C. Darren Dowell - NASA JPL

C. Darren Dowell
Are you C. Darren Dowell?

Claim your profile, edit publications, add additional information:

Contact Details

Name
C. Darren Dowell
Affiliation
NASA JPL
Location

Pubs By Year

Pub Categories

 
Cosmology and Nongalactic Astrophysics (34)
 
Instrumentation and Methods for Astrophysics (17)
 
Astrophysics of Galaxies (8)
 
Solar and Stellar Astrophysics (3)
 
High Energy Physics - Theory (2)
 
General Relativity and Quantum Cosmology (2)
 
High Energy Physics - Phenomenology (2)
 
Earth and Planetary Astrophysics (1)
 
High Energy Astrophysical Phenomena (1)

Publications Authored By C. Darren Dowell

2017Apr
Authors: Derek Ward-Thompson, Kate Pattle, Pierre Bastien, Ray S. Furuya, Woojin Kwon, Shih-Ping Lai, Keping Qiu, David Berry, Minho Choi, Simon Coudé, James Di Francesco, Thiem Hoang, Erica Franzmann, Per Friberg, Sarah F. Graves, Jane S. Greaves, Martin Houde, Doug Johnstone, Jason M. Kirk, Patrick M. Koch, Jungmi Kwon, Chang Won Lee, Di Li, Brenda C. Matthews, Joseph C. Mottram, Harriet Parsons, Andy Pon, Ramprasad Rao, Mark Rawlings, Hiroko Shinnaga, Sarah Sadavoy, Sven van Loo, Yusuke Aso, Do-Young Byun, Eswariah Chakali, Huei-Ru Chen, Mike C. -Y. Chen, Wen Ping Chen, Tao-Chung Ching, Jungyeon Cho, Antonio Chrysostomou, Eun Jung Chung, Yasuo Doi, Emily Drabek-Maunder, Stewart P. S. Eyres, Jason Fiege, Rachel K. Friesen, Gary Fuller, Tim Gledhill, Matt J. Griffin, Qilao Gu, Tetsuo Hasegawa, Jennifer Hatchell, Saeko S. Hayashi, Wayne Holland, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Ji-hyun Kang, Miju Kang, Sung-ju Kang, Koji S. Kawabata, Francisca Kemper, Gwanjeong Kim, Jongsoo Kim, Kee-Tae Kim, Kyoung Hee Kim, Mi-Ryang Kim, Shinyoung Kim, Kevin M. Lacaille, Jeong-Eun Lee, Sang-Sung Lee, Dalei Li, Hua-bai Li, Hong-Li Liu, Junhao Liu, Sheng-Yuan Liu, Tie Liu, A-Ran Lyo, Steve Mairs, Masafumi Matsumura, Gerald H. Moriarty-Schieven, Fumitaka Nakamura, Hiroyuki Nakanishi, Nagayoshi Ohashi, Takashi Onaka, Nicolas Peretto, Tae-Soo Pyo, Lei Qian, Brendan Retter, John Richer, Andrew Rigby, Jean-François Robitaille, Giorgio Savini, Anna M. M. Scaife, Archana Soam, Motohide Tamura, Ya-Wen Tang, Kohji Tomisaka, Hongchi Wang, Jia-Wei Wang, Anthony P. Whitworth, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Philippe André, C. Darren Dowell, Sam Falle, Yusuke Tsukamoto

We present the first results from the B-fields 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. Read More

Variable emission from Sgr~A*, the luminous counterpart to the super-massive black hole at the center of our Galaxy, arises from the innermost portions of the accretion flow. Better characterization of the variability is important for constraining models of the low-luminosity accretion mode powering Sgr~A*, and could further our ability to use variable emission as a probe of the strong gravitational potential in the vicinity of the $4\times10^{6}\mathrm{M}_{\odot}$ black hole. We use the \textit{Herschel} Spectral and Photometric Imaging Receiver (SPIRE) to monitor Sgr~A* at wavelengths that are difficult or impossible to observe from the ground. Read More

