps of the five SPIRE fields observed as part of the Herschel Multi-tiered Extragalactic Survey (HerMES) during the Science Demonstration Phase (SDP) of the Herschel mission. We have implemented an iterative map-making algorithm (SHIM; The SPIRE-HerMES Iterative Mapper) to produce high fidelity maps that preserve extended diffuse emission on the sky while exploiting the repeated observations of the same region of the sky with many detectors in multiple scan directions to minimize residual instrument noise. We specify here the SHIM algorithm and outline the various tests that were performed to determine and characterize the quality of the maps and verify that the astrometry, point source flux and power on all relevant angular scales meets the needs of the HerMES science goals. These include multiple jackknife tests, determination of the map transfer function and detailed examination of the power spectra of both sky and jackknife maps. The map transfer function is approximately unity on scales from one arcminute to one degree. Final maps (v1.0), including multiple jackknives, as well as the SHIM pipeline, have been used by the HerMES team for the production of SDP papers., Comment: 9 pages, 9 figure, MNRAS Accepted, 27 Sept, 2010

Published
2010
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5. HerMES: Deep Galaxy Number Counts from a P(D) Fluctuation Analysis of SPIRE Science Demonstration Phase Observations

Author

Glenn, J., Conley, A., Bethermin, 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., Conversi, L., Cooray, A., Dowell, C. D., Dwek, E., Eales, S., Elbaz, D., Ellsworth-Bowers, T. P., Fox, M., Franceschini, A., Gear, W., Griffin, M., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, K., Ivison, R. J., Lagache, G., Laurent, G., Levenson, L., Lu, N., Madden, S., Maffei, B., Mainetti, G., Marchetti, L., Marsden, G., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, A., Pearson, C. P., Perez-Fournon, I., Pohlen, M., Rigopoulou, D., Rizzo, D., Roseboom, I. G., Rowan-Robinson, M., Portal, M. Sanchez, Schulz, B., Scott, Douglas, Seymour, N., Shupe, D. L., Smith, A. J., Stevens, J. A., Symeonidis, M., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J. D., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dusty, star forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-SPIRE images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyze three fields from the HerMES programme in all three SPIRE bands (250, 350, and 500 microns); parameterized galaxy number count models are derived to a depth of ~2 mJy/beam, approximately 4 times the depth of previous analyses at these wavelengths, using a P(D) (probability of deflection) approach for comparison to theoretical number count models. Our fits account for 64, 60, and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number counts models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam., Comment: Accepted for publication in MNRAS

Published
2010
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6. The Type Ia Supernova 1999aw: a Probable 1999aa-like Event In a Low-Luminosity Host Galaxy

Author

Strolger, L. -G., Smith, R. C., Suntzeff, N. B., Phillips, M. M., Aldering, G., Nugent, P., Knop, R., Perlmutter, S., Schommer, R. A., Ho, L. C., Hamuy, M., Krisciunas, K., Germany, L. M., Covarrubias, R., Candia, P., Athey, A., Blanc, G., Bonacic, A., Bowers, T., Conley, A., Dahlen, T., Freedman, W., Galaz, G., Gates, E., Goldhaber, G., Goobar, A., Groom, D., Hook, I. M., Marzke, R., Mateo, M., McCarthy, P., Mendez, J., Muena, C., Persson, S. E., Quimby, R., Roth, M., Ruiz-Lapuente, P., Seguel, J., Szentgyorgyi, A., von Braun, K., Wood-Vasey, W. M., and York, T.

Subjects
Astrophysics
Abstract

SN 1999aw was discovered during the first campaign of the Nearby Galaxies Supernova Search (NGSS) project. This luminous, slow-declining (Delta m_{15} (B) = 0.81 \pm 0.03) Type Ia supernova was noteworthy in at least two respects. First, it occurred in an extremely low luminosity host galaxy that was not visible in the template images, nor in initial subsequent deep imaging. Secondly, the photometric and spectral properties of this supernova indicate that it very likely was similar to the subclass of Type Ia supernovae whose prototype is SN 1999aa. This paper presents the BVRI and J_{s} HK_{s} lightcurves of SN 1999aw (through 100 days past maximum light), as well as several epochs of optical spectra. From these data we calculate the bolometric light curve, and give estimates of the luminosity at maximum light and the initial ^{56}Ni mass. In addition, we present deep BVI images obtained recently with the Baade 6.5-meter telescope at Las Campanas Observatory which reveal the remarkably low-luminosity host galaxy., Comment: 18 pages, 10 figures, 8 tables, accepted for publication in AJ

