Galaxy formation and evolution

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HerMES: Herschel-SPIRE observations of Lyman Break Galaxies

(2010)

Authors:

D Rigopoulou, GE Magdis, RJ Ivison, A Amblard, V Arumugam, H Aussel, A Blain, J Bock, A Boselli, V Buat, D Burgarella, N Castro-Rodriguez, A Cava, P Chanial, DL Clements, A Conley, L Conversi, A Cooray, CD Dowell, E Dwek, S Eales, D Elbaz, D Farrah, A Franceschini, J Glenn, M Griffin, M Halpern, E Hatziminaoglou, J-S Huang, E Ibar, K Isaak, G Lagache, L Levenson, N Lu, S Madden, B Maffei, G Mainetti, L Marchetti, HT Nguyen, B O'Halloran, SJ Oliver, A Omont, MJ Page, P Panuzzo, A Papageorgiou, CP Pearson, I Perez-Fournon, M Pohlen, D Rizzo, IG Roseboom
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A first glimpse into the far-IR properties of high-z UV-selected galaxies: Herschel/PACS observations of z ∼ 3 LBGS

Astrophysical Journal Letters 720:2 PART 2 (2010) L185-L189

Authors:

GE Magdis, D Elbaz, HS Hwang, E Daddi, D Rigopoulou, B Altieri, P Andreani, H Aussel, S Berta, A Cava, A Bongiovanni, J Cepa, A Cimatti, M Dickinson, H Dominguez, N Förster Schreiber, R Genzel, JS Huang, D Lutz, R Maiolino, B Magnelli, GE Morrison, R Nordon, AM Pérez García, A Poglitsch, P Popesso, F Pozzi, L Riguccini, G Rodighiero, A Saintonge, P Santini, M Sanchez-Portal, L Shao, E Sturm, L Tacconi, I Valtchanov

Abstract:

We present first insights into the far-IR properties for a sample of IRAC and MIPS 24 μm detected Lyman break galaxies (LBGs) at z ∼ 3, as derived from observations in the northern field of the Great Observatories Origins Survey (GOODS-N) carried out with the PACS instrument on board the Herschel Space Observatory. Although none of our galaxies are detected by Herschel, we employ a stacking technique to construct, for the first time, the average spectral energy distribution (SED) of infrared luminous LBGs from UV to radio wavelengths. We derive a median IR luminosity of LIR = 1.6 × 1012 L⊙, placing the population in the class of ultra-luminous infrared galaxies (ULIRGs). Complementing our study with existing multi-wavelength data, we put constraints on the dust temperature of the population and find that for their LIR, MIPS-LBGs are warmer than submillimeter-luminous galaxies while they fall in the locus of the L IR-Td relation of the local ULIRGs. This, along with estimates based on the average SED, explains the marginal detection of LBGs in current submillimeter surveys and suggests that these latter studies introduce a bias toward the detection of colder ULIRGs in the high-z universe, while missing high-z ULIRGS with warmer dust. © 2010. The American Astronomical Society. All rights reserved.
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The Herschel Multi-Tiered Extragalactic Survey: Source Extraction and Cross-Identifications in Confusion-Dominated SPIRE Images

(2010)

Authors:

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

(2010)

Authors:

HS Hwang, D Elbaz, GE Magdis, E Daddi, M Symeonidis, B Altieri, A Amblard, P Andreani, V Arumugam, R Auld, H Aussel, T Babbedge, S Berta, A Blain, J Bock, A Bongiovanni, A Boselli, V Buat, D Burgarella, N Castro-Rodriguez, A Cava, J Cepa, P Chanial, E Chapin, R-R Chary, A Cimatti, DL Clements, A Conley, L Conversi, A Cooray, H Dannerbauer, M Dickinson, H Dominguez, CD Dowell, JS Dunlop, E Dwek, S Eales, D Farrah, N Forster Schreiber, M Fox, A Franceschini, W Gear, R Genzel, J Glenn, M Griffin, C Gruppioni, M Halpern, E Hatziminaoglou, E Ibar, K Isaak, RJ Ivison, W-S Jeong, G Lagache, D Le Borgne, E Le Floc'h, HM Lee, JC Lee, MG Lee, L Levenson, N Lu, D Lutz, S Madden, B Maffei, B Magnelli, G Mainetti, R Maiolino, L Marchetti, AMJ Mortier, HT Nguyen, R Nordon, B O'Halloran, K Okumura, SJ Oliver, A Omont, MJ Page, P Panuzzo, A Papageorgiou, CP Pearson, I Perez-Fournon, AM Perez Garcia, A Poglitsch, M Pohlen, P Popesso, F Pozzi, JI Rawlings, D Rigopoulou, L Riguccini, D Rizzo, G Rodighiero, IG Roseboom, M Rowan-Robinson, A Saintonge, M Sanchez Portal, P Santini, M Sauvage, B Schulz, Douglas Scott, N Seymour, L Shao, DL Shupe, AJ Smith, JA Stevens, E Sturm, L Tacconi, M Trichas, KE Tugwell, M Vaccari, I Valtchanov, JD Vieira, L Vigroux, L Wang, R Ward, G Wright, CK Xu, M Zemcov
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Using line intensity ratios to determine the geometry of plasma in stars via their apparent areas

High Energy Density Physics Elsevier 6:3 (2010) 301-304
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