BICEP2 and the Keck Array are polarization-sensitive microwave telescopes that observe the cosmic microwave background (CMB) from the South Pole at degree angular scales in search of a signature of inflation imprinted as B-mode polarization in the CMB. BICEP2 was deployed in late 2009, observed for three years until the end of 2012 at 150 GHz with 512 antenna-coupled transition edge sensor bolometers, and has reported a detection of B-mode polarization on degree angular scales. The Keck Array was first deployed in late 2010 and will observe through 2016 with five receivers at several frequencies (95, 150, and 220 GHz). Read More

2015Feb
Authors: BICEP2/Keck, Planck Collaborations, :, P. A. R. Ade, N. Aghanim, Z. Ahmed, R. W. Aikin, K. D. Alexander, M. Arnaud, J. Aumont, C. Baccigalupi, A. J. Banday, D. Barkats, R. B. Barreiro, J. G. Bartlett, N. Bartolo, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, S. J. Benton, J. -P. Bernard, M. Bersanelli, P. Bielewicz, C. A. Bischoff, J. J. Bock, A. Bonaldi, L. Bonavera, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, J. A. Brevik, M. Bucher, I. Buder, E. Bullock, C. Burigana, R. C. Butler, V. Buza, E. Calabrese, J. -F. Cardoso, A. Catalano, A. Challinor, R. -R. Chary, H. C. Chiang, P. R. Christensen, L. P. L. Colombo, C. Combet, J. Connors, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, J. -M. Delouis, F. -X. Désert, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, C. D. Dowell, L. Duband, A. Ducout, J. Dunkley, X. Dupac, C. Dvorkin, G. Efstathiou, F. Elsner, T. A. Enßlin, H. K. Eriksen, E. Falgarone, J. P. Filippini, F. Finelli, S. Fliescher, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, A. Frejsel, S. Galeotta, S. Galli, K. Ganga, T. Ghosh, M. Giard, E. Gjerløw, S. R. Golwala, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, J. E. Gudmundsson, M. Halpern, F. K. Hansen, D. Hanson, D. L. Harrison, M. Hasselfield, G. Helou, S. Henrot-Versillé, D. Herranz, S. R. Hildebrandt, G. C. Hilton, E. Hivon, M. Hobson, W. A. Holmes, W. Hovest, V. V. Hristov, K. M. Huffenberger, H. Hui, G. Hurier, K. D. Irwin, A. H. Jaffe, T. R. Jaffe, J. Jewell, W. C. Jones, M. Juvela, A. Karakci, K. S. Karkare, J. P. Kaufman, B. G. Keating, S. Kefeli, E. Keihänen, S. A. Kernasovskiy, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, J. M. Kovac, N. Krachmalnicoff, M. Kunz, C. L. Kuo, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. -M. Lamarre, A. Lasenby, M. Lattanzi, C. R. Lawrence, E. M. Leitch, R. Leonardi, F. Levrier, A. Lewis, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, M. Lueker, J. F. Macías-Pérez, B. Maffei, D. Maino, N. Mandolesi, A. Mangilli, M. Maris, P. G. Martin, E. Martínez-González, S. Masi, P. Mason, S. Matarrese, K. G. Megerian, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, A. Moss, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, H. T. Nguyen, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, R. O'Brient, R. W. Ogburn IV, A. Orlando, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, B. Partridge, F. Pasian, G. Patanchon, T. J. Pearson, O. Perdereau, L. Perotto, V. Pettorino, F. Piacentini, M. Piat, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, G. W. Pratt, S. Prunet, C. Pryke, J. -L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, A. Renzi, S. Richter, I. Ristorcelli, G. Rocha, M. Rossetti, G. Roudier, M. Rowan-Robinson, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, D. Santos, M. Savelainen, G. Savini, R. Schwarz, D. Scott, M. D. Seiffert, C. D. Sheehy, L. D. Spencer, Z. K. Staniszewski, V. Stolyarov, R. Sudiwala, R. Sunyaev, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, G. P. Teply, L. Terenzi, K. L. Thompson, L. Toffolatti, J. E. Tolan, M. Tomasi, M. Tristram, M. Tucci, A. D. Turner, L. Valenziano, J. Valiviita, B. Van Tent, L. Vibert, P. Vielva, A. G. Vieregg, F. Villa, L. A. Wade, B. D. Wandelt, R. Watson, A. C. Weber, I. K. Wehus, M. White, S. D. M. White, J. Willmert, C. L. Wong, K. W. Yoon, D. Yvon, A. Zacchei, A. Zonca