Published
2002
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7. The Type Ia Supernova 1999aw: A Probable 1999aa-like Event in a Low-Luminosity Host Galaxy

Author

Strolger, L-G, Smith, RC, Suntzeff, NB, Phillips, MM, Aldering, G, Nugent, P, Knop, R, Perlmutter, S, Schommer, RA, Ho, LC, Hamuy, M, Krisciunas, K, Germany, LM, Covarrubias, R, Candia, P, Athey, A, Blanc, G, Bonacic, A, Bowers, T, Conley, A, Dahlén, T, Freedman, W, Galaz, G, Gates, E, Goldhaber, G, Goobar, A, Groom, D, Hook, IM, Marzke, R, Mateo, M, McCarthy, P, Méndez, J, Muena, C, Persson, SE, Quimby, R, Roth, M, Ruiz-Lapuente, P, Seguel, J, Szentgyorgyi, A, von Braun, K, Wood-Vasey, WM, and York, T

Subjects
Astronomical Sciences, Physical Sciences, supernovae : general, supernovae : individual, astro-ph, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract

SN 1999aw was discovered during the first campaign of the Nearby Galaxies Supernova Search project. This luminous, slow-declining [Δm 15(B) = 0.81 ± 0.03] Type Ia supernova was noteworthy in at least two respects. First, it occurred in an extremely low luminosity host galaxy that was not visible in the template images nor in initial subsequent deep imaging. Second, the photometric and spectral properties of this supernova indicate that it very likely was similar to the subclass of Type Ia supernovae whose prototype is SN 1999aa. This paper presents the BVRI and J SHKS light curves of SN 1999aw (through ∼100 days past maximum light), as well as several epochs of optical spectra. From these data, we calculate the bolometric light curve and give estimates of the luminosity at maximum light and the initial 56Ni mass. In addition, we present deep BVI images obtained recently with the Baade 6.5 m telescope at Las Campanas Observatory that reveal the remarkably low-luminosity host galaxy.

Published
2002

16. HerMES: deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

Author

Glenn, J, Conley, A, Bethermin, 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, Conversi, L, Cooray, A, Dowell, C, Dwek, E, Eales, S, Elbaz, D, Ellsworth-Bowers, T, Fox, M, and Franceschini, A

Abstract

Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 μm); parametrized galaxy number count models are derived to a depth of ~2 mJy beam-1, approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam. © 2010 The Authors. Journal compilation © 2010 RAS.

Published
2016

17. DISCOVERY OF A MULTIPLY LENSED SUBMILLIMETER GALAXY IN EARLY HerMES HERSCHEL/SPIRE* DATA

Author

Conley, A., Cooray, A., Vieira, J. D., Gonzalez, Solares E. A., Kim, S., Aguirre, J. E., Amblard, A., Auld, R., Baker, A. J., Beelen, A., Blain, A., Blundell, R., Bock, J., Bradford, C. M., Bridge, C., Brisbin, D., Burgarella, D., Carpenter, J. M., Chanial, P., Chapin, E., Christopher, N., Clements, D. L., Cox, P., Djorgovski, S. G., Dowell, C. D., Eales, S., Earle, L., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Frayer, D., Fu, H., Gavazzi, R., Glenn, J., Griffin, M., Gurwell, M. A., Halpern, M., Ibar, E., Ivison, R. J., Jarvis, M., Kamenetzky, J., Krips, M., Levenson, L., Lupu, R., Mahabal, A., Maloney, P. D., Maraston, C., Marchetti, L., Marsden, G., Matsuhara, Hideo, Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Max-Planck-Institut für Radioastronomie (MPIFR), 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)-Centre National d’Études Spatiales [Paris] (CNES), Centre for Astronomy, Harvard University, Bucknell University, 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), AUTRES, Laboratoire Colloïdes et Matériaux Divisés (LCMD), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Earthquake Administration of Yunnan Province, School of Physics and Astronomy [Cardiff], Cardiff University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Service de Chimie Physique (SCP), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Centre de recherches Paul Pascal (CRPP), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de photonique et de nanostructures (LPN), 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), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), National Institute of Water and Atmospheric Research [Wellington] (NIWA), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), Cahill Center for Astronomy and Astrophysics, California Institute of Technology (CALTECH), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Harvard University [Cambridge], 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), Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and University of California-University of California

Subjects
Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Submillimeter Array, Luminosity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Image (category theory), Astronomy and Astrophysics, Redshift, Galaxy, Spire, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Spectral energy distribution, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 91名, Accepted: 2011-04-08, 資料番号: SA1003030000

Published
2016
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18. The Type Ia supernova 1999aw: A probable 1999aa-like event in a low-luminosity host galaxy

Author

Strolger, L, Smith, R, Suntzeff, N, Phillips, M, Aldering, G, Nugent, P, Knop, R, Perlmutter, S, Schommer, R, Ho, L, Hamuy, M, Krisciunas, K, Germany, L, Covarrubias, R, Candia, P, Athey, A, Blanc, G, Bonacic, A, Bowers, T, Conley, A, Dahlén, T, Freedman, W, Galaz, G, Gates, E, and Goldhaber, G

Abstract

SN 1999aw was discovered during the first campaign of the Nearby Galaxies Supernova Search project. This luminous, slow-declining [Δm 15(B) = 0.81 ± 0.03] Type Ia supernova was noteworthy in at least two respects. First, it occurred in an extremely low luminosity host galaxy that was not visible in the template images nor in initial subsequent deep imaging. Second, the photometric and spectral properties of this supernova indicate that it very likely was similar to the subclass of Type Ia supernovae whose prototype is SN 1999aa. This paper presents the BVRI and J SHKS light curves of SN 1999aw (through ∼100 days past maximum light), as well as several epochs of optical spectra. From these data, we calculate the bolometric light curve and give estimates of the luminosity at maximum light and the initial 56Ni mass. In addition, we present deep BVI images obtained recently with the Baade 6.5 m telescope at Las Campanas Observatory that reveal the remarkably low-luminosity host galaxy.

Published
2016
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21. Modeling of the Hermes Submillimeter Source Lensed by a Dark Matter Dominated Foreground Group of Galaxies

Author

Gavazzi, R., Cooray, A., Conley, A., Aguirre, J. E., Amblard, A., Auld, R., Beelen, A., Blain, A., Blundell, R., Bock, J., Bradford, C. M., Bridge, C., Brisbin, D., Burgarella, D., Chanial, P., Chapin, E., Christopher, N., Clements, D. L., Cox, P., Djorgovski, S. G., Dowell, C. D., Eales, S., Earle, L., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Fu, H., Glenn, J., Gonzalez Solares, E. A., Griffin, M., Gurwell, M. A., Halpern, M., Ibar, E., Ivison, R. J., Jarvis, M., Kamenetzky, J., Kim, S., Krips, M., Levenson, L., Lupu, R., Mahabal, A., Maloney, P. D., Maraston, C., Marchetti, L., Marsden, G., 松原, 英雄, Matsuhara, Hideo, Gavazzi, R., Cooray, A., Conley, A., Aguirre, J. E., Amblard, A., Auld, R., Beelen, A., Blain, A., Blundell, R., Bock, J., Bradford, C. M., Bridge, C., Brisbin, D., Burgarella, D., Chanial, P., Chapin, E., Christopher, N., Clements, D. L., Cox, P., Djorgovski, S. G., Dowell, C. D., Eales, S., Earle, L., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Fu, H., Glenn, J., Gonzalez Solares, E. A., Griffin, M., Gurwell, M. A., Halpern, M., Ibar, E., Ivison, R. J., Jarvis, M., Kamenetzky, J., Kim, S., Krips, M., Levenson, L., Lupu, R., Mahabal, A., Maloney, P. D., Maraston, C., Marchetti, L., Marsden, G., 松原, 英雄, and Matsuhara, Hideo