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 0h, Dec. $-57. Read More

We have developed antenna-coupled transition-edge sensor (TES) bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including BICEP2, Keck Array, and the balloon borne SPIDER. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%-30% bandwidth at 95, 150, or 220~GHz. Read More

2015Feb
Affiliations: 1Cardiff University, 2Cardiff University, 3Cardiff University, 4Cardiff University, 5Stanford University, 6Caltech, 7Harvard/CfA, 8ALMA, 9University of Toronto, 10Harvard/CfA, 11Caltech, 12Caltech, 13Harvard/CfA, 14Minnesota Institute for Astrophysics, 15Harvard/CfA, 16Harvard/CfA, 17Caltech, 18NASA JPL, 19Harvard/CfA, 20SBT Grenoble, 21Caltech, 22University of Minnesota, 23Caltech, 24University of British Columbia, 25University of British Columbia, 26Caltech, 27NIST, 28Caltech, 29Caltech, 30Stanford University, 31Harvard/CfA, 32UCSD, 33UCSD, 34Caltech, 35Stanford University, 36Harvard/CfA, 37Stanford University, 38KICP, 39Caltech, 40Caltech, 41NASA JPL, 42University of Toronto, 43NASA JPL, 44NASA JPL, 45Stanford University, 46UCSD, 47University of Minnesota, 48NIST, 49Harvard/CfA, 50University of Minnesota, 51KICP, 52Caltech, 53Cardiff University, 54Caltech, 55Stanford University, 56Stanford University, 57NASA JPL, 58KICP, 59NASA JPL, 60University of Minnesota, 61Harvard/CfA, 62Stanford University

The Keck Array is a system of cosmic microwave background (CMB) polarimeters, each similar to the BICEP2 experiment. In this paper we report results from the 2012 and 2013 observing seasons, during which the Keck Array consisted of five receivers all operating in the same (150 GHz) frequency band and observing field as BICEP2. We again find an excess of B-mode power over the lensed-$\Lambda$CDM expectation of $> 5 \sigma$ in the range $30 < \ell < 150$ and confirm that this is not due to systematics using jackknife tests and simulations based on detailed calibration measurements. Read More

2014Mar
Affiliations: 1Cardiff University, 2Caltech, 3ALMA, 4ALMA, 5University of Toronto, 6Harvard/CfA, 7Caltech, 8Caltech, 9Harvard/CfA, 10Minnesota Institute for Astrophysics, 11NASA JPL, 12NASA JPL, 13SBT Grenoble, 14Caltech, 15University of Minnesota, 16Caltech, 17Caltech, 18Caltech, 19Caltech, 20NIST, 21Caltech, 22Stanford University, 23Harvard/CfA, 24UCSD, 25UCSD, 26Stanford University, 27Harvard/CfA, 28Stanford University, 29University of Chicago, 30NASA JPL, 31Caltech, 32University of Toronto, 33NASA JPL, 34NASA JPL, 35Stanford University, 36UCSD, 37University of Minnesota, 38NIST, 39Harvard/CfA, 40University of Minnesota, 41University of Minnesota, 42Caltech, 43University of Chicago, 44Cardiff University, 45Caltech, 46Stanford University, 47NASA JPL, 48Harvard/CfA, 49NASA JPL, 50Harvard/CfA, 51Stanford University

We report on the design and performance of the BICEP2 instrument and on its three-year data set. BICEP2 was designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 1 to 5 degrees ($\ell$=40-200), near the expected peak of the B-mode polarization signature of primordial gravitational waves from cosmic inflation. Measuring B-modes requires dramatic improvements in sensitivity combined with exquisite control of systematics. Read More

2014Mar
Affiliations: 1Cardiff University, 2Caltech, 3ALMA, 4University of Toronto, 5Harvard/CfA, 6Caltech, 7Caltech, 8Harvard/CfA, 9Minnesota Institute for Astrophysics, 10NASA JPL, 11SBT Grenoble, 12Caltech, 13University of Minnesota, 14Caltech, 15University of British Columbia, 16University of British Columbia, 17Caltech, 18NIST, 19Caltech, 20Stanford University, 21Harvard/CfA, 22UCSD, 23UCSD, 24Stanford University, 25Harvard/CfA, 26Stanford University, 27University of Chicago, 28Caltech, 29Caltech, 30University of Toronto, 31NASA JPL, 32NASA JPL, 33Stanford University, 34UCSD, 35University of Minnesota, 36NIST, 37Harvard/CfA, 38University of Minnesota, 39University of Minnesota, 40Caltech, 41Cardiff University, 42Caltech, 43Stanford University, 44NASA JPL, 45Harvard/CfA, 46Harvard/CfA, 47Stanford University

(abridged for arXiv) 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 $\ell\sim80$. 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 $\approx300\mu\mathrm{K}_\mathrm{CMB}\sqrt{s}$. BICEP2 observed from the South Pole for three seasons from 2010 to 2012. Read More

Cosmic Microwave Background (CMB) polarimeters aspire to measure the faint $B$-mode signature predicted to arise from inflationary gravitational waves. They also have the potential to constrain cosmic birefringence which would produce non-zero expectation values for the CMB's $TB$ and $EB$ spectra. However, instrumental systematic effects can also cause these $TB$ and $EB$ correlations to be non-zero. Read More

The old, red stars which 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 from accretion onto black holes. It is widely suspected, but unproven, that the tight correlation in mass of the black hole and stellar components results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, while powerful star-forming galaxies are usually dust-obscured and are brightest at infrared to submillimetre wavelengths. Read More

BICEP1 is a millimeter-wavelength telescope designed specifically to measure the inflationary B-mode polarization of the Cosmic Microwave Background (CMB) at degree angular scales. We present results from an analysis of the data acquired during three seasons of observations at the South Pole (2006 to 2008). This work extends the two-year result published in Chiang et al. Read More

A set of six debris disk candidates identified with IRAS or WISE excesses were observed at either 350 um or 450 um with the CSO. Five of the targets - HIP 51658, HIP 68160, HIP 73512, HIP 76375, and HIP 112460 - have among the largest measured excess emission from cold dust from IRAS in the 25-100 um bands. Single temperature blackbody fits to the excess dust emission of these sources predict 350-450 um fluxes above 240 mJy. Read More

Photometric instruments operating at far infrared to millimetre wavelengths often have broad spectral passbands (central wavelength/bandwidth ~ 3 or less), especially those operating in space. A broad passband can result in significant variation of the beam profile and aperture efficiency across the passband, effects which thus far have not generally been taken into account in the flux calibration of such instruments. With absolute calibration uncertainties associated with the brightness of primary calibration standards now in the region of 5% or less, variation of the beam properties across the passband can be a significant contributor to the overall calibration accuracy for extended emission. Read More

We describe the procedure used to flux calibrate the three-band submillimetre photometer in the Spectral and Photometric Imaging REceiver (SPIRE) instrument on the Herschel Space Observatory. This includes the equations describing the calibration scheme, a justification for using Neptune as the primary calibration source, a description of the observations and data processing procedures used to derive flux calibration parameters (for converting from voltage to flux density) for every bolometer in each array, an analysis of the error budget in the flux calibration for the individual bolometers, and tests of the flux calibration on observations of primary and secondary calibrators. The procedure for deriving the flux calibration parameters is divided into two parts. Read More

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 halos at early epochs. However, it remains unknown how soon after the Big Bang such massive starburst progenitors exist. The measured redshift distribution of dusty, massive starbursts has long been suspected to be biased low in redshift owing to selection effects, as confirmed by recent findings of systems out to redshift z~5. Read More