Abstract

著者人数: 88名, Accepted: 2011-06-07

Published
2015

22. Modeling of the Hermes Submillimeter Source Lensed by a Dark Matter Dominated Foreground Group of Galaxies

Author

Gavazzi, R., Cooray, A., Conley, A., Aguirre, J. E., Amblard, A., Auld, R., Beelen, A., Blain, A., Blundell, R., Bock, J., Bradford, C. M., Bridge, C., Brisbin, D., Burgarella, D., Chanial, P., Chapin, E., Christopher, N., Clements, D. L., Cox, P., Djorgovski, S. G., Dowell, C. D., Eales, S., Earle, L., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Fu, H., Glenn, J., Gonzalez, Solares E. A., Griffin, M., Gurwell, M. A., Halpern, M., Ibar, E., Ivison, R. J., Jarvis, M., Kamenetzky, J., Kim, S., Krips, M., Levenson, L., Lupu, R., Mahabal, A., Maloney, P. D., Maraston, C., Marchetti, L., Marsden, G., Matsuhara, Hideo, 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
Effective radius, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Dark matter, Plateau de Bure Interferometer, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Einstein radius, Dark matter halo, Gravitational lens, Space and Planetary Science, Galaxy group, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

著者人数: 88名, Accepted: 2011-06-07, 資料番号: SA1003001000

Published
2011
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23. HerMES: Candidate high-redshift galaxies discovered with Herschel/Spire

Author

Dowell, C., 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, C., Chapman, S., Clements, D., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R., Laporte, N., Marchetti, L., Martínez-Navajas, P., Marsden, G., Morrison, G., Nguyen, H., O'Halloran, B., Oliver, S., Omont, A., Page, M., Papageorgiou, A., Pearson, C., Petitpas, G., Pérez-Fournon, I., Pohlen, M., Riechers, D., Rigopoulou, D., Roseboom, I., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, Nick, Shupe, D., Smith, A., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J., Viero, M., Wang, L., Wardlow, J., Xu, C., Zemcov, M., Dowell, C., 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, C., Chapman, S., Clements, D., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R., Laporte, N., Marchetti, L., Martínez-Navajas, P., Marsden, G., Morrison, G., Nguyen, H., O'Halloran, B., Oliver, S., Omont, A., Page, M., Papageorgiou, A., Pearson, C., Petitpas, G., Pérez-Fournon, I., Pohlen, M., Riechers, D., Rigopoulou, D., Roseboom, I., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, Nick, Shupe, D., Smith, A., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J., Viero, M., Wang, L., Wardlow, J., Xu, C., and Zemcov, M.

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.

Published
2014

24. HerMES: candidate high-redshift galaxies discovered with Herschel/SPIRE

Author

Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 mu m flux densities to search for red sources. We apply this method to 21 deg(2) 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 mu m) 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 (mu m) >= 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 similar to 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.

Published
2014
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25. HerMES: candidate high-redshift galaxies discovered with Herschel/SPIRE

Author

Physics, Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., Zemcov, M., Physics, Dowell, C. D., Conley, A., Glenn, J., Arumugam, V., Asboth, V., Aussel, H., Bertoldi, F., Bethermin, M., Bock, J., Boselli, A., Bridge, C. R., Buat, V., Burgarella, D., Cabrera-Lavers, A., Casey, C. M., Chapman, S. C., Clements, D. L., Conversi, L., Cooray, A., Dannerbauer, H., De Bernardis, F., Ellsworth-Bowers, T. P., Farrah, D., Franceschini, A., Griffin, M., Gurwell, M. A., Halpern, M., Hatziminaoglou, E., Heinis, S., Ibar, E., Ivison, R. J., Laporte, N., Marchetti, L., Martinez-Navajas, P., Marsden, G., Morrison, G. E., Nguyen, H. T., O'Halloran, B., Oliver, S. J., Omont, A., Page, M. J., Papageorgiou, A., Pearson, C. P., Petitpas, G., Perez-Fournon, I., Pohlen, M., Riechers, D. A., Rigopoulou, D., Roseboom, I. G., Rowan-Robinson, M., Sayers, J., Schulz, B., Scott, D., Seymour, N., Shupe, D. L., Smith, A. J., Streblyanska, A., Symeonidis, M., Vaccari, M., Valtchanov, I., Vieira, J. D., Viero, M., Wang, L., Wardlow, J., Xu, C. K., and Zemcov, M.

Abstract

We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 mu m flux densities to search for red sources. We apply this method to 21 deg(2) 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 mu m) 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 (mu m) >= 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 similar to 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.