We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after subtracting sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. Read More

We exploit the deep and extended far infrared data sets (at 70, 100 and 160 um) of the Herschel GTO PACS Evolutionary Probe (PEP) Survey, in combination with the HERschel Multi tiered Extragalactic Survey (HerMES) data at 250, 350 and 500 um, to derive the evolution of the restframe 35 um, 60 um, 90 um, and total infrared (IR) luminosity functions (LFs) up to z~4. We detect very strong luminosity evolution for the total IR LF combined with a density evolution. In agreement with previous findings, the IR luminosity density increases steeply to z~1, then flattens between z~1 and z~3 to decrease at z greater than 3. Read More

The design and performance of a wide bandwidth linear polarization modulator based on the Faraday effect is described. Faraday Rotation Modulators (FRMs) are solid-state polarization switches that are capable of modulation up to ~10 kHz. Six FRMs were utilized during the 2006 observing season in the Background Imaging of Cosmic Extragalactic Polarization (BICEP) experiment; three FRMs were used at each of BICEP's 100 and 150 GHz frequency bands. Read More

Submillimeter cameras now have up to $10^4$ pixels (SCUBA 2). The proposed CCAT 25-meter submillimeter telescope will feature a 1 degree field-of-view. Populating the focal plane at 350 microns would require more than $10^6$ photon-noise limited pixels. Read More

We present measurements of the auto- and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500um (1200, 860, and 600 GHz) from observations totaling ~ 70 deg^2 made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy dI / I = 14 +- 4%, detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear (2-halo) and non-linear (1-halo) regimes; and that the transition from the 2- to 1-halo terms, below which power originates predominantly from multiple galaxies within dark matter halos, occurs at k_theta ~ 0.1 - 0. Read More

Between the BICEP2 and Keck Array experiments, we have deployed over 1500 dual polarized antenna coupled bolometers to map the Cosmic Microwave Background's polarization. We have been able to rapidly deploy these detectors because they are completely planar with an integrated phased-array antenna. Through our experience in these experiments, we have learned of several challenges with this technology- specifically the beam synthesis in the antenna- and in this paper we report on how we have modified our designs to mitigate these challenges. Read More

The Keck Array (SPUD) is a set of microwave polarimeters that observes from the South Pole at degree angular scales in search of a signature of Inflation imprinted as B-mode polarization in the Cosmic Microwave Background (CMB). The first three Keck Array receivers were deployed during the 2010-2011 Austral summer, followed by two new receivers in the 2011-2012 summer season, completing the full five-receiver array. All five receivers are currently observing at 150 GHz. Read More

The Keck Array (SPUD) began observing the cosmic microwave background's polarization in the winter of 2011 at the South Pole. The Keck Array follows the success of the predecessor experiments Bicep and Bicep2, using five on-axis refracting telescopes. These have a combined imaging array of 2500 antenna-coupled TES bolometers read with a SQUID-based time domain multiplexing system. Read More

The BICEP2 and Keck Array experiments are designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 2-4 degrees (l=50-100). This is the region in which the B-mode signal, a signature prediction of cosmic inflation, is expected to peak. BICEP2 was deployed to the South Pole at the end of 2009 and is in the middle of its third year of observing with 500 polarization-sensitive detectors at 150 GHz. Read More

We present a list of 13 candidate gravitationally lensed submillimeter galaxies (SMGs) from 95 square degrees of the Herschel Multi-tiered Extragalactic Survey, a surface density of 0.14\pm0.04deg^{-2}. Read More

We measured polarized dust emission at 350um towards the high-mass star forming massive dense clump IRAS 20126+4104 using the SHARC II Polarimeter, SHARP, at the Caltech Submillimeter Observatory. Most of the observed magnetic field vectors agree well with magnetic field vectors obtained from a numerical simulation for the case when the global magnetic field lines are inclined with respect to the rotation axis of the dense clump. The results of the numerical simulation show that rotation plays an important role on the evolution of the massive dense clump and its magnetic field. Read More

2012Mar
Authors: HerMES Collaboration, S. J. Oliver1, J. Bock2, B. Altieri3, A. Amblard4, V. Arumugam5, H. Aussel6, T. Babbedge7, A. Beelen8, M. Béthermin9, A. Blain10, A. Boselli11, C. Bridge12, D. Brisbin13, V. Buat14, D. Burgarella15, N. Castro-Rodríguez16, A. Cava17, P. Chanial18, M. Cirasuolo19, D. L. Clements20, A. Conley21, L. Conversi22, A. Cooray23, C. D. Dowell24, E. N. Dubois25, E. Dwek26, S. Dye27, S. Eales28, D. Elbaz29, D. Farrah30, A. Feltre31, P. Ferrero32, N. Fiolet33, M. Fox34, A. Franceschini35, W. Gear36, E. Giovannoli37, J. Glenn38, Y. Gong39, E. A. González Solares40, M. Griffin41, M. Halpern42, M. Harwit43, E. Hatziminaoglou44, S. Heinis45, P. Hurley46, H. S. Hwang47, A. Hyde48, E. Ibar49, O. Ilbert50, K. Isaak51, R. J. Ivison52, G. Lagache53, E. Le Floc'h54, L. Levenson55, B. Lo Faro56, N. Lu57, S. Madden58, B. Maffei59, G. Magdis60, G. Mainetti61, L. Marchetti62, G. Marsden63, J. Marshall64, A. M. J. Mortier65, H. T. Nguyen66, B. O'Halloran67, A. Omont68, M. J. Page69, P. Panuzzo70, A. Papageorgiou71, H. Patel72, C. P. Pearson73, I. Pérez-Fournon74, M. Pohlen75, J. I. Rawlings76, G. Raymond77, D. Rigopoulou78, L. Riguccini79, D. Rizzo80, G. Rodighiero81, I. G. Roseboom82, M. Rowan-Robinson83, M. Sánchez Portal84, B. Schulz85, Douglas Scott86, N. Seymour87, D. L. Shupe88, A. J. Smith89, J. A. Stevens90, M. Symeonidis91, M. Trichas92, K. E. Tugwell93, M. Vaccari94, I. Valtchanov95, J. D. Vieira96, M. Viero97, L. Vigroux98, L. Wang99, R. Ward100, J. Wardlow101, G. Wright102, C. K. Xu103, M. Zemcov104
Affiliations: 1Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 2California Institute of Technology, Pasadena, CA, USA, 3Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, Madrid, Spain, 4NASA, Ames Research Center, Moffett Field, CA, USA, 5Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, UK, 6Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 7Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 8Institut d'Astrophysique Spatiale, 9Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 10California Institute of Technology, Pasadena, CA, USA, 11Laboratoire d'Astrophysique de Marseille, OAMP, Université Aix-marseille, Marseille, France, 12California Institute of Technology, Pasadena, CA, USA, 13Department of Astronomy, Space Science Building, Cornell University, Ithaca, NY, USA, 14Laboratoire d'Astrophysique de Marseille, OAMP, Université Aix-marseille, Marseille, France, 15Laboratoire d'Astrophysique de Marseille, OAMP, Université Aix-marseille, Marseille, France, 16Instituto de Astrofísica de Canarias, 17Departamento de Astrofísica, Facultad de CC. Físicas, Universidad Complutense de Madrid, Madrid, Spain, 18Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 19UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, UK, 20Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 21Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO, USA, 22Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, Madrid, Spain, 23Dept. of Physics and Astronomy, University of California, Irvine, CA, USA, 24California Institute of Technology, Pasadena, CA, USA, 25Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 26Observational Cosmology Lab, NASA Goddard Space Flight Center, Greenbelt, MD, USA, 27School of Physics and Astronomy, University of Nottingham, UK, 28School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, fCardif, UK, 29Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 30Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 31Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, Padova, Italy, 32Instituto de Astrofísica de Canarias, 33Institut d'Astrophysique de Paris, Univ. Paris, Paris, France, 34Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 35Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, Padova, Italy, 36School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, fCardif, UK, 37Laboratoire d'Astrophysique de Marseille, OAMP, Université Aix-marseille, Marseille, France, 38Dept. of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO, USA, 39Dept. of Physics and Astronomy, University of California, Irvine, CA, USA, 40Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, UK, 41School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, fCardif, UK, 42Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, Canada, 43Washington, DC, USA, 44ESO, München, Germany, 45Laboratoire d'Astrophysique de Marseille, OAMP, Université Aix-marseille, Marseille, France, 46Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 47Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 48Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 49UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, UK, 50Laboratoire d'Astrophysique de Marseille, OAMP, Université Aix-marseille, Marseille, France, 51ESA Research and Scientific Support Department, ESTEC/SRE-SA, AZ Noordwijk, The Netherlands, 52UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, UK, 53Institut d'Astrophysique Spatiale, 54Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 55California Institute of Technology, Pasadena, CA, USA, 56Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, Padova, Italy, 57California Institute of Technology, Pasadena, CA, USA, 58Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 59School of Physics and Astronomy, The University of Manchester, Alan Turing Building, Manchester, UK, 60Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 61Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, Padova, Italy, 62Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, Padova, Italy, 63Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, Canada, 64California Institute of Technology, Pasadena, CA, USA, 65Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 66Jet Propulsion Laboratory, Pasadena, CA, USA, 67Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 68Institut d'Astrophysique de Paris, Univ. Paris, Paris, France, 69Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, UK, 70Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 71School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, fCardif, UK, 72Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 73RAL Space, Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire, UK, 74Instituto de Astrofísica de Canarias, 75School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, fCardif, UK, 76Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, UK, 77School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, fCardif, UK, 78RAL Space, Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire, UK, 79Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, Gif-sur-Yvette, France, 80Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 81Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, Padova, Italy, 82Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 83Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London, UK, 84Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, Madrid, Spain, 85California Institute of Technology, Pasadena, CA, USA, 86Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, Canada, 87CSIRO Astronomy and Space Science, Epping, NSW, Australia, 88California Institute of Technology, Pasadena, CA, USA, 89Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 90Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Hertfordshire, UK, 91Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, UK, 92Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA, 93Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey, UK, 94Dipartimento di Astronomia, Università di Padova, vicolo Osservatorio, Padova, Italy, 95Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, Madrid, Spain, 96California Institute of Technology, Pasadena, CA, USA, 97California Institute of Technology, Pasadena, CA, USA, 98Institut d'Astrophysique de Paris, Univ. Paris, Paris, France, 99Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 100Astronomy Centre, Dept. of Physics and Astronomy, University of Sussex, Brighton, UK, 101Dept. of Physics and Astronomy, University of California, Irvine, CA, USA, 102UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, UK, 103California Institute of Technology, Pasadena, CA, USA, 104California Institute of Technology, Pasadena, CA, USA