Published
2014

26. Footprint timetable: the next step

Author

Cope, N, Sheridan-Ross, J, Bowers, T, Calvert, M, Gorra, A, Harrison, G, and Joslin, M

Subjects
education, ComputingMilieux_COMPUTERSANDEDUCATION, ComputingMilieux_MISCELLANEOUS
Published
2008

27. HerMES: CANDIDATE HIGH-REDSHIFT GALAXIES DISCOVERED WITHHERSCHEL/SPIRE,

Author

Dowell, C. Darren, primary, Conley, A., additional, Glenn, J., additional, Arumugam, V., additional, Asboth, V., additional, Aussel, H., additional, Bertoldi, F., additional, Béthermin, M., additional, Bock, J., additional, Boselli, A., additional, Bridge, C., additional, Buat, V., additional, Burgarella, D., additional, Cabrera-Lavers, A., additional, Casey, C. M., additional, Chapman, S. C., additional, Clements, D. L., additional, Conversi, L., additional, Cooray, A., additional, Dannerbauer, H., additional, De Bernardis, F., additional, Ellsworth-Bowers, T. P., additional, Farrah, D., additional, Franceschini, A., additional, Griffin, M., additional, Gurwell, M. A., additional, Halpern, M., additional, Hatziminaoglou, E., additional, Heinis, S., additional, Ibar, E., additional, Ivison, R. J., additional, Laporte, N., additional, Marchetti, L., additional, Martínez-Navajas, P., additional, Marsden, G., additional, Morrison, G. E., additional, Nguyen, H. T., additional, O'Halloran, B., additional, Oliver, S. J., additional, Omont, A., additional, Page, M. J., additional, Papageorgiou, A., additional, Pearson, C. P., additional, Petitpas, G., additional, Pérez-Fournon, I., additional, Pohlen, M., additional, Riechers, D., additional, Rigopoulou, D., additional, Roseboom, I. G., additional, Rowan-Robinson, M., additional, Sayers, J., additional, Schulz, B., additional, Scott, Douglas, additional, Seymour, N., additional, Shupe, D. L., additional, Smith, A. J., additional, Streblyanska, A., additional, Symeonidis, M., additional, Vaccari, M., additional, Valtchanov, I., additional, Vieira, J. D., additional, Viero, M., additional, Wang, L., additional, Wardlow, J., additional, Xu, C. K., additional, and Zemcov, M., additional

Published
2013
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31. DISCOVERY OF A MULTIPLY LENSED SUBMILLIMETER GALAXY IN EARLY HerMES HERSCHEL/SPIRE * DATA

Author

Conley, A., primary, Cooray, A., additional, Vieira, J. D., additional, Solares, E. A. González, additional, Kim, S., additional, Aguirre, J. E., additional, Amblard, A., additional, Auld, R., additional, Baker, A. J., additional, Beelen, A., additional, Blain, A., additional, Blundell, R., additional, Bock, J., additional, Bradford, C. M., additional, Bridge, C., additional, Brisbin, D., additional, Burgarella, D., additional, Carpenter, J. M., additional, Chanial, P., additional, Chapin, E., additional, Christopher, N., additional, Clements, D. L., additional, Cox, P., additional, Djorgovski, S. G., additional, Dowell, C. D., additional, Eales, S., additional, Earle, L., additional, Ellsworth-Bowers, T. P., additional, Farrah, D., additional, Franceschini, A., additional, Frayer, D., additional, Fu, H., additional, Gavazzi, R., additional, Glenn, J., additional, Griffin, M., additional, Gurwell, M. A., additional, Halpern, M., additional, Ibar, E., additional, Ivison, R. J., additional, Jarvis, M., additional, Kamenetzky, J., additional, Krips, M., additional, Levenson, L., additional, Lupu, R., additional, Mahabal, A., additional, Maloney, P. D., additional, Maraston, C., additional, Marchetti, L., additional, Marsden, G., additional, Matsuhara, H., additional, Mortier, A. M. J., additional, Murphy, E., additional, Naylor, B. J., additional, Neri, R., additional, Nguyen, H. T., additional, Oliver, S. J., additional, Omont, A., additional, Page, M. J., additional, Papageorgiou, A., additional, Pearson, C. P., additional, Pérez-Fournon, I., additional, Pohlen, M., additional, Rangwala, N., additional, Rawlings, J. I., additional, Raymond, G., additional, Riechers, D., additional, Rodighiero, G., additional, Roseboom, I. G., additional, Rowan-Robinson, M., additional, Schulz, B., additional, Scott, Douglas, additional, Scott, K., additional, Serra, P., additional, Seymour, N., additional, Shupe, D. L., additional, Smith, A. J., additional, Symeonidis, M., additional, Tugwell, K. E., additional, Vaccari, M., additional, Valiante, E., additional, Valtchanov, I., additional, Verma, A., additional, Viero, M. P., additional, Vigroux, L., additional, Wang, L., additional, Wiebe, D., additional, Wright, G., additional, Xu, C. K., additional, Zeimann, G., additional, Zemcov, M., additional, and Zmuidzinas, J., additional

Published
2011
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33. HerMES: deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations

Author

Glenn, J., primary, Conley, A., additional, Béthermin, M., additional, Altieri, B., additional, Amblard, A., additional, Arumugam, V., additional, Aussel, H., additional, Babbedge, T., additional, Blain, A., additional, Bock, J., additional, Boselli, A., additional, Buat, V., additional, Castro-Rodríguez, N., additional, Cava, A., additional, Chanial, P., additional, Clements, D. L., additional, Conversi, L., additional, Cooray, A., additional, Dowell, C. D., additional, Dwek, E., additional, Eales, S., additional, Elbaz, D., additional, Ellsworth-Bowers, T. P., additional, Fox, M., additional, Franceschini, A., additional, Gear, W., additional, Griffin, M., additional, Halpern, M., additional, Hatziminaoglou, E., additional, Ibar, E., additional, Isaak, K., additional, Ivison, R. J., additional, Lagache, G., additional, Laurent, G., additional, Levenson, L., additional, Lu, N., additional, Madden, S., additional, Maffei, B., additional, Mainetti, G., additional, Marchetti, L., additional, Marsden, G., additional, Nguyen, H. T., additional, O'Halloran, B., additional, Oliver, S. J., additional, Omont, A., additional, Page, M. J., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Pearson, C. P., additional, Pérez-Fournon, I., additional, Pohlen, M., additional, Rigopoulou, D., additional, Rizzo, D., additional, Roseboom, I. G., additional, Rowan-Robinson, M., additional, Portal, M. Sánchez, additional, Schulz, B., additional, Scott, Douglas, additional, Seymour, N., additional, Shupe, D. L., additional, Smith, A. J., additional, Stevens, J. A., additional, Symeonidis, M., additional, Trichas, M., additional, Tugwell, K. E., additional, Vaccari, M., additional, Valtchanov, I., additional, Vieira, J. D., additional, Vigroux, L., additional, Wang, L., additional, Ward, R., additional, Wright, G., additional, Xu, C. K., additional, and Zemcov, M., additional

Published
2010
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34. HerMES: SPIRE Science Demonstration Phase maps★†‡

Author

Levenson, L., primary, Marsden, G., additional, Zemcov, M., additional, Amblard, A., additional, Blain, A., additional, Bock, J., additional, Chapin, E., additional, Conley, A., additional, Cooray, A., additional, Dowell, C. D., additional, Ellsworth-Bowers, T. P., additional, Franceschini, A., additional, Glenn, J., additional, Griffin, M., additional, Halpern, M., additional, Nguyen, H. T., additional, Oliver, S. J., additional, Page, M. J., additional, Papageorgiou, A., additional, Pérez-Fournon, I., additional, Pohlen, M., additional, Rangwala, N., additional, Rowan-Robinson, M., additional, Schulz, B., additional, Scott, Douglas, additional, Serra, P., additional, Shupe, D. L., additional, Valiante, E., additional, Vieira, J. D., additional, Vigroux, L., additional, Wiebe, D., additional, Wright, G., additional, and Xu, C. K., additional

Published
2010
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35. The manic syndrome: factors which may predict a patient's response to lithium, carbamazepine and valproate

Author

Dilsaver, S C, Swann, A C, Shoaib, A M, and Bowers, T C

Subjects
Bipolar Disorder, Carbamazepine, Lithium Carbonate, Valproic Acid, mental disorders, behavior and behavior mechanisms, Humans, Prognosis, behavioral disciplines and activities, Research Article
Abstract