The Herschel Multi-tiered Extragalactic Survey, HerMES, is a legacy program designed to map a set of nested fields totalling ~380 deg^2. Fields range in size from 0.01 to ~20 deg^2, using Herschel-SPIRE (at 250, 350 and 500 \mu m), and Herschel-PACS (at 100 and 160 \mu m), with an additional wider component of 270 deg^2 with SPIRE alone. Read More

ABRIGED Herschel/SPIRE has provided confusion limited maps of deep fields at 250, 350, and 500um, as part of the HerMES survey. Due to confusion, only a small fraction of the Cosmic Infrared Background can be resolved into individually-detected sources. Our goal is to produce deep galaxy number counts and redshift distributions below the confusion limit, which we then use to place strong constraints on the origins of the cosmic infrared background and on models of galaxy evolution. Read More

We describe the generation of single-band point source catalogues from submillimetre Herschel-SPIRE observations taken as part of the Science Demonstration Phase of the Herschel Multi-tiered Extragalactic Survey (HerMES). Flux densities are found by means of peak-finding and the fitting of a Gaussian point-response function. With highly-confused images, careful checks must be made on the completeness and flux density accuracy of the detected sources. Read More

We investigate the potential of submm-mm and submm-mm-radio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500 {\mu}m by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm-sources with reliable radio identifications in the GOODS-N and Lockman Hole North fields 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm-sources are adequately described by a modified blackbody with constant optical depth {\tau} = ({\nu}/{\nu}0)^{\beta} where {\beta} = +1. Read More

Dynamical interactions between planets and debris disks may sculpt the disk structure and impact planetary orbits, but only a few systems with both imaged planets and spatially resolved debris disks are known. With the Caltech Submm Observatory (CSO), we have observed the HR 8799 debris disk at 350{\mu}m. The 350{\mu}m map is the first spatially resolved measurement of the debris disk encircling the HR 8799 planetary system at this wavelength. Read More

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. Read More

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. Read More

In addition to its potential to probe the Inflationary cosmological paradigm, millimeter-wave polarimetry is a powerful tool for studying the Milky Way galaxy's composition and magnetic field structure. Towards this end, presented here are Stokes I, Q, and U maps of the Galactic plane from the millimeter-wave polarimeter BICEP covering the Galactic longitude range 260 - 340 degrees in three atmospheric transmission windows centered on 100, 150, and 220 GHz. The maps sample an optical depth 1 < AV < 30, and are consistent with previous characterizations of the Galactic millimeter-wave frequency spectrum and the large-scale magnetic field structure permeating the interstellar medium. Read More

The extragalactic background light at far-infrared wavelengths originates from optically-faint, dusty, star-forming galaxies in the universe with star-formation rates at the level of a few hundred solar masses per year. Due to the relatively poor spatial resolution of far-infrared telescopes, the faint sub-millimetre galaxies are challenging to study individually. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations. Read More

We investigate the effect of the Milky Way's magnetic field in star forming regions using archived 350 micron polarization data on 52 Galactic star formation regions from the Hertz polarimeter module. The polarization angles and percentages for individual telescope beams were combined in order to produce a large-scale average for each source and for complexes of sources. In more than 80% of the sources, we find a meaningful mean magnetic field direction, implying the existence of an ordered magnetic field component at the scale of these sources. Read More

We have investigated the nature of flare emission from Sgr A* during multi-wavelength observations of this source that took place in 2004, 2005 and 2006. We present evidence for dimming of submm and radio flux during the peak of near-IR flares. This suggests that the variability of Sgr A* across its wavelength spectrum is phenomenologically related. Read More

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. Read More

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. Read More

2010Sep
Affiliations: 1and 17 others, 2and 17 others, 3and 17 others, 4and 17 others, 5and 17 others, 6and 17 others, 7and 17 others, 8and 17 others, 9and 17 others, 10and 17 others, 11and 17 others, 12and 17 others, 13and 17 others, 14and 17 others, 15and 17 others, 16and 17 others, 17and 17 others, 18and 17 others, 19and 17 others, 20and 17 others, 21and 17 others, 22and 17 others, 23and 17 others, 24and 17 others, 25and 17 others, 26and 17 others, 27and 17 others, 28and 17 others, 29and 17 others, 30and 17 others, 31and 17 others, 32and 17 others, 33and 17 others, 34and 17 others, 35and 17 others, 36and 17 others, 37and 17 others, 38and 17 others, 39and 17 others, 40and 17 others, 41and 17 others, 42and 17 others, 43and 17 others, 44and 17 others, 45and 17 others, 46and 17 others, 47and 17 others, 48and 17 others, 49and 17 others, 50and 17 others

We present first results of a study of the submillimetre (rest frame far-infrared) properties of z~3 Lyman Break Galaxies (LBGs) and their lower-redshift counterparts BX/BM galaxies, based on Herschel-SPIRE observations of the Northern field of the Great Observatories Origins Deep Survey (GOODS-N). We use stacking analysis to determine the properties of LBGs well below the current limit of the survey. Although LBGs are not detected individually, stacking the infrared luminous LBGs (those detected with Spitzer at 24 microns yields a statistically significant submm detection with mean flux = 5. Read More

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. Read More

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. Read More