Studies suggest that 80% to 90% of all patients in the manic state respond to lithium provided that they are relatively free of dysphoria ("pure mania"). In contrast, less than 40% of individuals in the manic state who cycle rapidly or are substantially dysphoric ("dysphoric mania") respond to lithium. These patients appear to be more responsive to carbamazepine and valproate. The authors conclude that carbamazepine and valproate are the drugs of choice if one desires to treat a rapidly cycling individual or patient with dysphoric mania with just one agent. However, they emphasize that a prospective study designed to identify the predictors of response of primary mania to lithium, carbamazepine and valproate is required. Studies assessing the relative value of lithium, carbamazepine or valproate as prophylactic agents in the care of patients with specific subtypes of mania are also needed. These studies would address the most important issues confronting researchers interested in the drug treatment of mania.

Published
1993

45. Composition of nifH in a wastewater treatment system reliant on N2 fixation.

Author

Bowers, T., Reid, N., and Lloyd-Jones, G.

Subjects
*WASTEWATER treatment, *NITROGEN fixation, *INDUSTRIAL wastes, *SEWAGE purification, *FOREST soils, *WOOD pulp industry, *BIOCHEMICAL oxygen demand, *PHYLOGENY, *NUCLEIC acid hybridization
Abstract

High levels of nitrogen fixation have been observed in the wastewaters of pulp and paper mills. In this study, we show that nitrogen fixation in a model pulp and paper wastewater treatment system is supported by a high density of nifH sequences that are of low diversity. Quantitative PCR revealed a ratio of nifH to 16S rDNA of 1.14 ± 0.76 which shows that very high levels of the nifH gene were enriched to support the high rates of nitrogen fixation that occur in this wastewater. Changes in wastewater composition and dissolved oxygen levels did not affect the nifH levels and allowed stable wastewater treatment. The nifH sequences identified display a similar profile to those seen in forest soil environments where nifH sequences derived from α- proteobacteria and β- proteobacteria are also prevalent. [ABSTRACT FROM AUTHOR]

Published
2008
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46. Rhythm and Its Position in the Hierarchy of a Teacher's Values.

Author

Bowers, T. Alan

Subjects
RHYTHM, OTOLARYNGOLOGISTS, MUSICAL meter & rhythm, MUSIC education
Abstract

The article discusses a brief celebration of rhythm and its formidable potential in reforming the singing of novice and professionals suggested by otolaryngologist Paul J. Moses. According to Moses, rhythm is movement, tension, release, and periodicity which implies virtues defining the rhythmic triad. In addition, rhythm is the catalyst of vocal efforts which calls techniques and unfolds musical structure.

Published
2007

49. Sliding hip screw versusthe Targon PF nail in the treatment of trochanteric fractures of the hip

Author

Parker, M. J., Bowers, T. R., and Pryor, G. A.

Abstract

In a randomised trial involving 598 patients with 600 trochanteric fractures of the hip, the fractures were treated with either a sliding hip screw (n = 300) or a Targon PF intramedullary nail (n = 300). The mean age of the patients was 82 years (26 to 104). All surviving patients were reviewed at one year with functional outcome assessed by a research nurse blinded to the treatment used. The intramedullary nail was found to have a slightly increased mean operative time (46 minutes (sd12.3) versus49 minutes (sd12.7), p < 0.001) and an increased mean radiological screening time (0.3 minutes (sd0.2) versus0.5 minutes (sd0.3), p <  0.001). Operative difficulties were more common with the intramedullary nail. There was no statistically significant difference between implants for wound healing complications (p = 1), or need for post-operative blood transfusion (p = 1), and medical complications were similarly distributed in both groups. There was a tendency to fewer revisions of fixation or conversion to an arthroplasty in the nail group, although the difference was not statistically significant (nine versusthree cases, p = 0.14). The extent of shortening, loss of hip flexion, mortality and degree of residual pain were similar in both groups. The recovery of mobility was superior for those treated with the intramedullary nails (p = 0.01 at one year from injury).In summary, both implants produced comparable results but there was a tendency to better return of mobility for those treated with the intramedullary nail.

Published
2012
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